FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Martens, B
Lievens, H
Colliander, A
Jackson, TJ
Verhoest, NEC
AF Martens, Brecht
Lievens, Hans
Colliander, Andreas
Jackson, Thomas J.
Verhoest, Niko E. C.
TI Estimating Effective Roughness Parameters of the L-MEB Model for Soil
Moisture Retrieval Using Passive Microwave Observations From SMAPVEX12
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Passive Active L-band Sensor (PALS); passive microwave remote sensing;
roughness modeling; soil moisture
ID L-BAND RADIOMETER; DISCHARGE PREDICTIONS; SURFACE-ROUGHNESS; OCEAN
SALINITY; SIMPLEX-METHOD; CROP FIELDS; CALIBRATION; EMISSION; RADAR;
SCALE
AB Despite the continuing efforts to improve existing soil moisture retrieval algorithms, the ability to estimate soil moisture from passive microwave observations is still hampered by problems in accurately modeling the observed microwave signal. This paper focuses on the estimation of effective surface roughness parameters of the L-band Microwave Emission from the Biosphere (L-MEB) model in order to improve soil moisture retrievals from passive microwave observations. Data from the SMAP Validation Experiment 2012 conducted in Canada are used to develop and validate a simple model for the estimation of effective roughness parameters. Results show that the L-MEB roughness parameters can be empirically related to the observed brightness temperatures and the leaf area index of the vegetation. These results indicate that the roughness parameters are compensating for both roughness and vegetation effects. It is also shown, using a leave-one-out cross validation, that the model is able to accurately estimate the roughness parameters necessary for the inversion of the L-MEB model. In order to demonstrate the usefulness of the roughness parameterization, the performance of the model is compared to more traditional roughness formulations. Results indicate that the soil moisture retrieval error can be reduced to 0.054 m(3)/m(3) if the roughness formulation proposed in this study is implemented in the soil moisture retrieval algorithm.
C1 [Martens, Brecht; Lievens, Hans; Verhoest, Niko E. C.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Martens, B (reprint author), Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
EM Brecht.Martens@ugent.be
RI Verhoest, Niko/C-9726-2010;
OI Verhoest, Niko/0000-0003-4116-8881; Martens, Brecht/0000-0002-7368-7953
FU National Aeronautics and Space Administration
FX The authors would like to thank the SMAPVEX12 investigators for making
the data of the campaigns publicly available to the scientific community
and the anonymous reviewers for their significant contribution to this
paper. The second author is a Postdoctoral Research Fellow with the
Research Foundation Flanders (FWO). Part of the work 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 49
TC 5
Z9 6
U1 4
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 JUL
PY 2015
VL 53
IS 7
BP 4091
EP 4103
DI 10.1109/TGRS.2015.2390259
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 CD9ZO
UT WOS:000351461000042
ER
PT J
AU Wallace, JK
Rider, S
Serabyn, E
Kuhn, J
Liewer, K
Deming, J
Showalter, G
Lindensmith, C
Nadeau, J
AF Wallace, J. Kent
Rider, Stephanie
Serabyn, Eugene
Kuehn, Jonas
Liewer, Kurt
Deming, Jody
Showalter, Gordon
Lindensmith, Chris
Nadeau, Jay
TI Robust, compact implementation of an off-axis digital holographic
microscope
SO OPTICS EXPRESS
LA English
DT Article
ID PHASE-CONTRAST MICROSCOPY; NUMERICAL RECONSTRUCTION; TUMOR-CELLS;
RESOLUTION; ALGORITHM; MOTILITY; BEHAVIOR
AB Recent advances in digital technologies, such as high-speed computers and large-format digital imagers, have led to a burgeoning interest in the science and engineering of digital holographic microscopy (DHM). Here we report on a novel off-axis DHM, based on a twin-beam optical design, which avoids the limitations of prior systems, and provides many advantages, including compactness, intrinsic stability, robustness against misalignment, ease of use, and cost. These advantages are traded for a physically constrained sample volume, as well as a fixed fringe spacing. The first trade is not overly restrictive for most applications, and the latter provides for a pre-set assembly alignment that optimizes the spatial frequency sampling. Moreover, our new design supports use in both routine laboratory settings as well as extreme environments without any sacrifice in performance, enabling ready observation of microbial species in the field. The instrument design is presented in detail here, along with a demonstration of bacterial video imaging at sub-micrometer resolution at temperatures down to -15 degrees C. (C) 2015 Optical Society of America
C1 [Wallace, J. Kent; Serabyn, Eugene; Kuehn, Jonas; Liewer, Kurt; Lindensmith, Chris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rider, Stephanie; Nadeau, Jay] CALTECH, Div Aerosp Engn, Pasadena, CA 91125 USA.
[Showalter, Gordon] Univ Washington, Dept Biol Oceanog, Seattle, WA 98105 USA.
[Nadeau, Jay] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada.
RP Wallace, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.k.wallace@jpl.nasa.gov
FU Gordon and Betty Moore Foundation [4037, 4038]
FX This work was funded by the Gordon and Betty Moore Foundation through
grants 4037 to McGill University and 4038 to the California Institute of
Technology. We also thank the Keck Institute for Space Studies for
allowing us use of the Tolman/Bacher House, which served as a meeting
location for our team on the Caltech campus. We appreciate the
contribution of Asphericon, Inc. for fabricating customized optical
elements to meet the packaging needs. This work was partially carried
out by the Jet Propulsion Laboratory, California Institute of
Technology.
NR 31
TC 6
Z9 6
U1 1
U2 10
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JUN 29
PY 2015
VL 23
IS 13
BP 17367
EP 17378
DI 10.1364/OE.23.017367
PG 12
WC Optics
SC Optics
GA CN6KI
UT WOS:000358543300086
PM 26191746
ER
PT J
AU Ingersoll, MA
Lyons, AS
Muniyan, S
D'Cunha, N
Robinson, T
Hoelting, K
Dwyer, JG
Bu, XR
Batra, SK
Lin, MF
AF Ingersoll, Matthew A.
Lyons, Anastesia S.
Muniyan, Sakthivel
D'Cunha, Napoleon
Robinson, Tashika
Hoelting, Kyle
Dwyer, Jennifer G.
Bu, Xiu R.
Batra, Surinder K.
Lin, Ming-Fong
TI Novel Imidazopyridine Derivatives Possess Anti-Tumor Effect on Human
Castration-Resistant Prostate Cancer Cells
SO PLOS ONE
LA English
DT Article
ID PHOSPHATIDYLINOSITOL 3-KINASE INHIBITOR; ANDROGEN RECEPTOR;
ACID-PHOSPHATASE; IN-VIVO; TYROSINE-PHOSPHATASE; INCREASED SURVIVAL;
P66(SHC) PROTEIN; GROWTH; EXPRESSION; APOPTOSIS
AB Prostate cancer (PCa) is the second leading cause of cancer-related death afflicting United States males. Most treatments to-date for metastatic PCa include androgen-deprivation therapy and second-generation anti-androgens such as abiraterone acetate and enzalutamide. However, a majority of patients eventually develop resistance to these therapies and relapse into the lethal, castration-resistant form of PCa to which no adequate treatment option remains. Hence, there is an immediate need to develop effective therapeutic agents toward this patient population. Imidazopyridines have recently been shown to possess Akt kinase inhibitory activity; thus in this study, we investigated the inhibitory effect of novel imidazopyridine derivatives HIMP, M-Mel, OMP, and EtOP on different human castration-resistant PCa cells. Among these compounds, HIMP and M-MeI were found to possess selective dose-and time-dependent growth inhibition: they reduced castration-resistant PCa cell proliferation and spared benign prostate epithelial cells. Using LNCaP C-81 cells as the model system, these compounds also reduced colony formation as well as cell adhesion and migration, and M-MeI was the most potent in all studies. Further investigation revealed that while HIMP primarily inhibits PCa cell growth via suppression of PI3K/Akt signaling pathway, M-MeI can inhibit both PI3K/Akt and androgen receptor pathways and arrest cell growth in the G2 phase. Thus, our results indicate the novel compound M-MeI to be a promising candidate for castration-resistant PCa therapy, and future studies investigating the mechanism of imidazopyridine inhibition may aid to the development of effective anti-PCa agents.
C1 [Ingersoll, Matthew A.; Muniyan, Sakthivel; Dwyer, Jennifer G.; Batra, Surinder K.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Dept Biochem & Mol Biol, Omaha, NE USA.
[Lyons, Anastesia S.; D'Cunha, Napoleon; Bu, Xiu R.] Clark Atlanta Univ, Dept Chem, Atlanta, GA 30314 USA.
[Robinson, Tashika] Clark Atlanta Univ, Dept Biol Sci, Atlanta, GA 30314 USA.
[Hoelting, Kyle] Univ Nebraska Med Ctr, Coll Pharm, Omaha, NE USA.
[Dwyer, Jennifer G.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Urol Sect, Dept Surg, Omaha, NE USA.
[Bu, Xiu R.] Clark Atlanta Univ, Lab Electopt Mat, Atlanta, GA USA.
[Bu, Xiu R.] Clark Atlanta Univ, NASA, Ctr High Performance Polymers & Composites, Atlanta, GA USA.
[Batra, Surinder K.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Eppley Inst Res Canc & Allied Dis, Omaha, NE USA.
[Lin, Ming-Fong] Kaohsiung Med Univ, Coll Pharm, Kaohsiung 807, Taiwan.
RP Bu, XR (reprint author), Clark Atlanta Univ, Dept Chem, Atlanta, GA 30314 USA.
EM JBu@cau.edu; mlin@unmc.edu
OI Muniyan, Sakthivel/0000-0001-9405-7857
FU National Cancer Institute, National Institutes of Health [CA88184,
CA138791]; Department of Defense PCa Training Grants [PC094594,
PC121645]; University of Nebraska Medical Center Bridge Fund; UNMC
Eppley Cancer Center grant [CA036727]
FX This work was supported in part by the National Cancer Institute,
National Institutes of Health [CA88184 (MFL), CA138791 (SKB)],
Department of Defense PCa Training Grants [PC094594 (MFL), PC121645
(MFL)], and the University of Nebraska Medical Center Bridge Fund (MFL).
The cell cycle analysis was performed at the UNMC Flow Cytometry Core
Facility in part supported by UNMC Eppley Cancer Center grant [CA036727]
(Ken Cowan). The funders had no role in study design, data collection
and analysis, decision to publish, or preparation of the manuscript.
NR 54
TC 1
Z9 2
U1 1
U2 2
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUN 29
PY 2015
VL 10
IS 6
AR e0131811
DI 10.1371/journal.pone.0131811
PG 20
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CN1BL
UT WOS:000358150400159
PM 26121643
ER
PT J
AU Restano, M
Plaut, JJ
Campbell, BA
Gim, Y
Nunes, D
Bernardini, F
Egan, A
Seu, R
Phillips, RJ
AF Restano, Marco
Plaut, Jeffrey J.
Campbell, Bruce A.
Gim, Yonggyu
Nunes, Daniel
Bernardini, Fabrizio
Egan, Anthony
Seu, Roberto
Phillips, Roger J.
TI Effects of the passage of Comet C/2013 A1 (Siding Spring) observed by
the Shallow Radar (SHARAD) on Mars Reconnaissance Orbiter
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Comet Siding Spring; SHARAD
ID IONS
AB The close passage of Comet C/2013 A1 (Siding Spring) to Mars provided a unique opportunity to observe the interaction of cometary materials with the Martian ionosphere and atmosphere using the sounding radar SHARAD (SHAllow RADar) aboard Mars Reconnaissance Orbiter. In two nightside observations, acquired in the 10h following the closest approach, the SHARAD data reveal a significant increase of the total electron content (TEC). The observed TEC values are typical for daylight hours just after dawn or before sunset but are unprecedented this deep into the night. Results support two predictions indicating that cometary pickup O+ ions, or ions generated from the ablation of cometary dust, are responsible for the creation of an additional ion layer.
C1 [Restano, Marco; Bernardini, Fabrizio; Seu, Roberto] Univ Roma La Sapienza, Dipartimento DIET, I-00185 Rome, Italy.
[Plaut, Jeffrey J.; Gim, Yonggyu; Nunes, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Campbell, Bruce A.] Smithsonian Inst, Washington, DC 20560 USA.
[Egan, Anthony] Southwest Res Inst, Space Operat Dept, Boulder, CO USA.
[Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO USA.
RP Restano, M (reprint author), Univ Roma La Sapienza, Dipartimento DIET, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
EM marco.res@inwind.it
FU ASI
FX The Shallow Subsurface Radar (SHARAD) was provided by the Italian Space
Agency (ASI), and its operations are led by the DIET Department,
University of Rome "La Sapienza" under an ASI science contract. The Mars
Reconnaissance Orbiter mission is managed by the Jet Propulsion
Laboratory, California Institute of Technology, for the NASA Science
Mission Directorate, Washington, DC. SHARAD data become available on the
Geosciences Node of NASA's Planetary Data System
(http://pds-geosciences.wustl.edu/) 6 months after the collection of the
observations.
NR 22
TC 9
Z9 9
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4663
EP 4669
DI 10.1002/2015GL064150
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500001
ER
PT J
AU Benna, M
Mahaffy, PR
Grebowsky, JM
Plane, JMC
Yelle, RV
Jakosky, BM
AF Benna, M.
Mahaffy, P. R.
Grebowsky, J. M.
Plane, J. M. C.
Yelle, R. V.
Jakosky, B. M.
TI Metallic ions in the upper atmosphere of Mars from the passage of comet
C/2013 A1 (Siding Spring)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Comet Siding Spring; Mars; atmosphere; metal ion
ID IONOSPHERE; DUST
AB We report the first in situ detection of metal ions in the upper atmosphere of Mars resulting from the ablation of dust particles from comet Siding Spring. This detection was carried out by the Neutral Gas and Ion Mass Spectrometer on board the Mars Atmosphere and Volatile Evolution Mission. Metal ions of Na, Mg, Al, K, Ti, Cr, Mn, Fe, Co, Ni, Cu, and Zn, and possibly of Si, and Ca, were identified in the ion spectra collected at altitudes of similar to 185km. The measurements revealed that Na+ was the most abundant species, and that the remaining metals were depleted with respect to the CI (type 1 carbonaceous Chondrites) abundance of Na+. The temporal profile and abundance ratios of these metal ions suggest that the combined effects of dust composition, partial ablation, differential upward transport, and differences in the rates of formation and removal of these metal ions are responsible for the observed depletion.
C1 [Benna, M.; Mahaffy, P. R.; Grebowsky, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Benna, M.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21228 USA.
[Plane, J. M. C.] Univ Leeds, Fac Math & Phys Sci, Leeds, W Yorkshire, England.
[Yelle, R. V.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Jakosky, B. M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Benna, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mehdi.benna@nasa.gov
RI Plane, John/C-7444-2015; Benna, Mehdi/F-3489-2012
OI Plane, John/0000-0003-3648-6893;
FU NASA; European Research Council [291332-CODITA]
FX The MAVEN/NGIMS investigation was supported by NASA. Instrument testing
and calibrations were completed at the Planetary Environment laboratory
of NASA's Goddard Space Flight Center. We are grateful for the
engineering/technical support especially from T. King (Instrument
Manager), E. Weidner, E. Lyness, K. Patel, (Instrument Operations), and
E. Raaen and M. Elrod (Calibration). J.M.C.P. acknowledges funding from
the European Research Council (project 291332-CODITA). The NGIMS data
supporting this article are provided in the supporting information
Dataset S1.
NR 30
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Z9 15
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4670
EP 4675
DI 10.1002/2015GL064159
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500002
ER
PT J
AU Samsonov, AA
Sergeev, VA
Kuznetsova, MM
Sibeck, DG
AF Samsonov, A. A.
Sergeev, V. A.
Kuznetsova, M. M.
Sibeck, D. G.
TI Asymmetric magnetospheric compressions and expansions in response to
impact of inclined interplanetary shock
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE inclined interplanetary shocks; sudden impulse; asymmetric magnetopause
motion
ID GEOMAGNETIC SUDDEN COMMENCEMENT; WIND; PROPAGATION; MOTION; MODEL
AB We use global MHD simulations to model the magnetospheric response to an inclined shock that first strikes the duskside magnetosphere. The simulations predict several phenomena related specifically to the inclined shocks. The magnetospheric compression on the duskside exceeds that on the dawnside, and the geocentric distance to the dusk magnetopause varies in a simple step-like form. The compression on the dawnside is preceded and followed by expansions. For a moderately strong shock, the expansion magnitude reaches several R-E behind the terminator plane. The magnetopause and cross-tail currents in the magnetotail are significantly deformed during and after the shock passage. The position of the magnetotail magnetopause moves by more than 10R(E). This asymmetric magnetopause deformation is mainly related to a strong |V-y| downstream from the inclined shock. The magnetospheric expansion results in a decrease in the horizontal magnetic field at low-latitude stations, as confirmed by observations.
C1 [Samsonov, A. A.; Sergeev, V. A.] St Petersburg State Univ, St Petersburg 199034, Russia.
[Kuznetsova, M. M.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Samsonov, AA (reprint author), St Petersburg State Univ, St Petersburg 199034, Russia.
EM andre.samsonov@gmail.com
RI Samsonov, Andrey/I-7057-2012
OI Samsonov, Andrey/0000-0001-8243-1151
FU Russian Science Foundation [14-17-00072]
FX Simulation results have been provided by the Community Coordinated
Modeling Center (http://ccmc.gsfc.nasa.gov) at Goddard Space Flight
Center. We have used results of the runs Andrey_Samsonov_041714_1,
Andrey_Samsonov_020515_1, Andrey_Samsonov_030315_1, and
Andrey_Samsonov_030315_1a. The SWMF was developed at the University of
Michigan. Wind data are available from the Coordinated Data Analysis Web
(CDAWeb). Ground magnetometer data are available from the World Data
Center for Geomagnetism at Kyoto (http://wdc.kugi.kyoto-u.ac.jp/). This
work was supported by the Russian Science Foundation grant 14-17-00072.
A.A.S. thanks Gabor Toth for valuable comments.
NR 27
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U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4716
EP 4722
DI 10.1002/2015GL064294
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500008
ER
PT J
AU Meng, X
Komjathy, A
Verkhoglyadova, OP
Yang, YM
Deng, Y
Mannucci, AJ
AF Meng, X.
Komjathy, A.
Verkhoglyadova, O. P.
Yang, Y. -M.
Deng, Y.
Mannucci, A. J.
TI A new physics-based modeling approach for tsunami-ionosphere coupling
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE traveling ionospheric disturbance; ionospheric modeling; gravity wave;
tsunami
ID INTERNAL GRAVITY-WAVES; ATMOSPHERE; THERMOSPHERE
AB Tsunamis can generate gravity waves propagating upward through the atmosphere, inducing total electron content (TEC) disturbances in the ionosphere. To capture this process, we have implemented tsunami-generated gravity waves into the Global Ionosphere-Thermosphere Model (GITM) to construct a three-dimensional physics-based model WP (Wave Perturbation)-GITM. WP-GITM takes tsunami wave properties, including the wave height, wave period, wavelength, and propagation direction, as inputs and time-dependently characterizes the responses of the upper atmosphere between 100km and 600km altitudes. We apply WP-GITM to simulate the ionosphere above the West Coast of the United States around the time when the tsunami associated with the March 2011 Tohuku-Oki earthquke arrived. The simulated TEC perturbations agree with Global Positioning System observations reasonably well. For the first time, a fully self-consistent and physics-based model has reproduced the GPS-observed traveling ionospheric signatures of an actual tsunami event.
C1 [Meng, X.; Komjathy, A.; Verkhoglyadova, O. P.; Yang, Y. -M.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Komjathy, A.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada.
[Deng, Y.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA.
RP Meng, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Xing.Meng@jpl.nasa.gov
RI Meng, Xing/A-1929-2016;
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NASA; NASA's Science Mission Directorate in Washington [ROSES
NNH10ZDA001N-GEOIM, NNH07ZDA001N-ESI]
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Funding
for the research came from NASA's Science Mission Directorate in
Washington (ROSES NNH10ZDA001N-GEOIM and NNH07ZDA001N-ESI). The authors
would like to acknowledge Aaron Ridley at the University of Michigan for
beneficial discussions during the model development. The authors also
thank J. H. King, N. Papatashvilli at AdnetSystems, NASA GSFC, and
CDAWeb for providing the OMNI data
(http://cdaweb.gsfc.nasa.gov/istp\_public/). GPS measurements used for
this research were obtained from stations in the Plate Boundary
Observation network. The computational resources were provided by the
JPL high-performance computing.
NR 29
TC 6
Z9 6
U1 1
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4736
EP 4744
DI 10.1002/2015GL064610
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500011
ER
PT J
AU Gurnett, DA
Morgan, DD
Persoon, AM
Granroth, LJ
Kopf, AJ
Plaut, JJ
Green, JL
AF Gurnett, D. A.
Morgan, D. D.
Persoon, A. M.
Granroth, L. J.
Kopf, A. J.
Plaut, J. J.
Green, J. L.
TI An ionized layer in the upper atmosphere of Mars caused by dust impacts
from comet Siding Spring
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE cometary dust; comet Siding Spring; comet Siding Spring encounter with
Mars; meteor impacts with Mars' atmosphere
ID C/2013; IONOSPHERE
AB We report the detection of a dense ionized layer in the upper atmosphere of Mars caused by the impact of dust from comet Siding Spring. The observations were made by the ionospheric radar sounder on the Mars Express spacecraft during two low-altitude passes approximately 7h and 14h after closest approach of the comet to Mars. During these passes an unusual transient layer of ionization was detected at altitudes of about 80 to 100km with peak electron densities of (1.5 to 2.5)x10(5)cm(-3), much higher than normally observed in the Martian ionosphere. From comparisons to previously observed ionization produced by meteors at Earth and Mars, we conclude that the layer was produced by dust from the comet impacting and ionizing the upper atmosphere of Mars.
C1 [Gurnett, D. A.; Morgan, D. D.; Persoon, A. M.; Granroth, L. J.; Kopf, A. J.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Plaut, J. J.] Jet Prop Lab, Pasadena, CA USA.
[Green, J. L.] NASA Headquarters, Washington, DC USA.
RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM donald-gurnett@uiowa.edu
FU NASA [1224107]; Jet Propulsion Laboratory
FX All the data used in this study are available at
http://www-pw.physics.uiowa.edu/marsx/Gurnett_etal_GRL_2015. The
research at the University of Iowa was supported by NASA through
contract 1224107 with the Jet Propulsion Laboratory. We thank the many
members of the scientific, technical, and management teams at NASA
Headquarters, the Jet Propulsion Laboratory, the European Space Agency,
and the Italian Space Agency for their effort in planning the spacecraft
operations required to successfully obtain these data.
NR 17
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U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4745
EP 4751
DI 10.1002/2015GL063726
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500012
ER
PT J
AU Lundgren, P
Samsonov, SV
Velez, CML
Ordonez, M
AF Lundgren, Paul
Samsonov, Sergey V.
Lopez Velez, Cristian Mauricio
Ordonez, Milton
TI Deep source model for Nevado del Ruiz Volcano, Colombia, constrained by
interferometric synthetic aperture radar observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Nevado del Ruiz Volcano; volcano deformation; InSAR
ID LOCAL STRESSES; 1985 ERUPTION; NOVEMBER 13; DEFORMATION; INVERSION;
ALGORITHM; CALDERA; ANDES
AB Nevado del Ruiz is part of a large volcano complex in the northern Andes of Colombia. Interferometric synthetic aperture radar observations from the RADARSAT-2 satellite since 2011 show steady inflation of the volcano since 2012 at 3-4cm/yr. The broad (>20km) deformation pattern from both ascending and descending track data constrain source models for either point or spheroidal sources, both located at >14km beneath the surface (mean elevation 4.2km) and 10km SW of Nevado del Ruiz, below nearby Santa Isabel Volcano. Stress change computations for both sources in the context of a compressive regional stress indicate that dikes propagating from the source should become trapped in sills, possibly leading to a more complex pathway to the surface and explaining the significant lateral separation of the source and Nevado del Ruiz Volcano.
C1 [Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Samsonov, Sergey V.] Nat Resources Canada, Canada Ctr Mapping & Earth Observat, Ottawa, ON, Canada.
[Lopez Velez, Cristian Mauricio; Ordonez, Milton] Colombian Geol Serv, Dept Geol Hazards, Manizales, Colombia.
RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM paul.lundgren@jpl.nasa.gov
OI Samsonov, Sergey/0000-0002-6798-4847
FU National Aeronautics and Space Administration
FX We thank the Canadian Space Agency for providing RADARSAT-2 data. We
thank Freysteinn Sigmundsson for a thorough review. 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. Data used in the modeling and modeling
software may be obtained at request by contacting the authors.
NR 35
TC 4
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U1 6
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2015
VL 42
IS 12
BP 4816
EP 4823
DI 10.1002/2015GL063858
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CM9CB
UT WOS:000358002500022
ER
PT J
AU Mackie, CJ
Candian, A
Huang, XC
Lee, TJ
Tielens, AGGM
AF Mackie, Cameron J.
Candian, Alessandra
Huang, Xinchuan
Lee, Timothy J.
Tielens, Alexander G. G. M.
TI Linear transformation of anharmonic molecular force constants between
normal and Cartesian coordinates
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID POTENTIAL-ENERGY SURFACE; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC
CONSTANTS; FIELD; C3H3+; CODE
AB A full derivation of the analytic transformation of the quadratic, cubic, and quartic force constants from normal coordinates to Cartesian coordinates is given. Previous attempts at this transformation have resulted in non-linear transformations; however, for the first time, a simple linear transformation is presented here. Two different approaches have been formulated and implemented, one of which does not require prior knowledge of the translation-rotation eigenvectors from diagonalization of the Hessian matrix. The validity of this method is tested using two molecules H2O and c-C3H2D+. (C) 2015 AIP Publishing LLC.
C1 [Mackie, Cameron J.; Candian, Alessandra; Tielens, Alexander G. G. M.] Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mackie, CJ (reprint author), Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
EM mackie@strw.leidenuniv.nl
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013;
OI Mackie, Cameron/0000-0003-2885-2021; Candian,
Alessandra/0000-0002-5431-4449
FU European Research Council [246976]; Spinoza award; NASA
[12-APRA12-0107]; NASA/SETI [NNX12AG96A]; SARA supercomputer center in
Almere (NL) [MP-270-13]
FX Helpful discussions with Dr. David Schwenke (NASA Ames), Professor Joel
Bowman (Emory) and Professor Dr. Walter Thiel (Max-Planck) are
gratefully acknowledged by the authors of this work. Studies of
interstellar chemistry at Leiden Observatory that are supported through
advanced European Research Council Grant No. 246976 and a Spinoza award.
X.H. and T.J.L. gratefully acknowledge support from the NASA
12-APRA12-0107 grant. X.H. acknowledges the support from NASA/SETI
Co-operative Agreement NNX12AG96A. The calculations were performed at
the SARA supercomputer center in Almere (NL) under Project No.
MP-270-13.
NR 25
TC 5
Z9 5
U1 0
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD JUN 28
PY 2015
VL 142
IS 24
AR 244107
DI 10.1063/1.4922891
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CM3WE
UT WOS:000357615100011
PM 26133410
ER
PT J
AU Jacobson, MZ
Nghiem, SV
Sorichetta, A
Whitney, N
AF Jacobson, Mark Z.
Nghiem, Son V.
Sorichetta, Alessandro
Whitney, Natasha
TI Ring of impact from the mega-urbanization of Beijing between 2000 and
2009
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE heat island; urban climate; urbanization; ozone
ID URBAN HEAT-ISLAND; SHALLOW-WATER EQUATIONS; POTENTIAL ENSTROPHY; SIZE
DISTRIBUTIONS; UNITED-STATES; GATOR-GCMM; SEA-ICE; LAND; MODEL;
OPENSTREETMAP
AB The transient climate, soil, and air quality impacts of the rapid urbanization of Beijing between 2000 and 2009 are investigated with three-dimensional computer model simulations. The simulations integrate a new satellite data set for urban extent and a geolocated crowd-sourced data set for road surface area and consider differences only in urban land cover and its physical properties. The simulations account for changes in meteorologically driven natural emissions but do not include changes in anthropogenic emissions resulting from urbanization and road network variations. The astounding urbanization, which quadrupled Beijing urban extent between 2000 and 2009 in terms of physical infrastructure change, created a ring of impact that decreased surface albedo, increased ground and near-surface air temperatures, increased vertical turbulent kinetic energy, and decreased the near-surface relative humidity and wind speed. The meteorological changes alone decreased near-surface particulate matter, nitrogen oxides (NOx), and many other chemicals due to vertical dilution but increased near-surface ozone due to the higher temperature and lower NO. Vertical dilution and wind stagnation increased elevated pollution layers and column aerosol extinction. In sum, the ring of impact around Beijing may have increased urban heating, dried soil, mixed pollutants vertically, aggravated air stagnation, and increased near-surface oxidant pollution even before accounting for changes in anthropogenic emissions.
C1 [Jacobson, Mark Z.; Whitney, Natasha] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
[Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Sorichetta, Alessandro] Univ Southampton, Geog & Environm, Southampton, Hants, England.
[Sorichetta, Alessandro] Univ Southampton, Inst Life Sci, Southampton, Hants, England.
RP Jacobson, MZ (reprint author), Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
EM jacobson@stanford.edu
FU NASA SMD Earth Sciences Division; National Aeronautics and Space
Administration (NASA) Land-Cover and Land-Use Change (LCLUC) Program;
Bill & Melinda Gates Foundation [OPP1106427, 1032350]
FX This project received funding from the NASA SMD Earth Sciences Division
and computer support from the NASA high-end computing center. The
research carried out at the Jet Propulsion Laboratory, California
Institute of Technology, was supported under a contract with the
National Aeronautics and Space Administration (NASA) Land-Cover and
Land-Use Change (LCLUC) Program. The research carried out at the
Department of Geography and Environment, University of Southampton, was
done in the framework of the WorldPop Project (www.worldpop.org.uk) and
supported by funding from the Bill & Melinda Gates Foundation
(OPP1106427 and 1032350). Data used to generate figures and the table
for this paper are available freely from the corresponding author at
jacobson@stanford.edu.
NR 77
TC 2
Z9 2
U1 4
U2 37
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 JUN 27
PY 2015
VL 120
IS 12
BP 5740
EP 5756
DI 10.1002/2014JD023008
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CM8MX
UT WOS:000357956800002
ER
PT J
AU Vogelmann, AM
Fridlind, AM
Toto, T
Endo, S
Lin, WY
Wang, J
Feng, S
Zhang, YY
Turner, DD
Liu, YG
Li, ZJ
Xie, SC
Ackerman, AS
Zhang, MH
Khairoutdinov, M
AF Vogelmann, Andrew M.
Fridlind, Ann M.
Toto, Tami
Endo, Satoshi
Lin, Wuyin
Wang, Jian
Feng, Sha
Zhang, Yunyan
Turner, David D.
Liu, Yangang
Li, Zhijin
Xie, Shaocheng
Ackerman, Andrew S.
Zhang, Minghua
Khairoutdinov, Marat
TI RACORO continental boundary layer cloud investigations: 1. Case study
development and ensemble large-scale forcings
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE continental boundary layer cloud; observation-based modeling case
studies; large-eddy simulation or LES; ensemble large-scale forcing; in
situ aerosol size distribution and hygroscopicity; RACORO aircraft
observations
ID SOUTHERN GREAT-PLAINS; SINGLE-COLUMN MODELS; SHALLOW CUMULUS CONVECTION;
OPERATIONAL RAMAN LIDAR; SGP CENTRAL FACILITY; LIQUID WATER PATH;
DIURNAL-CYCLE; ECMWF MODEL; ATMOSPHERIC RADIATION; AEROSOL ACTIVATION
AB Observation-based modeling case studies of continental boundary layer clouds have been developed to study cloudy boundary layers, aerosol influences upon them, and their representation in cloud- and global-scale models. Three 60 h case study periods span the temporal evolution of cumulus, stratiform, and drizzling boundary layer cloud systems, representing mixed and transitional states rather than idealized or canonical cases. Based on in situ measurements from the Routine AAF (Atmospheric Radiation Measurement (ARM) Aerial Facility) CLOWD (Clouds with Low Optical Water Depth) Optical Radiative Observations (RACORO) field campaign and remote sensing observations, the cases are designed with a modular configuration to simplify use in large-eddy simulations (LES) and single-column models. Aircraft measurements of aerosol number size distribution are fit to lognormal functions for concise representation in models. Values of the aerosol hygroscopicity parameter, , are derived from observations to be similar to 0.10, which are lower than the 0.3 typical over continents and suggestive of a large aerosol organic fraction. Ensemble large-scale forcing data sets are derived from the ARM variational analysis, European Centre for Medium-Range Weather Forecasts, and a multiscale data assimilation system. The forcings are assessed through comparison of measured bulk atmospheric and cloud properties to those computed in trial large-eddy simulations, where more efficient run times are enabled through modest reductions in grid resolution and domain size compared to the full-sized LES grid. Simulations capture many of the general features observed, but the state-of-the-art forcings were limited at representing details of cloud onset, and tight gradients and high-resolution transients of importance. Methods for improving the initial conditions and forcings are discussed. The cases developed are available to the general modeling community for studying continental boundary clouds.
C1 [Vogelmann, Andrew M.; Toto, Tami; Endo, Satoshi; Lin, Wuyin; Wang, Jian; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Feng, Sha; Li, Zhijin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Feng, Sha; Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Zhang, Yunyan; Xie, Shaocheng] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Zhang, Minghua; Khairoutdinov, Marat] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
RP Vogelmann, AM (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM vogelmann@bnl.gov
RI Xie, Shaocheng/D-2207-2013; Vogelmann, Andrew/M-8779-2014; Zhang,
Yunyan/F-9783-2011; Liu, Yangang/H-6154-2011; Wang, Jian/G-9344-2011
OI Xie, Shaocheng/0000-0001-8931-5145; Vogelmann,
Andrew/0000-0003-1918-5423;
FU U.S. Department of Energy Science Office of Biological and Environmental
Research Program; Earth System Modeling Program via the FASTER Project;
Atmospheric System Research Program [SC00112704, DE-SC0006988,
DE-SC0006898]; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]; NASA High-End Computing (HEC) Program through the
NASA Advanced Supercomputing (NAS) Division at Ames Research Center;
NASA Radiation Sciences Program; DOE ARM program; U.S. Department of
Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX Data used in this article are from the U.S. Department of Energy SGP ARM
Climate Research Facility (available from http://www.archive.arm.gov)
and the AAF RACORO Campaign (available from
http://www.arm.gov/campaigns/aaf2009racoro#data). We thank the entire
RACORO team: the RACORO scientific steering committee, Haf Jonsson for
the analysis and processing of the Twin Otter flight data and
recalibration of the PCASP, the instrument mentors for their analysis
and processing of data, and the DOE ARM Aerial Facility for its
coordination of RACORO. We also especially acknowledge Don Collins for
guidance using the SMPS data, David Cook provided informative
discussions regarding the surface roughness length over the SGP, Krista
Gaustad and Laura Riihimaki for special processing of MWRRET data for 8
May, and the Raman lidar mentor team of Chris Martin, John Goldsmith,
and Rob Newsom for their efforts in maintaining the Raman lidar. Ozone
measurements from the Ozone Monitoring Instrument (OMI) were provided by
the NASA/GSFC TOMS Ozone Processing Team (OPT) and obtained via the ARM
External Data Center. We would like to thank three anonymous reviewers
for their thoughtful comments on the manuscript. This research was
supported by the U.S. Department of Energy Science Office of Biological
and Environmental Research Program under the following grants/contracts:
the Earth System Modeling Program via the FASTER Project (A.M.V., T.T.,
W.L., S.E., Y.L., S.F., Z.L., M.Z., and M.K.), and the Atmospheric
System Research Program via DE-SC00112704 (A.M.V., Y.L., and J.W.),
DE-SC0006988 (A.M.F. and A.S.A.), and DE-SC0006898 (D.D.T.). A.M.F. and
A.S.A. 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 DE-AC02-05CH11231, and the NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center, and received
additional support from the NASA Radiation Sciences Program. Work at
LLNL was supported by the DOE ARM program and performed under the
auspices of the U.S. Department of Energy by Lawrence Livermore National
Laboratory under contract DE-AC52-07NA27344 (Y.Z. and S.X.).
NR 99
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Z9 6
U1 1
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 JUN 27
PY 2015
VL 120
IS 12
BP 5962
EP 5992
DI 10.1002/2014JD022713
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CM8MX
UT WOS:000357956800015
ER
PT J
AU Endo, S
Fridlind, AM
Lin, WY
Vogelmann, AM
Toto, T
Ackerman, AS
McFarquhar, GM
Jackson, RC
Jonsson, HH
Liu, YG
AF Endo, Satoshi
Fridlind, Ann M.
Lin, Wuyin
Vogelmann, Andrew M.
Toto, Tami
Ackerman, Andrew S.
McFarquhar, Greg M.
Jackson, Robert C.
Jonsson, Haflidi H.
Liu, Yangang
TI RACORO continental boundary layer cloud investigations: 2. Large-eddy
simulations of cumulus clouds and evaluation with in situ and
ground-based observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE LES; cumulus; cloud physics; RACORO; aircraft observations; boundary
layer
ID GENERAL HYDRODYNAMIC THEORY; ATMOSPHERIC RADIATION; AEROSOL ACTIVATION;
FALL SPEED; PART I; PARAMETERIZATION; MICROPHYSICS; CONVECTION; PHASE;
MODEL
AB A 60h case study of continental boundary layer cumulus clouds is examined using two large-eddy simulation (LES) models. The case is based on observations obtained during the RACORO Campaign (Routine Atmospheric Radiation Measurement (ARM) Aerial Facility (AAF) Clouds with Low Optical Water Depths (CLOWD) Optical Radiative Observations) at the ARM Climate Research Facility's Southern Great Plains site. The LES models are driven by continuous large-scale and surface forcings and are constrained by multimodal and temporally varying aerosol number size distribution profiles derived from aircraft observations. We compare simulated cloud macrophysical and microphysical properties with ground-based remote sensing and aircraft observations. The LES simulations capture the observed transitions of the evolving cumulus-topped boundary layers during the three daytime periods and generally reproduce variations of droplet number concentration with liquid water content (LWC), corresponding to the gradient between the cloud centers and cloud edges at given heights. The observed LWC values fall within the range of simulated values; the observed droplet number concentrations are commonly higher than simulated, but differences remain on par with potential estimation errors in the aircraft measurements. Sensitivity studies examine the influences of bin microphysics versus bulk microphysics, aerosol advection, supersaturation treatment, and aerosol hygroscopicity. Simulated macrophysical cloud properties are found to be insensitive in this nonprecipitating case, but microphysical properties are especially sensitive to bulk microphysics supersaturation treatment and aerosol hygroscopicity.
C1 [Endo, Satoshi; Lin, Wuyin; Vogelmann, Andrew M.; Toto, Tami; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[McFarquhar, Greg M.; Jackson, Robert C.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Jonsson, Haflidi H.] Naval Postgrad Sch, Ctr Interdisciplinary Remotely Piloted Aircraft S, Monterey, CA USA.
RP Endo, S (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM sendo@bnl.gov
RI Vogelmann, Andrew/M-8779-2014; Liu, Yangang/H-6154-2011;
OI Vogelmann, Andrew/0000-0003-1918-5423; McFarquhar,
Greg/0000-0003-0950-0135
FU U.S. Department of Energy Science Office of Biological and Environmental
Research Program under the Earth System Modeling Program via the FASTER
Project; U.S. Department of Energy Science Office of Biological and
Environmental Research Program under the Atmospheric System Research
Program [DE-SC00112704]
FX This research was supported by the U.S. Department of Energy Science
Office of Biological and Environmental Research Program under the Earth
System Modeling Program via the FASTER Project
(http://www.bnl.gov/faster/) and the Atmospheric System Research Program
via DE-SC00112704. Observational data sets were obtained from the U.S.
Department of Energy ARM Climate Research Facility
(https://www.arm.gov/) and Oklahoma Mesonet (https://www.mesonet.org/).
Processed forcing and observational data sets used for the 3 day case
study are also aggregated as an ARM PI data product
(http://iop.archive.arm.gov/arm-iop/0pi-data/vogelmann/racoro/case_studi
es). The research utilized resources at the New York Center for
Computational Sciences. Authors appreciate Marat Khairoutdinov for his
helpful comments on LES configurations, Kwinten Van Weverberg and Hugh
Morrison for providing and helping to use the two-moment microphysics
scheme, and Peter Blossey for providing the interface to RRTM radiation
scheme in WRF-FASTER.
NR 60
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Z9 7
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 JUN 27
PY 2015
VL 120
IS 12
BP 5993
EP 6014
DI 10.1002/2014JD022525
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CM8MX
UT WOS:000357956800016
ER
PT J
AU Lin, WY
Liu, YG
Vogelmann, AM
Fridlind, A
Endo, S
Song, H
Feng, S
Toto, T
Li, ZJ
Zhang, MH
AF Lin, Wuyin
Liu, Yangang
Vogelmann, Andrew M.
Fridlind, Ann
Endo, Satoshi
Song, Hua
Feng, Sha
Toto, Tami
Li, Zhijin
Zhang, Minghua
TI RACORO continental boundary layer cloud investigations: 3. Separation of
parameterization biases single-column model CAM5 simulations of shallow
cumulus
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE continental shallow cumulus; single-column model; RACORO
ID COMMUNITY ATMOSPHERE MODEL; FINE-RESOLUTION ANALYSES; DIURNAL CYCLE;
CLIMATE SENSITIVITY; PART I; TROPICAL CONVECTION; SGP SITE; LAND;
IMPACT; FLUX
AB Climatically important low-level clouds are commonly misrepresented in climate models. The FAst-physics System TEstbed and Research (FASTER) Project has constructed case studies from the Atmospheric Radiation Measurement Climate Research Facility's Southern Great Plain site during the RACORO aircraft campaign to facilitate research on model representation of boundary-layer clouds. This paper focuses on using the single-column Community Atmosphere Model version 5 (SCAM5) simulations of a multi-day continental shallow cumulus case to identify specific parameterization causes of low-cloud biases. Consistent model biases among the simulations driven by a set of alternative forcings suggest that uncertainty in the forcing plays only a relatively minor role. In-depth analysis reveals that the model's shallow cumulus convection scheme tends to significantly under-produce clouds during the times when shallow cumuli exist in the observations, while the deep convective and stratiform cloud schemes significantly over-produce low-level clouds throughout the day. The links between model biases and the underlying assumptions of the shallow cumulus scheme are further diagnosed with the aid of large-eddy simulations and aircraft measurements, and by suppressing the triggering of the deep convection scheme. It is found that the weak boundary layer turbulence simulated is directly responsible for the weak cumulus activity and the simulated boundary layer stratiform clouds. Increased vertical and temporal resolutions are shown to lead to stronger boundary layer turbulence and reduction of low-cloud biases.
C1 [Lin, Wuyin; Liu, Yangang; Vogelmann, Andrew M.; Endo, Satoshi; Song, Hua; Toto, Tami] Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA.
[Fridlind, Ann] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Feng, Sha; Li, Zhijin] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA.
[Feng, Sha; Li, Zhijin] Jet Prop Lab, Pasadena, CA USA.
[Feng, Sha; Li, Zhijin] JIFRESSE, Pasadena, CA USA.
[Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
RP Lin, WY (reprint author), Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA.
EM wlin@bnl.gov
RI Vogelmann, Andrew/M-8779-2014; Liu, Yangang/H-6154-2011
OI Vogelmann, Andrew/0000-0003-1918-5423;
FU U.S. Department of Energy Science Office of Biological and Environmental
Research Program under the Earth System Modeling Program via the FASTER
Project; U.S. Department of Energy Science Office of Biological and
Environmental Research Program under the Atmospheric System Research
Program [DE-SC0012704]
FX This research was supported by the U.S. Department of Energy Science
Office of Biological and Environmental Research Program under the Earth
System Modeling Program via the FASTER Project
(http://www.bnl.gov/faster), and the Atmospheric System Research Program
via DE-SC0012704. Data from the DOE's SGP ARM Climate Research Facility
(http://www.archive.arm.gov/) are used in this work. His-Yen Ma and
Shaocheng Xie provided the RACORO period CAPT simulations.
NR 69
TC 3
Z9 3
U1 0
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 JUN 27
PY 2015
VL 120
IS 12
BP 6015
EP 6033
DI 10.1002/2014JD022524
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CM8MX
UT WOS:000357956800017
ER
PT J
AU Kneifel, S
von Lerber, A
Tiira, J
Moisseev, D
Kollias, P
Leinonen, J
AF Kneifel, Stefan
von Lerber, Annakaisa
Tiira, Jussi
Moisseev, Dmitri
Kollias, Pavlos
Leinonen, Jussi
TI Observed relations between snowfall microphysics and triple-frequency
radar measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE triple-frequency radar; snowfall microphysics
ID RAYLEIGH-GANS APPROXIMATION; ICE PARTICLES; SCATTERING PROPERTIES;
AGGREGATE SNOWFLAKES; SOLID PRECIPITATION; FALLING SNOW; 225 GHZ;
MICROWAVE; REFLECTIVITY; MODELS
AB Recently published studies of triple-frequency radar observations of snowfall have demonstrated that naturally occurring snowflakes exhibit scattering signatures that are in some cases consistent with spheroidal particle models and in others can only be explained by complex aggregates. Until recently, no in situ observations have been available to investigate links between microphysical snowfall properties and their scattering properties. In this study, we investigate for the first time relations between collocated ground-based triple-frequency observations with in situ measurements of snowfall at the ground. The three analyzed snowfall cases obtained during a recent field campaign in Finland cover light to moderate snowfall rates with transitions from heavily rimed snow to open-structured, low-density snowflakes. The observed triple-frequency signatures agree well with the previously published findings from airborne radar observations. A rich spatiotemporal structure of triple-frequency observations throughout the cloud is observed during the three cases, which often seems to be related to riming and aggregation zones within the cloud. The comparison of triple-frequency signatures from the lowest altitudes with the ground-based in situ measurements reveals that in the presence of large (>5mm) snow aggregates, a bending away in the triple-frequency space from the curve of classical spheroid scattering models is always observed. Rimed particles appear along an almost horizontal line in the triple-frequency space, which was not observed before. Overall, the three case studies indicate a close connection of triple-frequency signatures and snow particle structure, bulk snowfall density, and characteristic size of the particle size distribution.
C1 [Kneifel, Stefan; Kollias, Pavlos] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada.
[von Lerber, Annakaisa; Moisseev, Dmitri] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Tiira, Jussi; Moisseev, Dmitri] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Leinonen, Jussi] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kneifel, S (reprint author), McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada.
EM skneifel@meteo.uni-koeln.de
RI Moisseev, Dmitri/A-3288-2008; Kneifel, Stefan/A-2044-2015;
OI Moisseev, Dmitri/0000-0002-4575-0409; Kneifel,
Stefan/0000-0003-2220-2968; Leinonen, Jussi/0000-0002-6560-6316; Tiira,
Jussi/0000-0003-0851-3989
FU German Academic Exchange Service (DAAD); U.S. Department of Energy
Atmospheric System Research (ASR) program; Finnish Funding Agency for
Technology and Innovation (TEKES) [3155/31/2009]; Academy of Finland
[255718]; Academy of Finland Finnish Center of Excellence program
[272041]; Cluster for Energy and Environment through the Measurement,
Monitoring, and Environmental Assessment (MMEA) research program;
National Aeronautics and Space Administration
FX We gratefully acknowledge the work of the Hyytiala station and ARM AMF2
personnel for the daily tasks with measurements, especially mentioning
Matti Leskinen and Janne Levula (UH). We thank the NASA GPM ground
validation program and Walter Petersen for providing ground-based
precipitation instrumentation used in this study. We also thank Larry
Bliven from NASA GSFC/Wallops Flight Facility for advices with PIP data
interpretation and Jarmo Koistinen from Finnish Meteorological Institute
(FMI) for his assistance with the synoptic analysis of the case studies.
Work carried out by S.K. was supported by a Postdoctoral Fellowship from
the German Academic Exchange Service (DAAD); additional funding for S.K.
and P.K. was provided by the U.S. Department of Energy Atmospheric
System Research (ASR) program. The research of A.L. was funded by grants
3155/31/2009 of the Finnish Funding Agency for Technology and Innovation
(TEKES) and 255718 of the Academy of Finland. D.M. and J.T. were
supported by the Academy of Finland Finnish Center of Excellence program
(grant 272041) and the Cluster for Energy and Environment through the
Measurement, Monitoring, and Environmental Assessment (MMEA) research
program. The research of J.L. described in this publication was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Peter Rodriguez from Environment Canada is acknowledged
for sharing his ideas on snow measurement setup. We further thank Robin
Hogan for his fruitful discussion and for providing his code to compute
DWR using SSRG. We also acknowledge valuable discussions with Chris
Westbrook, Jani Tyynela, and Maria Cadeddu. All remote sensing and in
situ data from the BAECC campaign used in this study are available from
the ARM data archive at http://www.archive.arm.gov.
NR 49
TC 11
Z9 11
U1 2
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2015
VL 120
IS 12
BP 6034
EP 6055
DI 10.1002/2015JD023156
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CM8MX
UT WOS:000357956800018
ER
PT J
AU Ulbricht, G
Mazin, BA
Szypryt, P
Walter, AB
Bockstiegel, C
Bumble, B
AF Ulbricht, Gerhard
Mazin, Benjamin A.
Szypryt, Paul
Walter, Alex B.
Bockstiegel, Clint
Bumble, Bruce
TI Highly multiplexible thermal kinetic inductance detectors for x-ray
imaging spectroscopy
SO APPLIED PHYSICS LETTERS
LA English
DT Article
AB For X-ray imaging spectroscopy, high spatial resolution over a large field of view is often as important as high energy resolution, but current X-ray detectors do not provide both in the same device. Thermal Kinetic Inductance Detectors (TKIDs) are being developed as they offer a feasible way to combine the energy resolution of transition edge sensors with pixel counts approaching CCDs and thus promise significant improvements for many X-ray spectroscopy applications. TKIDs are a variation of Microwave Kinetic Inductance Detectors (MKIDs) and share their multiplexibility: working MKID arrays with 2024 pixels have recently been demonstrated and much bigger arrays are under development. In this work, we present a TKID prototype, which is able to achieve an energy resolution of 75 eV at 5.9 keV, even though its general design still has to be optimized. We further describe TKID fabrication, characterization, multiplexing, and working principle and demonstrate the necessity of a data fitting algorithm in order to extract photon energies. With further design optimizations, we expect to be able to improve our TKID energy resolution to less than 10 eV at 5.9 keV. (C) 2015 AIP Publishing LLC.
C1 [Ulbricht, Gerhard; Mazin, Benjamin A.; Szypryt, Paul; Walter, Alex B.; Bockstiegel, Clint] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bumble, Bruce] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Ulbricht, G (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM ulbricht@physics.ucsb.edu
RI Mazin, Ben/B-8704-2011; Ulbricht, Gerhard/P-7487-2016
OI Mazin, Ben/0000-0003-0526-1114; Ulbricht, Gerhard/0000-0002-6497-3763
FU NASA Space Technology Research Fellowship (NSTRF) program [NNX13AL70H];
NASA ROSES-APRA [NNX13AH34G, NNX14AI79G]; NSF
FX The authors would like to thank the NASA Space Technology Research
Fellowship (NSTRF) program (Grant No. NNX13AL70H) for funding graduate
student P.S. The work was funded by the NASA ROSES-APRA detectors
program Grant Nos. NNX13AH34G and NNX14AI79G. Devices were made at the
UC Santa Barbara Nanofabrication Facility; a part of the NSF funded
National Nanotechnology Infrastructure Network.
NR 25
TC 5
Z9 5
U1 3
U2 9
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD JUN 22
PY 2015
VL 106
IS 25
AR 251103
DI 10.1063/1.4923096
PG 4
WC Physics, Applied
SC Physics
GA CL5XG
UT WOS:000357036600003
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Anderson, B
Atwood, WB
Baldini, L
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bonino, R
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caputo, R
Caragiulo, M
Caraveo, PA
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Godfrey, G
Gomez-Vargas, GA
Grenier, IA
Grove, JE
Guiriec, S
Gustafsson, M
Hewitt, JW
Hill, AB
Horan, D
Johannesson, G
Johnson, RP
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Malyshev, D
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Moiseev, AA
Monzani, ME
Morselli, A
Murgia, S
Nuss, E
Ohsugi, T
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Pesce-Rollins, M
Piron, F
Pivato, G
Raino, S
Rando, R
Razzano, M
Reimer, A
Reposeur, T
Ritz, S
Sanchez-Conde, M
Schulz, A
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Tajima, H
Takahashi, H
Thayer, JB
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Vianello, G
Werner, M
Winer, BL
Wood, KS
Wood, M
Zaharijas, G
Zimmer, S
AF Ackermann, M.
Ajello, M.
Albert, A.
Anderson, B.
Atwood, W. B.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caputo, R.
Caragiulo, M.
Caraveo, P. A.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Godfrey, G.
Gomez-Vargas, G. A.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Gustafsson, M.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Johannesson, G.
Johnson, R. P.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Malyshev, D.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mizuno, T.
Moiseev, A. A.
Monzani, M. E.
Morselli, A.
Murgia, S.
Nuss, E.
Ohsugi, T.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reposeur, T.
Ritz, S.
Sanchez-Conde, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Tajima, H.
Takahashi, H.
Thayer, J. B.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Werner, M.
Winer, B. L.
Wood, K. S.
Wood, M.
Zaharijas, G.
Zimmer, S.
TI Updated search for spectral lines from Galactic dark matter interactions
with pass 8 data from the Fermi Large Area Telescope
SO PHYSICAL REVIEW D
LA English
DT Article
ID CANDIDATES; GALAXIES; DENSITY
AB Dark matter in the Milky Way may annihilate directly into. rays, producing a monoenergetic spectral line. Therefore, detecting such a signature would be strong evidence for dark matter annihilation or decay. We search for spectral lines in the Fermi Large Area Telescope observations of the Milky Way halo in the energy range 200 MeV-500 GeV using analysis methods from our most recent line searches. The main improvements relative to previous works are our use of 5.8 years of data reprocessed with the Pass 8 event-level analysis and the additional data resulting from the modified observing strategy designed to increase exposure of the Galactic center region. We search in five sky regions selected to optimize sensitivity to different theoretically motivated dark matter scenarios and find no significant detections. In addition to presenting the results from our search for lines, we also investigate the previously reported tentative detection of a line at 133 GeV using the new Pass 8 data.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chekhtman, A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Tajima, H.; 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.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Caputo, R.; Johnson, R. P.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Caputo, R.; Johnson, R. P.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Cuoco, A.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Brandt, T. J.; Guiriec, S.; McEnery, J. E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univ & Particules Montpellier, Montpellier, France.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy.
[Anderson, B.; Conrad, J.; Larsson, S.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Anderson, B.; Conrad, J.; Cuoco, A.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Fukazawa, Y.; Takahashi, H.] 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, Dept Fis, Santiago, Chile.
[Grenier, I. A.] CEA Saclay, Univ Paris Diderot, CNRS, IRFU,Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France.
[Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Gustafsson, M.] Univ Gottingen, Fac Phys, Inst Theoret Phys, D-37077 Gottingen, Germany.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Hewitt, J. W.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] CSIC, IEEC, Inst Space Sci, E-08193 Barcelona, Spain.
[Li, L.] AlbaNova, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[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.
[Reimer, A.; Werner, M.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Werner, M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Reposeur, T.] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 USA.
[Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Nova Gor, Lab Astroparticle Phys, SI-5000 Nova Gorica, Slovenia.
RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany.
EM aalbert@slac.stanford.edu; rcaputo@ucsc.edu
RI Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Bonino,
Raffaella/S-2367-2016; Di Venere, Leonardo/C-7619-2017; Morselli,
Aldo/G-6769-2011; Funk, Stefan/B-7629-2015; 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;
Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016;
OI Gasparrini, Dario/0000-0002-5064-9495; Baldini,
Luca/0000-0002-9785-7726; Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791;
SPINELLI, Paolo/0000-0001-6688-8864; Pesce-Rollins,
Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094;
Giroletti, Marcello/0000-0002-8657-8852; Bonino,
Raffaella/0000-0002-4264-1215; Torres, Diego/0000-0002-1522-9065; Di
Venere, Leonardo/0000-0003-0703-824X; Morselli,
Aldo/0000-0002-7704-9553; 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;
Bissaldi, Elisabetta/0000-0001-9935-8106; Hill, Adam/0000-0003-3470-4834
FU Royal Swedish Academy of Sciences through the K. A. Wallenberg
Foundation; NASA postdoctoral fellowship; Marie Curie International
Outgoing Fellowship for Career Development through the FP7 Programme
[257861]; Italian Ministry of Education, University and Research (MIUR)
[FIRB-2012-RBFR12PM1F]
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), the High
Energy Accelerator Research Organization (KEK), and the Japan Aerospace
Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation,
the Swedish Research Council, and the Swedish National Space Board in
Sweden. Additional support for science analysis during the operations
phase is gratefully acknowledged from the Istituto Nazionale di
Astrofisica in Italy and the Centre National d'Etudes Spatiales in
France. B. Anderson is supported by the Royal Swedish Academy of
Sciences through a grant from the K. A. Wallenberg Foundation. S. G.
received support from a NASA postdoctoral fellowship. A. B. H. is
supported by the Marie Curie International Outgoing Fellowship for
Career Development through the FP7/20072013 Programme (Grant No.
257861). M. R. received funding from the Italian Ministry of Education,
University and Research (MIUR) through Contract No.
FIRB-2012-RBFR12PM1F.
NR 38
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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 JUN 22
PY 2015
VL 91
IS 12
AR 122002
DI 10.1103/PhysRevD.91.122002
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CK9TY
UT WOS:000356583600002
ER
PT J
AU Clementel, N
Madura, TI
Kruip, CJH
Paardekooper, JP
AF Clementel, N.
Madura, T. I.
Kruip, C. J. H.
Paardekooper, J. -P.
TI 3D radiative transfer simulations of Eta Carinae's inner colliding winds
- II. Ionization structure of helium at periastron
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; radiative transfer; binaries: close; stars: individual:
Eta Carinae; stars: mass-loss; stars: winds, outflows
ID SIMPLEX ALGORITHM; COMPANION; EVENTS; VARIABILITY; PARAMETERS;
COLLISION; EMISSION
AB Spectral observations of the massive colliding wind binary Eta Carinae show phase-dependent variations, in intensity and velocity, of numerous helium emission and absorption lines throughout the entire 5.54-yr orbit. Approaching periastron, the 3D structure of the wind-wind interaction region (WWIR) gets highly distorted due to the eccentric (e similar to 0.9) binary orbit. The secondary star (eta(B)) at these phases is located deep within the primary's dense wind photosphere. The combination of these effects is thought to be the cause of the particularly interesting features observed in the helium lines at periastron. We perform 3D radiative transfer simulations of eta Car's interacting winds at periastron. Using the SIMPLEX radiative transfer algorithm, we post-process output from 3D smoothed particle hydrodynamic simulations of the inner 150 au of the eta Car system for two different primary star mass-loss rates (M-eta A)(.) Using previous results from simulations at apastron as a guide for the initial conditions, we compute 3D helium ionization maps. We find that, for higher. M-eta A, (eta B) He0+-ionizing photons are not able to penetrate into the pre-shock primary wind. He+ due to eta(B) is only present in a thin layer along the leading arm of the WWIR and in a small region close to the stars. Lowering. M-eta A allows eta(B)'s ionizing photons to reach the expanding unshocked secondary wind on the apastron side of the system, and create a low fraction of He+ in the pre-shock primary wind. With apastron on our side of the system, our results are qualitatively consistent with the observed variations in strength and radial velocity of eta Car's helium emission and absorption lines, which helps better constrain the regions where these lines arise.
C1 [Clementel, N.; Kruip, C. J. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Clementel, N.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Madura, T. I.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Paardekooper, J. -P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Paardekooper, J. -P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Clementel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM clementel@saao.ac.za
FU NASA
FX TIM is supported by an appointment to the NASA Postdoctoral Programme at
the Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 34
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 21
PY 2015
VL 450
IS 2
BP 1388
EP 1398
DI 10.1093/mnras/stv696
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6LB
UT WOS:000356338500018
ER
PT J
AU Russell, TD
Miller-Jones, JCA
Curran, PA
Soria, R
Altamirano, D
Corbel, S
Coriat, M
Moin, A
Russell, DM
Sivakoff, GR
Slaven-Blair, TJ
Belloni, TM
Fender, RP
Heinz, S
Jonker, PG
Krimm, HA
Kording, EG
Maitra, D
Markoff, S
Middleton, M
Migliari, S
Remillard, RA
Rupen, MP
Sarazin, CL
Tetarenko, AJ
Torres, MAP
Tudose, V
Tzioumis, AK
AF Russell, T. D.
Miller-Jones, J. C. A.
Curran, P. A.
Soria, R.
Altamirano, D.
Corbel, S.
Coriat, M.
Moin, A.
Russell, D. M.
Sivakoff, G. R.
Slaven-Blair, T. J.
Belloni, T. M.
Fender, R. P.
Heinz, S.
Jonker, P. G.
Krimm, H. A.
Koerding, E. G.
Maitra, D.
Markoff, S.
Middleton, M.
Migliari, S.
Remillard, R. A.
Rupen, M. P.
Sarazin, C. L.
Tetarenko, A. J.
Torres, M. A. P.
Tudose, V.
Tzioumis, A. K.
TI Radio monitoring of the hard state jets in the 2011 outburst of MAXI
J1836-194
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE proper motions; stars: individual: MAXI J1836; 194; ISM: jets and
outflows; radio continuum: stars; X-rays: binaries
ID BLACK-HOLE CANDIDATE; X-RAY BINARIES; VLBA CALIBRATOR SURVEY; SPECTRAL
ENERGY-DISTRIBUTION; COMPACT OBJECT FORMATION; ACTIVE GALACTIC NUCLEUS;
BROAD-BAND SPECTRUM; GX 339-4; RELATIVISTIC JETS; INTERNAL SHOCKS
AB MAXI J1836-194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its 'failed' outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarized emission at a level of similar to 1 per cent early in the outburst, increasing to similar to 3 per cent as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show an similar to 15 mas jet along the position angle -21 +/- 2 degrees, in agreement with the electric vector position angle found from our polarization results (-21 +/- 4 degrees), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasisimultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of L-R alpha L-X(1.8 +/- 0.2), where L-R and LX denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting.
C1 [Russell, T. D.; Miller-Jones, J. C. A.; Curran, P. A.; Soria, R.; Slaven-Blair, T. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Altamirano, D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Corbel, S.] Univ Paris Diderot, CNRS INSU, Lab AIM CEA IRFU, CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France.
[Corbel, S.] Univ Orleans, CNRS INSU, Stn Radioastron Nancay, Observ Paris,USR 704,OSUC, F-18330 Nancay, France.
[Coriat, M.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Moin, A.; Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates.
[Moin, A.] Shanghai Astron Observ, Shanghai 200030, Peoples R China.
[Sivakoff, G. R.; Tetarenko, A. J.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Belloni, T. M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
[Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.; Koerding, E. G.; Torres, M. A. P.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H. A.] USRA, Columbia, MD 21044 USA.
[Maitra, D.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA.
[Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Middleton, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Migliari, S.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain.
[Migliari, S.] Univ Barcelona, Inst Cosm Sci, E-08028 Barcelona, Spain.
[Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Rupen, M. P.] Herzberg Astron & Astrophys, Natl Res Council, Penticton, BC V2A 6J9, Canada.
[Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Tudose, V.] Inst Space Sci, RO-077125 Bucharest, Romania.
[Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia.
RP Russell, TD (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
EM thomas.russell@icrar.org
RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; Tudose,
Valeriu/F-8976-2010;
OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff,
Gregory/0000-0001-6682-916X; Russell, David/0000-0002-3500-631X;
Russell, Thomas/0000-0001-6958-8891
FU Australian Research Council [DP 120102393]; Royal Society; French
Research National Agency: CHAOS project [ANR-12-BS05-0009]; Uni-vEarthS
Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023,
ANR-11-IDEX-0005-02]; NSERC Discovery Grant; INAF-PRIN [2012-6]; Spanish
Ministerio de Economia y Competitividad; European Social Funds through a
Ramon y Cajal Fellowship; Spanish Ministerio de Ciencia e Innovacion
[AYA2013-47447-C03-1-P]; state government of Western Australia;
Commonwealth of Australia
FX We would like to thank the anonymous referee for their helpful comments
and suggestions. We also thank Tom Maccarone for useful discussions.
This research was supported under the Australian Research Council's
Discovery Projects funding scheme (project number DP 120102393). DA
acknowledges support from the Royal Society. SC acknowledges funding
support from the French Research National Agency: CHAOS project
ANR-12-BS05-0009 (http://www.chaos-project.fr) and financial support
from the Uni-vEarthS Labex program of Sorbonne Paris Cite
(ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). GRS and AJT are supported by
an NSERC Discovery Grant. TMB acknowledges support from INAF-PRIN
2012-6. SM acknowledges support by the Spanish Ministerio de Economia y
Competitividad and European Social Funds through a Ramon y Cajal
Fellowship and the Spanish Ministerio de Ciencia e Innovacion (SM; grant
AYA2013-47447-C03-1-P). This research has made use of NASA's
Astrophysics Data System. The International Centre for Radio Astronomy
Research is a joint venture between Curtin University and the University
of Western Australia, funded by the state government of Western
Australia and the joint venture partners. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. The ATCA is
part of the Australia Telescope National Facility which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO.
NR 118
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 21
PY 2015
VL 450
IS 2
BP 1745
EP 1759
DI 10.1093/mnras/stv723
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6LB
UT WOS:000356338500047
ER
PT J
AU Tregloan-Reed, J
Southworth, J
Burgdorf, M
Novati, SC
Dominik, M
Finet, F
Jorgensen, UG
Maier, G
Mancini, L
Prof, S
Ricci, D
Snodgrass, C
Bozza, V
Browne, P
Dodds, P
Gerner, T
Harpsoe, K
Hinse, TC
Hundertmark, M
Kains, N
Kerins, E
Liebig, C
Penny, MT
Rahvar, S
Sahu, K
Scarpetta, G
Schafer, S
Schonebeck, F
Skottfelt, J
Surdej, J
AF Tregloan-Reed, Jeremy
Southworth, John
Burgdorf, M.
Novati, S. Calchi
Dominik, M.
Finet, F.
Jorgensen, U. G.
Maier, G.
Mancini, L.
Prof, S.
Ricci, D.
Snodgrass, C.
Bozza, V.
Browne, P.
Dodds, P.
Gerner, T.
Harpsoe, K.
Hinse, T. C.
Hundertmark, M.
Kains, N.
Kerins, E.
Liebig, C.
Penny, M. T.
Rahvar, S.
Sahu, K.
Scarpetta, G.
Schaefer, S.
Schoenebeck, F.
Skottfelt, J.
Surdej, J.
TI Transits and starspots in the WASP-6 planetary system
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; stars: fundamental parameters; stars:
individual: WASP-6; planetary systems; starspots
ID SPIN-ORBIT ALIGNMENT; HIGH-PRECISION PHOTOMETRY; EXTRASOLAR PLANETS;
DIFFERENTIAL EVOLUTION; TRANSMISSION SPECTRUM; EXOPLANETARY SYSTEM;
CIRCUMBINARY PLANET; PHYSICAL-PROPERTIES; HABITABLE ZONE; HOT JUPITERS
AB We present updates to PRISM, a photometric transit-starspot model, and GEMC, a hybrid optimization code combining MCMC and a genetic algorithm. We then present high-precision photometry of four transits in the WASP-6 planetary system, two of which contain a starspot anomaly. All four transits were modelled using PRISM and GEMC, and the physical properties of the system calculated. We find the mass and radius of the host star to be 0.836 +/- 0.063 M-circle dot and 0.864 +/- 0.024 R-circle dot, respectively. For the planet, we find a mass of 0.485 +/- 0.027M(Jup), a radius of 1.230 +/- 0.035 R-Jup and a density of 0.244 +/- 0.014 rho(Jup). These values are consistent with those found in the literature. In the likely hypothesis that the two spot anomalies are caused by the same starspot or starspot complex, we measure the stars rotation period and velocity to be 23.80 +/- 0.15 d and 1.78 +/- 0.20 km s(-1), respectively, at a colatitude of 75.8 degrees. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is lambda = 7.2 degrees +/- 3.7 degrees, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect. These results suggest thatWASP-6 b formed at amuch greater distance from its host star and suffered orbital decay through tidal interactions with the protoplanetary disc.
C1 [Tregloan-Reed, Jeremy] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tregloan-Reed, Jeremy; Southworth, John] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Burgdorf, M.] Univ Hamburg, Meteorol Inst, D-20146 Hamburg, Germany.
[Novati, S. Calchi] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, S. Calchi; Bozza, V.; 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.; Browne, P.; Dodds, P.; Hundertmark, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Finet, F.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Finet, F.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, Uttarakhand, India.
[Jorgensen, U. G.; Harpsoe, K.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen K, Denmark.
[Jorgensen, U. G.; Harpsoe, K.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Maier, G.; Prof, S.; Gerner, T.; Schoenebeck, F.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Ricci, D.] Univ Nacl Autonoma Mexico, Inst Astron, Observ Astron Nacl, Ensenada 22860, Baja California, Mexico.
[Ricci, D.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Ricci, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Hinse, T. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Kains, N.; Sahu, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Penny, M. T.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
RP Tregloan-Reed, J (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jeremy.j.tregloan-reed@nasa.gov
RI Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008;
OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Ricci,
Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905
FU The Danish Council for Independent Research (FNU); Department of
Culture, Arts Leisure (DCAL); STFC; ORAU (Oak Ridge Associated
Universities); NASA; Spanish Ministry of Economy and Competitiveness
(MINECO) [MINECO SEV-2011-0187]; Communaute francaise de Belgique -
Actions de recherche concertees - Academie Wallonie-Europe
FX We like to thank the anonymous referee for the helpful comments on the
manuscript. The operation of the Danish 1.54-m telescope at ESOs La
Silla observatory is financed by a grant to UGJ from The Danish Council
for Independent Research (FNU). Research at the Armagh Observatory is
funded by the Department of Culture, Arts & Leisure (DCAL). JTR
acknowledges financial support from STFC in the form of a PhD
Studentship (the majority of this work) and also acknowledges financial
support from ORAU (Oak Ridge Associated Universities) and NASA in the
form of a Post-Doctoral Programme (NPP) Fellowship. JS acknowledges
financial support from STFC in the form of an Advanced Fellowship. DR
acknowledges financial support from the Spanish Ministry of Economy and
Competitiveness (MINECO) under the 2011 Severo Ochoa Programme MINECO
SEV-2011-0187. FF, DR (boursier FRIA) and J Surdej acknowledge support
from the Communaute francaise de Belgique - Actions de recherche
concertees - Academie Wallonie-Europe.
NR 67
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 21
PY 2015
VL 450
IS 2
BP 1760
EP 1769
DI 10.1093/mnras/stv730
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6LB
UT WOS:000356338500048
ER
PT J
AU Ade, PAR
Aikin, RW
Barkats, D
Benton, SJ
Bischoff, CA
Bock, JJ
Bradford, KJ
Brevik, JA
Buder, I
Bullock, E
Dowell, CD
Duband, L
Filippini, JP
Fliescher, S
Golwala, SR
Halpern, M
Hasselfield, M
Hildebrandt, SR
Hilton, GC
Hui, H
Irwin, KD
Kang, JH
Karkare, KS
Kaufman, JP
Keating, BG
Kefeli, S
Kernasovskiy, SA
Kovac, JM
Kuo, CL
Leitch, EM
Lueker, M
Megerian, KG
Netterfield, CB
Nguyen, HT
O'Brient, R
Ogburn, RW
Orlando, A
Pryke, C
Richter, S
Schwarz, R
Sheehy, CD
Staniszewski, ZK
Sudiwala, RV
Teply, GP
Thompson, K
Tolan, JE
Turner, AD
Vieregg, AG
Weber, AC
Wong, CL
Yoon, KW
AF Ade, P. A. R.
Aikin, R. W.
Barkats, D.
Benton, S. J.
Bischoff, C. A.
Bock, J. J.
Bradford, K. J.
Brevik, J. A.
Buder, I.
Bullock, E.
Dowell, C. D.
Duband, L.
Filippini, J. P.
Fliescher, S.
Golwala, S. R.
Halpern, M.
Hasselfield, M.
Hildebrandt, S. R.
Hilton, G. C.
Hui, H.
Irwin, K. D.
Kang, J. H.
Karkare, K. S.
Kaufman, J. P.
Keating, B. G.
Kefeli, S.
Kernasovskiy, S. A.
Kovac, J. M.
Kuo, C. L.
Leitch, E. M.
Lueker, M.
Megerian, K. G.
Netterfield, C. B.
Nguyen, H. T.
O'Brient, R.
Ogburn, R. W.
Orlando, A.
Pryke, C.
Richter, S.
Schwarz, R.
Sheehy, C. D.
Staniszewski, Z. K.
Sudiwala, R. V.
Teply, G. P.
Thompson, K.
Tolan, J. E.
Turner, A. D.
Vieregg, A. G.
Weber, A. C.
Wong, C. L.
Yoon, K. W.
CA BICEP2
Keck Array Collaborations
TI BICEP2/KECK ARRAY. IV. OPTICAL CHARACTERIZATION AND PERFORMANCE OF THE
BICEP2 AND KECK ARRAY EXPERIMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; polarization
ID GRAVITY-WAVES; POLARIZATION; POLARIMETER
AB BICEP2. and the Keck Array. are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. BICEP2. was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array. was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). BICEP2. and the Keck Array. share a common optical design and employ the field-proven BICEP1. strategy of using small-aperture, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. Here we describe the optical design of both instruments and report a full characterization of the optical performance and beams of BICEP2. and the Keck Array. at 150 GHz.
C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hui, H.; Kefeli, S.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bischoff, C. A.; Bradford, K. J.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Weber, A. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France.
[Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61820 USA.
[Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Hilton, G. C.; Irwin, K. D.] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Irwin, K. D.; Kang, J. H.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Vieregg, A. G.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM avieregg@kicp.uchicago.edu
OI Orlando, Angiola/0000-0001-8004-5054; Karkare,
Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954
FU National Science Foundation (NSF) (Caltech/Harvard) [ANT-0742818,
ANT-1044978]; National Science Foundation (NSF) (Chicago/Minnesota)
[ANT-0742592, ANT-1110087]; NSF (Harvard) [ANT-1145172]; NSF (Minnesota)
[ANT-1145143]; NSF (Stanford) [ANT-1145248]; W. M. Keck Foundation
(Caltech); JPL Research and Technology Development Fund; NASA
[06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at
Caltech; Canada Foundation for Innovation; FAS Science Division Research
Computing Group at Harvard; U.S. Department of Energy Office of Science;
W. M. Keck Foundation
FX BICEP2 was supported by the National Science Foundation (NSF) under
grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and
ANT-1110087 (Chicago/Minnesota). The Keck Array. was supported by the
NSF under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and
ANT-1145248 (Stanford), and by the W. M. Keck Foundation (Caltech). The
development of antenna-coupled detector technology was supported by the
JPL Research and Technology Development Fund and grants 06-ARPA206-0040
and 10-SAT10-0017 from the NASA APRA and SAT programs. The development
and testing of focal planes were supported by the Gordon and Betty Moore
Foundation at Caltech. Readout electronics were supported by a Canada
Foundation for Innovation grant to UBC. Computations presented in this
paper were run on the Odyssey cluster supported by the FAS Science
Division Research Computing Group at Harvard. The analysis effort at
Stanford and SLAC was partially suported by the U.S. Department of
Energy Office of Science. The receiver development was supported in part
by a grant from the W. M. Keck Foundation. Tireless administrative
support was provided by Irene Coyle and Kathy Deniston.
NR 29
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 206
DI 10.1088/0004-637X/806/2/206
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500061
ER
PT J
AU An, HJ
Bellm, E
Bhalerao, V
Boggs, SE
Christensen, FE
Craig, WW
Fuerst, F
Hailey, CJ
Harrison, FA
Kaspi, VM
Natalucci, L
Stern, D
Tomsick, JA
Zhang, WW
AF An, Hongjun
Bellm, Eric
Bhalerao, Varun
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Fuerst, Felix
Hailey, Charles J.
Harrison, Fiona A.
Kaspi, Victoria M.
Natalucci, Lorenzo
Stern, Daniel
Tomsick, John A.
Zhang, William W.
TI BROADBAND X-RAY PROPERTIES OF THE GAMMA-RAY BINARY 1FGL J1018.6-5856
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; gamma rays: stars; stars: individual (1FGL
J1018.6-5856); X-rays: binaries
ID HIGH-ENERGY EMISSION; LS 5039; TIMING-EXPLORER; PULSAR;
I+61-DEGREES-303; MICROQUASARS; PSR-1259-63; RADIATION; SYSTEMS; MODEL
AB We report on NuSTAR, XMM-Newton, and Swift observations of the gamma-ray binary 1FGL J1018.6-5856. We measure the orbital period to be 16.544 +/- 0.008 days using Swift data spanning 1900 days. The orbital period is different from the 2011 gamma-ray measurement which was used in the previous X-ray study of An et al. using similar to 400 days of Swift data, but is consistent with a new gamma-ray solution reported in 2014. The light curve folded on the new period is qualitatively similar to that reported previously, having a spike at phase 0 and broad sinusoidal modulation. The X-ray flux enhancement at phase 0 occurs more regularly in time than was previously suggested. A spiky structure at this phase seems to be a persistent feature, although there is some variability. Furthermore, we find that the source flux clearly correlates with the spectral hardness throughout all orbital phases, and that the broadband X-ray spectra measured with NuSTAR, XMM-Newton, and Swift are well fit with an unbroken power-law model. This spectrum suggests that the system may not be accretion-powered.
C1 [An, Hongjun; Zhang, William W.] Stanford Univ, Dept Phys KIPAC, Stanford, CA 94305 USA.
[An, Hongjun; Kaspi, Victoria M.; Zhang, William W.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Bellm, Eric; Fuerst, Felix; Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Bhalerao, Varun] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Boggs, Steven E.; Craig, William W.; Tomsick, John A.] 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.
[Kaspi, Victoria M.] McGill Space Inst, Montreal, PQ H3A 2T8, Canada.
[Natalucci, Lorenzo] INAFIAPS, Ist Nazl Astrofis, I-00133 Rome, Italy.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP An, HJ (reprint author), Stanford Univ, Dept Phys KIPAC, Stanford, CA 94305 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348;
Bhalerao, Varun/0000-0002-6112-7609; An, Hongjun/0000-0002-6389-9012
FU NASA [NNG08FD60C, NAS5-00147]; National Aeronautics and Space
Administration; Kavli Institute for Particle Astrophysics and Cosmology
(KIPAC); ASI/INAF [I/037/12/0-011/13]
FX We thank R. W. Romani for useful discussions. This work was supported
under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR
mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the National
Aeronautics and Space Administration. We thank the NuSTAR Operations,
Software and Calibration teams for support with the execution and
analysis of these observations. This research has made use of the NuSTAR
Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(USA). This research has made use of data obtained from the High Energy
Astrophysics Science Archive Research Center (HEASARC), provided by
NASA's Goddard Space Flight Center. H.A. acknowledges supports provided
by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute
for Particle Astrophysics and Cosmology (KIPAC). LN wishes to
acknowledge the Italian Space Agency (ASI) for financial support by
ASI/INAF grant I/037/12/0-011/13.
NR 37
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 166
DI 10.1088/0004-637X/806/2/166
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500021
ER
PT J
AU D'Angelo, G
Podolak, M
AF D'Angelo, Gennaro
Podolak, Morris
TI CAPTURE AND EVOLUTION OF PLANETESIMALS IN CIRCUMJOVIAN DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; hydrodynamics; methods: numerical;
planet-disk interactions; planets and satellites: formation;
protoplanetary disks
ID PRIMORDIAL SOLAR NEBULA; GAS GIANT PLANETS; ACCRETION DISKS;
PROTOPLANETARY DISKS; MASS PLANETS; CIRCUMPLANETARY DISKS;
MECHANICAL-PROPERTIES; GALILEAN SATELLITES; CORE ACCRETION;
BINARY-SYSTEMS
AB We study the evolution of planetesimals in evolved gaseous disks that orbit a solar-mass star and harbor a Jupitermass planet at a(p) approximate to 5 AU. The gas dynamics are modeled with a three-dimensional hydrodynamics code that employs nested grids and achieves a resolution of one Jupiter radius in the circumplanetary disk. The code models solids as individual particles. Planetesimals are subjected to gravitational forces by the star and the planet, a drag force by the gas, disruption via ram pressure, and mass loss through ablation. The mass evolution of solids is calculated self-consistently with their temperature, velocity, and position. We consider icy and icy/rocky bodies of radius 0.1-100 km, initially deployed on orbits around the star within a few Hill radii (R-H) of the planet's orbit. Planetesimals are scattered inward, outward, and toward disk regions of radius r >> a(p). Scattering can relocate significant amounts of solids, provided that regions |r - a(p)| similar to 3R(H) are replenished with planetesimals. Scattered bodies can be temporarily captured on planetocentric orbits. Ablation consumes nearly all solids at gas temperatures greater than or similar to 220 K. Super-Keplerian rotation around and beyond the outer edge of the gas gap can segregate less than or similar to 0.1 km bodies, producing solid gap edges at size-dependent radial locations. Capture, break-up, and ablation of solids result in a dust-laden circumplanetary disk with low surface densities of kilometer sized planetesimals, implying relatively long timescales for satellite formation. After a giant planet acquires most of its mass, accretion of solids is unlikely to significantly alter its heavy element content. The luminosity generated by accretion of solids and the contraction luminosity can be of similar orders of magnitude.
C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA.
[Podolak, Morris] Tel Aviv Univ, Dept Geosci, IL-69978 Ramat Aviv, Israel.
RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM gennaro.dangelo@nasa.gov; morris@post.tau.ac.il
OI D'Angelo, Gennaro/0000-0002-2064-0801; Podolak,
Morris/0000-0003-4801-8691
FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins
of Solar Systems Program [NNX11AD20G, NNX11AK54G, NNX14AG92G]
FX We wish to express our gratitude to Jack Lissauer and Peter Bodenheimer
for their valuable feedback. We thank an anonymous referee for prompt
and constructive comments. G. D. acknowledges support from NASA Outer
Planets Research Program grant 202844.02.02.01.75 and from NASA Origins
of Solar Systems Program grants NNX11AD20G, NNX11AK54G, and NNX14AG92G.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center.
NR 118
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 203
DI 10.1088/0004-637X/806/2/203
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500058
ER
PT J
AU Gao, P
Hu, RY
Robinson, TD
Li, C
Yung, YL
AF Gao, Peter
Hu, Renyu
Robinson, Tyler D.
Li, Cheng
Yung, Yuk L.
TI STABILITY OF CO2 ATMOSPHERES ON DESICCATED M DWARF EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: physical
evolution; planets and satellites: terrestrial planets
ID IDEAL-GAS STATE; MARTIAN ATMOSPHERE; CARBON-DIOXIDE; HETEROGENEOUS
CHEMISTRY; THERMODYNAMIC FUNCTIONS; EARTH OBSERVATIONS; PLANETS;
ABSORPTION; OXYGEN; OZONE
AB We investigate the chemical stability of CO2-dominated atmospheres of desiccated M dwarf terrestrial exoplanets using a one-dimensional photochemical model. Around Sun-like stars, CO2 photolysis by Far-UV (FUV) radiation is balanced by recombination reactions that depend on water abundance. Planets orbiting M dwarf stars experience more FUV radiation, and could be depleted in water due to M dwarfs' prolonged, high-luminosity pre-main sequences. We show that, for water-depleted M dwarf terrestrial planets, a catalytic cycle relying on H2O2 photolysis can maintain a CO2 atmosphere. However, this cycle breaks down for atmospheric hydrogen mixing ratios < 1 ppm, resulting in similar to 40% of the atmospheric CO2 being converted to CO and O-2 on a timescale of 1 Myr. The increased O-2 abundance leads to high O-3 concentrations, the photolysis of which forms another CO(2)regenerating catalytic cycle. For atmospheres with < 0.1 ppm hydrogen, CO2 is produced directly from the recombination of CO and O. These catalytic cycles place an upper limit of similar to 50% on the amount of CO2 that can be destroyed via photolysis, which is enough to generate Earth-like abundances of (abiotic) O-2 and O-3. The conditions that lead to such high oxygen levels could be widespread on planets in the habitable zones of M dwarfs. Discrimination between biological and abiotic O-2 and O-3 in this case can perhaps be accomplished by noting the lack of water features in the reflectance and emission spectra of these planets, which necessitates observations at wavelengths longer than 0.95 mu m.
C1 [Gao, Peter; Hu, Renyu; Li, Cheng; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Gao, Peter] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
[Hu, Renyu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Robinson, Tyler D.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Robinson, Tyler D.] Oak Ridge Associated Univ, Oak Ridge, TN 37830 USA.
RP Gao, P (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM pgao@caltech.edu
OI Gao, Peter/0000-0002-8518-9601; Li, Cheng/0000-0002-8280-3119
FU Venus Express program via NASA [NNX10AP80G]; NASA through the NASA
Astrobiology Institute [NNH12ZDA002C]; NASA [NNA13AA93A, 51332, NAS
5-26555]; Space Telescope Science Institute; National Aeronautics and
Space Administration
FX We thank K. Willacy, M. Allen, and R. L. Shia for assistance with the
setting up and running of the KinetgenX code. We thank V. Meadows and R.
Barnes for their valuable inputs. This research was supported in part by
the Venus Express program via NASA NNX10AP80G grant to the California
Institute of Technology, and was performed as part of the NASA
Astrobiology Institute's Virtual Planetary Laboratory Lead Team,
supported by NASA through the NASA Astrobiology Institute under
solicitation NNH12ZDA002C and Cooperative Agreement Number NNA13AA93A.
Support for R.H.'s work was provided in part by NASA through Hubble
Fellowship grant #51332 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. 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 57
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 249
DI 10.1088/0004-637X/806/2/249
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500104
ER
PT J
AU Guo, F
Liu, YH
Daughton, W
Li, H
AF Guo, Fan
Liu, Yi-Hsin
Daughton, William
Li, Hui
TI PARTICLE ACCELERATION AND PLASMA DYNAMICS DURING MAGNETIC RECONNECTION
IN THE MAGNETICALLY DOMINATED REGIME
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; galaxies: jets; gamma-ray burst: general;
magnetic reconnection; pulsars: general; relativistic processes
ID GAMMA-RAY BURSTS; HYPERBOLIC FLUX TUBES; ELECTRON ACCELERATION;
CRAB-NEBULA; PULSAR WIND; MAGNETOHYDRODYNAMIC SIMULATIONS; RELATIVISTIC
RECONNECTION; NONTHERMAL PARTICLES; EXTRAGALACTIC JETS; SIGMA-PROBLEM
AB Magnetic reconnection is thought to be the driver for many explosive phenomena in the universe. The energy release and particle acceleration during reconnection have been proposed as a mechanism for producing high-energy emissions and cosmic rays. We carry out two- and three-dimensional (3D) kinetic simulations to investigate relativistic magnetic reconnection and the associated particle acceleration. The simulations focus on electron-positron plasmas starting with a magnetically dominated, force-free current sheet (sigma equivalent to B-2/(4 pi n(e)m(e)c(2)) >> 1). For this limit, we demonstrate that relativistic reconnection is highly efficient at accelerating particles through a first-order Fermi process accomplished by the curvature drift of particles along the electric field induced by the relativistic flows. This mechanism gives rise to the formation of hard power-law spectra f proportional to (gamma - 1)(-p) and approaches p = 1 for sufficiently large sigma and system size. Eventually most of the available magnetic free energy is converted into nonthermal particle kinetic energy. An analytic model is presented to explain the key results and predict a general condition for the formation of power-law distributions. The development of reconnection in these regimes leads to relativistic inflow and outflow speeds and enhanced reconnection rates relative to nonrelativistic regimes. In the 3D simulation, the interplay between secondary kink and tearing instabilities leads to strong magnetic turbulence, but does not significantly change the energy conversion, reconnection rate, or particle acceleration. This study suggests that relativistic reconnection sites are strong sources of nonthermal particles, which may have important implications for a variety of high-energy astrophysical problems.
C1 [Guo, Fan; Daughton, William; Li, Hui] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Liu, Yi-Hsin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Guo, F (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
EM guofan.ustc@gmail.com
RI Daughton, William/L-9661-2013; Guo, Fan/H-1723-2013;
OI Guo, Fan/0000-0003-4315-3755
FU DOE through LDRD program at LANL; DOE/OFES; CMSO; NASA through
Heliospheric Theory Program; NSF [OCI 07-25070]
FX We gratefully acknowledge useful discussions with and comments from
Andrey Beresnyak, Xuhui Chen, Wei Cui, Wei Deng, Brenda Dingus, Jim
Drake, Joe Giacalone, Dimitrios Giannios, Serguei Komissarov, Pawan
Kumar, Xiaocan Li, Maxim Lyutikov, Rob Preece, Marc Swisdak, Alexander
Tchekhovskoy, Dmitri Uzdensky, Yajie Yuan, Gary Zank, Bing Zhang, and
Haocheng Zhang. This work is supported by the DOE through the LDRD
program at LANL and DOE/OFES support to LANL in collaboration with CMSO,
and by NASA through the Heliospheric Theory Program. The research is
part of the Blue Waters sustained-petascale computing project, which is
supported by the NSF (Grant No. OCI 07-25070) and the state of Illinois.
Additional simulations were performed at the National Center for
Computational Sciences at ORNL and with LANL institutional computing.
NR 101
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 167
DI 10.1088/0004-637X/806/2/167
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500022
ER
PT J
AU Haynes, K
Mandell, AM
Madhusudhan, N
Deming, D
Knutson, H
AF Haynes, Korey
Mandell, Avi M.
Madhusudhan, Nikku
Deming, Drake
Knutson, Heather
TI SPECTROSCOPIC EVIDENCE FOR A TEMPERATURE INVERSION IN THE DAYSIDE
ATMOSPHERE OF HOT JUPITER WASP-33b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric; techniques:
spectroscopic
ID HUBBLE-SPACE-TELESCOPE; COLLISION-INDUCED ABSORPTION; HD 209458B;
THERMAL INVERSIONS; GIANT PLANETS; TRANSMISSION SPECTRUM;
INFRARED-EMISSION; SECONDARY ECLIPSE; C/O RATIO; EXOPLANET
AB We present observations of two occultations of the extrasolar planet WASP-33b using the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope, which allow us to constrain the temperature structure and composition of its dayside atmosphere. WASP-33b is the most highly irradiated hot Jupiter discovered to date, and the only exoplanet known to orbit a delta-Scuti star. We observed in spatial scan mode to decrease instrument systematic effects in the data, and removed fluctuations in the data due to stellar pulsations. The rms for our final, binned spectrum is 1.05 times the photon noise. We compare our final spectrum, along with previously published photometric data, to atmospheric models of WASP-33b spanning a wide range in temperature profiles and chemical compositions. We find that the data require models with an oxygen-rich chemical composition and a temperature profile that increases at high altitude. We find that our measured spectrum displays an excess in the measured flux toward short wavelengths that is best explained as emission from TiO. If confirmed by additional measurements at shorter wavelengths, this planet would become the first hot Jupiter with a thermal inversion that can be definitively attributed to the presence of TiO in its dayside atmosphere.
C1 [Haynes, Korey; Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Haynes, Korey] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Haynes, K (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM khaynes0112@gmail.com
FU NASA [NAS 5-26555]; NASA through Space Telescope Science Institute; NASA
Astrophysics Data Analysis Program; [GO-12495]
FX The authors would like to thank the anonymous referee for thoughtful
comments that improved the paper. This work is based on observations
made with the NASA/ESA Hubble Space Telescope that were 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 GO-12495.
Support for this work was provided by NASA through a grant from the
Space Telescope Science Institute, with additional support for data
analysis provided by a grant from the NASA Astrophysics Data Analysis
Program (for K.H. and A.M.M.).
NR 55
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
IS 2
AR 146
DI 10.1088/0004-637X/806/2/146
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500001
ER
PT J
AU Keck, ML
Brenneman, LW
Ballantyne, DR
Bauer, F
Boggs, SE
Christensen, FE
Craig, WW
Dauser, T
Elvis, M
Fabian, AC
Fuerst, F
Garcia, J
Grefenstette, BW
Hailey, CJ
Harrison, FA
Madejski, G
Marinucci, A
Matt, G
Reynolds, CS
Stern, D
Walton, DJ
Zoghbi, A
AF Keck, M. L.
Brenneman, L. W.
Ballantyne, D. R.
Bauer, F.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Dauser, T.
Elvis, M.
Fabian, A. C.
Fuerst, F.
Garcia, J.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Madejski, G.
Marinucci, A.
Matt, G.
Reynolds, C. S.
Stern, D.
Walton, D. J.
Zoghbi, A.
TI NUSTAR AND SUZAKU X-RAY SPECTROSCOPY OF NGC 4151: EVIDENCE FOR
REFLECTION FROM THE INNER ACCRETION DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
galaxies: individual (NGC 4151); galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-4151; BLACK-HOLE SPIN;
BROAD-BAND SPECTRUM; NARROW-LINE REGION; DEEP CHANDRA ACIS; XMM-NEWTON;
SWIFT J2127.4+5654; EMISSION-LINES; IRON LINES
AB We present X-ray timing and spectral analyses of simultaneous 150 ks Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku X-ray observations of the Seyfert 1.5 galaxy NGC 4151. We disentangle the continuum emission, absorption, and reflection properties of the active galactic nucleus (AGN) by applying inner accretion disk reflection and absorption-dominated models. With a time-averaged spectral analysis, we find strong evidence for relativistic reflection from the inner accretion disk. We find that relativistic emission arises from a highly ionized inner accretion disk with a steep emissivity profile, which suggests an intense, compact illuminating source. We find a preliminary, near-maximal black hole spin a > 0.9 accounting for statistical and systematic modeling errors. We find a relatively moderate reflection fraction with respect to predictions for the lamp post geometry, in which the illuminating corona is modeled as a point source. Through a time-resolved spectral analysis, we find that modest coronal and inner disk reflection (IDR) flux variation drives the spectral variability during the observations. We discuss various physical scenarios for the IDR model and we find that a compact corona is consistent with the observed features.
C1 [Keck, M. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Keck, M. L.; Brenneman, L. W.; Elvis, M.; Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, F.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Bauer, F.] 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, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Walton, D. J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Marinucci, A.; Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zoghbi, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Keck, ML (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM keckm@bu.edu
RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; Zoghbi,
Abderahmen/A-8445-2017;
OI Boggs, Steven/0000-0001-9567-4224; Zoghbi,
Abderahmen/0000-0002-0572-9613; Ballantyne, David/0000-0001-8128-6976
FU NASA [NNG08FD60C, NNX13AE90G]; National Aeronautics and Space
Administration; Italian Space Agency under ASI/INAF [I/037/12/0-011/13];
European Union [n.312789]; NASA-ADAP [NNX14AF86G, NNX14AF89G];
CONICYT-Chile (Basal-CATA) [PFB-06/2007]; CONICYT-Chile (FONDECYT)
[1141218]; CONICYT-Chile (Anillo) [ACT1101]; ICM [IC120009]
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. This
research made use of the NuSTAR Data Analysis Software (NuSTAR-DAS)
jointly developed by the ASI Science Data Center (ASDC, Italy) and the
California Institute of Technology (Caltech, USA). M.L.K. gratefully
acknowledges support through NASA grant #NNX13AE90G. G.M. and 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. C.S.R.
acknowledges support from the NASA-ADAP program under grants NNX14AF86G
and NNX14AF89G. F.E.B. acknowledges support from CONICYT-Chile
(Basal-CATA PFB-06/2007, FONDECYT 1141218, Anillo ACT1101) and ICM grant
IC120009, awarded to The Millennium Institute of Astrophysics, MAS. We
thank Alan Marscher for helpful discussions. We thank the anonymous
referee for comments, which have improved this manuscript. This research
made use of Astropy, a community-developed core Python package for
Astronomy (Astropy Collaboration et al. 2013), and Matplotlib (Hunter
2007).
NR 87
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
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AR 149
DI 10.1088/0004-637X/806/2/149
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500004
ER
PT J
AU Kogut, A
Dwek, E
Moseley, SH
AF Kogut, A.
Dwek, E.
Moseley, S. H.
TI SPECTRAL CONFUSION FOR COSMOLOGICAL SURVEYS OF REDSHIFTED C II EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: high-redshift; galaxies: luminosity
function, mass function; galaxies: star formation; line: identification
ID FINE-STRUCTURE LINES; STAR-FORMATION RATE; CII EMISSION; SUBMILLIMETER
GALAXY; EARLY UNIVERSE; MU-M; INTENSITY; REIONIZATION; INDICATOR; CARBON
AB Far-infrared cooling lines are ubiquitous features in the spectra of star-forming galaxies. Surveys of redshifted finestructure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of redshifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencilbeam surveys of redshifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150-1300 mu m wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 mu m [C II] line and other lines. Although the [C II] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [C II] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20 ''. and 10 ', sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources.
C1 [Kogut, A.; Dwek, E.; Moseley, S. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Alan.J.Kogut@nasa.gov
OI Kogut, Alan/0000-0001-9835-2351
FU NASA's Science Innovation Fund
FX We thank D. Leisawitz for encouraging the development of the
simulations. Support for this research came from NASA's Science
Innovation Fund.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
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AR 234
DI 10.1088/0004-637X/806/2/234
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500089
ER
PT J
AU Lien, A
Sakamoto, T
Gehrels, N
Palmer, DM
Barthelmy, SD
Graziani, C
Cannizzo, JK
AF Lien, Amy
Sakamoto, Takanori
Gehrels, Neil
Palmer, David M.
Barthelmy, Scott D.
Graziani, Carlo
Cannizzo, John K.
TI PROBING THE COSMIC GAMMA-RAY BURST RATE WITH TRIGGER SIMULATIONS OF THE
SWIFT BURST ALERT TELESCOPE (vol 783, pg 24, 2014)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Lien, Amy; Cannizzo, John K.] CRESST, Greenbelt, MD 20771 USA.
[Lien, Amy; Gehrels, Neil; Barthelmy, Scott D.; Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lien, Amy; Cannizzo, John K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Sakamoto, Takanori] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan.
[Palmer, David M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Graziani, Carlo] Univ Chicago, Dept Astron, Chicago, IL 60637 USA.
[Graziani, Carlo] Univ Chicago, Flash Ctr Computat Sci, Chicago, IL 60637 USA.
RP Lien, A (reprint author), CRESST, Greenbelt, MD 20771 USA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
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AR 276
DI 10.1088/0004-637X/806/2/276
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500131
ER
PT J
AU Matson, RA
Gies, DR
Guo, Z
Quinn, SN
Buchhave, LA
Latham, DW
Howell, SB
Rowe, JF
AF Matson, Rachel A.
Gies, Douglas R.
Guo, Zhao
Quinn, Samuel N.
Buchhave, Lars A.
Latham, David W.
Howell, Steve B.
Rowe, Jason F.
TI HST/COS DETECTION OF THE SPECTRUM OF THE SUBDWARF COMPANION OF KOI-81
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; stars: evolution; stars: individual (KOI-81);
subdwarfs
ID MASS WHITE-DWARFS; TOMOGRAPHIC SEPARATION; ULTRAVIOLET DETECTION;
COMPOSITE SPECTRA; COMPACT OBJECTS; MAIN-SEQUENCE; BINARY-SYSTEM;
PHI-PERSEI; STARS; DISCOVERY
AB KOI-81 is a totally eclipsing binary discovered by the Kepler mission that consists of a rapidly rotating B-type star and a small, hot companion. The system was forged through large-scale mass transfer that stripped the mass donor of its envelope and spun up the mass gainer star. We present an analysis of UV spectra of KOI-81 that were obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope that reveal for the first time the spectral features of the faint, hot companion. We present a double-lined spectroscopic orbit for the system that yields mass estimates of 2.92 M-circle dot and 0.19 M-circle dot for the B-star and hot subdwarf, respectively. We used a Doppler tomography algorithm to reconstruct the UV spectra of the components, and a comparison of the reconstructed and model spectra yields effective temperatures of 12 and 19-27 kK for the B-star and hot companion, respectively. The B-star is pulsating, and we identified a number of peaks in the Fourier transform of the light curve, including one that may indicate an equatorial rotation period of 11.5 hr. The B-star has an equatorial velocity that is 74% of the critical velocity where centrifugal and gravitational accelerations balance at the equator, and we fit the transit light curve by calculating a rotationally distorted model for the photosphere of the B-star.
C1 [Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[Buchhave, Lars A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Howell, Steve B.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
RP Matson, RA (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 5060, Atlanta, GA 30302 USA.
EM rmatson@chara.gsu.edu; gies@chara.gsu.edu; guo@chara.gsu.edu;
quinn@astro.gsu.edu; lbuchhave@cfa.harvard.edu; dlatham@cfa.harvard.edu;
steve.b.howell@nasa.gov; Jason.Rowe@nasa.gov
OI Buchhave, Lars A./0000-0003-1605-5666; Gies,
Douglas/0000-0001-8537-3583; Latham, David/0000-0001-9911-7388
FU NASA through Space Telescope Science Institute [12288]; NASA [NAS
5-26555]; National Science Foundation [AST-1411654]; GSU ACI Fellowship;
GSU College of Arts and Sciences; Research Program Enhancement fund of
the Board of Regents of the University System of Georgia
FX We are grateful to Charles Proffitt and Denise Taylor of STScI for their
aid in planning the observations with HST. Support for program #12288
was provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. This
material is also based upon work supported by the National Science
Foundation under Grant No. AST-1411654. Institutional support has been
provided from a GSU ACI Fellowship (RAM), the GSU College of Arts and
Sciences, and the Research Program Enhancement fund of the Board of
Regents of the University System of Georgia, administered through the
GSU Office of the Vice President for Research and Economic Development.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
VL 806
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AR 155
DI 10.1088/0004-637X/806/2/155
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500010
ER
PT J
AU Nitta, NV
Mason, GM
Wang, LH
Cohen, CMS
Wiedenbeck, ME
AF Nitta, Nariaki V.
Mason, Glenn M.
Wang, Linghua
Cohen, Christina M. S.
Wiedenbeck, Mark E.
TI SOLAR SOURCES OF He-3-RICH SOLAR ENERGETIC PARTICLE EVENTS IN SOLAR
CYCLE 24
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: flares; Sun: magnetic fields; Sun: particle emission;
Sun: UV radiation
ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; IMPULSIVE
ELECTRON EVENTS; III RADIO-BURSTS; MAGNETIC-FIELD; ISOTOPE SPECTROMETER;
WIND SPACECRAFT; FLARES; ACCELERATION; PLASMA
AB Using high-cadence EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, we investigate the solar sources of 26 He-3-rich solar energetic particle events at. less than or similar to 1 MeV nucleon(-1) that were well-observed by the Advanced Composition Explorer during solar cycle 24. Identification of the solar sources is based on the association of He-3-rich events with type III radio bursts and electron events as observed by Wind. The source locations are further verified in EUV images from the Solar and Terrestrial Relations Observatory, which provides information on solar activities in the regions not visible from the Earth. Based on AIA observations, He-3-rich events are not only associated with coronal jets as emphasized in solar cycle 23 studies, but also with more spatially extended eruptions. The properties of the He-3-rich events do not appear to be strongly correlated with those of the source regions. As in the previous studies, the magnetic connection between the source region and the observer is not always reproduced adequately by the simple potential field source surface model combined with the Parker spiral. Instead, we find a broad longitudinal distribution of the source regions extending well beyond the west limb, with the longitude deviating significantly from that expected from the observed solar wind speed.
C1 [Nitta, Nariaki V.] Lockheed Martin Adv Technol Ctr, Dept A021S, Palo Alto, CA 94304 USA.
[Mason, Glenn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wang, Linghua] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China.
[Cohen, Christina M. S.] CALTECH, Pasadena, CA 91125 USA.
[Wiedenbeck, Mark E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nitta, NV (reprint author), Lockheed Martin Adv Technol Ctr, Dept A021S, B-252,3251 Hanover St, Palo Alto, CA 94304 USA.
EM nitta@lmsal.com; glenn.mason@jhuapl.edu; wanglhwang@gmail.com;
cohen@srl.caltech.edu; mark.e.wiedenbeck@jpl.nasa.gov
RI Wang, Linghua/C-4938-2014
OI Wang, Linghua/0000-0001-7309-4325
FU NSF [AGS-1259549, 1156138/112111]; NASA [NNX10AQ68G, NNX10AT75G,
44A-1089749, NNX11A075G, NNX13AH66G]; NASA AIA contract [NNG04EA00C];
NASA STEREO mission under NRL [N00173-02-C-2035]; UC Berkeley under NASA
[SA2715-26309, NAS5-03131 T]
FX We thank the referee for finding and correcting some problems in the
original manuscript. This work has been supported by the NSF grant
AGS-1259549, NASA grant NNX10AQ68G, NASA AIA contract NNG04EA00C and the
NASA STEREO mission under NRL Contract No. N00173-02-C-2035. GMM
acknowledges NASA grant NNX10AT75G, 44A-1089749, and NSF grant
1156138/112111. C.M.S.C. and M.E.W. acknowledge support at Caltech and
JPL from subcontract SA2715-26309 from UC Berkeley under NASA contract
NAS5-03131 T, and by NASA grants NNX11A075G and NNX13AH66G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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AR 235
DI 10.1088/0004-637X/806/2/235
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500090
ER
PT J
AU Schnittman, JD
AF Schnittman, Jeremy D.
TI THE DISTRIBUTION AND ANNIHILATION OF DARK MATTER AROUND BLACK HOLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; black hole physics; relativistic processes
ID PENROSE MECHANISM; CONSTRAINTS; RADIATION; GALAXIES
AB We use a Monte Carlo code to calculate the geodesic orbits of test particles around Kerr black holes, generating a distribution function of both bound and unbound populations of dark matter (DM) particles. From this distribution function, we calculate annihilation rates and observable gamma-ray spectra for a few simple DM models. The features of these spectra are sensitive to the black hole spin, observer inclination, and detailed properties of the DM annihilation cross-section and density profile. Confirming earlier analytic work, we find that for rapidly spinning black holes, the collisional Penrose process can reach efficiencies exceeding 600%, leading to a high-energy tail in the annihilation spectrum. The high particle density and large proper volume of the region immediately surrounding the horizon ensures that the observed flux from these extreme events is non-negligible.
C1 [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schnittman, Jeremy D.] Joint Space Sci Inst, College Pk, MD 20742 USA.
RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jeremy.schnittman@nasa.gov
FU NASA [ATP12-0139, ATP13-0077]
FX This work was partially supported by NASA grants ATP12-0139 and
ATP13-0077. We thank Alessandra Buonanno, Francesc Ferrer, Ted Jacobson,
Henric Krawczynski, Tzvi Piran, Laleh Sadeghian, and Joe Silk for
helpful comments and discussion.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2015
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AR 264
DI 10.1088/0004-637X/806/2/264
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500119
ER
PT J
AU Ursino, E
Galeazzi, M
Gupta, A
Kelley, RL
Mitsuishi, I
Ohashi, T
Sato, K
AF Ursino, E.
Galeazzi, M.
Gupta, A.
Kelley, R. L.
Mitsuishi, I.
Ohashi, T.
Sato, K.
TI EXPLORING THE BRIDGE BETWEEN A3556 AND A3558 IN THE SHAPLEY SUPERCLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; intergalactic medium; large-scale structure of
universe; X-rays: diffuse background
ID HOT INTERGALACTIC MEDIUM; X-RAY-ABSORPTION; GALAXY CLUSTERS; MISSING
BARYONS; MASS; CHANDRA; FILAMENT; ABSORBERS; CORE; GAS
AB Looking at the region connecting two clusters is a promising way to identify and study the Warm-Hot Intergalactic Medium. Observations show that the spectrum of the bridge between A3556 and A3558 has a stronger soft X-ray emission than the nearby region. Suzaku. observations could not discriminate the origin of the extra emission. In this work we analyze a dedicated Chandra. observation of the same target to identify point sources and characterize the background emission in the bridge. We find that the count number of the point sources is much higher than average field population (using CDFS 4Ms as a reference). Moreover, the shape of the cumulative distribution resembles that of galaxy distribution suggesting that the point sources are galaxies in a filament. The Suzaku. extra emission is well explained by the high abundance of point sources identified by Chandra. Furthermore, we used optical/ IR observations of point sources in the same field to estimate the density of the putative filament as rho approximate to 150 rho(b), below Suzaku. sensitivity.
C1 [Ursino, E.; Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33155 USA.
[Gupta, A.] Columbus State Community Coll, Dept Biol & Phys Sci, Columbus, OH 43215 USA.
[Gupta, A.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kelley, R. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mitsuishi, I.] Nagoya Univ, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.
[Ohashi, T.] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan.
[Sato, K.] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan.
RP Ursino, E (reprint author), Univ Miami, Dept Phys, Coral Gables, FL 33155 USA.
EM galeazzi@physics.miami.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Ursino, Eugenio /0000-0002-2567-2036
FU SAO award [GO1-12179X]
FX This work has been supported in part by SAO award #GO1-12179X. The
authors would like to thank R. K. Smith and W. Liu for the useful
discussion and suggestions.
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
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AR 211
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PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7DA
UT WOS:000357129500066
ER
PT J
AU Furst, F
Pottschmidt, K
Miyasaka, H
Bhalerao, V
Bachetti, M
Boggs, SE
Christensen, FE
Craig, WW
Grinberg, V
Hailey, CJ
Harrison, FA
Kennea, JA
Rahoui, F
Stern, D
Tendulkar, SP
Tomsick, JA
Walton, DJ
Wilms, J
Zhang, WW
AF Fuerst, F.
Pottschmidt, K.
Miyasaka, H.
Bhalerao, V.
Bachetti, M.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Grinberg, V.
Hailey, C. J.
Harrison, F. A.
Kennea, J. A.
Rahoui, F.
Stern, D.
Tendulkar, S. P.
Tomsick, J. A.
Walton, D. J.
Wilms, J.
Zhang, W. W.
TI DISTORTED CYCLOTRON LINE PROFILE IN CEP X-4 AS OBSERVED BY NuSTAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; radiation: dynamics; stars: neutron; X-rays:
binaries; X-rays: individual (Cep X-4)
ID X-RAY PULSAR; CEPHEUS X-4; RESONANCE FEATURE; GX 304-1; DISCOVERY;
ENERGY; OUTBURST; TELESCOPE; HERCULES-X-1; ABSORPTION
AB We present spectral analysis of Nuclear Spectroscopic Telescope Array and Swift observations of Cep X-4 during its outburst in 2014. We observed the source once during the peak of the outburst and once during the decay, finding good agreement in the spectral shape between the observations. We describe the continuum using a power law with a Fermi-Dirac cutoff at high energies. Cep X-4 has a very strong cyclotron resonant scattering feature (CRSF) around 30 keV. A simple absorption-like line with a Gaussian optical depth or a pseudo-Lorentzian profile both fail to describe the shape of the CRSF accurately, leaving significant deviations at the red side of the line. We characterize this asymmetry with a second absorption feature around 19 keV. The line energy of the CRSF, which is not influenced by the addition of this feature, shows a small but significant positive luminosity dependence. With luminosities between (1-6) x 10(36) erg s(-1), Cep X-4 is below the theoretical limit where such a correlation is expected. This behavior is similar to Vela X-1 and we discuss parallels between the two systems.
C1 [Fuerst, F.; Miyasaka, H.; Harrison, F. A.; Tendulkar, S. P.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Pottschmidt, K.] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, K.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bhalerao, V.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Bachetti, M.] Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
[Boggs, S. E.; Craig, W. W.; Tomsick, J. A.] 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.
[Grinberg, V.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Rahoui, F.] European So Observ, D-85748 Garching, Germany.
[Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
RP Fuerst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015;
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224;
Bachetti, Matteo/0000-0002-4576-9337; Bhalerao,
Varun/0000-0002-6112-7609
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX We thank the anonymous referee for valuable comments. This work was
supported under NASA contract No. NNG08FD60C, and made use of data from
the NuSTAR mission, a project led by the California Institute of
Technology, managed by the Jet Propulsion Laboratory, and funded by the
National Aeronautics and Space Administration. We thank the NuSTAR
Operations, Software and Calibration teams for support with the
execution and analysis of these observations. This research has made use
of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by
the ASI Science Data Center (ASDC, Italy) and the California Institute
of Technology (USA).
NR 36
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 20
PY 2015
VL 806
IS 2
AR L24
DI 10.1088/2041-8205/806/2/L24
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2KO
UT WOS:000356772700003
ER
PT J
AU Pulkkinen, A
Bernabeu, E
Eichner, J
Viljanen, A
Ngwira, C
AF Pulkkinen, Antti
Bernabeu, Emanuel
Eichner, Jan
Viljanen, Ari
Ngwira, Chigomezyo
TI Regional-scale high-latitude extreme geoelectric fields pertaining to
geomagnetically induced currents
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE Geomagnetically induced currents; Extreme events; Spatial scales
ID ELECTRIC-FIELDS; SURFACE; STORM; EARTH
AB Motivated by the needs of the high-voltage power transmission industry, we use data from the high-latitude IMAGE magnetometer array to study characteristics of extreme geoelectric fields at regional scales. We use 10-s resolution data for years 1993-2013, and the fields are characterized using average horizontal geoelectric field amplitudes taken over station groups that span about 500-km distance. We show that geoelectric field structures associated with localized extremes at single stations can be greatly different from structures associated with regionally uniform geoelectric fields, which are well represented by spatial averages over single stations. Visual extrapolation and rigorous extreme value analysis of spatially averaged fields indicate that the expected range for 1-in-100-year extreme events are 3-8 V/km and 3.4-7.1 V/km, respectively. The Quebec reference ground model is used in the calculations.
C1 [Pulkkinen, Antti; Ngwira, Chigomezyo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bernabeu, Emanuel] PJM Interconnect, Audubon, PA USA.
[Eichner, Jan] Munich Re, Geo Risks Res, Munich, Germany.
[Viljanen, Ari] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Ngwira, Chigomezyo] Catholic Univ Amer, Washington, DC 20064 USA.
RP Pulkkinen, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM antti.a.pulkkinen@nasa.gov
FU EU's 7th Framework Programme (FP7) [260330 (EURISGIC)]
FX We thank the institutes who maintain the IMAGE magnetometer array. The
IMAGE array data used in this paper are publicly available at
http://space.fmi.fi/image. We acknowledge discussions with Drs L. Marti
(Hydro One), R. Horton (Southern Company), as well as with Mr. F. Koza
(PJM) and Mr M. Olson (NERC). The work of A.V. was partially supported
from the EU's 7th Framework Programme (FP7/2007-2013) under grant
agreement no. 260330 (EURISGIC).
NR 22
TC 8
Z9 8
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD JUN 19
PY 2015
VL 67
BP 1
EP 8
AR 93
DI 10.1186/s40623-015-0255-6
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CL4HX
UT WOS:000356914300001
ER
PT J
AU Werner, MW
Soifer, BT
Lombardi, LS
Helou, G
AF Werner, M. W.
Soifer, B. T.
Lombardi, L. Storrie
Helou, G.
TI Spitzer's stellar work
SO SCIENCE
LA English
DT Letter
C1 [Werner, M. W.] CALTECH, Jet Prop Lab, Spitzer Space Telescope, Pasadena, CA 91109 USA.
[Soifer, B. T.; Lombardi, L. Storrie; Helou, G.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Werner, MW (reprint author), CALTECH, Jet Prop Lab, Spitzer Space Telescope, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mww@ipac.caltech.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
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 JUN 19
PY 2015
VL 348
IS 6241
BP 1326
EP 1326
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CK7XK
UT WOS:000356449500036
PM 26089504
ER
PT J
AU Jontof-Hutter, D
Rowe, JF
Lissauer, JJ
Fabrycky, DC
Ford, EB
AF Jontof-Hutter, Daniel
Rowe, Jason F.
Lissauer, Jack J.
Fabrycky, Daniel C.
Ford, Eric B.
TI The mass of the Mars-sized exoplanet Kepler-138 b from transit timing
SO NATURE
LA English
DT Article
ID LOW-DENSITY PLANETS; CHAIN MONTE-CARLO; SUN-LIKE STAR; 1ST 16 MONTHS;
LIGHT-CURVE; DIFFERENTIAL EVOLUTION; EXTRASOLAR PLANETS; CANDIDATES;
SYSTEM; ORBITS
AB Extrasolar planets that pass in front of their host star (transit) cause a temporary decrease in the apparent brightness of the star, providing a direct measure of the planet's size and orbital period. In some systems with multiple transiting planets, the times of the transits are measurably affected by the gravitational interactions between neighbouring planets(1,2). In favourable cases, the departures from Keplerian orbits (that is, unaffected by gravitational effects) implied by the observed transit times permit the planetary masses to be measured, which is key to determining their bulk densities(3). Characterizing rocky planets is particularly difficult, because they are generally smaller and less massive than gaseous planets. Therefore, few exoplanets near the size of Earth have had their masses measured. Here we report the sizes and masses of three planets orbiting Kepler-138, a star much fainter and cooler than the Sun. We determine that the mass of the Mars-sized inner planet, Kepler-138 b, is 0.066(-0.037)(+0.059) Earth masses. Its density is 2.6(-1.5)(+2.4) grams per cubic centimetre. The middle and outer planets are both slightly larger than Earth. The middle planet's density (6.2(-3.4)(+5.8) grams per cubic centimetre) is similar to that of Earth, and the outer planet is less than half as dense at 2.1(-1.2)(+2.2) grams per cubic centimetre, implying that it contains a greater portion of low-density components such as water and hydrogen.
C1 [Jontof-Hutter, Daniel; Ford, Eric B.] Penn State Univ, Dept Astron, Davey Lab, University Pk, PA 16802 USA.
[Jontof-Hutter, Daniel; Rowe, Jason F.; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
RP Jontof-Hutter, D (reprint author), Penn State Univ, Dept Astron, Davey Lab, University Pk, PA 16802 USA.
EM dxj14@psu.edu
OI Fabrycky, Daniel/0000-0003-3750-0183
FU NASA Postdoctoral Program; Center for Exoplanets and Habitable Worlds;
Pennsylvania State University; Eberly College of Science; Pennsylvania
Space Grant Consortium; NASA [NNX14AB92G]; Kepler Participating
Scientist Program award [NNX14AB87G]; NASA Kepler Participating
Scientist Program award [NNX14AN76G]; NASA Exoplanet Research Program
award [NNX15AE21G]
FX D.J-H. acknowledges support through the NASA Postdoctoral Program and
funding from the Center for Exoplanets and Habitable Worlds. The Center
for Exoplanets and Habitable Worlds is supported by the Pennsylvania
State University, the Eberly College of Science and the Pennsylvania
Space Grant Consortium. J.F.R. acknowledges NASA grant NNX14AB92G issued
through the Kepler Participating Scientist Program. D.C.F. is an Alfred
P. Sloane Fellow and was supported by the Kepler Participating Scientist
Program award NNX14AB87G. E.B.F. was supported in part by NASA Kepler
Participating Scientist Program award NNX14AN76G and NASA Exoplanet
Research Program award NNX15AE21G, as well as the Center for Exoplanets
and Habitable Worlds.
NR 56
TC 19
Z9 19
U1 1
U2 9
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 JUN 18
PY 2015
VL 522
IS 7556
BP 321
EP +
DI 10.1038/nature14494
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CK7PU
UT WOS:000356425400048
PM 26085271
ER
PT J
AU Hornbuckle, BC
Sasaki, TT
Bigelow, GS
Noebe, RD
Weaver, ML
Thompson, GB
AF Hornbuckle, B. C.
Sasaki, T. T.
Bigelow, G. S.
Noebe, R. D.
Weaver, M. L.
Thompson, G. B.
TI Structure-property relationships in a precipitation strengthened
Ni-29.7Ti-20Hf (at%) shape memory alloy
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Nitinol; Precipitation strengthening; NiTiHf; Microstructural
characterization; Atom probe tomography
ID MARTENSITIC-TRANSFORMATION; PHASE; NITI; MICROSTRUCTURE; BEHAVIOR
AB The martensitic transformation temperatures, load-biased thermomechanical properties, and microstructure (characterized by transmission electron microscopy and atom probe tomography) were investigated for a Ni-29.7Ti-20Hf (at%) alloy aged at 550 degrees C for 0-300 h. Aging for three hours and longer resulted in the precipitation of a face-centered orthorhombic phase, previously denoted as the H-phase. The number density, size, and composition of this phase did not change significantly upon aging from 3 to 30 h. However, continued aging to 300 h resulted in a decrease in the number density and significant coarsening of the precipitates at 550 degrees C. The alloy exhibited near optimum response for shape memory behavior and dimensional stability after aging for three hours, though transformation temperatures continued to increase with aging time. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Hornbuckle, B. C.; Sasaki, T. T.; Weaver, M. L.; Thompson, G. B.] Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA.
[Bigelow, G. S.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Thompson, GB (reprint author), Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA.
EM gthompson@eng.ua.edu
FU NASA [NNX09AO61A]; Transformative Aeronautics Concepts Program,
Transformational Tools & Technologies Project
FX The authors gratefully acknowledge funding for this research under the
NASA Grant NNX09AO61A and from the Transformative Aeronautics Concepts
Program, Transformational Tools & Technologies Project (Dale Hopkins,
Technical Lead for Structures & Materials Discipline). UA's Central
Analytical Facility (www.caf.ua.edu) is recognized for additional
support and access to the microscopes used in this study. Also, Dr. M.
Moody is thanked for helpful discussions on atom probe analysis.
NR 34
TC 6
Z9 6
U1 5
U2 14
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 JUN 18
PY 2015
VL 637
BP 63
EP 69
DI 10.1016/j.msea.2015.03.123
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA CK4QF
UT WOS:000356207600008
ER
PT J
AU Gopalswamy, N
Tsurutani, B
Yan, YH
AF Gopalswamy, Nat
Tsurutani, Bruce
Yan, Yihua
TI Short-term variability of the Sun-Earth system: an overview of progress
made during the CAWSES-II period
SO PROGRESS IN EARTH AND PLANETARY SCIENCE
LA English
DT Review
DE Solar activity; Space weather; Coronal mass ejections; Flares; Solar
energetic particle events; Geospace impact; Geomagnetic storms
ID CORONAL MASS EJECTIONS; SOLAR-CYCLE 24; ENERGETIC PARTICLE EVENTS;
GROUND-LEVEL ENHANCEMENT; EXTREME-ULTRAVIOLET WAVE; MAGNETIC-FLUX ROPES;
RELATIVISTIC ELECTRON ACCELERATION; DST LESS-THAN-OR-EQUAL-TO-50 NT;
PARALLEL INTERPLANETARY SHOCK; ACTIVITY HILDCAA EVENTS
AB This paper presents an overview of results obtained during the CAWSES-II period on the short-term variability of the Sun and how it affects the near-Earth space environment. CAWSES-II was planned to examine the behavior of the solar-terrestrial system as the solar activity climbed to its maximum phase in solar cycle 24. After a deep minimum following cycle 23, the Sun climbed to a very weak maximum in terms of the sunspot number in cycle 24 (MiniMax24), so many of the results presented here refer to this weak activity in comparison with cycle 23. The short-term variability that has immediate consequence to Earth and geospace manifests as solar eruptions from closed-field regions and high-speed streams from coronal holes. Both electromagnetic (flares) and mass emissions (coronal mass ejections - CMEs) are involved in solar eruptions, while coronal holes result in high-speed streams that collide with slow wind forming the so-called corotating interaction regions (CIRs). Fast CMEs affect Earth via leading shocks accelerating energetic particles and creating large geomagnetic storms. CIRs and their trailing high-speed streams (HSSs), on the other hand, are responsible for recurrent small geomagnetic storms and extended days of auroral zone activity, respectively. The latter leads to the acceleration of relativistic magnetospheric 'killer' electrons. One of the major consequences of the weak solar activity is the altered physical state of the heliosphere that has serious implications for the shock-driving and storm-causing properties of CMEs. Finally, a discussion is presented on extreme space weather events prompted by the 23 July 2012 super storm event that occurred on the backside of the Sun. Many of these studies were enabled by the simultaneous availability of remote sensing and in situ observations from multiple vantage points with respect to the Sun-Earth line.
C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Tsurutani, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yan, Yihua] Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
NR 356
TC 7
Z9 7
U1 1
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 2197-4284
J9 PROG EARTH PLANET SC
JI Prog. Earth Planet. Sci.
PD JUN 17
PY 2015
VL 2
AR UNSP 13
DI 10.1186/s40645-015-0043-8
PG 41
WC Geosciences, Multidisciplinary
SC Geology
GA CV0MF
UT WOS:000363944100001
ER
PT J
AU Clement, GP
Bukley, AP
Paloski, WH
AF Clement, Gilles P.
Bukley, Angelia P.
Paloski, William H.
TI Artificial gravity as a countermeasure for mitigating physiological
deconditioning during long-duration space missions
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Review
DE gravity; adaptation; international space station; microgravity;
centrifuge; countermeasure
ID DOWN BED REST; SHORT-RADIUS CENTRIFUGATION; NEGATIVE-PRESSURE EXERCISE;
INDUCED BONE LOSS; SIMULATED MICROGRAVITY; ORTHOSTATIC INTOLERANCE;
ROTATING ENVIRONMENT; LINEAR ACCELERATION; TREADMILL EXERCISE; UPRIGHT
EXERCISE
AB In spite of the experience gained in human space flight since Yuri Gagarin's historical flight in 1961, there has yet to be identified a completely effective countermeasure for mitigating the effects of weightlessness on humans. Were astronauts to embark upon a journey to Mars today, the 6-month exposure to weightlessness en route would leave them considerably debilitated, even with the implementation of the suite of piece meal countermeasures currently employed. Continuous or intermittent exposure to simulated gravitational states on board the spacecraft while traveling to and from Mars, also known as artificial gravity, has the potential for enhancing adaptation to Mars gravity and re adaptation to Earth gravity. Many physiological functions are adversely affected by the weightless environment of spaceflight because they are calibrated for normal, Earth's gravity. Hence, the concept of artificial gravity is to provide a broad-spectrum replacement for the gravitational forces that naturally occur on the Earth's surface, thereby avoiding the physiological deconditioning that takes place in weightlessness. Because researchers have long been concerned by the adverse sensorimotor effects that occur in weightlessness as well as in rotating environments, additional study of the complex interactions among sensorimotor and other physiological systems in rotating environments must be undertaken both on Earth and in space before artificial gravity can be implemented.
C1 [Clement, Gilles P.] Wyle Sci & Engn Grp, Houston, TX 77058 USA.
[Bukley, Angelia P.] Int Space Univ, Arlincton, VA USA.
[Paloski, William H.] NASA, Johnson Space Ctr, Houston, TX USA.
RP Clement, GP (reprint author), Wyle Sci & Engn Grp, 1290 Hercules Ave, Houston, TX 77058 USA.
EM gilles.r.clement@nasa.gov
NR 66
TC 5
Z9 6
U1 1
U2 6
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD JUN 17
PY 2015
VL 9
AR 92
DI 10.3389/fnsys.2015.00092
PG 11
WC Neurosciences
SC Neurosciences & Neurology
GA CU9CY
UT WOS:000363841800001
PM 26136665
ER
PT J
AU Ritchie, LE
Taddeo, SS
Weeks, BR
Lima, F
Bloomfield, SA
Azcarate-Peril, MA
Zwart, SR
Smith, SM
Turner, ND
AF Ritchie, Lauren E.
Taddeo, Stella S.
Weeks, Brad R.
Lima, Florence
Bloomfield, Susan A.
Azcarate-Peril, M. Andrea
Zwart, Sara R.
Smith, Scott M.
Turner, Nancy D.
TI Space Environmental Factor Impacts upon Murine Colon Microbiota and
Mucosal Homeostasis
SO PLOS ONE
LA English
DT Article
ID INFLAMMATORY-BOWEL-DISEASE; LONG-DURATION SPACEFLIGHT; TOLL-LIKE
RECEPTORS; INTESTINAL MICROBIOTA; GUT MICROBIOTA; ULCERATIVE-COLITIS;
GENE-EXPRESSION; IMMUNE-SYSTEM; RADIATION; IRRADIATION
AB Astronaut intestinal health may be impacted by microgravity, radiation, and diet. The aim of this study was to characterize how high and low linear energy transfer (LET) radiation, microgravity, and elevated dietary iron affect colon microbiota (determined by 16S rDNA pyrosequencing) and colon function. Three independent experiments were conducted to achieve these goals: 1) fractionated low LET. radiation (Cs-137, 3 Gy, RAD), high Fe diet (IRON) (650 mg/kg diet), and a combination of low LET. radiation and high Fe diet (IRON+RAD) in male Sprague-Dawley rats; 2) high LET Si-38 particle exposure (0.050 Gy), 1/6 G partial weight bearing (PWB), and a combination of high (LETSi)-Si-38 particle exposure and PWB in female BalbC/ByJ mice; and 3) 13 d spaceflight in female C57BL/6 mice. Low LET radiation, IRON and spaceflight increased Bacteroidetes and decreased Firmicutes. RAD and IRON+RAD increased Lactobacillales and lowered Clostridiales compared to the control (CON) and IRON treatments. Low LET radiation, IRON, and spaceflight did not significantly affect diversity or richness, or elevate pathogenic genera. Spaceflight increased Clostridiales and decreased Lactobacillales, and similar trends were observed in the experiment using a ground-based model of microgravity, suggesting altered gravity may affect colonic microbiota. Although we noted no differences in colon epithelial injury or inflammation, spaceflight elevated TGF beta gene expression. Microbiota and mucosal characterization in these models is a first step in understanding the impact of the space environment on intestinal health.
C1 [Ritchie, Lauren E.; Turner, Nancy D.] Texas A&M Univ, Intercollegiate Fac Genet, College Stn, TX 77843 USA.
[Taddeo, Stella S.; Turner, Nancy D.] Texas A&M Univ, Nutr & Food Sci Dept, College Stn, TX USA.
[Weeks, Brad R.] Texas A&M Univ, Dept Vet Pathobiol, College Stn, TX USA.
[Lima, Florence] Univ Kentucky, Dept Med, Div Nephrol, Lexington, KY 40506 USA.
[Bloomfield, Susan A.] Texas A&M Univ, Dept Hlth & Kinesiol, College Stn, TX USA.
[Azcarate-Peril, M. Andrea] Univ N Carolina, Sch Med, Dept Cell Biol & Physiol, Chapel Hill, NC USA.
[Zwart, Sara R.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA.
RP Turner, ND (reprint author), Texas A&M Univ, Intercollegiate Fac Genet, College Stn, TX 77843 USA.
EM n-turner@tamu.edu
FU NASA; National Institutes of Health/National Institute of Diabetes and
Digestive and Kidney Diseases [P30 DK34987]; National Space Biomedical
Research Institute [NCC 9-58]
FX This study was funded by the NASA Human Research Program's Human Health
Countermeasures Element by a grant to SRZ, SMS, and NDT; a National
Institutes of Health/National Institute of Diabetes and Digestive and
Kidney Diseases grant (P30 DK34987) to MAAP, and a National Space
Biomedical Research Institute grant (NCC 9-58) to NDT. The funders had
no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 69
TC 1
Z9 1
U1 0
U2 7
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 JUN 17
PY 2015
VL 10
IS 6
AR UNSP e0125792
DI 10.1371/journal.pone.0125792
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CK9NS
UT WOS:000356567400004
PM 26083373
ER
PT J
AU Schwalm, CR
Huntzinger, DN
Fisher, JB
Michalak, AM
Bowman, K
Ciais, P
Cook, R
El-Masri, B
Hayes, D
Huang, MY
Ito, A
Jain, A
King, AW
Lei, HM
Liu, JJ
Lu, CQ
Mao, JF
Peng, SS
Poulter, B
Ricciuto, D
Schaefer, K
Shi, XY
Tao, B
Tian, HQ
Wang, WL
Wei, YX
Yang, J
Zeng, N
AF Schwalm, Christopher R.
Huntzinger, Deborah N.
Fisher, Joshua B.
Michalak, Anna M.
Bowman, Kevin
Ciais, Philippe
Cook, Robert
El-Masri, Bassil
Hayes, Daniel
Huang, Maoyi
Ito, Akihiko
Jain, Atul
King, Anthony W.
Lei, Huimin
Liu, Junjie
Lu, Chaoqun
Mao, Jiafu
Peng, Shushi
Poulter, Benjamin
Ricciuto, Daniel
Schaefer, Kevin
Shi, Xiaoying
Tao, Bo
Tian, Hanqin
Wang, Weile
Wei, Yaxing
Yang, Jia
Zeng, Ning
TI Toward "optimal" integration of terrestrial biosphere models
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE modeling; carbon cycle; model integration
ID PROGRAM MULTISCALE SYNTHESIS; AIR CO2 ENRICHMENT; CLIMATE-CHANGE; CARBON
STORAGE; INTERCOMPARISON PROJECT; NITROGEN-CYCLE; FOREST BIOMASS;
LAND-USE; PREDICTION; UNCERTAINTY
AB Multimodel ensembles (MME) are commonplace in Earth system modeling. Here we perform MME integration using a 10-member ensemble of terrestrial biosphere models (TBMs) from the Multiscale synthesis and Terrestrial Model Intercomparison Project (MsTMIP). We contrast optimal (skill based for present-day carbon cycling) versus naive (one model-one vote) integration. MsTMIP optimal and naive mean land sink strength estimates (-1.16 versus -1.15 Pg C per annum respectively) are statistically indistinguishable. This holds also for grid cell values and extends to gross uptake, biomass, and net ecosystem productivity. TBM skill is similarly indistinguishable. The added complexity of skill-based integration does not materially change MME values. This suggests that carbon metabolism has predictability limits and/or that all models and references are misspecified. Resolving this issue requires addressing specific uncertainty types (initial conditions, structure, and references) and a change in model development paradigms currently dominant in the TBM community.
C1 [Schwalm, Christopher R.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA.
[Schwalm, Christopher R.; Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
[Huntzinger, Deborah N.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA.
[Fisher, Joshua B.; Bowman, Kevin; Liu, Junjie] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Ciais, Philippe; Peng, Shushi; Tao, Bo] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Cook, Robert; Hayes, Daniel; King, Anthony W.; Mao, Jiafu; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[El-Masri, Bassil; Jain, Atul] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA.
[Huang, Maoyi] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
[Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China.
[Lu, Chaoqun; Tian, Hanqin; Yang, Jia] Auburn Univ, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA.
[Lu, Chaoqun; Tian, Hanqin; Yang, Jia] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Schaefer, Kevin] Natl Snow & Ice Data Ctr, Boulder, CO USA.
[Wang, Weile] Ames Res Ctr, Natl Aeronaut & Space Adm, Moffett Field, CA USA.
[Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Schwalm, CR (reprint author), No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA.
EM christopher.schwalm@nau.edu
RI Mao, Jiafu/B-9689-2012; Lei, Huimin/H-9596-2015; Tian,
Hanqin/A-6484-2012; Wei, Yen/H-5329-2012; Peng, Shushi/J-4779-2014;
Ricciuto, Daniel/I-3659-2016; Zeng, Ning/A-3130-2008; Yang,
Jia/A-6483-2012; Jain, Atul/D-2851-2016
OI Fisher, Joshua/0000-0003-4734-9085; Poulter,
Benjamin/0000-0002-9493-8600; Huang, Maoyi/0000-0001-9154-9485; Mao,
Jiafu/0000-0002-2050-7373; Lei, Huimin/0000-0002-1175-2334; Tian,
Hanqin/0000-0002-1806-4091; Peng, Shushi/0000-0001-5098-726X; Ricciuto,
Daniel/0000-0002-3668-3021; Cook, Robert/0000-0001-7393-7302; Zeng,
Ning/0000-0002-7489-7629; Yang, Jia/0000-0003-2019-9603; Jain,
Atul/0000-0002-4051-3228
FU National Aeronautics and Space Administration (NASA) [NNX12AP74G,
NNX10AG01A, NNX11AO08A]; Multiscale synthesis and Terrestrial Model
Intercomparison Project (MsTMIP); NASA ROSES [NNX10AG01A, NNH10AN681];
Modeling and Synthesis Thematic Data Center at Oak Ridge National
Laboratory (ORNL); DOE [DE-AC05-00OR22725]; U.S. Department of Energy
(DOE), Office of Science, Biological and Environmental Research (BER)
through the Earth System Modeling program; Environmental Molecular
Sciences Laboratory(EMSL); U.S. DOE-BER; U.S. DOE-BER through the
Subsurface Biogeochemical Research Program (SBR) as part of the SBR
Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory
(PNNL); U.S. DOE [DE-AC05-76RLO1830]; NASA Interdisciplinary Science
Program (IDS); NASA Land Cover/Land Use Change Program (LCLUC); NASA
Terrestrial Ecology Program; NASA Atmospheric Composition Modeling and
Analysis Program (ACMAP); NSF Dynamics of Coupled Natural-Human System
Program (CNH); Decadal and Regional Climate Prediction using Earth
System Models (EaSM); DOE National Institute for Climate Change
Research; USDA AFRI Program; EPA STAR Program; U.S. National Science
Foundation [NSF-AGS-12-43071, NSF-EFRI083598]; USDA National Institute
of Food and Agriculture (NIFA) [2011-68002-30220]; U.S. Department of
Energy (DOE) Office of Science [DOE-DE-SC0006706]; NASA Land Cover and
Land Use Change Program [NNX14AD94G]; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]; National Science Foundation
[OCI-0725070, ACI-1238993]; GhG Europe FP7
FX C.R.S. was supported by National Aeronautics and Space Administration
(NASA) grants NNX12AP74G, NNX10AG01A, and NNX11AO08A. J.B.F. carried out
this research at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Funding for the Multiscale
synthesis and Terrestrial Model Intercomparison Project (MsTMIP;
http://nacp.ornl.gov/MsTMIP.shtml) activity was provided through NASA
ROSES grant NNX10AG01A. Data management support for preparing,
documenting, and distributing model driver and output data was performed
by the Modeling and Synthesis Thematic Data Center at Oak Ridge National
Laboratory (ORNL; http://nacp.ornl.gov), with funding through NASA ROSES
grant NNH10AN681. Finalized MsTMIP data products are archived at the
ORNL DAAC (http://daac.ornl.gov). This is MsTMIP contribution 5.
Acknowledgments for specific MsTMIP participating models: Biome-BGC:
Biome-BGC code was provided by the Numerical Terradynamic Simulation
Group at the University of Montana. The computational facilities
provided by NASA Earth Exchange at NASA Ames Research Center. CLM: This
research is supported in part by the U.S. Department of Energy (DOE),
Office of Science, Biological and Environmental Research. Oak Ridge
National Laboratory is managed by UT-BATTELLE for DOE under contract
DE-AC05-00OR22725. CLM4VIC: CLM4VIC simulations were supported in part
by the U.S. Department of Energy (DOE), Office of Science, Biological
and Environmental Research (BER) through the Earth System Modeling
program and performed using the Environmental Molecular Sciences
Laboratory(EMSL), a national scientific user facility sponsored by the
U.S. DOE-BER and located at Pacific Northwest National Laboratory
(PNNL). Participation of M. Huang in the MsTMIP synthesis is supported
by the U.S. DOE-BER through the Subsurface Biogeochemical Research
Program (SBR) as part of the SBR Scientific Focus Area (SFA) at the
Pacific Northwest National Laboratory (PNNL). PNNL is operated for the
U.S. DOE by BATTELLE Memorial Institute under contract
DE-AC05-76RLO1830. DLEM: The Dynamic Land Ecosystem Model (DLEM)
developed in the International Center for Climate and Global Change
Research at Auburn University has been supported by NASA
Interdisciplinary Science Program (IDS), NASA Land Cover/Land Use Change
Program (LCLUC), NASA Terrestrial Ecology Program, NASA Atmospheric
Composition Modeling and Analysis Program (ACMAP); NSF Dynamics of
Coupled Natural-Human System Program (CNH), Decadal and Regional Climate
Prediction using Earth System Models (EaSM); DOE National Institute for
Climate Change Research; USDA AFRI Program; and EPA STAR Program.
Integrated Science Assessment Model (ISAM) simulations were supported by
the U.S. National Science Foundation (NSF-AGS-12-43071 and
NSF-EFRI083598), the USDA National Institute of Food and Agriculture
(NIFA) (2011-68002-30220), the U.S. Department of Energy (DOE) Office of
Science (DOE-DE-SC0006706), and the NASA Land Cover and Land Use Change
Program (NNX14AD94G). ISAM simulations were carried out at the National
Energy Research Scientific Computing Center (NERSC), which is supported
by the Office of Science of the U.S. Department of Energy under contract
DE-AC02-05CH11231, and at the Blue Waters sustained-petascale computing,
University of Illinois at Urbana-Champaign, which is supported by the
National Science Foundation (awards OCI-0725070 and ACI-1238993) and the
state of Illinois. LPJ-wsl: This work was conducted at LSCE, France,
using a modified version of the LPJ version 3.; 1 model, originally made
available by the Potsdam Institute for Climate Impact Research.
ORCHIDEE-LSCE: ORCHIDEE is a global land surface model developed at the
IPSL institute in France. The simulations were performed with the
support of the GhG Europe FP7 grant with computing facilities provided
by LSCE (Laboratoire des Sciences du Climat et de l'Environnement) or
TGCC (Tres Grand Centre de Calcul). VISIT: VISIT was developed at the
National Institute for Environmental Studies, Japan. This work was
mostly conducted during a visiting stay at Oak Ridge National
Laboratory.
NR 95
TC 7
Z9 7
U1 4
U2 30
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 JUN 16
PY 2015
VL 42
IS 11
BP 4418
EP 4428
DI 10.1002/2015GL064002
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA CM2LI
UT WOS:000357511200022
ER
PT J
AU Forrister, H
Liu, J
Scheuer, E
Dibb, J
Ziemba, L
Thornhill, KL
Anderson, B
Diskin, G
Perring, AE
Schwarz, JP
Campuzano-Jost, P
Day, DA
Palm, BB
Jimenez, JL
Nenes, A
Weber, RJ
AF Forrister, Haviland
Liu, Jiumeng
Scheuer, Eric
Dibb, Jack
Ziemba, Luke
Thornhill, Kenneth L.
Anderson, Bruce
Diskin, Glenn
Perring, Anne E.
Schwarz, Joshua P.
Campuzano-Jost, Pedro
Day, Douglas A.
Palm, Brett B.
Jimenez, Jose L.
Nenes, Athanasios
Weber, Rodney J.
TI Evolution of brown carbon in wildfire plumes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE brown carbon; biomass burning; lifetime; plume evolution;
photooxidation; bleaching
ID SOUTHEASTERN UNITED-STATES; AEROSOL MASS-SPECTROMETRY; LIGHT-ABSORPTION;
ORGANIC AEROSOL; OPTICAL-PROPERTIES; BLACK CARBON; SOLAR-RADIATION;
HIGH-RESOLUTION; SECONDARY; COMBUSTION
AB Particulate brown carbon (BrC) in the atmosphere absorbs light at subvisible wavelengths and has poorly constrained but potentially large climate forcing impacts. BrC from biomass burning has virtually unknown lifecycle and atmospheric stability. Here, BrC emitted from intense wildfires was measured in plumes transported over 2days from two main fires, during the 2013 NASA SEAC4RS mission. Concurrent measurements of organic aerosol (OA) and black carbon (BC) mass concentration, BC coating thickness, absorption angstrom ngstrom exponent, and OA oxidation state reveal that the initial BrC emitted from the fires was largely unstable. Using back trajectories to estimate the transport time indicates that BrC aerosol light absorption decayed in the plumes with a half-life of 9 to 15 h, measured over day and night. Although most BrC was lost within a day, possibly through chemical loss and/or evaporation, the remaining persistent fraction likely determines the background BrC levels most relevant for climate forcing.
C1 [Forrister, Haviland; Liu, Jiumeng; Nenes, Athanasios; Weber, Rodney J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Scheuer, Eric; Dibb, Jack] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Ziemba, Luke; Thornhill, Kenneth L.; Anderson, Bruce; Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Perring, Anne E.; Schwarz, Joshua P.] Natl Ocean & Atmospher Adm, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA.
[Perring, Anne E.; Schwarz, Joshua P.; Campuzano-Jost, Pedro; Day, Douglas A.; Palm, Brett B.; Jimenez, Jose L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Campuzano-Jost, Pedro; Day, Douglas A.; Palm, Brett B.; Jimenez, Jose L.] Univ Colorado, Dept Chem & Biogeochem, Boulder, CO 80309 USA.
[Nenes, Athanasios] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA.
RP Weber, RJ (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
EM rodney.weber@eas.gatech.edu
RI Liu, Jiumeng/K-2024-2012; Perring, Anne/G-4597-2013; Jimenez,
Jose/A-5294-2008; schwarz, joshua/G-4556-2013; Manager, CSD
Publications/B-2789-2015
OI Liu, Jiumeng/0000-0001-7238-593X; Perring, Anne/0000-0003-2231-7503;
Jimenez, Jose/0000-0001-6203-1847; schwarz, joshua/0000-0002-9123-2223;
FU GIT NASA [NNX12AB83G, NNX14AP74G]; UNH NASA [NNX12AB80G]; NASA
[NNX12AC03G]
FX All data used in this paper were collected as part of the NASA SEAC4RS
mission and became available to the general public on 15 October 2014
through the NASA data archive. This project was funded by GIT NASA
contracts NNX12AB83G and NNX14AP74G and UNH NASA contract NNX12AB80G.
P.C.J., D.A.D., and J.L.J. were supported by NASA NNX12AC03G.
NR 47
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U1 12
U2 83
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 JUN 16
PY 2015
VL 42
IS 11
BP 4623
EP 4630
DI 10.1002/2015GL063897
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CM2LI
UT WOS:000357511200046
ER
PT J
AU Wallace, WT
Gazda, DB
Limero, TF
Minton, JM
Macatangay, AV
Dwivedi, P
Fernandez, FM
AF Wallace, William T.
Gazda, Daniel B.
Limero, Thomas F.
Minton, John M.
Macatangay, Ariel V.
Dwivedi, Prabha
Fernandez, Facundo M.
TI Electrothermal Vaporization Sample Introduction for Spaceflight Water
Quality Monitoring via Gas Chromatography-Differential Mobility
Spectrometry
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID MASS-SPECTROMETRY; DIMETHYLSILANEDIOL
AB In the history of manned spaceflight, environmental monitoring has relied heavily on archival sampling. However, with the construction of the International Space Station (ISS) and the subsequent extension in mission duration up to one year, an enhanced, real-time method for environmental monitoring is necessary. The station air is currently monitored for trace volatile organic compounds (VOCs) using gas chromatography-differential mobility spectrometry (GC-DMS) via the Air Quality Monitor (AQM), while water is analyzed to measure total organic carbon and biocide concentrations using the Total Organic Carbon Analyzer (TOCA) and the Colorimetric Water Quality Monitoring Kit (CWQMK), respectively. As mission scenarios extend beyond low Earth orbit, a convergence in analytical instrumentation to analyze both air and water samples is highly desirable. Since the AQM currently provides quantitative, compound-specific information for air samples and many of the targets in air are also common to water, this platform is a logical starting point for developing a multimatrix monitor. Here, we report on the interfacing of an electrothermal vaporization (ETV) sample introduction unit with a ground-based AQM for monitoring target analytes in water. The results show that each of the compounds tested from water have similar GC-DMS parameters as the compounds tested in air. Moreover, the ETV enabled AQM detection of dimethlsilanediol (DMSD), a compound whose analysis had proven challenging using other sample introduction methods. Analysis of authentic ISS water samples using the ETV-AQM showed that DMSD could be successfully quantified, while the concentrations obtained for the other compounds also agreed well with laboratory results.
C1 [Wallace, William T.; Gazda, Daniel B.; Limero, Thomas F.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Minton, John M.] Univ Arkansas, Little Rock, AR 72204 USA.
[Macatangay, Ariel V.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Dwivedi, Prabha] Ctr Dis Control & Prevent, Atlanta, GA 30341 USA.
[Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
RP Wallace, WT (reprint author), Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
EM william.wallace-1@nasa.gov; facundo.fernandez@chemistry.gatech.edu
FU NASA [NAS 9-02078, NNX13AF51G S02]; Arkansas Space Grant Consortium
FX W.T.W., D.B.G., and T.F.L. acknowledge funding under NASA contract # NAS
9-02078. The work of J.M.M. was supported through the Arkansas Space
Grant Consortium. W.T.W. would like to thank Sarah Castro (NASA Johnson
Space Center) for critical editing and Zachary Pickett for his work on
our early DMSD studies. F.M.F. thanks NASA for award number NNX13AF51G
S02.
NR 30
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U1 9
U2 22
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD JUN 16
PY 2015
VL 87
IS 12
BP 5981
EP 5988
DI 10.1021/acs.analchem.5b00055
PG 8
WC Chemistry, Analytical
SC Chemistry
GA CL2DZ
UT WOS:000356755100019
PM 25971650
ER
PT J
AU Del Genio, AD
Chen, YH
AF Del Genio, Anthony D.
Chen, Yonghua
TI Cloud-radiative driving of the Madden-Julian oscillation as seen by the
A-Train
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Madden-Julian oscillation; clouds; radiative heating; convection
ID STATIC ENERGY BUDGET; TROPICAL INTRASEASONAL OSCILLATION;
MOISTURE-CONVECTION FEEDBACKS; TROPOPAUSE TRANSITION LAYER; COUPLED
EQUATORIAL WAVES; STRATIFORM INSTABILITY; CLIMATE MODELS; PART I; MJO;
VARIABILITY
AB Cloud and water vapor radiative heating anomalies associated with convection may be an effective source of moist static energy driving the Madden-Julian Oscillation (MJO). In this paper 5years of radiative heating profiles derived from CloudSat radar and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation data are analyzed to document radiative heating anomalies during the MJO. Atmospheric shortwave absorption and surface longwave radiation anomalies are of opposite sign and 10-20% as large as top-of-atmosphere outgoing longwave radiation (OLR) anomalies, confirming that OLR provides a useful estimate of the total column radiative heating anomaly. Positive anomalies generally peak about 1week before the MJO peak and are smallest over the Indian Ocean. Anomalies over the Maritime Continent are strongest and coincident with the MJO peak. Shortwave heating profile anomalies are weaker than longwave anomalies in the active region of the MJO but generally of opposite sign; thus, shortwave heating damps the longwave destabilization of the lower troposphere. The exception is the onset phase of the MJO, where shortwave and longwave heating anomalies due to thin cirrus are both positive in the upper troposphere and exert a stabilizing influence. Specific humidity anomalies in the middle troposphere reach 0.5gkg(-1), but the associated clear-sky heating anomaly is small. Radiative enhancement of column moist static energy becomes significant as precipitation increases before the MJO peak and remains high after the MJO peak as precipitation begins to decline. Elevated radiative heating after the peak may contribute to destabilizing the MJO.
C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Chen, Yonghua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM anthony.d.delgenio@nasa.gov
FU NASA CloudSat-CALIPSO Mission; NASA Modeling and Analysis Program
FX The authors thank three anonymous reviewers for their constructive
comments that improved the manuscript. The A-Train data used in this
paper are available from the CloudSat Data Processing Center
(http://www.cloudsat.cira.colostate.edu/dataHome.php). The
Wheeler-Hendon MJO index is available at
http://www.cawcr.gov.au/staff/mwheeler/maproom/. The NOAA Climate
Prediction Center MJO indices are available at
http://www.cpc.ncep.noaa.gov/products/precip/CWlink/daily_mjo_index/pent
ad.html. The specific subsets of data used in our analysis are available
from Y. Chen (yonghuachen@gmail.com). This research was supported by the
NASA CloudSat-CALIPSO Mission and the NASA Modeling and Analysis
Program.
NR 60
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Z9 4
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 JUN 16
PY 2015
VL 120
IS 11
BP 5344
EP 5356
DI 10.1002/2015JD023278
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700004
ER
PT J
AU Shindell, DT
Faluvegi, G
Rotstayn, L
Milly, G
AF Shindell, Drew T.
Faluvegi, Greg
Rotstayn, Leon
Milly, George
TI Spatial patterns of radiative forcing and surface temperature response
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosols; climate; regional climate; aerosol forcing
ID CLIMATE-CHANGE; ANTHROPOGENIC AEROSOLS; MODEL; SENSITIVITY; SPREAD;
OZONE; CMIP5
AB Examination of effective radiative forcing (ERF), a measure of changes in Earth's energy balance, facilitates understanding the role of various drivers of climate change. For short-lived compounds, ERF can be highly inhomogeneous geographically. The relationship between the spatial patterns of ERF and surface temperature response is poorly characterized, however. We examine that relationship in the latest generation of global climate models. We find that the uneven distribution of historical aerosol, ozone, and land use forcing leads to substantial differences compared to the well-mixed greenhouse gases (WMGHG). There is a stronger response per unit global mean forcing to historical inhomogeneous forcing than to WMGHG both globally and in much of the Northern Hemisphere (NH) extratropics, in fairly good agreement with results inferred from observations. Our results indicate that the enhanced global mean response is attributable to the concentration of inhomogeneous forcing in the NH extratropics, where there is strongest sensitivity to forcing, rather than to processes specific to the inhomogeneous forcers. In many regions, inclusion of inhomogeneous forcing greatly increases the spread in historical temperature changes simulated by the models, suggesting that better forcing characterization could play an important role in improving modeling of decadal-scale regional climate change. Finally, incorporating observed temperatures, the results provide estimates of global historical aerosol forcing (-1.00.4Wm(-2)) consistent with other studies (though with narrower uncertainties) and also provide constraints on NH and NH extratropical historical aerosol forcing (-1.40.6 and -1.20.6Wm(-2), respectively) and aerosol+ozone forcing.
C1 [Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Faluvegi, Greg; Milly, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rotstayn, Leon] CSIRO, Oceans & Atmosphere Flagship, Aspendale, Vic, Australia.
RP Shindell, DT (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
EM drew.shindell@duke.edu
RI Shindell, Drew/D-4636-2012; Rotstayn, Leon/A-1756-2012
OI Rotstayn, Leon/0000-0002-2385-4223
FU NASA
FX We thank the World Climate Research Programme's Working Group on Coupled
Modelling, the U.S. Department of Energy's Program for Climate Model
Diagnosis and Intercomparison, and the climate modeling groups from CMIP
and the Atmospheric Chemistry and Climate Model Intercomparison Project
for making available their model output. Data used in this analysis are
available via the CMIP5 or ACCMIP archives (models;
http://cmip-pcmdi.llnl.gov/cmip5/data_portal.html and
http://www.giss.nasa.gov/projects/accmip/) and from the University of
York (observations; http://www-users.york.ac.uk/similar to
kdc3/papers/coverage2013/series.html). We also thank David Considine for
support via NASA's Modeling, Analysis and Prediction Program, and Piers
Forster and two anonymous reviewers for comments. Computational
resources supporting this work were provided by the NASA High-End
Computing Program through the NASA Center for Climate Simulation at
Goddard Space Flight Center.
NR 44
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Z9 8
U1 3
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2015
VL 120
IS 11
BP 5385
EP 5403
DI 10.1002/2014JD022752
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700007
ER
PT J
AU Garfinkel, CI
Hurwitz, MM
Oman, LD
AF Garfinkel, C. I.
Hurwitz, M. M.
Oman, L. D.
TI Effect of recent sea surface temperature trends on the Arctic
stratospheric vortex
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Arctic stratosphere; SST trends; ozone trends; ozone loss
ID PACIFIC DECADAL OSCILLATION; OZONE-DEPLETING SUBSTANCES; ATMOSPHERIC
CIRCULATION; NORTHERN-HEMISPHERE; PROPAGATION; MODEL; TROPOSPHERE;
EVENTS; MSU
AB Comprehensive chemistry-climate model experiments and observational data are used to show that up to half of the satellite era early springtime cooling trend in the Arctic lower stratosphere was caused by changing sea surface temperatures (SSTs). An ensemble of experiments forced only by changing SSTs is compared to an ensemble of experiments in which both the observed SSTs and chemically and radiatively active trace species are changing. By comparing the two ensembles, it is shown that warming of Indian Ocean, North Pacific, and North Atlantic SSTs and cooling of the tropical Pacific have strongly contributed to recent polar stratospheric cooling in late winter and early spring. When concentrations of ozone-depleting substances and greenhouse gases are fixed, polar ozone concentrations show a small but robust decline due to changing SSTs. Ozone loss is larger in the presence of changing concentrations of ozone-depleting substances and greenhouse gases. The stratospheric changes can be understood by examining the tropospheric height and heat flux anomalies generated by the anomalous SSTs. Finally, recent SST changes have contributed to a decrease in the frequency of late winter stratospheric sudden warmings.
C1 [Garfinkel, C. I.] Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
[Hurwitz, M. M.; Oman, L. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurwitz, M. M.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
RP Garfinkel, CI (reprint author), Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
EM chaim.garfinkel@mail.huji.ac.il
RI Oman, Luke/C-2778-2009
OI Oman, Luke/0000-0002-5487-2598
FU Hebrew University of Jerusalem; Israel Science Foundation [1558/14];
NASA ACMAP program
FX This work was supported by a startup grant from Hebrew University of
Jerusalem and by the Israel Science Foundation (grant 1558/14). M.M.H.
acknowledges support from the NASA ACMAP program. We would also like to
thank those involved in model development at GSFC and the
high-performance computing resources that were provided by NASA's
Advanced Supercomputing Division. We would also like to thank Feng Li
for making available the coupled ocean-atmosphere integration. We thank
the three anonymous reviewers for their helpful comments. We would like
to thank Greg Bodeker of Bodeker Scientific for providing the combined
total column ozone database available at
http://www.bodekerscientific.com/data/total-column-ozone. All data
necessary to understand, evaluate, replicate, and build upon the
reported research will be made available and accessible upon request to
C.I.G. (chaim.garfinkel@mail.huji.ac.il).
NR 60
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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 JUN 16
PY 2015
VL 120
IS 11
BP 5404
EP 5416
DI 10.1002/2015JD023284
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700008
ER
PT J
AU Yasunari, TJ
Koster, RD
Lau, WKM
Kim, KM
AF Yasunari, Teppei J.
Koster, Randal D.
Lau, William K. M.
Kim, Kyu-Myong
TI Impact of snow darkening via dust, black carbon, and organic carbon on
boreal spring climate in the Earth system
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE snow darkening; dust; black carbon; organic carbon; climate; global
model
ID ASIAN SUMMER MONSOON; LIGHT-ABSORBING IMPURITIES; CATCHMENT-BASED
APPROACH; LAND-SURFACE PROCESSES; HIMALAYAN GLACIERS; TIBETAN PLATEAU;
GOCART MODEL; ICE CORE; PREMONSOON SEASON; WATER EQUIVALENT
AB Dust, black carbon (BC), and organic carbon (OC) aerosols, when deposited onto snow, are known to reduce the albedo of the snow (i.e., snow darkening effect (SDE)). Here using the NASA Goddard Earth Observing System Model, Version 5 (GEOS-5) with aerosol tracers and a state-of-the-art snow darkening module (GOddard SnoW Impurity Module: GOSWIM) for the land surface, we examine the role of SDE on climate in the boreal spring snowmelt season. SDE is found to produce significant surface warming (over 15Wm(-2)) over broad areas in midlatitudes, with dust being the most important contributor to the warming in central Asia and the western Himalayas and with BC having larger impact in the Europe, eastern Himalayas, East Asia, and North America. The contribution of OC to the warming is generally low but still significant mainly over southeastern Siberia, northeastern East Asia, and western Canada (similar to 19% of the total solar visible absorption by these snow impurities). The simulations suggest that SDE strengthens the boreal spring water cycle in East Asia through water recycling and moisture advection from the ocean and contributes to the maintenance of dry conditions in parts of a region spanning Europe to central Asia, partially through feedback on the model's background climatology. Overall, our study suggests that the existence of SDE in the Earth system associated with dust, BC, and OC contributes significantly to enhanced surface warming over continents in northern hemisphere midlatitudes during boreal spring, raising the surface skin temperature by approximately 3-6K near the snowline.
C1 [Yasunari, Teppei J.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[Yasunari, Teppei J.; Koster, Randal D.; Lau, William K. M.; Kim, Kyu-Myong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lau, William K. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Yasunari, TJ (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
EM teppei.j.yasunari@nasa.gov
RI Kim, Kyu-Myong/G-5398-2014; Koster, Randal/F-5881-2012; Yasunari,
Teppei/E-5374-2010; Lau, William /E-1510-2012
OI Koster, Randal/0000-0001-6418-6383; Yasunari,
Teppei/0000-0002-9896-9404; Lau, William /0000-0002-3587-3691
FU NASA Modeling, Analysis, and Prediction (MAP) Program by NASA
Headquarters
FX The NASA Modeling, Analysis, and Prediction (MAP) Program by NASA
Headquarters supported this work. We thank the MODIS snow and ice team
for the development of the snow cover fraction data product; NASA Center
for Climate Simulation for the GEOS-5 simulations; the NASA Global
Modeling and Assimilation Office (GMAO) for the development of GEOS-5,
producing the initial conditions and the MERRA data product; and the
NASA GES DISC for the online provision of MERRA data. We also thank
Lawrence L. Takacs (Science Systems and Applications, Inc.), Arlindo da
Silva (NASA), and Peter R. Colarco (NASA) at NASA Goddard Space Flight
Center for helping us in this work. Useful information on our discussion
was obtained from Taichu Y. Tanaka (Japan Meteorological Agency), Teruo
Aoki (Meteorological Research Institute), and Ritesh Gautam (Indian
Institute of Technology). The GEOS-5 outputs and/or other data used in
this study are available via contact with Teppei J. Yasunari
(teppei.j.yasunari@nasa.gov or t.j.yasunari@eng.hokudai.ac.jp, as of 1
July 2015) and/or Kyu-Myong Kim (kyu-myong.kim-1@nasa.gov).
NR 116
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U1 4
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2015
VL 120
IS 11
BP 5485
EP 5503
DI 10.1002/2014JD022977
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700013
ER
PT J
AU Meyer, K
Platnick, S
Zhang, ZB
AF Meyer, Kerry
Platnick, Steven
Zhang, Zhibo
TI Simultaneously inferring above-cloud absorbing aerosol optical thickness
and underlying liquid phase cloud optical and microphysical properties
using MODIS
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Clouds; Aerosols; Remote Sensing
ID CALIPSO LIDAR MEASUREMENTS; SATELLITE-OBSERVATIONS; MULTIPLE-SCATTERING;
RADIATIVE-TRANSFER; C-130 AIRCRAFT; SAFARI 2000; CALIOP; DEPTH;
RETRIEVAL; ALGORITHM
AB The regional haze over the southeast (SE) Atlantic Ocean induced by biomass burning in southern Africa can be problematic for passive imager-based retrievals of the underlying quasi-permanent marine boundary layer (MBL) clouds and for estimates of top-of-atmosphere (TOA) aerosol direct radiative effect (DRE). Here an algorithm is introduced to simultaneously retrieve above-cloud aerosol optical thickness (AOT), the cloud optical thickness (COT), and cloud effective particle radius (CER) of the underlying MBL clouds while also providing pixel-level estimates of retrieval uncertainty. This approach utilizes reflectance measurements at six Moderate Resolution Imaging Spectroradiometer (MODIS) channels from the visible to the shortwave infrared. Retrievals are run under two aerosol model assumptions on 8years (2006-2013) of June-October Aqua MODIS data over the SE Atlantic, from which a regional cloud and above-cloud aerosol climatology is produced. The cloud retrieval methodology is shown to yield COT and CER consistent with those from the MODIS operational cloud product (MOD06) when forcing AOT to zero, while the full COT-CER-AOT retrievals that account for the above-cloud aerosol attenuation increase regional monthly mean COT and CER by up to 9% and 2%, respectively. Retrieved AOT is roughly 3 to 5 times larger than the collocated 532nm Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) retrievals, though closer agreement is observed with the CALIOP 1064nm retrievals, a result consistent with previous case study analyses. Regional cloudy-sky above-cloud aerosol DRE calculations are also performed that illustrate the importance of the aerosol model assumption and underlying cloud retrievals.
C1 [Meyer, Kerry] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[Meyer, Kerry; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
RP Meyer, K (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
EM kerry.meyer@nasa.gov
RI Meyer, Kerry/E-8095-2016; Platnick, Steven/J-9982-2014
OI Meyer, Kerry/0000-0001-5361-9200; Platnick, Steven/0000-0003-3964-3567
FU NASA Radiation Sciences Program; NASA [NNH14CK44C, NNX14AI35G]
FX The authors would like to thank Rob Levy for his expertise with the
MODIS Dark Target aerosol models, and Nandana Amarasinghe for his
efforts toward enhancing our forward radiative transfer modeling
capabilities. The authors would also like to thank Robert J. Swap for
invaluable discussions about aerosol transport over the southern
Atlantic Ocean. This research was supported by the NASA Radiation
Sciences Program and by funding from NASA CloudSat and CALIPSO Science
Team grant NNH14CK44C managed by David Considine; Z. Zhang acknowledges
funding support from the NASA New Investigator Program (NNX14AI35G)
managed by Ming-Ying Wei. The MODIS data used in this study are
publically available from the NASA Level 1 and Atmosphere Archive and
Distribution System (LAADS) (http://ladsweb.nascom.nasa.gov); the CALIOP
data are publically available from the NASA Langley Research Center's
Atmospheric Science Data Center (ASDC) CALIPSO Search and Subsetting web
application (https://www-calipso.larc.nasa.gov/search/login.php).
NR 73
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U1 5
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 JUN 16
PY 2015
VL 120
IS 11
BP 5524
EP 5547
DI 10.1002/2015JD023128
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700015
ER
PT J
AU Haddad, ZS
Steward, JL
Tseng, HC
Vukicevic, T
Chen, SH
Hristova-Veleva, S
AF Haddad, Z. S.
Steward, J. L.
Tseng, H. -C.
Vukicevic, T.
Chen, S. -H.
Hristova-Veleva, S.
TI A data assimilation technique to account for the nonlinear dependence of
scattering microwave observations of precipitation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE precipitation; data assimilation; microwave
ID SATELLITE DATA ASSIMILATION; CLOUD; IMPLEMENTATION; RETRIEVAL; SYSTEM;
MODEL
AB Satellite microwave observations of rain, whether from radar or passive radiometers, depend in a very crucial way on the vertical distribution of the condensed water mass and on the types and sizes of the hydrometeors in the volume resolved by the instrument. This crucial dependence is nonlinear, with different types and orders of nonlinearity that are due to differences in the absorption/emission and scattering signatures at the different instrument frequencies. Because it is not monotone as a function of the underlying condensed water mass, the nonlinearity requires great care in its representation in the observation operator, as the inevitable uncertainties in the numerous precipitation variables are not directly convertible into an additive white uncertainty in the forward calculated observations. In particular, when attempting to assimilate such data into a cloud-permitting model, special care needs to be applied to describe and quantify the expected uncertainty in the observations operator in order not to turn the implicit white additive uncertainty on the input values into complicated biases in the calculated radiances. One approach would be to calculate the means and covariances of the nonlinearly calculated radiances given an a priori joint distribution for the input variables. This would be a very resource-intensive proposal if performed in real time. We propose a representation of the observation operator based on performing this moment calculation off line, with a dimensionality reduction step to allow for the effective calculation of the observation operator and the associated covariance in real time during the assimilation. The approach is applicable to other remotely sensed observations that depend nonlinearly on model variables, including wind vector fields. The approach has been successfully applied to the case of tropical cyclones, where the organization of the system helps in identifying the dimensionality-reducing variables.
C1 [Haddad, Z. S.; Steward, J. L.; Hristova-Veleva, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Haddad, Z. S.; Steward, J. L.; Hristova-Veleva, S.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Tseng, H. -C.; Chen, S. -H.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Vukicevic, T.] NOAA, AOML, Miami, FL USA.
RP Haddad, ZS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM zhaddad@jifresse.ucla.edu
RI Chen, Hua/B-7664-2014
OI Chen, Hua/0000-0002-9493-6939
FU National Aeronautics and Space Administration; National Oceanic and
Atmospheric Administration through Hurricane Forecasting Improvement
Project
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. The research was supported by a grant from the
National Oceanic and Atmospheric Administration through the Hurricane
Forecasting Improvement Project. The TRMM data and our forward
simulations can be found at http://trmm.jpl.nasa.gov/2015JD023107_data/.
NR 19
TC 3
Z9 3
U1 1
U2 5
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 JUN 16
PY 2015
VL 120
IS 11
BP 5548
EP 5563
DI 10.1002/2015JD023107
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700016
ER
PT J
AU Rong, PP
Yue, J
Russell, JM
Lumpe, JD
Gong, J
Wu, DL
Randall, CE
AF Rong, P. P.
Yue, J.
Russell, J. M., III
Lumpe, J. D.
Gong, J.
Wu, D. L.
Randall, C. E.
TI Horizontal winds derived from the polar mesospheric cloud images as
observed by the CIPS instrument on the AIM satellite
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CIPS; PMCs; horizontal winds; pattern matching
ID PARTICLE-SIZE EXPERIMENT; NOCTILUCENT CLOUDS; GRAVITY-WAVES; MODEL; ICE;
THERMOSPHERE; TEMPERATURE; NLC
AB A cloud pattern matching technique is applied to polar mesospheric cloud (PMC) images taken by the Cloud Imaging and Particle Size instrument (CIPS) to infer the wind velocities in the mesopause region. CIPS measurements are analyzed to detect patterns that repeat from one orbit to the next but are displaced in location; the displacement provides a measure of the wind velocity. Pattern matching is achieved by resampling the CIPS data to longitude and latitude grids with the grid-box size forced at similar to 5km in both directions. The correlated patterns are searched within a geographic region referred to as a frame of similar to 500km in longitudex400km in latitude. The histograms of the derived velocities indicate that easterly winds prevail, with a mean zonal wind of -20 to -15m/s. Mean meridional winds are overall small, but in late summer the histogram indicated a poleward wind of similar to 20-30m/s. The variability of CIPS cloud albedo on consecutive orbits is also examined at fixed geolocations. The statistical results suggest that similar to 86% of pairs underwent mean cloud albedo variation of < 50% on consecutive orbits, suggesting a moderate change. It is also found that the correlation of the cloud structures between two consecutive orbits at a fixed location is generally poor. These findings suggest that cloud patterns are subject to wind advection, but the cloud patches are more extended in size than the movement that occurs. Cloud voids are found to be more likely to remain at the same geolocations.
C1 [Rong, P. P.; Yue, J.; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Lumpe, J. D.] Computat Phys Inc, Boulder, CO USA.
[Gong, J.] Univ Space Res Assoc, Greenbelt, MD USA.
[Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Rong, PP (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
EM ppr@jhu.edu
RI Yue, Jia/D-8177-2011; Wu, Dong/D-5375-2012; Randall, Cora/L-8760-2014
OI Randall, Cora/0000-0002-4313-4397
FU NASA Small Explorer Program [NAS5-03132]
FX This work was supported by the NASA Small Explorer Program through
contract NAS5-03132. We acknowledge all members of AIM science team,
especially the CIPS team, for the consistent support on this project
over a 2 year period. CIPS data can be accessed through website
http://lasp.colorado.edu/aim/download-data.html. The data used in this
study were processed by Jerry Lumpe (lumpe@cpi.com) from Computational
Physics, Inc., Boulder, Colorado.
NR 42
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2015
VL 120
IS 11
BP 5564
EP 5584
DI 10.1002/2014JD022813
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700017
ER
PT J
AU Marchenko, S
Krotkov, NA
Lamsal, LN
Celarier, EA
Swartz, WH
Bucsela, EJ
AF Marchenko, S.
Krotkov, N. A.
Lamsal, L. N.
Celarier, E. A.
Swartz, W. H.
Bucsela, E. J.
TI Revising the slant column density retrieval of nitrogen dioxide observed
by the Ozone Monitoring Instrument
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE remote sensing; instruments and techniques; atmosphere: composition and
chemistry
ID ABSORPTION CROSS-SECTION; TROPOSPHERIC NO2; SATELLITE RETRIEVALS;
RAMAN-SCATTERING; EMISSIONS; OMI; MODEL; SCIAMACHY; CHEMISTRY; SPACE
AB Nitrogen dioxide retrievals from the Aura/Ozone Monitoring Instrument (OMI) have been used extensively over the past decade, particularly in the study of tropospheric air quality. Recent comparisons of OMI NO2 with independent data sets and models suggested that the OMI values of slant column density (SCD) and stratospheric vertical column density (VCD) in both the NASA OMNO2 and Royal Netherlands Meteorological Institute DOMINO products are too large, by around 10-40%. We describe a substantially revised spectral fitting algorithm, optimized for the OMI visible light spectrometer channel. The most important changes comprise a flexible adjustment of the instrumental wavelength shifts combined with iterative removal of the ring spectral features; the multistep removal of instrumental noise; iterative, sequential estimates of SCDs of the trace gases in the 402-465nm range. These changes reduce OMI SCD(NO2) by 10-35%, bringing them much closer to SCDs retrieved from independent measurements and models. The revised SCDs, submitted to the stratosphere-troposphere separation algorithm, give tropospheric VCDs approximate to 10-15% smaller in polluted regions, and up to approximate to 30% smaller in unpolluted areas. Although the revised algorithm has been optimized specifically for the OMI NO2 retrieval, our approach could be more broadly applicable.
C1 [Marchenko, S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Marchenko, S.; Krotkov, N. A.; Lamsal, L. N.; Celarier, E. A.; Swartz, W. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lamsal, L. N.; Celarier, E. A.] Univ Space Res Assoc, Columbia, MD USA.
[Swartz, W. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Bucsela, E. J.] SRI Int, Menlo Pk, CA 94025 USA.
RP Marchenko, S (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM sergey_marchenko@ssaihq.com
RI Krotkov, Nickolay/E-1541-2012; Swartz, William/A-1965-2010
OI Krotkov, Nickolay/0000-0001-6170-6750; Swartz,
William/0000-0002-9172-7189
FU NASA's Earth Science Division
FX We thank A. Richter for kindly providing us with the preliminary
SCD(NO2) fitting results for the OMI orbits #03610 and #03622
(both from 20 March 2005). The OMI OMNO2 data used in this analysis are
publicly available at
http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/OMI, and the DOMINO
product is available at http://www.temis.nl. The SCIAMACHY data were
obtained from the Aura Validation Data Center,
http://avdc.gsfc.nasa.gov. This work was supported by NASA's Earth
Science Division through an Aura science team grant. The Dutch-and
Finnish-built OMI instrument is part of the NASA EOS Aura satellite
payload. The OMI instrument is managed by KNMI and the Netherlands
Agency for Aerospace Programs. We wish to thank the referees for their
constructive, helpful criticism.
NR 69
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U1 2
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2015
VL 120
IS 11
BP 5670
EP 5692
DI 10.1002/2014JD022913
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700023
PM 27708989
ER
PT J
AU Prather, MJ
Hsu, J
DeLuca, NM
Jackman, CH
Oman, LD
Douglass, AR
Fleming, EL
Strahan, SE
Steenrod, SD
Sovde, OA
Isaksen, ISA
Froidevaux, L
Funke, B
AF Prather, Michael J.
Hsu, Juno
DeLuca, Nicole M.
Jackman, Charles H.
Oman, Luke D.
Douglass, Anne R.
Fleming, Eric L.
Strahan, Susan E.
Steenrod, Stephen D.
Sovde, O. Amund
Isaksen, Ivar S. A.
Froidevaux, Lucien
Funke, Bernd
TI Measuring and modeling the lifetime of nitrous oxide including its
variability
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE nitrous oxide; atmospheric lifetime; perturbation lifetime;
stratospheric photochemistry; models and measurements; anthropogenic
emissions
ID ATMOSPHERIC CHEMISTRY; TIME SCALES; STRATOSPHERIC OZONE; TRANSPORT; N2O;
NOY; CFC-12; GASES; CYCLE
AB The lifetime of nitrous oxide, the third-most-important human-emitted greenhouse gas, is based to date primarily on model studies or scaling to other gases. This work calculates a semiempirical lifetime based on Microwave Limb Sounder satellite measurements of stratospheric profiles of nitrous oxide, ozone, and temperature; laboratory cross-section data for ozone and molecular oxygen plus kinetics for O(D-1); the observed solar spectrum; and a simple radiative transfer model. The result is 1169years. The observed monthly-to-biennial variations in lifetime and tropical abundance are well matched by four independent chemistry-transport models driven by reanalysis meteorological fields for the period of observation (2005-2010), but all these models overestimate the lifetime due to lower abundances in the critical loss region near 32km in the tropics. These models plus a chemistry-climate model agree on the nitrous oxide feedback factor on its own lifetime of 0.940.01, giving N2O perturbations an effective residence time of 109years. Combining this new empirical lifetime with model estimates of residence time and preindustrial lifetime (123years) adjusts our best estimates of the human-natural balance of emissions today and improves the accuracy of projected nitrous oxide increases over this century.
C1 [Prather, Michael J.; Hsu, Juno; DeLuca, Nicole M.] Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA.
[Jackman, Charles H.; Oman, Luke D.; Douglass, Anne R.; Fleming, Eric L.; Steenrod, Stephen D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.; Strahan, Susan E.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Steenrod, Stephen D.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Ctr, Columbia, MD USA.
[Sovde, O. Amund] Ctr Int Climate & Environm Res Oslo, Oslo, Norway.
[Isaksen, Ivar S. A.] Univ Oslo, Dept Geosci, Oslo, Norway.
[Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Funke, Bernd] CSIC, Inst Astrofis Andalucia, Granada, Spain.
RP Prather, MJ (reprint author), Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA.
EM mprather@uci.edu
RI Jackman, Charles/D-4699-2012; Douglass, Anne/D-4655-2012; Funke,
Bernd/C-2162-2008; Oman, Luke/C-2778-2009; Sovde Haslerud,
Amund/H-2850-2016;
OI Funke, Bernd/0000-0003-0462-4702; Oman, Luke/0000-0002-5487-2598; Sovde
Haslerud, Amund/0000-0002-3812-3837; Prather,
Michael/0000-0002-9442-8109
FU NASA [NNX09AJ47G, NNX13AL12G]; DOE [DE-SC0007021, DE-SC0012536]; UCI NSF
REU [1005042]; NASA MAP program; Spanish MCINN [AYA2011-23552]; EC FEDER
funds; NASA
FX Tabulated data sets used in the figures here will be posted at
ftp://halo.ess.uci.edu or are otherwise available from the corresponding
author (mprather@uci.edu). Research at UCI was supported by NASA grants
NNX09AJ47G and NNX13AL12G and DOE awards DE-SC0007021 and DE-SC0012536.
N.M.D. was supported by UCI NSF REU 1005042. The GEOSCCM contribution
was supported by the NASA MAP program. B.F. was supported by the Spanish
MCINN under grant AYA2011-23552 and EC FEDER funds. Work at the Jet
Propulsion Laboratory was performed under contract with NASA. The
assistance of Ryan Fuller (at JPL) for the creation of MLS data sets
used here is acknowledged. The GSFC 2-D model contribution was supported
by the NASA Atmospheric Composition: Modeling and Analysis Program.
NR 54
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2015
VL 120
IS 11
BP 5693
EP 5705
DI 10.1002/2015JD023267
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL5BV
UT WOS:000356975700024
ER
PT J
AU Bernard, F
McGillen, MR
Fleming, EL
Jackman, CH
Burkholder, JB
AF Bernard, Francois
McGillen, Max R.
Fleming, Eric L.
Jackman, Charles H.
Burkholder, James B.
TI CBrF3 (Halon-1301): UV absorption spectrum between 210 and 320 K,
atmospheric lifetime, and ozone depletion potential
SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY A-CHEMISTRY
LA English
DT Article
DE Bromotrifluoromethane; ozone depletion potential; UV absorption
spectrum; temperature dependence; photolysis lifetime
ID TEMPERATURE-DEPENDENCE; CROSS-SECTIONS; ULTRAVIOLET; METHANE; IMPACT;
PHASE; BR
AB CBrF3 (Halon-1301) is a man-made ozone depleting substance that is a major source of bromine in the Earth's stratosphere. Halon-1301 is predominantly removed from the atmosphere by UV photolysis in the stratosphere at wavelengths between 200 and 225 nm. The existing level of uncertainty in the Halon-1301 UV absorption spectrum temperature-dependence directly impacts the ability to model stratospheric ozone chemistry and climate change. In this work, the UV absorption spectrum of Halon-1301 between 195 and 235 nm was measured over the temperature range 210-320 K. An empirical parameterization of the spectrum and its temperature dependence is presented. The present results are critically compared with results from previous studies and the current recommendation for use in atmospheric models. A global annually averaged lifetime for Halon-1301 of 74.6 (73.7-75.5) years was calculated using a 2-D atmospheric model and the present results. The range of lifetimes given in parenthesis represents the possible values due solely to the 2 sigma uncertainty in the Halon-1301 UV spectrum obtained in this work. In addition, the CBrF3 ozone depletion potential was calculated using the 2-D model to be 18.6 (+/- 0.1) using the UV spectrum and 2 sigma uncertainty from this work. Published by Elsevier B.V.
C1 [Bernard, Francois; McGillen, Max R.; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Dept Commerce, Boulder, CO 80305 USA.
[Bernard, Francois; McGillen, Max R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, Dept Commerce, Boulder, CO 80305 USA.
EM james.b.burkholder@noaa.gov
RI Jackman, Charles/D-4699-2012; McGillen, Max/G-5196-2011; BERNARD,
Francois/F-2864-2014; Manager, CSD Publications/B-2789-2015
OI McGillen, Max/0000-0002-1623-5985; BERNARD,
Francois/0000-0002-6116-3167;
FU NOAA's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) Program;
NASA's Atmospheric Composition Program
FX This work was supported in part by NOAA's Atmospheric Chemistry, Carbon
Cycle, and Climate (AC4) Program and NASA's Atmospheric Composition
Program.
NR 19
TC 3
Z9 3
U1 0
U2 8
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1010-6030
J9 J PHOTOCH PHOTOBIO A
JI J. Photochem. Photobiol. A-Chem.
PD JUN 15
PY 2015
VL 306
BP 13
EP 20
DI 10.1016/j.jphotochem.2015.03.012
PG 8
WC Chemistry, Physical
SC Chemistry
GA CK3JJ
UT WOS:000356112100002
ER
PT J
AU Yavasli, DD
Tucker, CJ
Melocik, KA
AF Yavasli, Dogukan Dogu
Tucker, Compton J.
Melocik, Katherine A.
TI Change in the glacier extent in Turkey during the Landsat Era
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Mountain glaciers; Satellite data; Climate change; Turkey; Landsat;
ASTER
ID NORTH-ATLANTIC OSCILLATION; TRENDS; VARIABILITY; PRECIPITATION; NUMBERS;
COVER
AB We report the latest study for small glaciers, using Turkey as an example, and update previous studies of glaciers in Turkey from the 1970s to 2012-2013. We used seventy-two Landsat scenes from the Multispectral Scanner (MSS), Return Beam Vidicon-3 (RBV-3), Thematic Mapper (TM), Enhanced Thematic Mapper plus (ETM+), and Operational Land Imager (OLI); five Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) images; and forty-one commercial satellite images. IKONOS, Quickbird-2, GeoEye-1, and WorldView-1 and -2 commercial satellite images were used to evaluate mapping accuracies, to understand debris-covered glacial margins, to map glacier margins in shadows, and to better determine the area of the smaller glaciers in Turkey. We also used nine Landsat-5 simultaneously acquired TM and MSS images to more accurately process MSS imagery from the 1970s. The area of the glaciers in Turkey decreased from 25 km(2) in the 1970s to 10.85 km(2) in 2012-2013. By 2012-2013, five glaciers had disappeared, six were less than 0.5 km(2), one was 0.8 km(2), and only two were 3.0 km(2) or larger. No trends in 1980 to 2012 annual precipitation, 1980 to 2012 winter precipitation, and 1980 to 2008 cloud cover extent were found, while surface temperatures increased, with summer minimum temperatures showing the greatest increases. We attribute glacier recession in Turkey from the 1970s to 2012-2013 to increasing summer minimum temperatures with no changes in precipitation or cloud cover over this time period. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Yavasli, Dogukan Dogu] Ege Univ, Dept Geog, Izmir, Turkey.
[Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
RP Yavasli, DD (reprint author), Ege Univ, Dept Geog, Izmir, Turkey.
EM dogukan.yavasli@ege.edu.tr; compton.j.tucker@nasa.gov;
katherine.a.melocik@nasa.gov
RI Yavasli, Dogukan/D-7623-2015
OI Yavasli, Dogukan/0000-0002-0150-867X
NR 26
TC 4
Z9 4
U1 1
U2 8
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 JUN 15
PY 2015
VL 163
BP 32
EP 41
DI 10.1016/j.rse.2015.03.002
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CJ8RN
UT WOS:000355771300004
ER
PT J
AU Sorek-Hamer, M
Kloog, I
Koutrakis, P
Strawa, AW
Chatfield, R
Cohen, A
Ridgway, WL
Broday, DM
AF Sorek-Hamer, Meytar
Kloog, Itai
Koutrakis, Petros
Strawa, Anthony W.
Chatfield, Robert
Cohen, Ayala
Ridgway, William L.
Broday, David M.
TI Assessment of PM2.5 concentrations over bright surfaces using MODIS
satellite observations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Dark Target; Deep Blue; Aerosol optical depth (AOD); MODIS; PM2.5; Mixed
effects models
ID AEROSOL OPTICAL DEPTH; GROUND-LEVEL PM2.5; PARTICULATE MATTER
CONCENTRATIONS; IMAGING SPECTRORADIOMETER MODIS; AIR-QUALITY;
UNITED-STATES; RETRIEVALS; MORTALITY; THICKNESS; PRODUCTS
AB Exposure to particles with an aerodynamic diameter smaller than 2.5 mu m (PM2.5) adversely impacts human health. In many geographical regions where ground PM2.5 monitoring is spatially sparse and unsuitable for environmental health inference, satellite remote sensing can potentially be used for estimating human exposure to PM2.5. However, retrieval of the aerosol optical depth (AOD) using the Dark Target (DT) algorithm is uncertain in many regions worldwide (e.g. western USA, the Middle East and central Asia) due to low signal-to-noise ratio as a result of high surface reflectivity in the spectral bands used by the algorithm. In this study we use the Deep Blue (DB) algorithm as well as a combined DB-DT algorithm for AOD retrievals. The AOD products are used to predict ground PM2.5 using mixed effects models and the daily calibration approach. Models for the two study areas (Israel and San Joaquin Valley, Central California) were developed independently and then compared to each other. Using the AOD(DB) within a mixed effects model considerably improved PM2.5 prediction in high reflectance regions, revealing in both study areas enhanced model performance (in terms of both R-2 and the root mean square prediction error), significant increase in the spatiotemporal availability of the AOD product, and improved PM2.5 prediction relative to using AOD(DT) retrievals. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Sorek-Hamer, Meytar; Broday, David M.] Civil & Environm Engn, Haifa, Israel.
[Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, Beer Sheva, Israel.
[Koutrakis, Petros] Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02115 USA.
[Strawa, Anthony W.; Chatfield, Robert] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cohen, Ayala] Technion Israel Inst Technol, Ind & Management Engn, Haifa, Israel.
[Ridgway, William L.] Sci Syst & Applicat Inc, Lanham, MD 20771 USA.
RP Broday, DM (reprint author), Technion Israel Inst Technol, Civil & Environm Engn, Haifa, Israel.
EM dbroday@tx.technion.acil
OI Broday, David/0000-0002-6525-3979
FU Environment and Health Fund, Israel
FX M.S.H. would like to thank the Environment and Health Fund, Israel, for
supporting her studies with a doctoral fellowship, and NASA AMES
Research Center, CA, USA for hosting her in summer 2012. The research
was done at the Technion Center of Excellence in Exposure Science and
Environmental Health (TCEEH). The authors thank the reviewers for their
valuable comments.
NR 37
TC 9
Z9 9
U1 5
U2 38
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 JUN 15
PY 2015
VL 163
BP 180
EP 185
DI 10.1016/j.rse.2015.03.014
PG 6
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CJ8RN
UT WOS:000355771300016
ER
PT J
AU Schrijver, CJ
Kauristie, K
Aylward, AD
Denardini, CM
Gibson, SE
Glover, A
Gopalswamy, N
Grande, M
Hapgood, M
Heynderickx, D
Jakowski, N
Kalegaev, VV
Lapenta, G
Linker, JA
Liu, SP
Mandrini, CH
Mann, IR
Nagatsuma, T
Nandy, D
Obara, T
O'Brien, TP
Onsager, T
Opgenoorth, HJ
Terkildsen, M
Valladares, CE
Vilmer, N
AF Schrijver, Carolus J.
Kauristie, Kirsti
Aylward, Alan D.
Denardini, Clezio M.
Gibson, Sarah E.
Glover, Alexi
Gopalswamy, Nat
Grande, Manuel
Hapgood, Mike
Heynderickx, Daniel
Jakowski, Norbert
Kalegaev, Vladimir V.
Lapenta, Giovanni
Linker, Jon A.
Liu, Siqing
Mandrini, Cristina H.
Mann, Ian R.
Nagatsuma, Tsutomu
Nandy, Dibyendu
Obara, Takahiro
O'Brien, T. Paul
Onsager, Terrance
Opgenoorth, Hermann J.
Terkildsen, Michael
Valladares, Cesar E.
Vilmer, Nicole
TI Understanding space weather to shield society: A global road map for
2015-2025 commissioned by COSPAR and ILWS
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space weather; COSPAR/ILWS road map panel
ID INTERPLANETARY SCINTILLATION
AB There is a growing appreciation that the environmental conditions that we call space weather impact the technological infrastructure that powers the coupled economies around the world. With that comes the need to better shield society against space weather by improving forecasts, environmental specifications, and infrastructure design. We recognize that much progress has been made and continues to be made with a powerful suite of research observatories on the ground and in space, forming the basis of a Sun Earth system observatory. But the domain of space weather is vast extending from deep within the Sun to far outside the planetary orbits and the physics complex including couplings between various types of physical processes that link scales and domains from the microscopic to large parts of the solar system. Consequently, advanced understanding of space weather requires a coordinated international approach to effectively provide awareness of the processes within the Sun Earth system through observation-driven models. This roadmap prioritizes the scientific focus areas and research infrastructure that are needed to significantly advance our understanding of space weather of all intensities and of its implications for society. Advancement of the existing system observatory through the addition of small to moderate state-of-the-art capabilities designed to fill observational gaps will enable significant advances. Such a strategy requires urgent action: key instrumentation needs to be sustained, and action needs to be taken before core capabilities are lost in the aging ensemble. We recommend advances through priority focus (1) on observation-based modeling throughout the Sun Earth system, (2) on forecasts more than 12 h ahead of the magnetic structure of incoming coronal mass ejections, (3) on understanding the geospace response to variable solar-wind stresses that lead to intense geomagnetically-induced currents and ionospheric and radiation storms, and (4) on developing a comprehensive specification of space climate, including the characterization of extreme space storms to guide resilient and robust engineering of technological infrastructures. The roadmap clusters its implementation recommendations by formulating three action pathways, and outlines needed instrumentation and research programs and infrastructure for each of these. An executive summary provides an overview of all recommendations. (C) 2015 COSPAR. Published by Elsevier Ltd.
C1 [Schrijver, Carolus J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Kauristie, Kirsti] Finnish Meteorol Inst, FI-00560 Helsinki, Finland.
[Aylward, Alan D.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Denardini, Clezio M.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil.
[Gibson, Sarah E.] HAO NCAR, Boulder, CO 80307 USA.
[Glover, Alexi] RHEA Syst, D-64293 Darmstadt, Germany.
[Glover, Alexi] ESA SSA Programme Off, D-64293 Darmstadt, Germany.
[Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grande, Manuel] Aberystwyth Univ, Penglais STY23 3B, Scotland.
[Hapgood, Mike] RAL Space, Didcot OX11 0QX, Oxon, England.
[Hapgood, Mike] STFC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Heynderickx, Daniel] DH Consultancy BVBA, B-3000 Leuven, Belgium.
[Jakowski, Norbert] German Aerosp Ctr, D-17235 Neustrelitz, Germany.
[Kalegaev, Vladimir V.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119991, Russia.
[Lapenta, Giovanni] Katholieke Univ Leuven, B-3001 Leuven, Belgium.
[Linker, Jon A.] Predict Sci Inc, San Diego, CA 92121 USA.
[Liu, Siqing] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China.
[Mandrini, Cristina H.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Mann, Ian R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada.
[Nagatsuma, Tsutomu] Natl Inst Informat & Commun Technol, Space Weather & Environm Informat Lab, Tokyo 1848795, Japan.
[Nandy, Dibyendu] Ctr Excellence Space Sci, Kolkata 74125, Mohanpur, India.
[Nandy, Dibyendu] Indian Inst Sci Educ & Res, Kolkata 74125, Mohanpur, India.
Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[O'Brien, T. Paul] Aerosp Corp, Dept Space Sci, Chantilly, Chantilly, VA 20151 USA.
[Onsager, Terrance] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA.
[Opgenoorth, Hermann J.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden.
[Terkildsen, Michael] Space Weather Serv, Bur Meteorol, Surry Hills, NSW, Australia.
[Valladares, Cesar E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA.
[Vilmer, Nicole] Univ Paris Diderot, CNRS, Observ Paris, LENA, F-92195 Meudon, France.
RP Schrijver, CJ (reprint author), Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St, Palo Alto, CA 94304 USA.
EM schrijver@lmsal.com
RI De Nardin, Clezio/C-4103-2012; Grande, Manuel/C-2242-2013;
OI De Nardin, Clezio/0000-0002-3624-2461; Grande,
Manuel/0000-0002-2233-2618; Nagatsuma, Tsutomu/0000-0002-9334-0738;
Lapenta, Giovanni/0000-0002-3123-4024
NR 48
TC 22
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U1 2
U2 16
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JUN 15
PY 2015
VL 55
IS 12
BP 2745
EP 2807
DI 10.1016/j.asr.2015.03.023
PG 63
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CJ3FA
UT WOS:000355367600001
ER
PT J
AU Vaisberg, O
Artemyev, A
Avanov, L
AF Vaisberg, O.
Artemyev, A.
Avanov, L.
TI Nonadiabatic ion acceleration at the nightside highlatitude
magnetopause: Fine structure of the velocity distribution function
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Magnetopause; Magnetic reconnection; Ion acceleration
ID SHEARED MAGNETIC-FIELD; CURRENT SHEET ACCELERATION; INTERBALL TAIL
PROBE; GEOMAGNETIC TAIL; EARTHS MAGNETOPAUSE; PARTICLE MOTION;
RECONNECTION; MAGNETOTAIL; PLASMA; MODEL
AB In this paper we use Interball-tail observations and numerical modeling to investigate ion acceleration in reconnected nightside magnetopause. We consider magnetic field configuration corresponding to the superposition of the magnetopause current sheet and reconnected fluxtube, which moves tailward. This fluxtube creates normal component of the magnetic field and the transverse electric field component. Initial current sheet geometry includes tangential and shear components of the magnetic field. Interaction of cold magnetosheath ions with the reconnected current sheet results in particle acceleration and transition through the magnetopause. Reflected and transited ions form velocity distributions with a halo in the (v(parallel to),v(perpendicular to)) plane. Numerical modeling reproduce these velocity distributions quite well. Comparison of numerical results and spacecraft observation indicates that nonadibatic ion acceleration plays essential role in formation of such velocity distributions. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Vaisberg, O.] RAS, Space Res Inst, Moscow, Russia.
[Artemyev, A.; Avanov, L.] Univ Maryland, NASA, Goddard Space Flight Ctr, Baltimore, MD USA.
RP Vaisberg, O (reprint author), RAS, Space Res Inst, Moscow, Russia.
EM olegv@iki.rssi.ru; ante0226@gmail.com
NR 46
TC 0
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U1 1
U2 2
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 JUN 15
PY 2015
VL 55
IS 12
BP 2840
EP 2850
DI 10.1016/j.asr.2015.02.036
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CJ3FA
UT WOS:000355367600005
ER
PT J
AU Joseph, OO
Yamazak, Y
Cilliers, P
Baki, P
Ngwira, CM
Mito, C
AF Joseph, Olwendo Ouko
Yamazak, Yosuke
Cilliers, Pierre
Baki, Paul
Ngwira, Chigomezyo M.
Mito, Collins
TI A study on the response of the Equatorial Ionization Anomaly over the
East Africa sector during the geomagnetic storm of November 13, 2012
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE IGS; Ionospheric ionization anomaly; East African region; Geomagnetic
storm
ID TOTAL ELECTRON-CONTENT; IONOSPHERIC DISTURBANCE DYNAMO; INSTRUMENTAL
BIASES; REGION; TEC; SATELLITE; PERIODS; FIELDS; MODEL; JAPAN
AB Using a set of up to 12 International GNSS Services (IGS) receivers around the East African region, we present the formation of the peak of ionospheric Equatorial Ionization Anomaly during the geomagnetic storm of 13th November 2012. The diurnal pattern of total electron content (TEC) shows a strong negative storm during the main phase of the storm. Latitudinal variation of TEC shows development of strong Equatorial Ionization Anomaly (EIA) on the recovery phase. Evidence in terms of magnetic variations during the storm period, indicates that the penetration of interplanetary electric fields is the main cause of the negative ionospheric effect during the main phase of the storm. Observation shows the occurrence of very strong westward electric fields arising from the IMF Bz turning southward a few hours after sunset local time. TEC enhancement during the recovery phase on the 16th are attributed to the increased ionospheric disturbance dynamo electric fields. In addition the EIA crest was found to intensify in amplitude as well as expand in latitudinal extent. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Joseph, Olwendo Ouko] Pwani Univ, Sch Pure & Appl Sci, Dept Math & Phys, Kilifi, Kenya.
[Yamazak, Yosuke] Univ Lancaster, Dept Phys, Lancaster, England.
[Cilliers, Pierre] South African Natl Space Agcy, Space Sci Directorate, Hermanus, South Africa.
[Baki, Paul] Kenya Tech Univ, Sch Pure & Appl Sci, Dept Phys, Nairobi, Kenya.
[Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Mito, Collins] Univ Nairobi, Dept Phys, Nairobi, Kenya.
RP Joseph, OO (reprint author), Pwani Univ, Sch Pure & Appl Sci, Dept Math & Phys, POB 195-80108, Kilifi, Kenya.
EM castrajoseph@yahoo.com; y.yamaza-ki@lancaster.ac.uk;
pjcilliers@sansa.org.za; paul.baki@gmail.com; Collins@uonbi.ac.ke
NR 32
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U1 2
U2 6
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 JUN 15
PY 2015
VL 55
IS 12
BP 2863
EP 2872
DI 10.1016/j.asr.2015.03.011
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CJ3FA
UT WOS:000355367600007
ER
PT J
AU Harpold, AA
Molotch, NP
Musselman, KN
Bales, RC
Kirchner, PB
Litvak, M
Brooks, PD
AF Harpold, Adrian A.
Molotch, Noah P.
Musselman, Keith N.
Bales, Roger C.
Kirchner, Peter B.
Litvak, Marcy
Brooks, Paul D.
TI Soil moisture response to snowmelt timing in mixed-conifer subalpine
forests
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snowmelt; soil moisture; snow-vegetation interactions; cross-site
comparison
ID SURFACE-ENERGY EXCHANGES; WESTERN UNITED-STATES; HIGH-ELEVATION;
SIERRA-NEVADA; NEW-MEXICO; STREAMFLOW GENERATION; WATER RETENTION;
BOREAL FOREST; ACCUMULATION; COVER
AB Western US forest ecosystems and downstream water supplies are reliant on seasonal snowmelt. Complex feedbacks govern forest-snow interactions in which forests influence the distribution of snow and the timing of snowmelt but are also sensitive to snow water availability. Notwithstanding, few studies have investigated the influence of forest structure on snow distribution, snowmelt and soil moisture response. Using a multi-year record from co-located observations of snow depth and soil moisture, we evaluated the influence of forest-canopy position on snow accumulation and snow depth depletion, and associated controls on the timing of soil moisture response at Boulder Creek, Colorado, Jemez River Basin, New Mexico, and the Wolverton Basin, California. Forest-canopy controls on snow accumulation led to 12-42cm greater peak snow depths in open versus under-canopy positions. Differences in accumulation and melt across sites resulted in earlier snow disappearance in open positions at Jemez and earlier snow disappearance in under-canopy positions at Boulder and Wolverton sites. Irrespective of net snow accumulation, we found that peak annual soil moisture was nearly synchronous with the date of snow disappearance at all sites with an average deviation of 12, 3 and 22days at Jemez, Boulder and Wolverton sites, respectively. Interestingly, sites in the Sierra Nevada showed peak soil moisture prior to snow disappearance at both our intensive study site and the nearby snow telemetry stations. Our results imply that the duration of soil water stress may increase as regional warming or forest disturbance lead to earlier snow disappearance and soil moisture recession in subalpine forests. Copyright (c) 2014 John Wiley & Sons, Ltd.
C1 [Harpold, Adrian A.; Molotch, Noah P.] Univ Nevada, Insitutute Arctic & Alpine Res, Boulder, CO 80304 USA.
[Harpold, Adrian A.] Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Boulder, CO 80304 USA.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80304 USA.
[Molotch, Noah P.] Univ Colorado, INSTAAR, Boulder, CO 80304 USA.
[Musselman, Keith N.] Univ Calif Los Angeles, Civil & Environm Engn, Los Angeles, CA 90095 USA.
[Bales, Roger C.; Kirchner, Peter B.] Univ Calif, Sierra Nevada Res Inst, Merced, CA 95343 USA.
[Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Brooks, Paul D.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
RP Harpold, AA (reprint author), Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA.
EM aharpold@cabnr.unr.edu
RI Molotch, Noah/C-8576-2009;
OI Harpold, Adrian/0000-0002-2566-9574
FU NSF EAR Postdoctoral Fellowship [EAR 1144894]; Office of Science (BER)
at DOE; NSF CZO [EAR 724960, EAR 725097, EAR 724958]
FX The first author was supported by an NSF EAR Postdoctoral Fellowship
(EAR 1144894). The Office of Science (BER) at DOE and the NSF CZO (EAR
724960, EAR 725097 and EAR 724958) also provided support for this study.
NR 74
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U1 8
U2 39
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 JUN 15
PY 2015
VL 29
IS 12
BP 2782
EP 2798
DI 10.1002/hyp.10400
PG 17
WC Water Resources
SC Water Resources
GA CJ7TD
UT WOS:000355701700010
ER
PT J
AU Lin, YN
Jolivet, R
Simons, M
Agram, PS
Martens, HR
Li, Z
Lodi, SH
AF Lin, Y. N.
Jolivet, R.
Simons, M.
Agram, P. S.
Martens, H. R.
Li, Z.
Lodi, S. H.
TI High interseismic coupling in the Eastern Makran (Pakistan) subduction
zone
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Makran subduction zone; interseismic coupling; InSAR
ID CURRENT PLATE VELOCITIES; ACCRETIONARY WEDGE; CRUSTAL DEFORMATION; GPS
MEASUREMENTS; OKI EARTHQUAKE; MOTION MODEL; CHILE; FAULT; SLIP; IRAN
AB Estimating the extent of interseismic coupling along subduction zone megathrusts is essential for quantitative assessments of seismic and tsunami hazards. Up to now, quantifying the seismogenic potential of the eastern Makran subduction zone at the northern edge of the Indian ocean has remained elusive due to a paucity of geodetic observations. Furthermore, non-tectonic processes obscure the signature of accumulating elastic strain. Historical earthquakes of magnitudes greater than 7 have been reported. In particular, the 1945 Mw 8.1 earthquake resulted in a significant tsunami that swept the shores of the Arabian Sea and the Indian Ocean. A quantitative estimate of elastic strain accumulation along the subduction plate boundary in eastern Makran is needed to confront previous indirect and contradictory conclusions about the seismic potential in the region. Here, we infer the distribution of interseismic coupling on the eastern Makran megathrust from time series of satellite Interferometric Synthetic Aperture Radar (InSAR) images acquired between 2003 and 2010, applying a consistent series of corrections to extract the low amplitude, long wavelength deformation signal associated with elastic strain on the megathrust We find high interseismic coupling (i.e. the megathrust does not slip and elastic strain accumulates) in the central section of eastern Makran, where the 1945 earthquake occurred, while lower coupling coincides spatially with the subduction of the Sonne Fault Zone. The inferred accumulation of elastic strain since the 1943 earthquake is consistent with the future occurrence of magnitude 7+ earthquakes and we cannot exclude the possibility of a multi-segment rupture (Mw 8+). However, the likelihood for such scenarios might be modulated by partitioning of plate convergence between slip on the megathrust and internal deformation of the overlying, actively deforming, accretionary wedge. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Lin, Y. N.; Jolivet, R.; Simons, M.; Martens, H. R.] CALTECH, Seismol Lab, Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Agram, P. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Li, Z.] Newcastle Univ, Sch Civil Engn & Geosci, COMET, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Lodi, S. H.] NED Univ Engn & Technol, Dept Civil Engn, Karachi 75270, Pakistan.
[Jolivet, R.] Univ Cambridge, Dept Earth Sci, COMET, Bullard Labs, Cambridge CB3 0EZ, England.
RP Jolivet, R (reprint author), CALTECH, Seismol Lab, Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM rpj29@cam.ac.uk
RI Li, Zhenhong/F-8705-2010;
OI Li, Zhenhong/0000-0002-8054-7449; Jolivet, Romain/0000-0002-9896-3651;
Simons, Mark/0000-0003-1412-6395
NR 73
TC 4
Z9 4
U1 2
U2 13
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 JUN 15
PY 2015
VL 420
BP 116
EP 126
DI 10.1016/j.epsl.2015.03.037
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CH6LU
UT WOS:000354148900012
ER
PT J
AU Bhattacharjee, AK
Balakrishnan, K
Garcia, AL
Bell, JB
Donev, A
AF Bhattacharjee, Amit Kumar
Balakrishnan, Kaushik
Garcia, Alejandro L.
Bell, John B.
Donev, Aleksandar
TI Fluctuating hydrodynamics of multi-species reactive mixtures
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID STOCHASTIC DIFFERENTIAL-EQUATIONS; CHEMICAL LANGEVIN EQUATION;
REACTION-DIFFUSION MODEL; MONTE-CARLO METHOD; MASTER-EQUATION;
NONEQUILIBRIUM FLUCTUATIONS; MICROSCOPIC SIMULATION; HOMOGENEOUS
SYSTEMS; PATTERN-FORMATION; COMPLEX FLUIDS
AB We formulate and study computationally the fluctuating compressible Navier-Stokes equations for reactive multi-species fluid mixtures. We contrast two different expressions for the covariance of the stochastic chemical production rate in the Langevin formulation of stochastic chemistry, and compare both of them to predictions of the chemical master equation for homogeneous well-mixed systems close to and far from thermodynamic equilibrium. We develop a numerical scheme for inhomogeneous reactive flows, based on our previous methods for non-reactive mixtures [Balakrishnan, Phys. Rev. E 89, 013017 (2014)]. We study the suppression of non-equilibrium long-ranged correlations of concentration fluctuations by chemical reactions, as well as the enhancement of pattern formation by spontaneous fluctuations. Good agreement with available theory demonstrates that the formulation is robust and a useful tool in the study of fluctuations in reactive multi-species fluids. At the same time, several problems with Langevin formulations of stochastic chemistry are identified, suggesting that future work should examine combining Langevin and master equation descriptions of hydrodynamic and chemical fluctuations. (C) 2015 AIP Publishing LLC.
C1 [Bhattacharjee, Amit Kumar; Donev, Aleksandar] NYU, Courant Inst Math Sci, New York, NY 10012 USA.
[Balakrishnan, Kaushik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Garcia, Alejandro L.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Bell, John B.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA.
RP Bhattacharjee, AK (reprint author), NYU, Courant Inst Math Sci, 251 Mercer St, New York, NY 10012 USA.
RI Bhattacharjee, Amit/A-5596-2013
OI Bhattacharjee, Amit/0000-0002-1475-743X
FU U.S. Department of Energy Office of Science, Office of Advanced
Scientific Computing Research, Applied Mathematics program
[DE-SC0008271, DE-AC02-05CH11231]
FX We would like to thank M. Malek-Mansour, Jonathan Goodman, Eric
Vanden-Eijnden, Samuel Isaacson, Hans Christian Ottinger, Dick Bedeaux,
Annie Lemarchand, Florence Baras, John Pearson, Sorin Tanase Nicola, and
Signe Kjelstrup for informative discussions. This material is based upon
work supported by the U.S. Department of Energy Office of Science,
Office of Advanced Scientific Computing Research, Applied Mathematics
program under Award No. DE-SC0008271 and under Contract No.
DE-AC02-05CH11231.
NR 142
TC 9
Z9 9
U1 6
U2 12
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD JUN 14
PY 2015
VL 142
IS 22
AR 224107
DI 10.1063/1.4922308
PG 21
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CK4FG
UT WOS:000356176600009
PM 26071701
ER
PT J
AU Rozo, E
Rykoff, ES
Bartlett, JG
Melin, JB
AF Rozo, E.
Rykoff, E. S.
Bartlett, James G.
Melin, Jean-Baptiste
TI redMaPPer - III. A detailed comparison of the Planck 2013 and SDSS DR8
redMaPPer cluster catalogues
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: groups: general
ID MASSIVE GALAXY CLUSTERS; ALL-SKY SURVEY; X-RAY SEARCH; SCALING
RELATIONS; COSMOLOGICAL CONSTRAINTS; DATA RELEASE; MILKY-WAY; SZ;
PERFORMANCE; CHANDRA
AB We compare the Planck Sunyaev-Zeldovich (SZ) cluster sample (PSZ1) to the Sloan Digital Sky Survey (SDSS) redMaPPer catalogue, finding that all Planck clusters within the redMaPPer mask and within the redshift range probed by redMaPPer are contained in the redMaPPer cluster catalogue. These common clusters define a tight scaling relation in the richness-SZ mass (lambda-M-SZ) plane, with an intrinsic scatter in richness of sigma(lambda vertical bar MSZ) = 0.266 +/- 0.017. The corresponding intrinsic scatter in true cluster halo mass at fixed richness is approximate to 21 per cent. The regularity of this scaling relation is used to identify failures in both catalogues. The failure rates for redMaPPer and PSZ1 1.2 per cent and 14.7 per cent, respectively. The PSZ1 failure rates decreases to 9.8 per cent after removing incorrect redshifts that were drawn from the literature. We note the failure rates in the PSZ1 from this analysis are specific to the SDSS overlap region, and may not be indicative of failure rates over the full Planck survey. We have further identified five PSZ1 sources that suffer from projection effects (multiple rich systems along the line of sight of the SZ detection) and 17 new high-redshift (z greater than or similar to 0.6) cluster candidates of varying degrees of confidence.
C1 [Rozo, E.; Rykoff, E. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Bartlett, James G.] Univ Paris Diderot, Sorbonne Paris Cite, CEA Lrfu Observat Paris, APC,CNRS IN2P3, F-75205 Paris 13, France.
[Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Melin, Jean-Baptiste] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
RP Rozo, E (reprint author), SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
EM erozo@email.arizona.edu
FU US Department of Energy [DE-AC02-76SF00515]; Institut Universitaire de
France; National Aeronautics and Space Administration
FX The authors wish to thank the anonymous referee for comments that helped
improved the presentation of this work. We thank August Evrard for
comments on an early draft of this manuscript. We also thank Nabila
Aghanim for help with accessing the full Planck cluster catalogue and
validation table. This work was supported in part by the US Department
of Energy contract to SLAC no. DE-AC02-76SF00515. JGB gratefully
acknowledges support from the Institut Universitaire de France. A
portion of the research described in this paper was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 52
TC 15
Z9 15
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 11
PY 2015
VL 450
IS 1
BP 592
EP 605
DI 10.1093/mnras/stv605
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6BA
UT WOS:000356311600043
ER
PT J
AU Sutton, AD
Roberts, TP
Gladstone, JC
Walton, DJ
AF Sutton, Andrew D.
Roberts, Timothy P.
Gladstone, Jeanette C.
Walton, Dominic J.
TI The hyperluminous X-ray source candidate in IC 4320: another HLX bites
the dust
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; X-rays: binaries;
X-rays: galaxies
ID MASS BLACK-HOLE; ACTIVE GALACTIC NUCLEI; ESO 243-49 HLX-1; HOLMBERG IX
X-1; GALAXY NGC 2276; XMM-NEWTON; CARTWHEEL RING; OPTICAL
IDENTIFICATIONS; ULTRALUMINOUS STATE; ACCRETION FLOWS
AB The known members of the class of hyperluminous X-ray sources (HLXs) are few in number, yet they are of great interest as they are regarded as the likeliest intermediate-mass black hole (IMBH) candidates amongst the wider population of ultraluminous X-ray sources (ULXs). Here we report optical photometry and spectroscopy of an HLX candidate associated with the galaxy IC 4320, that reveal it is a background AGN. We discuss the implications of the exclusion of this object from the small number of well-studied HLXs, that appears to accentuate the difference in characteristics between the good IMBH candidate ESO 243-49 HLX-1 and the small handful of other HLXs.
C1 [Sutton, Andrew D.; Roberts, Timothy P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Sutton, Andrew D.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[Gladstone, Jeanette C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Walton, Dominic J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
RP Sutton, AD (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM andrew.d.sutton@nasa.gov
FU Science and Technology Facilities Council [ST/K000861/1, ST/L00075X/1];
ESO telescopes at the La Silla Paranal Observatory [090.D-0300(A),
092.D-0212(A)]
FX ADS and TPR acknowledge funding from the Science and Technology
Facilities Council as part of the consolidated grants ST/K000861/1 and
ST/L00075X/1. This work is based on observations made with ESO
telescopes at the La Silla Paranal Observatory under programme IDs
090.D-0300(A) and 092.D-0212(A). It is also based in part on
observations made by the Chandra X-ray Observatory, and made use of data
supplied by the UK Swift Science Data Centre at the University of
Leicester.
NR 63
TC 7
Z9 7
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 11
PY 2015
VL 450
IS 1
BP 787
EP 793
DI 10.1093/mnras/stv505
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6BA
UT WOS:000356311600054
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Adams, C
Adams, T
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, RA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Ast, S
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barker, D
Barnum, SH
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Bell, C
Belopolski, I
Bergmann, G
Berliner, JM
Bertolini, A
Bessis, D
Betzwieser, J
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Bose, S
Bosi, L
Bowers, J
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brannen, CA
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Bruckner, F
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Colombini, M
Constancio, M
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
Debreczeni, G
Degallaix, J
Deleeuw, E
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
De Rosa, R
DeRosa, RT
DeSalvo, R
Dhurandhar, S
Di az, M
Dietz, A
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Dmitry, K
Donovan, F
Dooley, KL
Doravari, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eichholz, J
Eikenberry, SS
Endroczi, G
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farr, B
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, R
Flaminio, R
Foley, E
Foley, S
Forsi, E
Forte, LA
Fotopoulos, N
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Garcia, J
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Gergely, L
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, KE
Gustafson, EK
Gustafson, R
Hall, B
Hall, E
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hong, T
Hooper, S
Horrom, T
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Hua, Z
Huang, V
Huerta, EA
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Huynh-Dinh, T
Iafrate, J
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jaranowski, P
Jimenez-Forteza, F
Johnson, WW
Jones, D
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasprzack, M
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kaufman, K
Kawabe, K
Kawamura, S
Kawazoe, F
Kefelian, F
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, W
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Koehlenbeck, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kremin, A
Kringel, V
Krishnan, B
Krolak, A
Kucharczyk, C
Kudla, S
Kuehn, G
Kumar, A
Kumar, DN
Kumar, P
Kumar, R
Kurdyumov, R
Kwee, P
Landry, M
Lantz, B
Larson, S
Lasky, PD
Lawrie, C
Lazzarini, A
Leaci, P
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, J
Lee, J
Leonardi, M
Leong, JR
Le Roux, A
Leroy, N
Letendre, N
Levine, B
Lewis, JB
Lhuillier, V
Li, TGF
Lin, AC
Littenberg, TB
Litvine, V
Liu, F
Liu, H
Liu, Y
Liu, Z
Lloyd, D
Lockerbie, NA
Lockett, V
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, MJ
Luck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Manca, GM
Mandel, I
Mandic, V
Mangano, V
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martellini, L
Martin, IW
Martin, RM
Martynov, D
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
May, G
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
Meacher, D
Meadors, GD
Mehmet, M
Meidam, J
Meier, T
Melatos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Mikhailov, EE
Milano, L
Miller, J
Minenkov, Y
Mingarelli, CMF
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moe, B
Mohan, M
Mohapatra, SRP
Mokler, F
Moraru, D
Moreno, G
Morgado, N
Mori, T
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nagy, MF
Nardecchia, I
Nash, T
Naticchioni, L
Nayak, R
Necula, V
Neri, I
Newton, G
Nguyen, T
Nishida, E
Nishizawa, A
Nitz, A
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TI Characterization of the LIGO detectors during their sixth science run
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE LIGO; gravitational waves; detector characterization
ID GRAVITATIONAL-WAVE DETECTOR; THERMAL NOISE; INTERFEROMETER; READOUT;
LASER
AB In 2009-2010, the Laser Interferometer Gravitational-Wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves (GWs) of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the GW readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources.
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[Haris, K.; Mazumder, N.; Pai, A.] CET, IISER TVM, Trivandrum 695016, Kerala, India.
[Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Larson, S.] Utah State Univ, Logan, UT 84322 USA.
[Lasky, P. D.; Melatos, A.; Pindor, B.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Liu, F.] Univ Brussels, B-1050 Brussels, Belgium.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartmento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Shah, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Vedovato, G.; Zendri, J-P] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Vecchio, Alberto/F-8310-2015; Ferrante, Isidoro/F-1017-2012; McClelland,
David/E-6765-2010; 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; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011;
Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; M,
Manjunath/N-4000-2014; Gammaitoni, Luca/B-5375-2009; Gorodetsky,
Michael/C-5938-2008; Prokhorov, Leonid/I-2953-2012; Heidmann,
Antoine/G-4295-2016; Ott, Christian/G-2651-2011; Marchesoni,
Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi,
Franco/K-1068-2016; Kumar, Prem/B-6691-2009; Pinto,
Innocenzo/L-3520-2016; Deleglise, Samuel/B-1599-2015; Neri,
Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Steinlechner,
Sebastian/D-5781-2013; Chen, Yanbei/A-2604-2013; Shaddock,
Daniel/A-7534-2011; Strigin, Sergey/I-8337-2012; Vicere,
Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring,
Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Graef,
Christian/J-3167-2015; Hild, Stefan/A-3864-2010; Bell,
Angus/E-7312-2011; Iyer, Bala R./E-2894-2012; Gemme,
Gianluca/C-7233-2008; Ottaway, David/J-5908-2015; Leonardi,
Matteo/G-9694-2015; prodi, giovanni/B-4398-2010; Danilishin,
Stefan/K-7262-2012; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012;
Tacca, Matteo/J-1599-2015; Garufi, Fabio/K-3263-2015; Di Virgilio,
Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms,
Jan/J-4359-2012; Ward, Robert/I-8032-2014;
OI Vecchio, Alberto/0000-0002-6254-1617; Ferrante,
Isidoro/0000-0002-0083-7228; McClelland, David/0000-0001-6210-5842;
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; Frey, Raymond/0000-0003-0341-2636;
Ciani, Giacomo/0000-0003-4258-9338; Miao, Haixing/0000-0003-4101-9958;
Howell, Eric/0000-0001-7891-2817; M, Manjunath/0000-0001-8710-0730;
Gammaitoni, Luca/0000-0002-4972-7062; Gorodetsky,
Michael/0000-0002-5159-2742; Heidmann, Antoine/0000-0002-0784-5175; Ott,
Christian/0000-0003-4993-2055; Marchesoni, Fabio/0000-0001-9240-6793;
Zhu, Xingjiang/0000-0001-7049-6468; Frasconi,
Franco/0000-0003-4204-6587; Deleglise, Samuel/0000-0002-8680-5170; Neri,
Igor/0000-0002-9047-9822; Steinlechner, Sebastian/0000-0003-4710-8548;
Shaddock, Daniel/0000-0002-6885-3494; Vicere,
Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Gehring,
Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Graef,
Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Iyer,
Bala R./0000-0002-4141-5179; Gemme, Gianluca/0000-0002-1127-7406; prodi,
giovanni/0000-0001-5256-915X; Danilishin, Stefan/0000-0001-7758-7493;
Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015;
Tacca, Matteo/0000-0003-1353-0441; Garufi, Fabio/0000-0003-1391-6168;
Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X;
Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439;
Principe, Maria/0000-0002-6327-0628; Del Pozzo,
Walter/0000-0003-3978-2030; Allen, Bruce/0000-0003-4285-6256; Granata,
Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577; Freise,
Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587;
Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard
F/0000-0002-8501-8669; 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; Bondu,
Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Husa,
Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298;
Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319;
Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200;
Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431;
Pierro, Vincenzo/0000-0002-6020-5521; Coccia,
Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Di
Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Swinkels,
Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci,
Fulvio/0000-0001-5475-4447; O'Shaughnessy, Richard/0000-0001-5832-8517;
Vedovato, Gabriele/0000-0001-7226-1320; Matichard,
Fabrice/0000-0001-8982-8418
FU United States National Science Foundation for the construction and
operation of the LIGO Laboratory; Science and Technology Facilities
Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare;
French Centre National de la Recherche Scientifique; Australian Research
Council; International Science Linkages program of the Commonwealth of
Australia; Council of Scientific and Industrial Research of India;
Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de
Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of
the Govern de les Illes Balears; Foundation for Fundamental Research on
Matter by the Netherlands Organization for Scientific Research; Polish
Ministry of Science and Higher Education; FOCUS Programme of Foundation
for Polish Science; Royal Society; Scottish Funding Council; Scottish
Universities Physics Alliance; National Aeronautics and Space
Administration; National Research Foundation of Korea; Industry Canada;
Province of Ontario through the Ministry of Economic Development and
Innovation; National Science and Engineering Research Council Canada;
Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation;
Research Corporation; Alfred P Sloan Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society, and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organization for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the Royal Society, the Scottish Funding
Council, the Scottish Universities Physics Alliance, The National
Aeronautics and Space Administration, the National Research Foundation
of Korea, Industry Canada and the Province of Ontario through the
Ministry of Economic Development and Innovation, the National Science
and Engineering Research Council Canada, the Carnegie Trust, the
Leverhulme Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P Sloan Foundation.
NR 60
TC 59
Z9 59
U1 13
U2 87
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 JUN 11
PY 2015
VL 32
IS 11
AR 115012
DI 10.1088/0264-9381/32/11/115012
PG 30
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA CJ1IX
UT WOS:000355238400013
ER
PT J
AU Ghisellini, G
Tagliaferri, G
Sbarrato, T
Gehrels, N
AF Ghisellini, G.
Tagliaferri, G.
Sbarrato, T.
Gehrels, N.
TI SDSS J013127.34-032100.1: a candidate blazar with an 11 billion solar
mass black hole at z=5.18
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE quasars: general; X-rays: general
ID ACTIVE GALACTIC NUCLEI; RADIO-LOUD QUASARS; X-RAY; FERMI BLAZARS; DATA
RELEASE; LINE REGION; SKY SURVEY; SWIFT; TELESCOPE; EMISSION
AB The radio-loud quasar SDSS J013127.34-032100.1 at a redshift z = 5.18 is one of the most distant radio-loud objects. The radio to optical flux ratio (i.e. the radio-loudness) of the source is large, making it a promising blazar candidate. Its overall spectral energy distribution, completed by the X-ray flux and spectral slope derived through Target of Opportunity Swift/X-ray Telescope observations, is interpreted by a non-thermal jet plus an accretion disc and molecular torus model. We estimate that its black hole mass is (1.1 +/- A 0.2) x 10(10) M-aS (TM) for an accretion efficiency eta = 0.08, scaling roughly linearly with eta. Although there is a factor a parts per thousand(3)2 of systematic uncertainty, this black hole mass is the largest found at these redshifts. We derive a viewing angle between 3 and 5 deg. This implies that there must be other (hundreds) sources with the same black hole mass of SDSS J013127.34-032100.1, but whose jets are pointing away from Earth. We discuss the problems posed by the existence of such large black hole masses at such redshifts, especially in jetted quasars. In fact, if they are associated with rapidly spinning black holes, the accretion efficiency is high, implying a slower pace of black hole growth with respect to radio-quiet quasars.
C1 [Ghisellini, G.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
[Sbarrato, T.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Ghisellini, G (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy.
EM gabriele.ghisellini@brera.inaf.it
OI Ghisellini, Gabriele/0000-0002-0037-1974; Sbarrato,
Tullia/0000-0002-3069-9399
FU NASA; National Science Foundation
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/Caltech,
funded by NASA. It also makes use of data products from the Two Micron
All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/Caltech,
funded by NASA and the National Science Foundation. Part of this work is
based on archival data and online service provided by the ASI Science
Data Center (ASDC).
NR 41
TC 3
Z9 3
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 11
PY 2015
VL 450
IS 1
BP L34
EP L38
DI 10.1093/mnrasl/slv042
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2WS
UT WOS:000355346000008
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Antolini, E
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Burnett, TH
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Charles, E
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Costamante, L
Cutini, S
De Angelis, A
De Palma, F
Dermer, CD
Digel, SW
Silva, EDCE
Drell, PS
Dubois, R
Escande, L
Favuzzi, C
Fegan, SJ
Ferrara, EC
Finke, J
Focke, WB
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Gustafsson, M
Hadasch, D
Hayashida, M
Hays, E
Healey, SE
Horan, D
Hou, X
Hughes, RE
Iafrate, G
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Mazziotta, MN
McConville, W
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Moretti, E
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nolan, PL
Norris, P
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piranomonte, S
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Ritz, S
Rochester, LS
Romani, RW
Roth, M
Sanchez, DA
Sbarra, C
Scargle, JD
Schalk, TL
Sgro, C
Shaw, MS
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Suson, DJ
Tajima, H
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wallace, E
Wang, P
Winer, BL
Wood, DL
Wood, KS
Zimmer, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Antolini, E.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Bouvier, A.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Burnett, T. H.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Costamante, L.
Cutini, S.
De Angelis, A.
De Palma, F.
Dermer, C. D.
Digel, S. W.
Silva, E. Do Couto E.
Drell, P. S.
Dubois, R.
Escande, L.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Finke, J.
Focke, W. B.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hayashida, M.
Hays, E.
Healey, S. E.
Horan, D.
Hou, X.
Hughes, R. E.
Iafrate, G.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knodlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Moretti, E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nolan, P. L.
Norris, P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piranomonte, S.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Ritz, S.
Rochester, L. S.
Romani, R. W.
Roth, M.
Sanchez, D. A.
Sbarra, C.
Scargle, J. D.
Schalk, T. L.
Sgro, C.
Shaw, M. S.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Suson, D. J.
Tajima, H.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wallace, E.
Wang, P.
Winer, B. L.
Wood, D. L.
Wood, K. S.
Zimmer, S.
TI SECOND CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE
AREA TELESCOPE (vol 743, 171, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Larsson, S.; Moretti, E.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Moretti, E.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, Inst Ciencies Espai IEEE, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France.
[Conrad, J.; Larsson, S.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, S-10691 Stockholm, Sweden.
[De Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[De Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Ferrara, E. C.; Gehrels, N.; Hays, E.; McConville, W.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Frailis, M.; Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hou, X.] Univ Bordeaux 1, IN2P3, CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knodlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knodlseder, J.] Univ Toulouse, GAHEC, IRAP, UPS OMP, Toulouse, France.
[McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Piranomonte, S.] Osserv Astron Roma, I-00040 Rome, Italy.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
RP Ackermann, M (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
EM elisabetta.cavazzuti@asdc.asi.it; sarac@slac.stanford.edu;
charles.dermer@nrl.navy.mil; lott@cenbg.in2p3.fr; gasparrini@asdc.asi.it
RI 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; Torres, Diego/O-9422-2016;
Orlando, E/R-5594-2016; Reimer, Olaf/A-3117-2013; Funk,
Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015
OI 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;
Torres, Diego/0000-0002-1522-9065; Reimer, Olaf/0000-0001-6953-1385;
Funk, Stefan/0000-0002-2012-0080; Johannesson,
Gudlaugur/0000-0003-1458-7036
NR 1
TC 1
Z9 1
U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 144
DI 10.1088/0004-637X/806/1/144
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300144
ER
PT J
AU Arai, T
Matsuura, S
Bock, J
Cooray, A
Kim, MG
Lanz, A
Lee, DH
Lee, HM
Sano, K
Smidt, J
Matsumoto, T
Nakagawa, T
Onishi, Y
Korngut, P
Shirahata, M
Tsumura, K
Zemcov, M
AF Arai, T.
Matsuura, S.
Bock, J.
Cooray, A.
Kim, M. G.
Lanz, A.
Lee, D. H.
Lee, H. M.
Sano, K.
Smidt, J.
Matsumoto, T.
Nakagawa, T.
Onishi, Y.
Korngut, P.
Shirahata, M.
Tsumura, K.
Zemcov, M.
TI MEASUREMENTS OF THE MEAN DIFFUSE GALACTIC LIGHT SPECTRUM IN THE
0.95-1.65 mu m BAND FROM CIBER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: general; scattering
ID INFRARED-BACKGROUND-EXPERIMENT; LOW-RESOLUTION SPECTRUM; 100 MICRON
CIRRUS; ZODIACAL LIGHT; MILKY-WAY; INTERSTELLAR GRAINS; SIZE
DISTRIBUTION; RED CAMERA; DUST CLOUD; H-I
AB We report measurements of the diffuse galactic light (DGL) spectrum in the near-infrared, spanning the wavelength range 0.95-1.65 mu m by the Cosmic Infrared Background ExpeRiment. Using the low-resolution spectrometer calibrated for absolute spectro-photometry, we acquired long-slit spectral images of the total diffuse sky brightness toward six high-latitude fields spread over four sounding rocket flights. To separate the DGL spectrum from the total sky brightness, we correlated the spectral images with a 100 mu m intensity map, which traces the dust column density in optically thin regions. The measured DGL spectrum shows no resolved features and is consistent with other DGL measurements in the optical and at near-infrared wavelengths longer than 1.8 mu m. Our result implies that the continuum is consistently reproduced by models of scattered starlight in the Rayleigh scattering regime with a few large grains.
C1 [Arai, T.; Matsuura, S.; Sano, K.; Matsumoto, T.; Nakagawa, T.; Onishi, Y.] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Dept Space Astron & Astrophys, Sagamihara, Kanagawa 2525210, Japan.
[Arai, T.; Tsumura, K.] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan.
[Bock, J.; Lanz, A.; Korngut, P.; Zemcov, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Bock, J.; Korngut, P.; Zemcov, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cooray, A.; Smidt, J.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Kim, M. G.; Lee, H. M.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Lee, D. H.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Matsumoto, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Shirahata, M.] Natl Astron Observ Japan, Natl Inst Nat Sci, Tokyo 1818588, Japan.
[Smidt, J.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Matsuura, S.] Kwansei Gakuin Univ, Dept Phys, Kobe, Hyogo 6691337, Japan.
RP Arai, T (reprint author), Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Dept Space Astron & Astrophys, Sagamihara, Kanagawa 2525210, Japan.
RI Matsuura, Shuji/B-5658-2016
OI Matsuura, Shuji/0000-0002-5698-9634
FU NASA APRA research grants [NNX07AI54G, NNG05WC18G, NNX07AG43G,
NNX07AJ24G, NNX10AE12G]; Jet Propulsion Laboratory's Director's Research
and Development Fund; KAKENHI from the Japan Society for the Promotion
of Science (JSPS) [2034, 18204018, 19540250, 21340047, 21111004,
26800112]; Ministry of Education, Culture, Sports, Science, and
Technology (MEXT); Pioneer Project from the Korea Astronomy and Space
Science Institute (KASI); NASA Postdoctoral Fellowship; NSF CAREER award
[AST-0645427]; JSPS Research Fellowship; NSF [AST-1313319];
[2012R1A4A1028713]
FX This work was supported by NASA APRA research grants NNX07AI54G,
NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was
provided by an award to J.B. from the Jet Propulsion Laboratory's
Director's Research and Development Fund. CIBER was supported by KAKENHI
(2034, 18204018, 19540250, 21340047, 21111004, and 26800112) from the
Japan Society for the Promotion of Science (JSPS), and the Ministry of
Education, Culture, Sports, Science, and Technology (MEXT). Korean
participation in CIBER was supported by the Pioneer Project from the
Korea Astronomy and Space Science Institute (KASI). We would like to
acknowledge the dedicated efforts of the sounding rocket staff at the
NASA Wallops Flight Facility and the White Sands Missile Range. P.K. and
M.Z. acknowledge support from a NASA Postdoctoral Fellowship, A.C.
acknowledges support from an NSF CAREER award, and T.A. acknowledges
support from the JSPS Research Fellowship for Young Scientists. A.C.
acknowledges support from an NSF CAREER award AST-0645427 and NSF
AST-1313319. H.M.L acknowledges support from grant 2012R1A4A1028713. We
thank T.D. Brandt for kindly providing data and models.
NR 48
TC 8
Z9 8
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 JUN 10
PY 2015
VL 806
IS 1
AR 69
DI 10.1088/0004-637X/806/1/69
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300069
ER
PT J
AU Boersma, C
Bregman, J
Allamandola, LJ
AF Boersma, C.
Bregman, J.
Allamandola, L. J.
TI PROPERTIES OF POLYCYCLIC AROMATIC HYDROCARBONS IN THE NORTHWEST PHOTON
DOMINATED REGION OF NGC 7023. III. QUANTIFYING THE TRADITIONAL PROXY FOR
PAH CHARGE AND ASSESSING ITS ROLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: individual objects (NGC 7023);
techniques: spectroscopic
ID INFRARED-EMISSION BANDS; SPITZER-SPACE-TELESCOPE; BLIND SIGNAL
SEPARATION; HERBIG AE/BE STARS; SPECTROSCOPIC DATABASE; FEATURES;
EXCITATION; NGC-7023; GALAXIES; SPECTRUM
AB Polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer/IRS spectral map of the northwest photon dominated region (PDR) in NGC 7023 is analyzed. Here, results from fitting the 5.2-14.5 mu m spectrum at each pixel using exclusively PAH spectra from the NASA Ames PAH IR Spectroscopic Database (www.astrochem.org/pahdb/) and observed PAH band strength ratios, determined after isolating the PAH bands, are combined. This enables the first quantitative and spectrally consistent calibration of PAH charge proxies. Calibration is straightforward because the 6.2/11.2 mu m PAH band strength ratio varies linearly with the ionized fraction (PAH ionization parameter) as determined from the intrinsic properties of the individual PAHs comprising the database. This, in turn, can be related to the local radiation field, electron density, and temperature. From these relations diagnostic templates are developed to deduce the PAH ionization fraction and astronomical environment in other objects. The commonly used 7.7/11.2 mu m PAH band strength ratio fails as a charge proxy over a significant fraction of the nebula. The 11.2/12.7 mu m PAH band strength ratio, commonly used as a PAH erosion indicator, is revealed to be a better tracer for PAH charge across NGC 7023. Attempting to calibrate the 12.7/11.2 mu m PAH band strength ratio against the PAH hydrogen adjacency ratio (duo+trio)/solo is, unexpectedly, anti-correlated. This work both validates and extends the results from Paper I and Paper II.
C1 [Boersma, C.; Bregman, J.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM Christiaan.Boersma@nasa.gov
FU NASA [1407]; NASA's Laboratory Astrophysics, Carbon in the Galaxy/
consortium grant [NNH10ZDA001N]; NASA's Astrobiology; Astronomy +
Physics Research and Analysis (APRA) [NNX07AH02G]; Spitzer Space
Telescope Support Programs [50082]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. Support
from NASA's Laboratory Astrophysics, Carbon in the Galaxy/ consortium
grant (NNH10ZDA001N); and NASA's Astrobiology; Astronomy + Physics
Research and Analysis (APRA; NNX07AH02G), and Spitzer Space Telescope
Support Programs (50082) are greatly acknowledged. C.B. is grateful for
an appointment at NASA Ames Research Center through the San Jose State
University Research Foundation (NNX14AG80A).
NR 37
TC 10
Z9 10
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 JUN 10
PY 2015
VL 806
IS 1
AR 121
DI 10.1088/0004-637X/806/1/121
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300121
ER
PT J
AU Bowler, BP
Shkolnik, EL
Liu, MC
Schlieder, JE
Mann, AW
Dupuy, TJ
Hinkley, S
Crepp, JR
Johnson, JA
Howard, AW
Flagg, L
Weinberger, AJ
Aller, KM
Allers, KN
Best, WMJ
Kotson, MC
Montet, BT
Herczeg, GJ
Baranec, C
Riddle, R
Law, NM
Nielsen, EL
Wahhaj, Z
Biller, BA
Hayward, TL
AF Bowler, Brendan P.
Shkolnik, Evgenya L.
Liu, Michael C.
Schlieder, Joshua E.
Mann, Andrew W.
Dupuy, Trent J.
Hinkley, Sasha
Crepp, Justin R.
Johnson, John Asher
Howard, Andrew W.
Flagg, Laura
Weinberger, Alycia J.
Aller, Kimberly M.
Allers, Katelyn N.
Best, William M. J.
Kotson, Michael C.
Montet, Benjamin T.
Herczeg, Gregory J.
Baranec, Christoph
Riddle, Reed
Law, Nicholas M.
Nielsen, Eric L.
Wahhaj, Zahed
Biller, Beth A.
Hayward, Thomas L.
TI PLANETS AROUND LOW-MASS STARS (PALMS). V. AGE-DATING LOW-MASS COMPANIONS
TO MEMBERS AND INTERLOPERS OF YOUNG MOVING GROUPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; brown dwarfs; stars: individual (2MASS
J02155892, 0929121, 2MASS J15594729+4403595, HD 23514)
ID TW-HYDRAE ASSOCIATION; DIGITAL SKY SURVEY; VERY-LOW MASS; BRIGHT SOURCE
CATALOG; X-RAY SOURCES; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; CANDIDATE
SUBSTELLAR COMPANION; SUPERNOVA FACTORY OBSERVATIONS; FINDING CAMPAIGN
DISCOVERY; EXTRASOLAR GIANT PLANETS
AB We present optical and near-infrared adaptive optics (AO) imaging and spectroscopy of 13 ultracool (>M6) companions to late-type stars (K7-M4.5), most of which have recently been identified as candidate members of nearby young moving groups (YMGs; 8-120 Myr) in the literature. Three of these are new companions identified in our AO imaging survey, and two others are confirmed to be comoving with their host stars for the first time. The inferred masses of the companions (similar to 10-100 M-Jup) are highly sensitive to the ages of the primary stars; therefore we critically examine the kinematic and spectroscopic properties of each system to distinguish bona fide YMG members from old field interlopers. The new M7 substellar companion 2MASS J02155892-0929121 C (40-60 M-Jup) shows. clear spectroscopic signs of low gravity and, hence, youth. The primary, possibly a member of the similar to 40 Myr Tuc-Hor moving group, is visually resolved into three components, making it a young low-mass quadruple system in a compact (less than or similar to 100 AU) configuration. In addition, LiI lambda 6708 absorption in the intermediate-gravity M7.5 companion 2MASS J15594729+4403595 B provides unambiguous evidence that it is young (less than or similar to 200 Myr) and resides below the hydrogen-burning limit. Three new close-separation (<1 '') companions (2MASS J06475229-2523304 B, PYC J11519+0731 B, and GJ 4378 Ab) orbit stars previously reported as candidate YMG members, but instead are likely old (greater than or similar to 1Gyr) tidally locked spectroscopic binaries without convincing kinematic associations with any known moving group. The high rate of false positives in the form of old active stars with YMG-like kinematics underscores the importance of radial velocity and parallax measurements to validate candidate young stars identified via proper motion and activity selection alone. Finally, we spectroscopically confirm the cool temperature and substellar nature of HD 23514 B, a recently discovered M8 benchmark brown dwarf orbiting the dustiest-known member of the Pleiades.
C1 [Bowler, Brendan P.; Montet, Benjamin T.; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA.
[Shkolnik, Evgenya L.; Flagg, Laura] Lowell Observ, Flagstaff, AZ 86001 USA.
[Liu, Michael C.; Howard, Andrew W.; Aller, Kimberly M.; Best, William M. J.; Kotson, Michael C.; Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Schlieder, Joshua E.] NASA, Ames Res Ctr, Postdoctoral Program Fellow, Moffett Field, CA 94035 USA.
[Mann, Andrew W.; Dupuy, Trent J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hinkley, Sasha] Univ Exeter, Phys & Astron, Exeter EX4 4QL, Devon, England.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Johnson, John Asher; Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Flagg, Laura] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
[Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Allers, Katelyn N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA.
[Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Nielsen, Eric L.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Nielsen, Eric L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA USA.
[Wahhaj, Zahed] European So Observ, Santiago, Chile.
[Biller, Beth A.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Hayward, Thomas L.] Southern Operat Ctr AURA, Gemini Observ, La Serena, Chile.
RP Bowler, BP (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM bpbowler@caltech.edu
OI Montet, Benjamin/0000-0001-7516-8308; Nielsen, Eric/0000-0001-6975-9056;
Herczeg, Gregory/0000-0002-7154-6065
FU NASA Grant [NNX11AC31G]; NSF Grant [AST09-09222]; National Science
Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba
Astronomical Foundation; Alfred P. Sloan Foundation; National Science
Foundation Graduate Research Fellowship [DGE1144469]; National
Aeronautics and Space Administration; National Science Foundation
FX We thank the referee for their helpful suggestions and Niall Deacon for
obtaining some of the IRTF observations presented here. M.C.L. has been
supported by NASA Grant NNX11AC31G and NSF Grant AST09-09222. This paper
is based on observations at Cerro Tololo Inter-American Observatory,
National Optical Astronomy Observatory (NOAO Prop. ID: 2014B-0083; PI:
Bowler), which is operated by the Association of Universities for
Research in Astronomy (AURA) under a cooperative agreement with the
National Science Foundation. This research is also based in part on
observations obtained at the Gemini Observatory, which is operated by
AURA 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). The Robo-AO
system was developed by collaborating partner institutions, the
California Institute of Technology and the Inter-University Centre for
Astronomy and Astrophysics, and with the support of the National Science
Foundation under Grants AST-0906060, AST-0960343, and AST-1207891, the
Mt. Cuba Astronomical Foundation, and by a gift from Samuel Oschin.
Ongoing science operation support of Robo-AO is provided by the
California Institute of Technology and the University of Hawai'i. C.B.
acknowledges support from the Alfred P. Sloan Foundation. B.T.M. is
supported by a National Science Foundation Graduate Research Fellowship
under Grant DGE1144469. We utilized data products from the Two Micron
All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation. NASA's Astrophysics
Data System Bibliographic Services together with the VizieR catalog
access tool and SIMBAD database operated at CDS, Strasbourg, France,
were invaluable resources for this work. This research has made use of
the Washington Double Star Catalog maintained at the U.S. Naval
Observatory. Finally, mahalo nui loa to the kama'aina of Hawai'i for
their support of Keck and the Maunakea observatories. We are grateful to
conduct observations from this mountain.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 62
DI 10.1088/0004-637X/806/1/62
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300062
ER
PT J
AU Brodwin, M
Greer, CH
Leitch, EM
Stanford, SA
Gonzalez, AH
Gettings, DP
Abdulla, Z
Carlstrom, JE
Decker, B
Eisenhardt, PR
Lin, HW
Mantz, AB
Marrone, DP
McDonald, M
Stalder, B
Stern, D
Wylezalek, D
AF Brodwin, M.
Greer, C. H.
Leitch, E. M.
Stanford, S. A.
Gonzalez, A. H.
Gettings, D. P.
Abdulla, Z.
Carlstrom, J. E.
Decker, B.
Eisenhardt, P. R.
Lin, H. W.
Mantz, A. B.
Marrone, D. P.
McDonald, M.
Stalder, B.
Stern, D.
Wylezalek, D.
TI THE MASSIVE AND DISTANT CLUSTERS OF WISE SURVEY. III. SUNYAEV-ZEL'DOVICH
MASSES OF GALAXY CLUSTERS AT z similar to 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; galaxies:
clusters: intracluster medium; galaxies: high-redshift; infrared:
galaxies
ID SOUTH-POLE TELESCOPE; 720 SQUARE DEGREES; X-RAY-PROPERTIES;
SPECTROSCOPIC CONFIRMATION; STAR-FORMATION; COSMOLOGICAL IMPLICATIONS;
SKY SURVEY; DISCOVERY; SAMPLE; CATALOG
AB We present CARMA 30 GHz Sunyaev-Zel'dovich (SZ) observations of five high-redshift (z greater than or similar to 1), infrared-selected galaxy clusters discovered as part of the all-sky Massive and Distant Clusters of WISE Survey (MaDCoWS). The SZ decrements measured toward these clusters demonstrate that the MaDCoWS selection is discovering evolved, massive galaxy clusters with hot intracluster gas. Using the SZ scaling relation calibrated with South Pole Telescope clusters at similar masses and redshifts, we find these MaDCoWS clusters have masses in the range M-200 approximate to 2-6 x 10(14) M-circle dot. Three of these are among the most massive clusters found to date at z greater than or similar to 1, demonstrating that MaDCoWS is sensitive to the most massive clusters to at least z = 1.3. The added depth of the AllWISE data release will allow all-sky infrared cluster detection to z approximate to 1.5 and beyond.
C1 [Brodwin, M.; Decker, B.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Greer, C. H.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA.
[Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
[Gonzalez, A. H.; Gettings, D. P.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Eisenhardt, P. R.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lin, H. W.; Stalder, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Wylezalek, D.] European So Observ, Garching, Germany.
RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
OI Marrone, Daniel/0000-0002-2367-1080
FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris
Foundation; James S. McDonnell Foundation; Associates of the California
Institute of Technology; University of Chicago; state of California;
state of Illinois; state of Maryland; National Science Foundation; CARMA
partner universities; NSF [AST-1140019]; National Aeronautics and Space
Administration; NASA Astrophysics Data Analysis Program (ADAP)
[NNX12AE15G]; NASA Keck PI Data Award; W. M. Keck Foundation;
[PHY-0114422]; [GN-2013A-Q-44]; [GN-2013B-Q-8]
FX We thank the anonymous referee for helpful comments that improved the
paper. We thank L. Bleem for providing the code and data to produce
Figure 4 and B. Benson for helpful conversations. Support for CARMA
construction was derived from the Gordon and Betty Moore Foundation; the
Kenneth T. and Eileen L. Norris Foundation; the James S. McDonnell
Foundation; the Associates of the California Institute of Technology;
the University of Chicago; the states of California, Illinois, and
Maryland; 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; the work at
Chicago was supported by NSF grant AST-1140019. Additional support was
provided by PHY-0114422. 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. M.B., D.P.G., A.H.G., and S.A.S.
acknowledge support for this research from the NASA Astrophysics Data
Analysis Program (ADAP) through grant NNX12AE15G. This work was
supported by a NASA Keck PI Data Award, administered by the NASA
Exoplanet Science Institute. This work is based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. This work is 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 the National Aeronautics and Space Administration. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. Based in part 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). Data were obtained in
Program IDs GN-2013A-Q-44 and GN-2013B-Q-8. This paper includes data
gathered with the 6.5 meter Magellan Telescopes located at Las Campanas
Observatory, Chile.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 26
DI 10.1088/0004-637X/806/1/26
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300026
ER
PT J
AU Cohen, O
Ma, Y
Drake, JJ
Glocer, A
Garraffo, C
Bell, JM
Gombosi, TI
AF Cohen, O.
Ma, Y.
Drake, J. J.
Glocer, A.
Garraffo, C.
Bell, J. M.
Gombosi, T. I.
TI THE INTERACTION OF VENUS-LIKE, M-DWARF PLANETS WITH THE STELLAR WIND OF
THEIR HOST STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); planets and satellites: atmospheres; planets
and satellites: magnetic fields; planets and satellites: terrestrial
planets
ID RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY;
CLOSE-IN EXOPLANETS; MASS M-STARS; HABITABLE ZONES; HOT JUPITERS;
GANYMEDES MAGNETOSPHERE; TERRESTRIAL EXOPLANETS; ATMOSPHERIC ESCAPE
AB We study the interaction between the atmospheres of Venus-like, non-magnetized exoplanets orbiting an M-dwarf star, and the stellar wind using a multi-species MHD model. We focus our investigation on the effect of enhanced stellar wind and enhanced EUV flux as the planetary distance from the star decreases. Our simulations reveal different topologies of the planetary space environment for sub- and super-Alfvenic stellar wind conditions, which could lead to dynamic energy deposition into the atmosphere during the transition along the planetary orbit. We find that the stellar wind penetration for non-magnetized planets is very deep, up to a few hundreds of kilometers. We estimate a lower limit for the atmospheric mass-loss rate and find that it is insignificant over the lifetime of the planet. However, we predict that when accounting for atmospheric ion acceleration, a significant amount of the planetary atmosphere could be eroded over the course of a billion years.
C1 [Cohen, O.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ma, Y.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Glocer, A.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Bell, J. M.] NIA, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA.
[Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Gombosi, Tamas/G-4238-2011;
OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215
FU Smithsonian Institution Consortium; Smithsonian Institute Competitive
Grants Program for Science (CGPS) grant "Can Exoplanets Around Red
Dwarfs Maintain Habitable Atmospheres?"; NASA Astrobiology Institute
grant [NNX15AE05G]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; NASA
[NAS8-03060]
FX We thank an anonymous referee for his/her useful comments. The work
presented here was funded by the Smithsonian Institution Consortium for
Unlocking the Mysteries of the Universe grant "Lessons from Mars: Are
Habitable Atmospheres on Planets around M Dwarfs Viable?", by the
Smithsonian Institute Competitive Grants Program for Science (CGPS)
grant "Can Exoplanets Around Red Dwarfs Maintain Habitable
Atmospheres?", and by NASA Astrobiology Institute grant NNX15AE05G.
Simulation results were obtained using the Space Weather Modeling
Framework, developed by the Center for Space Environment Modeling, at
the University of Michigan with funding support from NASA ESS, NASA
ESTO-CT, NSF KDI, and DoD MURI. The simulations were performed on the
Smithsonian Institute HYDRA cluster. J.J.D. was supported by NASA
contract NAS8-03060 to the Chandra X-ray Center during the course of
this research and thanks the Director, B. Wilkes, for continuing support
and encouragement.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 41
DI 10.1088/0004-637X/806/1/41
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300041
ER
PT J
AU Czakon, NG
Sayers, J
Mantz, A
Golwala, SR
Downes, TP
Koch, PM
Lin, KY
Molnar, SM
Moustakas, LA
Mroczkowski, T
Pierpaoli, E
Shitanishi, JA
Siegel, S
Umetsu, K
AF Czakon, N. G.
Sayers, J.
Mantz, A.
Golwala, S. R.
Downes, T. P.
Koch, P. M.
Lin, K. -Y.
Molnar, S. M.
Moustakas, L. A.
Mroczkowski, T.
Pierpaoli, E.
Shitanishi, J. A.
Siegel, S.
Umetsu, K.
TI GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV-ZEL'DOVICH
EFFECT AND CHANDRA X-RAY MEASUREMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium
ID SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; 720 SQUARE DEGREES;
COSMOLOGICAL CONSTRAINTS; MACS J0717.5+3745; SECONDARY CALIBRATORS;
TEMPERATURE RELATION; OBSERVED GROWTH; RICH CLUSTERS; XMM-NEWTON
AB We present scaling relations between the integrated Sunyaev-Zel'dovich effect (SZE) signal, Y-SZ, its X-ray analogue, Y-X = MgasTX, and total mass, M-tot, for the 45 galaxy clusters in the Bolocam X-ray SZ (BOXSZ) sample. All parameters are integrated within r(2500). Y-2500 values are measured using SZE data collected with Bolocam, operating at 140 GHz at the Caltech Submillimeter Observatory. The temperature, T-X, and mass, M-gas,M- 2500, of the intracluster medium are determined using X-ray data collected with Chandra, and M-tot is derived from M-gas assuming a constant gas mass fraction. Our analysis accounts for several potential sources of bias, including selection effects, contamination from radio point sources, and the loss of SZE signal due to noise filtering and beam-smoothing effects. We measure the Y-2500-Y-X scaling to have a power-law index of 0.84 +/- 0.07, and a fractional intrinsic scatter in Y-2500 of (21 +/- 7)% at fixed Y-X, both of which are consistent with previous analyses. We also measure the scaling between Y-2500 and M-2500, finding a power-law index of 1.06 +/- 0.12 and a fractional intrinsic scatter in Y-2500 at fixed mass of (25 +/- 9)%. While recent SZE scaling relations using X-ray mass proxies have found power-law indices consistent with the self-similar prediction of 5/3, our measurement stands apart by differing from the self-similar prediction by approximately 5 sigma. Given the good agreement between the measured Y-2500-Y-X scalings, much of this discrepancy appears to be caused by differences in the calibration of the X-ray mass proxies adopted for each particular analysis.
C1 [Czakon, N. G.; Koch, P. M.; Lin, K. -Y.; Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Sayers, J.; Golwala, S. R.; Downes, T. P.; Siegel, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Molnar, S. M.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan.
[Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mroczkowski, T.] Naval Res Lab, Washington, DC 20375 USA.
[Pierpaoli, E.; Shitanishi, J. A.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
RP Czakon, NG (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM czakon@asiaa.sinica.edu.tw
OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu,
Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360;
Pierpaoli, Elena/0000-0002-7957-8993
FU Gordon and Betty Moore Foundation; Jet Propulsion Laboratory Research
and Technology Development Program; National Science Council of Taiwan
[NSC100-2112-M-001-008-MY3]; NASA Graduate Student Research Fellowship;
NASA Postdoctoral Program; Norris Foundation CCAT Postdoctoral
Fellowship; NSF [AST-0838187, AST-1140019]; NASA - Chandra X-ray Center
[PF0-110077]; NASA [NAS8-03060]; National Research Council Fellowship;
Academia Sinica Career Development Award; [NSF/AST-9618798];
[NSF/AST-0098737]; [NSF/AST-9980846]; [NSF/AST-0229008];
[NSF/AST-0206158]; [NASA/NNX07AH59G]
FX This material is based upon work at the CSO, which, when the data used
in this analysis were taken, was operated by the California Institute of
Technology under cooperative agreement with the National Science
Foundation. Bolocam was constructed and commissioned using funds from
NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and
NSF/AST-0206158. Bolocam observations were partially supported by the
Gordon and Betty Moore Foundation, the Jet Propulsion Laboratory
Research and Technology Development Program, as well as the National
Science Council of Taiwan grant NSC100-2112-M-001-008-MY3. We
acknowledge the assistance of: the Bolocam instrument team: P.A.R. Ade,
J.E. Aguirre, J.J. Bock, S.F. Edgington, J. Glenn, A. Goldin, S.R.
Golwala, D. Haig, A.E. Lange, G.T. Laurent, P.D. Mauskopf, H.T. Nguyen,
P. Rossinot, and J. Sayers; Matt Ferry, who helped collect the data for
Abell 1835 and MS 1054.4-0321; the day crew and Hilo staff of the CSO,
who provided invaluable assistance during commissioning and data-taking
for this survey data set; and Kathy Deniston, Barbara Wertz, and Diana
Bisel, who provided effective administrative support at Caltech and in
Hilo. This research made extensive use of high performance computing
resources at the U.S. Planck Data Center, which is a part of the
Infrared Processing and Analysis Center at Caltech. We also thank an
anonymous referee for a detailed report that substantially improved the
quality of this paper. N.C. was partially supported by a NASA Graduate
Student Research Fellowship; J.S. was partially supported by a NASA
Graduate Student Research Fellowship, a NASA Postdoctoral Program
fellowship, and a Norris Foundation CCAT Postdoctoral Fellowship; A.M.
was funded by NSF AST-0838187 and AST-1140019. The work of L.A.M. was
carried out at Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA; support for T.M. was provided by
NASA through Einstein Fellowship Program grant No. PF0-110077 awarded by
the Chandra X-ray Center, which is operated by the Smithsonian
Astrophysical Observatory for NASA under contract NAS8-03060, and by a
National Research Council Fellowship. E.P. and J.A.S. were partially
supported by NASA/NNX07AH59G. K.U. acknowledges partial support from the
Academia Sinica Career Development Award.
NR 109
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
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DI 10.1088/0004-637X/806/1/18
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300018
ER
PT J
AU De Rosa, G
Peterson, BM
Ely, J
Kriss, GA
Crenshaw, DM
Horne, K
Korista, KT
Netzer, H
Pogge, RW
Arevalo, P
Barth, AJ
Bentz, MC
Brandt, WN
Breeveld, AA
Brewer, BJ
Bonta, ED
De Lorenzo-Caceres, A
Denney, KD
Dietrich, M
Edelson, R
Evans, PA
Fausnaugh, MM
Gehrels, N
Gelbord, JM
Goad, MR
Grier, CJ
Grupe, D
Hall, PB
Kaastra, J
Kelly, BC
Kennea, JA
Kochanek, CS
Lira, P
Mathur, S
McHardy, IM
Nousek, JA
Pancoast, A
Papadakis, I
Pei, L
Schimoia, JS
Siegel, M
Starkey, D
Treu, T
Uttley, P
Vaughan, S
Vestergaard, M
Villforth, C
Yan, H
Young, S
Zu, Y
AF De Rosa, G.
Peterson, B. M.
Ely, J.
Kriss, G. A.
Crenshaw, D. M.
Horne, Keith
Korista, K. T.
Netzer, H.
Pogge, R. W.
Arevalo, P.
Barth, A. J.
Bentz, M. C.
Brandt, W. N.
Breeveld, A. A.
Brewer, B. J.
Bonta, E. Dalla
De Lorenzo-Caceres, A.
Denney, K. D.
Dietrich, M.
Edelson, R.
Evans, P. A.
Fausnaugh, M. M.
Gehrels, N.
Gelbord, J. M.
Goad, M. R.
Grier, C. J.
Grupe, D.
Hall, P. B.
Kaastra, J.
Kelly, B. C.
Kennea, J. A.
Kochanek, C. S.
Lira, P.
Mathur, S.
McHardy, I. M.
Nousek, J. A.
Pancoast, A.
Papadakis, I.
Pei, L.
Schimoia, J. S.
Siegel, M.
Starkey, D.
Treu, T.
Uttley, P.
Vaughan, S.
Vestergaard, M.
Villforth, C.
Yan, H.
Young, S.
Zu, Y.
TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. I.
ULTRAVIOLET OBSERVATIONS OF THE SEYFERT 1 GALAXY NGC 5548 WITH THE
COSMIC ORIGINS SPECTROGRAPH ON HUBBLE SPACE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei;
galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; BLACK-HOLE MASS;
RADIUS-LUMINOSITY RELATIONSHIP; PEAKED EMISSION-LINES; TERM PROFILE
VARIABILITY; VELOCITY-DELAY MAPS; H-BETA EMISSION; IONIZED ABSORPTION;
QUASAR VARIABILITY
AB We describe the first results from a six-month long reverberation-mapping experiment in the ultraviolet based on 171 observations of the Seyfert 1 galaxy NGC 5548 with the Cosmic Origins Spectrograph on the Hubble Space Telescope. Significant correlated variability is found in the continuum and broad emission lines, with amplitudes ranging from similar to 30% to a factor of two in the emission lines and a factor of three in the continuum. The variations of all the strong emission lines lag behind those of the continuum, with He II lambda 1640 lagging behind the continuum by similar to 2.5 days and Ly alpha lambda 1215, CIV lambda 1550, and Si IV lambda 1400 lagging by similar to 5-6 days. The relationship between the continuum and emission lines is complex. In particular, during the second half of the campaign, all emission-line lags increased by a factor of 1.3-2 and differences appear in the detailed structure of the continuum and emission-line light curves. Velocity-resolved cross-correlation analysis shows coherent structure in lag versus line of sight velocity for the emission lines; the high-velocity wings of C-IV respond to continuum variations more rapidly than the line core, probably indicating higher velocity broad-line region clouds at smaller distances from the central engine. The velocity-dependent response of Ly alpha, however, is more complex and will require further analysis.
C1 [De Rosa, G.; Peterson, B. M.; Pogge, R. W.; Fausnaugh, M. M.; Grier, C. J.; Kochanek, C. S.; Mathur, S.; Schimoia, J. S.; Zu, Y.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[De Rosa, G.; Peterson, B. M.; Pogge, R. W.; Kochanek, C. S.; Mathur, S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[De Rosa, G.; Ely, J.; Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Crenshaw, D. M.; Bentz, M. C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Horne, Keith; De Lorenzo-Caceres, A.; Starkey, D.; Villforth, C.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Korista, K. T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Brandt, W. N.; Grier, C. J.; Kennea, J. A.; Nousek, J. A.; Siegel, M.] Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, University Pk, PA 16802 USA.
[Breeveld, A. A.; Denney, K. D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Brewer, B. J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand.
[Bonta, E. Dalla] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35122 Padua, Italy.
[Bonta, E. Dalla] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Dietrich, M.] Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA.
[Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Evans, P. A.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gehrels, N.; Vaughan, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Gelbord, J. M.] Spectral Sci Inc, Burlington, MA 01803 USA.
[Gelbord, J. M.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Grupe, D.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA.
[Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, NL-3508 Utrecht, Netherlands.
[Kaastra, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kelly, B. C.; Pancoast, A.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece.
[Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil.
[Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Vestergaard, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Vestergaard, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Zu, Y.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Denney, K. D.] NSF, Arlington, VA USA.
[Treu, T.] Packard, Detroit, MI USA.
RP De Rosa, G (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
RI Brandt, William/N-2844-2015; Papadakis, Iossif/C-3235-2011; Lira,
Paulina/G-8536-2016;
OI Brandt, William/0000-0002-0167-2453; Vestergaard,
Marianne/0000-0001-9191-9837; Zu, Ying/0000-0001-6966-6925; Peterson,
Bradley/0000-0001-6481-5397; Pogge, Richard/0000-0003-1435-3053; Barth,
Aaron/0000-0002-3026-0562
FU NASA from the Space Telescope Science Institute [GO-13330]; NASA
[NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G, NNH13CH61C]; National
Science Foundation [AST-1008882]; NSF [AST-1412693, AST-1009756,
AST-1412315, AST-1253702, AST-1302093]; NSERC; NWO; Netherlands
Organization for Scientific Research; UC Center for Galaxy Evolution;
Fondecyt grant [1120328]; NSF; UCSB; CNPq; National Council for
Scientific and Technological Development (Brazil); Packard Foundation;
Danish National Research Foundation; Danish Council for Independent
Research [DFF 4002-00275]
FX Support for HST program number GO-13330 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. We are grateful for the dedication and hard
work by the Institute staff to make this program a success. G.D.R.,
B.M.P.,C.J.G., M.M.F., and R.W.P. are grateful for the support of the
National Science Foundation through grant AST-1008882 to The Ohio State
University. A.J.B. and L.P. have been supported by NSF grant
AST-1412693. M.C.B. gratefully acknowledges support through NSF CAREER
grant AST-1253702 to Georgia State University. K.D.D. is supported by an
NSF Fellowship awarded under grant AST-1302093. R.E. gratefully
acknowledges support from NASA under awards NNX13AC26G, NNX13AC63G, and
NNX13AE99G. J.M.G. gratefully acknowledges support from NASA under award
NNH13CH61C. P.B.H. is supported by NSERC. SRON is financially supported
by NWO, the Netherlands Organization for Scientific Research. B.C.K. is
partially supported by the UC Center for Galaxy Evolution. C.S.K.
acknowledges the support of NSF grant AST-1009756. P.L. acknowledges
support from Fondecyt grant #1120328. A.P. acknowledges support from a
NSF graduate fellowship and a UCSB Dean's Fellowship. J.S.S.
acknowledges CNPq, National Council for Scientific and Technological
Development (Brazil) for partial support and The Ohio State University
for warm hospitality. T.T. has been supported by NSF grant AST-1412315.
T.T. and B.C.K. acknowledge support from the Packard Foundation in the
form of a Packard Research Fellowship to T.T. T.T. thanks the American
Academy in Rome and thee Observatory of Monteporzio Catone for kind
hospitality. The Dark Cosmology Centre is funded by the Danish National
Research Foundation. MV gratefully acknowledges support from the Danish
Council for Independent Research via grant No. DFF 4002-00275. This
research has made use of the NASA/IPAC Extragalactic Database (NED),
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. The authors acknowledge with great sadness the loss of
our longtime collaborator in the planning phases of this project,
Professor David J. Axon, who passed away on 2012 April 5.
NR 124
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 128
DI 10.1088/0004-637X/806/1/128
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300128
ER
PT J
AU Dressler, A
Henry, A
Martin, CL
Sawicki, M
McCarthy, P
Villaneuva, E
AF Dressler, Alan
Henry, Alaina
Martin, Crystal L.
Sawicki, Marcin
McCarthy, Patrick
Villaneuva, Edward
TI CONFIRMATION OF A STEEP LUMINOSITY FUNCTION FOR Ly alpha EMITTERS AT
z=5.7: A MAJOR COMPONENT OF REIONIZATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID LYMAN-BREAK GALAXIES; ULTRA-DEEP-FIELD; STAR-FORMATION RATE; 7 CANDIDATE
GALAXIES; SIMILAR-TO 8; ESCAPE FRACTION; COSMIC REIONIZATION; KECK
SPECTROSCOPY; FORMATION HISTORY; IONIZING PHOTONS
AB We report the first direct and robust measurement of the faint-end slope of the Ly alpha emitter (LAE) luminosity function (LF) at z = 5.7. Candidate LAEs from a low-spectral-resolution blind search with IMACS on Magellan-Baade were targeted at higher resolution to distinguish high-redshift LAEs from foreground galaxies. All but 2 of our 42 single-emission-line systems have flux F < 2.0x10(-17) ergs s(-1) cm(-2), making these the faintest emission-lines observed for a z = 5.7 sample with known completeness, an essential property for determining the faint end slope of the LAE LF. We find 13 LAEs as compared to 29 foreground galaxies, in very good agreement with the modeled foreground counts predicted in Dressler et al. that had been used to estimate a faint-end slope of alpha = -2.0 for the LAE LF. A 32% LAE fraction, LAE/(LAE+foreground) within the flux interval F = 2-20 x 10(-18) ergs s(-1) cm(-2) constrains the faint end slope of the LF to -2.35 < alpha < -1.95 (1 sigma). We show how this steep LF should provide, to the limit of our observations, M-UV similar to -16, more than 20% of the flux necessary to maintain ionization at z = 5.7, with a factor of 10 extrapolation in flux reaching more than 50%. This is in addition to the comparable contribution by brighter Lyman Break Galaxies M-UV less than or similar to -18. We suggest that this bodes well for a sufficient supply of Lyman continuum photons by similar, low-mass star-forming galaxies within the reionization epoch at z approximate to 7, only 250 Myr earlier.
C1 [Dressler, Alan; McCarthy, Patrick; Villaneuva, Edward] Carnegie Observ, Pasadena, CA 91101 USA.
[Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Sawicki, Marcin] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
RP Dressler, A (reprint author), Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM dressler@obs.carnegiescience.edu; alaina.henry@nasa.gov;
cmartin@physics.ucsb.edu; sawicki@ap.smu.ca;
pmc2@obs.carnegiescience.edu; edwardv@obs.carnegiescience.edu
NR 55
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 19
DI 10.1088/0004-637X/806/1/19
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300019
ER
PT J
AU Edelson, R
Gelbord, JM
Horne, K
McHardy, IM
Peterson, BM
Arevalo, P
Breeveld, AA
De Rosa, G
Evans, PA
Goad, MR
Kriss, GA
Brandt, WN
Gehrels, N
Grupe, D
Kennea, JA
Kochanek, CS
Nousek, JA
Papadakis, I
Siegel, M
Starkey, D
Uttley, P
Vaughan, S
Young, S
Barth, AJ
Bentz, MC
Brewer, BJ
Crenshaw, DM
Bonta, ED
De Lorenzo-Caceres, A
Denney, KD
Dietrich, M
Ely, J
Fausnaugh, MM
Grier, CJ
Hall, PB
Kaastra, J
Kelly, BC
Korista, KT
Lira, P
Mathur, S
Netzer, H
Pancoast, A
Pei, L
Pogge, RW
Schimoia, JS
Treu, T
Vestergaard, M
Villforth, C
Yan, H
Zu, Y
AF Edelson, R.
Gelbord, J. M.
Horne, K.
McHardy, I. M.
Peterson, B. M.
Arevalo, P.
Breeveld, A. A.
De Rosa, G.
Evans, P. A.
Goad, M. R.
Kriss, G. A.
Brandt, W. N.
Gehrels, N.
Grupe, D.
Kennea, J. A.
Kochanek, C. S.
Nousek, J. A.
Papadakis, I.
Siegel, M.
Starkey, D.
Uttley, P.
Vaughan, S.
Young, S.
Barth, A. J.
Bentz, M. C.
Brewer, B. J.
Crenshaw, D. M.
Bonta, E. Dalla
De Lorenzo-Caceres, A.
Denney, K. D.
Dietrich, M.
Ely, J.
Fausnaugh, M. M.
Grier, C. J.
Hall, P. B.
Kaastra, J.
Kelly, B. C.
Korista, K. T.
Lira, P.
Mathur, S.
Netzer, H.
Pancoast, A.
Pei, L.
Pogge, R. W.
Schimoia, J. S.
Treu, T.
Vestergaard, M.
Villforth, C.
Yan, H.
Zu, Y.
TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. II. SWIFT AND
HST REVERBERATION MAPPING OF THE ACCRETION DISK OF NGC 5548
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei;
galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; RADIUS-LUMINOSITY
RELATIONSHIP; X-RAY; CONTINUUM EMISSION; SEYFERT-GALAXIES;
ULTRAVIOLET/OPTICAL TELESCOPE; EMITTING REGIONS; MR 2251-178;
VARIABILITY
AB Recent intensive Swift monitoring of the Seyfert 1 galaxy NGC 5548 yielded 282 usable epochs over 125 days across six UV/optical bands and the X-rays. This is the densest extended active galactic nucleus (AGN) UV/optical continuum sampling ever obtained, with a mean sampling rate <0.5 day. Approximately daily Hubble Space Telescope UV sampling was also obtained. The UV/optical light curves show strong correlations (r(max) = 0.57 - 0.90) and the clearest measurement to date of interband lags. These lags are well-fit by a tau alpha lambda(4/3) wavelength dependence, with a normalization that indicates an unexpectedly large disk radius of similar to 0.35 +/- 0.05 lt-day at 1367 angstrom, assuming a simple face-on model. The U band shows a marginally larger lag than expected from the fit and surrounding bands, which could be due to Balmer continuum emission from the broad-line region as suggested by Korista and Goad. The UV/X-ray correlation is weaker (r(max) < 0.45) and less consistent over time. This indicates that while Swift is beginning to measure UV/optical lags in general agreement with accretion disk theory (although the derived size is larger than predicted), the relationship with X-ray variability is less well understood. Combining this accretion disk size estimate with those from quasar microlensing studies suggests that AGN disk sizes scale approximately linearly with central black hole mass over a wide range of masses.
C1 [Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gelbord, J. M.] Spectral Sci Inc, Burlington, MA 01803 USA.
[Gelbord, J. M.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Horne, K.; Starkey, D.; De Lorenzo-Caceres, A.; Villforth, C.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Peterson, B. M.; De Rosa, G.; Kochanek, C. S.; Denney, K. D.; Fausnaugh, M. M.; Grier, C. J.; Mathur, S.; Pogge, R. W.; Schimoia, J. S.; Zu, Y.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Peterson, B. M.; De Rosa, G.; Kochanek, C. S.; Denney, K. D.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Breeveld, A. A.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[De Rosa, G.; Kriss, G. A.; Ely, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Evans, P. A.; Goad, M. R.; Vaughan, S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Brandt, W. N.; Kennea, J. A.; Nousek, J. A.; Siegel, M.; Grier, C. J.] Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, Davey Lab 525, University Pk, PA 16802 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Grupe, D.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA.
[Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece.
[Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Barth, A. J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bentz, M. C.; Crenshaw, D. M.; Pei, L.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Brewer, B. J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand.
[Bonta, E. Dalla] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35122 Padua, Italy.
[Bonta, E. Dalla] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Dietrich, M.] Worcester State Univ, Dept Phys & Earth Sci, Worcester, MA 01602 USA.
[Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, NL-3508 Utrecht, Netherlands.
[Kaastra, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kelly, B. C.; Pancoast, A.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Korista, K. T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil.
[Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Vestergaard, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Vestergaard, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Yan, H.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Denney, K. D.] NSF, Arlington, VA USA.
[Treu, T.] Packard, Detroit, MI USA.
RP Edelson, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Brandt, William/N-2844-2015; Papadakis, Iossif/C-3235-2011; Lira,
Paulina/G-8536-2016;
OI Brandt, William/0000-0002-0167-2453; Barth, Aaron/0000-0002-3026-0562;
Vestergaard, Marianne/0000-0001-9191-9837; Zu, Ying/0000-0001-6966-6925
FU NASA from the Space Telescope Science Institute [GO-13330]; NASA
[NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G, NNH13CH61C]; National
Science Foundation [AST-1008882]; NSF grant [AST-1412693]; NSF CAREER
grant [AST-1253702]; NSF Fellowship [AST-1302093]; NSERC; NWO, the
Netherlands Organization for Scientific Research; UC Center for Galaxy
Evolution; NSF [AST-1009756, AST-1412315]; Fondecyt grant [1120328]; NSF
graduate fellowship; UCSB Dean's Fellowship; CNPq; National Council for
Scientific and Technological Development (Brazil); Packard Foundation in
the form of a Packard Research Fellowship; Danish National Research
Foundation; Danish Council for Independent Research [DFF 4002-00275];
National Aeronautics and Space Administration
FX Support for HST program number GO-13330 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. R.E. gratefully acknowledges support from NASA
under awards NNX13AC26G, NNX13AC63G, and NNX13AE99G. J.M.G. gratefully
acknowledges support from NASA under award NNH13CH61C. B.M.P., G.D.R.,
C.J.G., M.M.F., and R.W.P. are grateful for the support of the National
Science Foundation through grant AST-1008882 to The Ohio State
University. A.J.B. and L.P. have been supported by NSF grant
AST-1412693. M.C.B. gratefully acknowledges support through NSF CAREER
grant AST-1253702 to Georgia State University. K.D.D. is supported by an
NSF Fellowship awarded under grant AST-1302093. P.B.H. is supported by
NSERC. SRON is financially supported by NWO, the Netherlands
Organization for Scientific Research. B.C.K. is partially supported by
the UC Center for Galaxy Evolution. C.S.K. acknowledges the support of
NSF grant AST-1009756. P.L. acknowledges support from Fondecyt grant
#1120328. A.P. acknowledges support from a NSF graduate fellowship and a
UCSB Dean's Fellowship. J.S.S. acknowledges CNPq, National Council for
Scientific and Technological Development (Brazil) for the partial
support and The Ohio State University for warm hospitality. T.T. has
been supported by NSF grant AST-1412315. T.T. and B.C.K. acknowledge
support from the Packard Foundation in the form of a Packard Research
Fellowship to T.T. T.T. thanks the American Academy in Rome and the
Observatory of Monteporzio Catone for kind hospitality. The Dark
Cosmology Centre is funded by the Danish National Research Foundation.
M.V. gratefully acknowledges support from the Danish Council for
Independent Research via grant No. DFF 4002-00275. This research has
made use of the NASA/IPAC Extragalactic Database (NED), which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 65
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 129
DI 10.1088/0004-637X/806/1/129
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300129
ER
PT J
AU Gopalswamy, N
Makela, P
Akiyama, S
Yashiro, S
Xie, H
Thakur, N
Kahler, SW
AF Gopalswamy, N.
Maekelae, P.
Akiyama, S.
Yashiro, S.
Xie, H.
Thakur, N.
Kahler, S. W.
TI LARGE SOLAR ENERGETIC PARTICLE EVENTS ASSOCIATED WITH FILAMENT ERUPTIONS
OUTSIDE ACTIVE REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; Sun: coronal mass ejections (CMEs); Sun: filaments,
prominences; Sun: flares; Sun: particle emission; Sun: radio radiation
ID CORONAL MASS EJECTIONS; SHOCK FORMATION; SOHO MISSION; CYCLE 24; RADIO;
SPACE; WAVES; ACCELERATION; SPECTRA; BURSTS
AB We report on four large filament eruptions (FEs) from solar cycles 23 and 24 that were associated with large solar energetic particle (SEP) events and interplanetary type II radio bursts. The post-eruption arcades corresponded mostly to C-class soft X-ray enhancements, but an M1.0 flare was associated with one event. However, the associated coronal mass ejections (CMEs) were fast (speeds similar to 1000 km s(-1)) and appeared as halo CMEs in the coronagraph field of view. The interplanetary type II radio bursts occurred over a wide wavelength range, indicating the existence of strong shocks throughout the inner heliosphere. No metric type II bursts were present in three events, indicating that the shocks formed beyond 2-3 Rs. In one case, there was a metric type II burst with low starting frequency, indicating a shock formation height of similar to 2 Rs. The FE-associated SEP events did have softer spectra (spectral index >4) in the 10-100 MeV range, but there were other low-intensity SEP events with spectral indices >= 4. Some of these events are likely FE-SEP events, but were not classified as such in the literature because they occurred close to active regions. Some were definitely associated with large active region flares, but the shock formation height was large. We definitely find a diminished role for flares and complex type III burst durations in these large SEP events. Fast CMEs and shock formation at larger distances from the Sun seem to be the primary characteristics of the FE-associated SEP events.
C1 [Gopalswamy, N.; Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.; Thakur, N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.; Thakur, N.] Catholic Univ Amer, Washington, DC 20064 USA.
[Kahler, S. W.] Air Force Res Lab, Albuquerque, NM 87117 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
FU NASA/LWS program; NSF [AGS-1358274]; NASA [NNX15AB77G, NNX15AB70G]
FX We thank the Big Bear Solar Observatory and the Hida Observatory for
making their H-alpha data available on line. We thank NOAA/NGDC for
making the GOES proton data available. This work benefitted greatly from
the open data policy of NASA. STEREO is a mission in NASA's Solar
Terrestrial Probes program. SOHO is a project of international
collaboration between ESA and NASA. The work of N.G., S.Y., S.A., and
N.T. was supported by NASA/LWS program. P. M. was partially supported by
NSF grant AGS-1358274 and NASA grant NNX15AB77G. H.X. was partially
supported by NASA grant NNX15AB70G.
NR 45
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 8
DI 10.1088/0004-637X/806/1/8
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300008
ER
PT J
AU Huffenberger, KM
Araujo, D
Bischoff, C
Buder, I
Chinone, Y
Cleary, K
Kusaka, A
Monsalve, R
Naess, SK
Newburgh, LB
Reeves, R
Ruud, TM
Wehus, IK
Zwart, JTL
Dickinson, C
Eriksen, HK
Gaier, T
Gundersen, JO
Hasegawa, M
Hazumi, M
Miller, AD
Radford, SJE
Readhead, ACS
Staggs, ST
Tajima, O
Thompson, KL
AF Huffenberger, K. M.
Araujo, D.
Bischoff, C.
Buder, I.
Chinone, Y.
Cleary, K.
Kusaka, A.
Monsalve, R.
Naess, S. K.
Newburgh, L. B.
Reeves, R.
Ruud, T. M.
Wehus, I. K.
Zwart, J. T. L.
Dickinson, C.
Eriksen, H. K.
Gaier, T.
Gundersen, J. O.
Hasegawa, M.
Hazumi, M.
Miller, A. D.
Radford, S. J. E.
Readhead, A. C. S.
Staggs, S. T.
Tajima, O.
Thompson, K. L.
CA QUIET Collaboration
TI THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF RADIO SOURCES
AT 43 AND 95 GHz
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: active; galaxies: individual (Cen
A, Pict A); methods: statistical; polarization
ID ACTIVE GALACTIC NUCLEI; MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP
OBSERVATIONS; SCALE ROTATION MEASURES; HIGH-FREQUENCY; POINT SOURCES;
EXTRAGALACTIC SOURCES; SOURCE CATALOG; FARADAYS FOG; BRIGHT
AB We present polarization measurements of extragalactic radio sources observed during the cosmic microwave background polarization survey of the Q/U Imaging Experiment (QUIET), operating at 43 GHz (Q-band) and 95GHz (W-band). We examine sources selected at 20 GHz from the public, >40 mJy catalog of the Australia Telescope (AT20G) survey. There are similar to 480 such sources within QUIET's four low-foreground survey patches, including the nearby radio galaxies Centaurus A and Pictor A. The median error on our polarized flux density measurements is 30-40 mJy per Stokes parameter. At signal-to-noise ratio >3 significance, we detect linear polarization for seven sources in Q-band and six in W-band; only 1.3 +/- 1.1 detections per frequency band are expected by chance. For sources without a detection of polarized emission, we find that half of the sources have polarization amplitudes below 90 mJy (Q-band) and 106 mJy (W-band), at 95% confidence. Finally, we compare our polarization measurements to intensity and polarization measurements of the same sources from the literature. For the four sources with WMAP and Planck intensity measurements >1 Jy, the polarization fractions are above 1% in both QUIET bands. At high significance, we compute polarization fractions as much as 10%-20% for some sources, but the effects of source variability may cut that level in half for contemporaneous comparisons. Our results indicate that simple models-ones that scale a fixed polarization fraction with frequency-are inadequate to model the behavior of these sources and their contributions to polarization maps.
C1 [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Huffenberger, K. M.; Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Buder, I.; Tajima, O.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bischoff, C.; Buder, I.; Tajima, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bischoff, C.; Buder, I.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Chinone, Y.; Hasegawa, M.; Hazumi, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Chinone, Y.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Kusaka, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Kusaka, A.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Kusaka, A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Monsalve, R.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Naess, S. K.; Ruud, T. M.; Eriksen, H. K.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada.
[Newburgh, L. B.] Univ Concepcion, Dept Astron, CePIA, Concepcion, Chile.
[Reeves, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wehus, I. K.; Gaier, T.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Zwart, J. T. L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Dickinson, C.] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway.
[Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
RP Huffenberger, KM (reprint author), Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA.
EM huffenbe@physics.fsu.edu
OI radford, simon/0000-0001-9113-1660; Huffenberger,
Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart,
Jonathan/0000-0002-4967-946X
FU NSF [AST-0506648, PHY-0855887, PHY-0355328, AST-0448909, AST-1010016,
PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284];
KIPAC Enterprise grant; Strategic Alliance for the Implementation of New
Technologies (SAINT); Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]; Fermilab; Kavli Institute for Cosmological Physics;
University of Chicago; JPL RTD program; ERC [307209]
FX Bruce Winstein, who led the QUIET project, died in 2011, soon after
observations concluded. The project's success owes a great debt to his
intellectual and scientific leadership. Support for the QUIET instrument
and operation was provided through the NSF cooperative agreement
AST-0506648. Support was also provided by NSF awards PHY-0855887,
PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI
20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise
grant; and by the Strategic Alliance for the Implementation of New
Technologies (SAINT). This research used resources of the National
Energy Research Scientific Computing Center (NERSC), which is supported
by the Office of Science of the U.S. Department of Energy under Contract
No. DE-AC02-05CH11231.; Some work was performed on the Joint
Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab,
the Kavli Institute for Cosmological Physics, and the University of
Chicago. Some work was performed on the Abel Cluster, owned and
maintained by the University of Oslo and NOTUR (the Norwegian High
Performance Computing Consortium), and on the Central Computing System,
owned and operated by the Computing Research Center at KEK. Portions of
this work were performed at the Jet Propulsion Laboratory (JPL) and
California Institute of Technology, operating under a contract with the
National Aeronautics and Space Administration. The Q-band modules were
developed using funding from the JPL R&TD program. We acknowledge the
Northrop Grumman Corporation for collaboration in the development and
fabrication of HEMT-based cryogenic temperature-compatible MMICs.; C.D.
acknowledges an STFC Advanced Fellowship, an EU Marie-Curie IRG grant
under the FP7 and an ERC Starting Grant (No. 307209). H. K. E.
acknowledges an ERC Starting Grant under FP7. A. D. M. acknowledges a
Sloan foundation fellowship. J. Z. gratefully acknowledges a South
Africa National Research Foundation Square Kilometre Array Research
Fellowship.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 112
DI 10.1088/0004-637X/806/1/112
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300112
ER
PT J
AU Johnson, TJ
Ray, PS
Roy, J
Cheung, CC
Harding, AK
Pletsch, HJ
Fort, S
Camilo, F
Deneva, J
Bhattacharyya, B
Stappers, BW
Kerr, M
AF Johnson, T. J.
Ray, P. S.
Roy, J.
Cheung, C. C.
Harding, A. K.
Pletsch, H. J.
Fort, S.
Camilo, F.
Deneva, J.
Bhattacharyya, B.
Stappers, B. W.
Kerr, M.
TI DISCOVERY OF GAMMA-RAY PULSATIONS FROM THE TRANSITIONAL REDBACK PSR
J1227-4853
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (J1227-4853); binaries: eclipsing; gamma rays: stars
ID LARGE-AREA TELESCOPE; BINARY MILLISECOND PULSAR; HIGH-ENERGY EMISSION;
BLACK-WIDOW PULSARS; X-RAY; XSS J12270-4859; LIGHT CURVES;
NEUTRON-STARS; STATE CHANGE; SLOT GAPS
AB The 1.69 ms spin period of PSR J1227-4853 was recently discovered in radio observations of the low-mass X-ray binary XSS J12270-4859 following the announcement of a possible transition to a rotation-powered millisecond pulsar state, inferred from decreases in optical, X-ray, and gamma-ray flux from the source. We report the detection of significant (5s) gamma-ray pulsations after the transition, at the known spin period, using similar to 1 year of data from the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. The gamma-ray light curve of PSR J1227-4853 can be fit by one broad peak, which occurs at nearly the same phase as the main peak in the 1.4 GHz radio profile. The partial alignment of light-curve peaks in different wavebands suggests that at least some of the radio emission may originate at high altitude in the pulsar magnetosphere, in extended regions co-located with the gamma-ray emission site. We folded the LAT data at the orbital period, both pre- and post-transition, but find no evidence for significant modulation of the gamma-ray flux. Analysis of the gamma-ray flux over the mission suggests an approximate transition time of 2012 November 30. Continued study of the pulsed emission and monitoring of PSR J1227-4853, and other known redback systems, for subsequent flux changes will increase our knowledge of the pulsar emission mechanism and transitioning systems.
C1 [Johnson, T. J.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Ray, P. S.; Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Roy, J.; Bhattacharyya, B.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Roy, J.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pletsch, H. J.; Fort, S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Pletsch, H. J.; Fort, S.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Deneva, J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Kerr, M.] CSIRO, Australia Telescope Natl Facil, Astron & Space Sci, Epping, NSW 1710, Australia.
[Deneva, J.] Naval Res Lab, Washington, DC 20375 USA.
RP Johnson, TJ (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
EM tyrel.j.johnson@gmail.com; Paul.Ray@nrl.navy.mil;
jayanta.roy@manchester.ac.uk
OI Ray, Paul/0000-0002-5297-5278
FU Commonwealth Government; NASA [DPR S-15633 Y]
FX The Parkes radio telescope is part of the Australia Telescope which is
funded by the Commonwealth Government for operation as a National
Facility managed by CSIRO.; Portions of this research performed at the
Naval Research Laboratory are sponsored by NASA DPR S-15633 Y.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300091
ER
PT J
AU Jun, HD
Im, M
Lee, HM
Ohyama, Y
Woo, JH
Fan, XH
Goto, T
Kim, D
Kim, JH
Kim, M
Lee, MG
Nakagawa, T
Pearson, C
Serjeant, S
AF Jun, Hyunsung David
Im, Myungshin
Lee, Hyung Mok
Ohyama, Youichi
Woo, Jong-Hak
Fan, Xiaohui
Goto, Tomotsugu
Kim, Dohyeong
Kim, Ji Hoon
Kim, Minjin
Lee, Myung Gyoon
Nakagawa, Takao
Pearson, Chris
Serjeant, Stephen
TI REST-FRAME OPTICAL SPECTRA AND BLACK HOLE MASSES OF 3 < z < 6 QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; quasars: emission lines; quasars:
supermassive black holes
ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; NEAR-INFRARED SPECTROSCOPY;
HIGH-REDSHIFT QUASARS; EMISSION-LINE PROPERTIES; WIDE-FIELD CAMERA;
LUMINOSITY FUNCTION; DATA RELEASE; Z-GREATER-THAN-5.7 QUASARS;
ADDITIONAL QUASARS
AB We present the rest-frame optical spectral properties of 155 luminous quasars at 3.3 < z < 6.4 taken with the AKARI space telescope, including the first detection of the Ha emission line as far out as z similar to 6. We extend the scaling relation between the rest-frame optical continuum and the line luminosity of active galactic nuclei (AGNs) to the high-luminosity, high-redshift regime that has rarely been probed before. Remarkably, we find that a single log-linear relation can be applied to the 5100 angstrom and H alpha AGN luminosities over a wide range of luminosity (10(42) < L-5100 < 10(47) ergs s(-1)) or redshift (0 < z < 6), suggesting that the physical mechanism governing this relation is unchanged from z = 0 to. 6, over five decades in luminosity. Similar scaling relations are found between the optical and the UV continuum luminosities or line widths. Applying the scaling relations to the H beta black hole (BH) mass (MBH) estimator of local AGNs, we derive the MBH estimators based on the H alpha, Mg (II), and C (IV) lines, finding that the UV-line-based masses are overall consistent with the Balmer-line-based, but with a large intrinsic scatter of 0.40 dex for the C (IV) estimates. Our 43 MBH estimates from Ha confirm the existence of BHs as massive as similar to 10(10) M-circle dot out to z similar to 5. and provide a secure footing for previous results from Mg (II)-line-based studies that a rapid MBH growth has occurred in the early universe.
C1 [Jun, Hyunsung David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jun, Hyunsung David; Im, Myungshin; Kim, Dohyeong; Kim, Ji Hoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul 151742, South Korea.
[Im, Myungshin; Lee, Hyung Mok; Woo, Jong-Hak; Kim, Dohyeong; Lee, Myung Gyoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea.
[Ohyama, Youichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Goto, Tomotsugu] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Goto, Tomotsugu] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Kim, Ji Hoon] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kim, Minjin] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Kim, Minjin] Univ Sci & Technol, Taejon 305350, South Korea.
[Nakagawa, Takao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Pearson, Chris; Serjeant, Stephen] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Pearson, Chris] CCLRC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Pearson, Chris] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England.
RP Im, M (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul 151742, South Korea.
EM hyunsung.jun@jpl.nasa.gov; mim@astro.snu.ac.kr
RI Kim, Ji Hoon/A-8989-2009;
OI Kim, Ji Hoon/0000-0002-1418-3309; Im, Myungshin/0000-0002-8537-6714
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA;
National Research Foundation of Korea (NRF) [2008-0060544,
2012R1A2A2A01006087, 2012R1A4A1028713]; NRF-2014-Fostering Core Leaders
of Future Program - Korea government (MSIP) [2014-009728]; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of Energy
Office of Science; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; Carnegie Mellon University; University
of Florida; French Participation Group; German Participation Group;
Harvard University; Instituto de Astrofisica de Canarias; Michigan
State/Notre Dame/JINA Participation Group; Johns Hopkins University;
Lawrence Berkeley National Laboratory; Max Planck Institute for
Astrophysics; Max Planck Institute for Extraterrestrial Physics; New
Mexico State University; New York University; Ohio State University;
Pennsylvania State University; University of Portsmouth; Princeton
University; Spanish Participation Group; University of Tokyo; University
of Utah; Vanderbilt University; University of Virginia; University of
Washington; Yale University; National Aeronautics and Space
Administration; [MOST100-2112-M-001-001-MY3]
FX We thank Todd Boroson, Jenny Greene, Lisa Storrie-Lombardi, Celine
Peroux, and Donald Schneider for kindly providing the iron template
derived from I Zw 1, the rest-frame optical luminosities and line widths
of local AGNs, and the optical spectra of APM-UKST quasars and Q0000-26.
Also, we thank Eduardo Banados, Hyunjin Shim, and Doosoo Yoon for useful
communication. 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. This
work was supported by the National Research Foundation of Korea (NRF)
grant. No. 2008-0060544 (H.D.J. and M.I.), 2012R1A2A2A01006087 (J.H.W),
2012R1A4A1028713 (H.M.L. and M.G.L.), and NRF-2014-Fostering Core
Leaders of Future Program, No. 2014-009728 (D.K.), funded by the Korea
government (MSIP). This work was supported by grant
MOST100-2112-M-001-001-MY3 (Y.O.).; This research is based on
observations with AKARI, a JAXA project with the participation of ESA.
Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the participating institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III web site is. http://www.sdss3.org/. SDSS-III is managed by the
Astrophysical Research Consortium for the participating institutions of
the SDSS-III Collaboration, including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory, Carnegie
Mellon University, University of Florida, the French Participation
Group, the German Participation Group, Harvard University, the Instituto
de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University. This publication makes use of data products from the Two
Micron All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation. This publication
makes use of data products from the United Kingdom Infrared Deep Sky
Survey. The UKIDSS project is defined in Lawrence et al. (2007). UKIDSS
uses the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007). The
photometric system is described in Hewett et al. (2006), and the
calibration is described in Hodgkin et al. (2009). The pipeline
processing and science archive are described in M.J. Irwin et al. (2009,
in preparation) and Hambly et al. (2008). 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
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DI 10.1088/0004-637X/806/1/109
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300109
ER
PT J
AU Kastner, JH
Qi, CH
Gorti, U
Hily-Blant, P
Oberg, K
Forveille, T
Andrews, S
Wilner, D
AF Kastner, Joel H.
Qi, Chunhua
Gorti, Uma
Hily-Blant, Pierre
Oberg, Karin
Forveille, Thierry
Andrews, Sean
Wilner, David
TI A RING OF C2H IN THE MOLECULAR DISK ORBITING TW Hya
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; protoplanetary disks; stars: individual (TW Hya);
stars: pre-main sequence
ID PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; HYDRAE; LINE; CHEMISTRY; CO;
EXCITATION; ACCRETION
AB We have used the Submillimeter Array to image, at similar to 1.'' 5 resolution, C2H N = 3 -> 2 emission from the circumstellar disk orbiting the nearby (D = 54 pc), similar to 8 Myr-old, similar to 0.8 M-circle dot classical T Tauri star TW Hya. The SMA imaging reveals that the C2H emission exhibits a ring-like morphology. Based on a model in which the C2H column density follows a truncated radial power-law distribution, we find that the inner edge of the ring lies at similar to 45 AU, and that the ring extends to at least similar to 120 AU. Comparison with previous (single-dish) observations of C2H N = 4 -> 3 emission indicates that the C2H molecules are subthermally excited and, hence, that the emission arises from the relatively warm (T greater than or similar to 40 K), tenuous (n << 10(7) cm(-3)) upper atmosphere of the disk. Based on these results and comparisons of the SMA C2H map with previous submillimeter and scattered-light imaging, we propose that the C2H emission most likely traces particularly efficient photo-destruction of small grains and/or photodesorption and photodissociation of hydrocarbons derived from grain ice mantles in the surface layers of the outer disk. The presence of a C2H ring in the TW Hya disk hence likely serves as a marker of dust grain processing and radial and vertical grain size segregation within the disk.
C1 [Kastner, Joel H.] Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
[Kastner, Joel H.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
[Qi, Chunhua; Oberg, Karin; Andrews, Sean; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gorti, Uma] SETI Inst, Mountain View, CA 94043 USA.
[Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hily-Blant, Pierre; Forveille, Thierry] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Hily-Blant, Pierre; Forveille, Thierry] CNRS, IPAG, F-38000 Grenoble, France.
[Hily-Blant, Pierre] Inst Univ France, F-38000 Grenoble, France.
RP Kastner, JH (reprint author), Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
EM jhk@cis.rit.edu
OI Kastner, Joel/0000-0002-3138-8250
FU Smithsonian Institution; Academia Sinica; National Science Foundation
[AST-1108950]; NASA Origins of Solar Systems grant [NNX11AK63]
FX 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. We gratefully acknowledge Alexander Faure for providing
electron impact rates for C2H, and we thank the anonymous
referee for helpful comments and suggestions. This research is supported
by National Science Foundation grant AST-1108950 to RIT and NASA Origins
of Solar Systems grant NNX11AK63 to SAO.
NR 34
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 75
DI 10.1088/0004-637X/806/1/75
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300075
ER
PT J
AU Lehmer, BD
Tyler, JB
Hornschemeier, AE
Wik, DR
Yukita, M
Antoniou, V
Boggs, S
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Maccarone, TJ
Ptak, A
Stern, D
Zezas, A
Zhang, WW
AF Lehmer, B. D.
Tyler, J. B.
Hornschemeier, A. E.
Wik, D. R.
Yukita, M.
Antoniou, V.
Boggs, S.
Christensen, F. E.
Craig, W. W.
Hailey, C. J.
Harrison, F. A.
Maccarone, T. J.
Ptak, A.
Stern, D.
Zezas, A.
Zhang, W. W.
TI THE 0.3-30 keV SPECTRA OF POWERFUL STARBURST GALAXIES: NuSTAR AND
CHANDRA OBSERVATIONS OF NGC 3256 AND NGC 3310
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 3256 and NGC 3310);
galaxies: starburst; galaxies: star formation; X-rays: galaxies
ID X-RAY-EMISSION; STAR-FORMING GALAXIES; LUMINOUS INFRARED GALAXIES;
XMM-NEWTON OBSERVATIONS; INITIAL MASS FUNCTION; MERGER NGC-3256;
FORMATION HISTORY; CLUSTER FORMATION; SPIRAL GALAXIES; LOW-METALLICITY
AB We present nearly simultaneous Chandra and NuSTAR observations of two actively star-forming galaxies within 50 Mpc: NGC 3256 and NGC 3310. Both galaxies are significantly detected by both Chandra and NuSTAR, which together provide the first-ever spectra of these two galaxies spanning 0.3-30 keV. The X-ray emission from both galaxies is spatially resolved by Chandra; we find that hot gas dominates the E < 1-3 keV emission while ultraluminous X-ray sources (ULXs) provide majority contributions to the emission at E > 1-3 keV. The NuSTAR galaxy-wide spectra of both galaxies follow steep power-law distributions with Gamma approximate to 2.6 at E > 5-7 keV. Using new and archival Chandra data, we search for signatures of heavily obscured or low luminosity active galactic nuclei (AGNs). We find that both NGC 3256 and NGC 3310 have X-ray detected sources coincident with nuclear regions; however, the steep NuSTAR spectra of both galaxies restricts these sources to be either low luminosity AGNs (L2-10 keV/L-Edd less than or similar to 10(-5)) or non-AGNs in nature (e.g., ULXs or crowded X-ray sources that reach L2-10 keV similar to 10(40) erg s(-1) cannot be ruled out). Combining our constraints on the 0.3-30 keV spectra of NGC 3256 and NGC 3310 with equivalent measurements for nearby star-forming galaxies M83 and NGC 253, we analyze the star formation rate (SFR) normalized spectra of these starburst galaxies. The spectra of all four galaxies show sharply declining power-law slopes at energies above 3-6 keV primarily due to ULX populations. Our observations therefore constrain the average spectral shape of galaxy-wide populations of luminous accreting binaries (i.e., ULXs). Interestingly, despite a completely different galaxy sample selection, emphasizing here a range of SFRs and stellar masses, these properties are similar to those of super-Eddington accreting ULXs that have been studied individually in a targeted NuSTAR ULX program. We also find that NGC 3310 exhibits a factor of approximate to 3-10 elevation of X-ray emission over the other star-forming galaxies due to a corresponding overabundance of ULXs. We argue that the excess of ULXs in NGC 3310 is most likely explained by the relatively low metallicity of the young stellar population in this galaxy, a property that is expected to produce an excess of luminous X-ray binaries for a given SFR.
C1 [Lehmer, B. D.; Wik, D. R.; Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Tyler, J. B.; Hornschemeier, A. E.; Wik, D. R.; Yukita, M.; Ptak, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tyler, J. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Antoniou, V.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Boggs, S.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94720 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Zezas, A.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece.
[Zezas, A.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece.
RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
RI Boggs, Steven/E-4170-2015; Yukita, Mihoko/E-4135-2017; Zezas,
Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013
OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X;
Antoniou, Vallia/0000-0001-7539-1593
FU Chandra X-ray Center grant [GO4-15086 Z]; NASA ADAP grant [NNX13AI48G];
European Research Council under the European Union's Seventh Framework
Programme (FP)/ERC Grant [617001]; NASA [NNG08FD60C]; National
Aeronautics and Space Administration
FX We thank the anonymous referee for helpful comments, which have improved
the quality of this paper. We gratefully acknowledge financial support
from Chandra X-ray Center grant GO4-15086 Z (B.D.L., J.B.T.) and NASA
ADAP grant NNX13AI48G (B.D.L.). A. Z. acknowledges funding from the
European Research Council under the European Union's Seventh Framework
Programme (FP/2007-2013)/ERC Grant Agreement n. 617001. 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. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed
by the ASI Science Data Center (Italy) and the California Institute of
Technology (USA).
NR 88
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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 JUN 10
PY 2015
VL 806
IS 1
AR 126
DI 10.1088/0004-637X/806/1/126
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300126
ER
PT J
AU Makela, P
Gopalswamy, N
Akiyama, S
Xie, H
Yashiro, S
AF Maekelae, P.
Gopalswamy, N.
Akiyama, S.
Xie, H.
Yashiro, S.
TI ESTIMATING THE HEIGHT OF CMEs ASSOCIATED WITH A MAJOR SEP EVENT AT THE
ONSET OF THE METRIC TYPE II RADIO BURST DURING SOLAR CYCLES 23 AND 24
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: radio
radiation
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; MAGNETIC
RECONNECTION; OUTER CORONA; SHOCK-WAVES; LARGE-ANGLE; EXPANSION;
EMISSION; ERUPTION; FLARES
AB We studied the coronal mass ejection (CME) height at the onset of 59 metric type II radio bursts associated with major solar energetic particle (SEP) events, excluding ground level enhancements (GLEs), during solar cycles 23 and 24. We calculated CME heights using a simple flare-onset method used by Gopalswamy et al. to estimate CME heights at the metric type II onset for cycle 23 GLEs. We found the mean CME height for non-GLE events (1.72 R-circle dot) to be similar to 12% greater than that (1.53 R-circle dot) for cycle 23 GLEs. The difference could be caused by more impulsive acceleration of the GLE-associated CMEs. For cycle 24 non-GLE events, we compared the CME heights obtained using the flare-onset method and the three-dimensional spherical-shock fitting method and found the correlation to be good (CC = 0.68). We found the mean CME height for cycle 23 non-GLE events (1.79 R-circle dot) to be greater than that for cycle 24 non-GLE events (1.58 R-circle dot), but statistical tests do not definitely reject the possibility of coincidence. We suggest that the lower formation height of the shocks during cycle 24 indicates a change in the Alfven speed profile because solar magnetic fields are weaker and plasma density levels are closer to the surface than usual during cycle 24. We also found that complex type III bursts showing diminution of type III emission in the 7-14 MHz frequency range are more likely associated with events with a CME height at the type II onset above 2 R-circle dot, supporting suggestions that the CME/shock structure causes the feature.
C1 [Maekelae, P.; Akiyama, S.; Xie, H.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Maekelae, P.; Gopalswamy, N.; Akiyama, S.; Xie, H.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Makela, P (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.
EM pertti.makela@nasa.gov
OI Gopalswamy, Nat/0000-0001-5894-9954
FU NASA [NNX10AL50A, NNG11PL10A]
FX We thank the Wind/WAVES, SDO/AIA, and STEREO/SECCHI teams for providing
data. This research was done as part of the LWS Focused Science Topic,
"SEP Variability" supported by NASA grants NNX10AL50A and NNG11PL10A.
SOHO is a project of international cooperation between ESA and NASA. The
authors thank the anonymous referee for helpful comments.
NR 61
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 13
DI 10.1088/0004-637X/806/1/13
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300013
ER
PT J
AU McCauliff, SD
Jenkins, JM
Catanzarite, J
Burke, CJ
Coughlin, JL
Twicken, JD
Tenenbaum, P
Seader, S
Li, J
Cote, M
AF McCauliff, Sean D.
Jenkins, Jon M.
Catanzarite, Joseph
Burke, Christopher J.
Coughlin, Jeffrey L.
Twicken, Joseph D.
Tenenbaum, Peter
Seader, Shawn
Li, Jie
Cote, Miles
TI AUTOMATIC CLASSIFICATION OF KEPLER PLANETARY TRANSIT CANDIDATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astronomical databases: miscellaneous; binaries: eclipsing; catalogs;
methods: statistical; planets and satellites: detection; techniques:
photometric
ID ERROR-CORRECTION; FALSE POSITIVES; VARIABLE-STARS; LIGHT CURVES;
IDENTIFICATION; MISSION
AB In the first three years of operation, the Kepler mission found 3697 planet candidates (PCs) from a set of 18,406 transit-like features detected on more than 200,000 distinct stars. Vetting candidate signals manually by inspecting light curves and other diagnostic information is a labor intensive effort. Additionally, this classification methodology does not yield any information about the quality of PCs; all candidates are as credible as any other. The torrent of exoplanet discoveries will continue after Kepler, because a number of exoplanet surveys will have an even broader search area. This paper presents the application of machine-learning techniques to the classification of the exoplanet transit-like signals present in the Kepler light curve data. Transit-like detections are transformed into a uniform set of real-numbered attributes, the most important of which are described in this paper. Each of the known transit-like detections is assigned a class of PC; astrophysical false positive; or systematic, instrumental noise. We use a random forest algorithm to learn the mapping from attributes to classes on this training set. The random forest algorithm has been used previously to classify variable stars; this is the first time it has been used for exoplanet classification. We are able to achieve an overall error rate of 5.85% and an error rate for classifying exoplanets candidates of 2.81%.
C1 [McCauliff, Sean D.] NASA, Ames Res Ctr, Wyle, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.; Cote, Miles] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Catanzarite, Joseph; Burke, Christopher J.; Coughlin, Jeffrey L.; Twicken, Joseph D.; Tenenbaum, Peter; Seader, Shawn; Li, Jie] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP McCauliff, SD (reprint author), NASA, Ames Res Ctr, Wyle, Moffett Field, CA 94035 USA.
EM sean.d.mccauliff@nasa.gov
FU NASA's Space Mission Directorate
FX Kepler was competitively selected as NASA's 10th Discovery mission. We
would like to thank Abhishek Jaiantilal for use of the
randomforest-matlab code. This paper would not be possible without the
work of the members of the Kepler TCE Review Team. Funding for the
Kepler mission is provided by NASA's Space Mission Directorate. This
research has made use of the NASA Exoplanet Archive, which is operated
by the California Institute of Technology, under contract with NASA
under the Exoplanet Exploration Program.
NR 37
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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 JUN 10
PY 2015
VL 806
IS 1
AR 6
DI 10.1088/0004-637X/806/1/6
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300006
ER
PT J
AU Merten, J
Meneghetti, M
Postman, M
Umetsu, K
Zitrin, A
Medezinski, E
Nonino, M
Koekemoer, A
Melchior, P
Gruen, D
Moustakas, LA
Bartelmann, M
Host, O
Donahue, M
Coe, D
Molino, A
Jouvel, S
Monna, A
Seitz, S
Czakon, N
Lemze, D
Sayers, J
Balestra, I
Rosati, P
Benitez, N
Biviano, A
Bouwens, R
Bradley, L
Broadhurst, T
Carrasco, M
Ford, H
Grillo, C
Infante, L
Kelson, D
Lahav, O
Massey, R
Moustakas, J
Rasia, E
Rhodes, J
Vega, J
Zheng, W
AF Merten, J.
Meneghetti, M.
Postman, M.
Umetsu, K.
Zitrin, A.
Medezinski, E.
Nonino, M.
Koekemoer, A.
Melchior, P.
Gruen, D.
Moustakas, L. A.
Bartelmann, M.
Host, O.
Donahue, M.
Coe, D.
Molino, A.
Jouvel, S.
Monna, A.
Seitz, S.
Czakon, N.
Lemze, D.
Sayers, J.
Balestra, I.
Rosati, P.
Benitez, N.
Biviano, A.
Bouwens, R.
Bradley, L.
Broadhurst, T.
Carrasco, M.
Ford, H.
Grillo, C.
Infante, L.
Kelson, D.
Lahav, O.
Massey, R.
Moustakas, J.
Rasia, E.
Rhodes, J.
Vega, J.
Zheng, W.
TI CLASH: THE CONCENTRATION-MASS RELATION OF GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: clusters: general; gravitational lensing: strong;
gravitational lensing: weak
ID HUBBLE-SPACE-TELESCOPE; WEAK-LENSING ANALYSIS; DARK-MATTER HALOES;
OBSERVATIONS COSMOLOGICAL INTERPRETATION; ACT-CL J0102-4915;
LINE-OF-SIGHT; X-RAY; LAMBDA-CDM; PHOTOMETRIC REDSHIFTS; RXC
J2248.7-4431
AB We present a new determination of the concentration-mass (c-M) relation for galaxy clusters based on our comprehensive lensing analysis of 19 X-ray selected galaxy clusters from the Cluster Lensing and Supernova Survey with Hubble (CLASH). Our sample spans a redshift range between 0.19 and 0.89. We combine weak-lensing constraints from the Hubble Space Telescope (HST) and from ground-based wide-field data with strong lensing constraints from HST. The results are reconstructions of the surface-mass density for all CLASH clusters on multi-scale grids. Our derivation of Navarro-Frenk-White parameters yields virial masses between 0.53 x 10(15) M-circle dot/h and 1.76 x 10(15) M-circle dot/h and the halo concentrations are distributed around c(200c) similar to 3.7 with a 1 sigma significant negative slope with cluster mass. We find an excellent 4% agreement in the median ratio of our measured concentrations for each cluster and the respective expectation from numerical simulations after accounting for the CLASH selection function based on X-ray morphology. The simulations are analyzed in two dimensions to account for possible biases in the lensing reconstructions due to projection effects. The theoretical c-M relation from our X-ray selected set of simulated clusters and the c-M relation derived directly from the CLASH data agree at the 90% confidence level.
C1 [Merten, J.; Meneghetti, M.; Moustakas, L. A.; Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Merten, J.; Zitrin, A.; Sayers, J.; Rhodes, J.] CALTECH, Pasadena, CA 91125 USA.
[Merten, J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Postman, M.; Koekemoer, A.; Coe, D.; Bradley, L.; Zheng, W.] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Umetsu, K.; Czakon, N.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Medezinski, E.; Lemze, D.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Nonino, M.; Balestra, I.; Biviano, A.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Gruen, D.; Monna, A.; Seitz, S.] Univ Munich, D-81679 Munich, Germany.
[Gruen, D.; Monna, A.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bartelmann, M.; Carrasco, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Host, O.; Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Donahue, M.; Benitez, N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Molino, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Jouvel, S.; Lahav, O.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Barcelona, Spain.
[Jouvel, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Balestra, I.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
[Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands.
[Broadhurst, T.] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain.
[Broadhurst, T.] Basque Fdn Sci, Ikerbasque, Santiago 48011, Chile.
[Carrasco, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofs, Santiago 22, Chile.
[Infante, L.] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile.
[Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Massey, R.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Rasia, E.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Vega, J.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Zitrin, A.; Vega, J.] Observ Paris, CNRS, LERMA, UMR 8112, F-75014 Paris, France.
RP Merten, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jmerten@caltech.edu
RI Meneghetti, Massimo/O-8139-2015;
OI Meneghetti, Massimo/0000-0003-1225-7084; Nonino,
Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Vega
Ferrero, Jesus/0000-0003-2338-5567; rasia, elena/0000-0003-4175-002X;
Umetsu, Keiichi/0000-0002-7196-4822; Biviano,
Andrea/0000-0002-0857-0732; Moustakas, Leonidas/0000-0003-3030-2360;
Koekemoer, Anton/0000-0002-6610-2048; Benitez,
Narciso/0000-0002-0403-7455
FU People Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme (FP7) under REA grant [627288]; ORAU; NASA; National
Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica
Career Development Award; NASA - STScI [HST-HF-51334.01 A]; Deutsche
Forschungsgemeinschaft (DFG) [SFB Transregio 33]; DFG cluster of
excellence "Origin and Structure of the universe"; Baden Wurttemberg
Stiftung; DNRF; Norris Foundation CCAT Postdoctoral Fellowship; National
Science Foundation [AST-1210973, SAO TM3-14008X]; NASA [NAS8-03060];
MIUR; [ASI/INAF I/023/12/0]; [INFN/PD51]; [NSF/AST1313447];
[NASA/NNX11AB07G]
FX The research was in part carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. J. M. has received funding from
the People Programme (Marie Curie Actions) of the European Union's
Seventh Framework Programme (FP7/2007-2013) under REA grant agreement
number 627288. M. M. thanks ORAU and NASA for supporting his research at
JPL and acknowledges support from the contract ASI/INAF I/023/12/0,
INFN/PD51, and the PRIN MIUR 20102011 "The dark universe and the cosmic
evolution of baryons: from current surveys to Euclid." K. U.
acknowledges support from the National Science Council of Taiwan (grant
NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career
Development Award. Support for A.Z. is provided by NASA through Hubble
Fellowship grant #HST-HF-51334.01 A awarded by STScI. D.G., S.S. and
P.R. were supported by SFB Transregio 33 "The Dark universe" by the
Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence
"Origin and Structure of the universe." This work was supported in part
by contract research "Internationale Spitzenforschung II/2-6" of the
Baden Wurttemberg Stiftung. The Dark Cosmology Centre is funded by the
DNRF. J. S. was supported by NSF/AST1313447, NASA/NNX11AB07G, and the
Norris Foundation CCAT Postdoctoral Fellowship. E.R. acknowledges
support from the National Science Foundation AST-1210973, SAO TM3-14008X
(issued under NASA Contract No. NAS8-03060)
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 4
DI 10.1088/0004-637X/806/1/4
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300004
ER
PT J
AU Moore, RL
Sterling, AC
Falconer, DA
AF Moore, Ronald L.
Sterling, Alphonse C.
Falconer, David A.
TI MAGNETIC UNTWISTING IN SOLAR JETS THAT GO INTO THE OUTER CORONA IN POLAR
CORONAL HOLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: activity; Sun: chromosphere; Sun: corona; Sun: magnetic
fields
ID X-RAY JETS; EXTREME-ULTRAVIOLET; ALFVENIC WAVES; II SPICULES; BLOWOUT
JETS; HINODE; TELESCOPE; WIND; REGION; ENERGY
AB We study 14 large solar jets observed in polar coronal holes. In EUV movies from the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), each jet appears similar to most X-ray jets and EUV jets that erupt in coronal holes; but each is exceptional in that it goes higher than most, so high that it is observed in the outer corona beyond 2.2 R-Sun in images from the Solar and Heliospheric Observatory/Large Angle Spectroscopic Coronagraph (LASCO)/C2 coronagraph. From AIA He II 304 angstrom movies and LASCO/C2 running-difference images of these high-reaching jets, we find: (1) the front of the jet transits the corona below 2.2 RSun at a speed typically several times the sound speed; (2) each jet displays an exceptionally large amount of spin as it erupts; (3) in the outer corona, most of the jets display measureable swaying and bending of a few degrees in amplitude; in three jets the swaying is discernibly oscillatory with a period of order 1 hr. These characteristics suggest that the driver in these jets is a magnetic-untwisting wave that is basically a large-amplitude (i.e., nonlinear) torsional Alfven wave that is put into the reconnected open field in the jet by interchange reconnection as the jet erupts. From the measured spinning and swaying, we estimate that the magnetic-untwisting wave loses most of its energy in the inner corona below 2.2 RSun. We point out that the torsional waves observed in Type-II spicules might dissipate in the corona in the same way as the magnetic-untwisting waves in our big jets, and thereby power much of the coronal heating in coronal holes.
C1 [Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David A.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, Huntsville, AL 35812 USA.
[Moore, Ronald L.; Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RP Moore, RL (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA.
EM ron.moore@nasa.gov
FU Heliophysics Division of NASA's Science Mission Directorate through the
Living With a Star Targeted Research and Technology Program
FX This work was funded by the Heliophysics Division of NASA's Science
Mission Directorate through the Living With a Star Targeted Research and
Technology Program. ACS benefited from discussions held at the
International Space Science Institute's (ISSI; Bern, Switzerland)
International Team on Solar Coronal Jets.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 11
DI 10.1088/0004-637X/806/1/11
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300011
ER
PT J
AU Petrosian, V
Kitanidis, E
Kocevski, D
AF Petrosian, Vahe
Kitanidis, Ellie
Kocevski, Daniel
TI COSMOLOGICAL EVOLUTION OF LONG GAMMA-RAY BURSTS AND THE STAR FORMATION
RATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; gamma-ray burst: general; methods: statistical; stars:
formation
ID OPTICAL LUMINOSITY EVOLUTION; REDSHIFT DISTRIBUTION; FORMATION HISTORY;
TRUNCATED DATA; QUASARS; SELECTION; RADIO; PEAK; AFTERGLOWS; TESTS
AB Gamma-ray bursts (GRBs), by virtue of their high luminosities, can be detected up to very high redshifts. and therefore can be excellent probes of the early universe. This task is hampered by the fact that most of their characteristics have a broad range,. so we first need to obtain an accurate description of the distribution of these characteristics. and,. especially, their cosmological evolution. We use a sample of about 200 Swift long GRBs with known redshifts to determine the evolution of the. luminosity, formation rate, and the general shape of the luminosity function (LF). In contrast to most other forward-fitting methods of treating this problem, we use the Efron-Petrosian methods, which allow a non-parametric determination of the above quantities. We find a relatively strong luminosity evolution, an LF that can be fitted to a broken power law, and an unusually high formation rate at low redshifts, a rate more than one order of magnitude higher than the star formation rate (SFR). On the other hand, our results seem to agree with the almost constant SFR in redshifts 1-3 and the decline above this redshift.
C1 [Petrosian, Vahe] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Petrosian, Vahe] Stanford Univ, KIPAC, Stanford, CA 94305 USA.
[Petrosian, Vahe] Stanford Univ, Dept Appl Phys, Stanford, CA 94305 USA.
[Kitanidis, Ellie] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Kocevski, Daniel] NASA, Goddard Space Flight Ctr, College Pk, MD USA.
RP Petrosian, V (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
OI Petrosian, Vahe'/0000-0002-2670-8942
FU Swift [NASA NNX12AE74G]
FX This work was partially supported by Swift guest investigator grant NASA
NNX12AE74G and is based on Ellie Kitanidis's senior honor thesis at
Stanford University (see http://purl.stanford.edu/xp981bq5003).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 44
DI 10.1088/0004-637X/806/1/44
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300044
ER
PT J
AU Rangwala, N
Maloney, PR
Wilson, CD
Glenn, J
Kamenetzky, J
Spinoglio, L
AF Rangwala, Naseem
Maloney, Philip R.
Wilson, Christine D.
Glenn, Jason
Kamenetzky, Julia
Spinoglio, Luigi
TI MORPHOLOGY AND KINEMATICS OF WARM MOLECULAR GAS IN THE NUCLEAR REGION OF
ARP 220 AS REVEALED BY ALMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: ISM; galaxies: kinematics and dynamics;
techniques: interferometric
ID HERSCHEL-SPIRE SPECTROSCOPY; STAR-FORMATION; INTERSTELLAR-MEDIUM; NGC
1068; LINE; CO; EMISSION; GALAXIES; ARP-220; SHOCKS
AB We present Atacama Large Millimeter Array (ALMA) Cycle-0 observations of the CO J = 6-5 line in the advanced galaxy merger Arp 220. This line traces warm molecular gas, which dominates the total CO luminosity. The CO emission from the two nuclei is well resolved by the 0 ''.39x0 ''.22 beam and the exceptional sensitivity and spatial/spectral resolution reveal new complex features in the morphology and kinematics of the warm gas. The line profiles are asymmetric between the red and blue sides of the nuclear disks and the peak of the line emission is offset from the peak of the continuum emission in both nuclei by about 100 pc in the same direction. CO self-absorption is detected at the centers of both nuclei but it is much deeper in the eastern nucleus. We also clearly detect strong, highly redshifted CO absorption located near the southwest side of each nucleus. For the eastern nucleus, we reproduce the major line profile features with a simple kinematic model of a highly turbulent, rotating disk with a substantial line center optical depth and a large gradient in the excitation temperature. The red/blue asymmetries and line-to-continuum offset are likely produced by absorption of the blue (SW) sides of the two nuclei by blueshifted, foreground molecular gas; the mass of the absorber is comparable to the nuclear warm gas mass (similar to 10(8) M-circle dot). We measure an unusually high L-CO/L-FIR ratio in the eastern nucleus, suggesting there is an additional energy source, such as mechanical energy from shocks, present in this nucleus.
C1 [Rangwala, Naseem; Maloney, Philip R.; Glenn, Jason; Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
[Rangwala, Naseem] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Spinoglio, Luigi] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
RP Rangwala, N (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 1255 38th St, Boulder, CO 80303 USA.
FU NASA ROSES grant [NNX13AL16G]; NASA grant [1487846, 1472566]; Natural
Sciences and Engineering Research Council of Canada
FX The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. This paper makes use of the following ALMA data:
ADS/JAO. ALMA2011.0.00403.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. We are very grateful to Adam Leroy for doing a custom reduction
for our observations and providing very useful recommendations. We thank
Kazushi Sakamoto for sharing his CO J = 3-2 data cube observed by the
Submillimeter Array. The research of Naseem Rangwala is supported by
NASA ROSES grant NNX13AL16G. The research of Philip R. Maloney is
supported by NASA grant 1487846. The research of Christine D. Wilson
(C.D.W.) is supported by grants from the Natural Sciences and
Engineering Research Council of Canada. C.D.W. also thanks the European
Southern Observatory and the National Radio Astronomy Observatory for
visitor support. The research of Jason Glenn is supported by NASA grant
1472566.
NR 33
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 17
DI 10.1088/0004-637X/806/1/17
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300017
ER
PT J
AU Schnittman, JD
Krolik, JH
AF Schnittman, Jeremy D.
Krolik, Julian H.
TI EVOLUTION OF A BINARY BLACK HOLE WITH A RETROGRADE CIRCUMBINARY
ACCRETION DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; gravitational waves
ID ACTIVE GALACTIC NUCLEI; MERGER RATE; SUPERMASSIVE BINARY;
RADIATION-PRESSURE; MASSIVE GALAXIES; OBSCURING TORI; CENTRAL CAVITY;
GAS; SIMULATIONS; DUSTY
AB We consider the evolution of a supermassive black hole binary (SMBHB) surrounded by a retrograde accretion disk. Assuming the disk is exactly in the binary plane and transfers energy and angular momentum to the binary via direct gas accretion, we calculate the time evolution of the binary's semimajor axis a and eccentricity e. Because the gas is predominantly transferred when the binary is at apocenter, we find the eccentricity grows rapidly while maintaining constant a (1+e). After accreting only a fraction of the secondary's mass, the eccentricity grows to nearly unity; from then on, gravitational wave (GW) emission dominates the evolution, preserving constant a (1-e). The high-eccentricity waveforms redistribute the peak GW power from the nHz to mu Hz bands, substantially affecting the signal that might be detected with pulsar timing arrays. We also estimate the torque coupling binaries of arbitrary eccentricity with obliquely aligned circumbinary disks. If the outer edge of the disk is not an extremely large multiple of the binary separation, retrograde accretion can drive the binary into the GW-dominated state before these torques align the binary with the angular momentum of the mass supply.
C1 [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krolik, Julian H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Krolik, Julian/0000-0002-2995-7717
FU National Science Foundation [AST-1028111]; NASA [ATP12-0139]
FX This work was partially supported by National Science Foundation grant
AST-1028111 and NASA grant ATP12-0139. We thank Cole Miller for helpful
comments and discussion. We also thank the referee for leading us to
pursue the properties of binary-circumbinary disk (counter) alignment
much further than we had initially.
NR 61
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 88
DI 10.1088/0004-637X/806/1/88
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300088
ER
PT J
AU Singer, LP
Kasliwal, MM
Cenko, SB
Perley, DA
Anderson, GE
Anupama, GC
Arcavi, I
Bhalerao, V
Bue, BD
Cao, Y
Connaughton, V
Corsi, A
Cucchiara, A
Fender, RP
Fox, DB
Gehrels, N
Goldstein, A
Gorosabel, J
Horesh, A
Hurley, K
Johansson, J
Kann, DA
Kouveliotou, C
Huang, K
Kulkarni, SR
Masci, F
Nugent, P
Rau, A
Rebbapragada, UD
Staley, TD
Svinkin, D
Thone, CC
Postigo, ADU
Urata, Y
Weinstein, A
AF Singer, Leo P.
Kasliwal, Mansi M.
Cenko, S. Bradley
Perley, Daniel A.
Anderson, Gemma E.
Anupama, G. C.
Arcavi, Iair
Bhalerao, Varun
Bue, Brian D.
Cao, Yi
Connaughton, Valerie
Corsi, Alessandra
Cucchiara, Antonino
Fender, Rob P.
Fox, Derek B.
Gehrels, Neil
Goldstein, Adam
Gorosabel, J.
Horesh, Assaf
Hurley, Kevin
Johansson, Joel
Kann, D. A.
Kouveliotou, Chryssa
Huang, Kuiyun
Kulkarni, S. R.
Masci, Frank
Nugent, Peter
Rau, Arne
Rebbapragada, Umaa D.
Staley, Tim D.
Svinkin, Dmitry
Thoene, C. C.
Postigo, A. De Ugarte
Urata, Yuji
Weinstein, Alan
TI THE NEEDLE IN THE 100 deg(2) HAYSTACK: UNCOVERING AFTERGLOWS OF FERMI
GRBs. WITH THE PALOMAR TRANSIENT FACTORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 130702A, GRB 140606B); gravitational
waves; methods: observational; supernovae: general; surveys
ID GAMMA-RAY BURST
AB The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star. mergers that may soon be detected by Advanced LIGO and Virgo.
C1 [Singer, Leo P.; Weinstein, Alan] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Singer, Leo P.; Cenko, S. Bradley; Cucchiara, Antonino; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Perley, Daniel A.; Cao, Yi; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Anderson, Gemma E.; Fender, Rob P.] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England.
[Anderson, Gemma E.; Fender, Rob P.] Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Anupama, G. C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Arcavi, Iair] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
[Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Bhalerao, Varun] IUCAA, Pune 411007, Maharashtra, India.
[Bue, Brian D.; Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Connaughton, Valerie; Rebbapragada, Umaa D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Connaughton, Valerie] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Corsi, Alessandra] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Fox, Derek B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Goldstein, Adam; Kouveliotou, Chryssa] NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA.
[Gorosabel, J.; Thoene, C. C.; Postigo, A. De Ugarte] CSIC, IAA, E-18008 Granada, Spain.
[Gorosabel, J.] Univ Basque Country, UPV EHU, Unidad Asociada Grp Ciencia Planetarias, Dept Fis Aplicada 1,ETS Ingn,IAA,CSIC, E-48013 Bilbao, Spain.
[Gorosabel, J.] Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain.
[Horesh, Assaf] Benoziyo Ctr Astrophys, Weizmann Inst Sci, IL-76100 Rehovot, Israel.
[Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Johansson, Joel] Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Kann, D. A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Huang, Kuiyun] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan.
[Masci, Frank] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Nugent, Peter] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Svinkin, Dmitry] Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Postigo, A. De Ugarte] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
RP Singer, LP (reprint author), CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
EM leo.p.singer@nasa.gov
RI Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Thone, Christina/0000-0002-7978-7648;
Singer, Leo/0000-0001-9898-5597; Anderson, Gemma/0000-0001-6544-8007;
Staley, Tim/0000-0002-4474-5253; Bhalerao, Varun/0000-0002-6112-7609; de
Ugarte Postigo, Antonio/0000-0001-7717-5085
FU National Science Foundation (NSF); Swift Guest Investigator Program
Cycle 9 award 10522 (NASA grant) [NNX14AC24G]; Cycle 10 award 10553
(NASA grant) [NNX14AI99G]; W.M. Keck Foundation; European Research
Council Advanced Grant [267697]; Gordon and Betty Moore Foundation;
Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell
Foundation; Associates of the California Institute of Technology;
University of Chicago; state of California; state of Illinois; states of
Maryland; NSF; Discovery Communications; NSF [AST-1005313]; Spanish
research project [AYA2012-39362-C0202]; European Commission under the
Marie Curie Career Integration Grant programme (FP7-PEOPLE-CIG 322307);
Research and Technology Development Grant; NASA [NNX07AR71G, NNX13AP09G,
NNX11AP96G, NNX13AI54G]; Russian Space Agency contract; RFBR
[15-02-00532, 13-02-12017-ofi-m]; NASA
FX L.P.S. thanks generous support from the National Science Foundation
(NSF) in the form of a Graduate Research Fellowship. The National Radio
Astronomy Observatory is a facility of the NSF operated under
cooperative agreement by Associated Universities, Inc. This paper is
based on observations obtained with the Palomar 48 inch Oschin telescope
and the Palomar 60 inch telescope at the Palomar Observatory as part of
the Intermediate Palomar Transient Factory project, a scientific
collaboration among the California Institute of Technology, Los Alamos
National Laboratory, the University of Wisconsin, Milwaukee, the Oskar
Klein Center, the Weizmann Institute of Science, the TANGO Program of
the University System of Taiwan, and the Kavli Institute for the Physics
and Mathematics of the Universe. The present work is partly funded by
Swift Guest Investigator Program Cycle 9 award 10522 (NASA grant
NNX14AC24G) and Cycle 10 award 10553 (NASA grant NNX14AI99G). Some of
the data presented herein were obtained at the W.M. Keck Observatory,
which is operated as a scientific partnership among the California
Institute of Technology, the University of California, and NASA; the
Observatory was made possible by the generous financial support of the
W.M. Keck Foundation. We thank Thomas Kruhler for reducing the X-shooter
spectrum of GRB 131011A/iPTF13dsw. We thank the staff of the Mullard
Radio Astronomy Observatory for their invaluable assistance in the
operation of AMI. G.E.A., R.P.F., and T.D.S. acknowledge the support of
the European Research Council Advanced Grant 267697, "4 Pi Sky: Extreme
Astrophysics with Revolutionary Radio Telescopes." Support for CARMA
construction was derived from the Gordon and Betty Moore Foundation; the
Kenneth T. and Eileen L. Norris Foundation; the James S. 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 under a cooperative agreement. and by the CARMA
partner universities. These results made use of Lowell Observatory's
DCT. Lowell operates the DCT in partnership with Boston University,
Northern Arizona University, the University of Maryland, and the
University of Toledo. Partial support of the DCT was provided by
Discovery Communications. LMI was built by Lowell Observatory using
funds from the NSF (AST-1005313). This work is partly based on
observations made with GTC, at the Roque de los Muchachos Observatory
(La Palma, Spain). The research activity of A.d.U.P., C.T., and J.G. is
supported by Spanish research project AYA2012-39362-C0202. A.d.U.P.
acknowledges support by the European Commission under the Marie Curie
Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). A
portion of this work was carried out at the Jet Propulsion Laboratory
under a Research and Technology Development Grant, under contract with
NASA. US Government Support Acknowledged. K.H. acknowledges support for
the IPN under the following NASA grants: NNX07AR71G, NNX13AP09G,
NNX11AP96G, and NNX13AI54G. The Konus-Wind experiment is partially
supported by a Russian Space Agency contract and RFBR grants 15-02-00532
and 13-02-12017-ofi-m. IRAF is distributed by the National Optical
Astronomy Observatory, which is operated by the Association of
Universities for Research in Astronomy (AURA) under cooperative
agreement with the NSF.; This research has made use of data, software,
and/or web tools obtained from HEASARC, a service of the Astrophysics
Science Division at NASA/GSFC and of the Smithsonian Astrophysical
Observatory's High Energy Astrophysics Division. This research has made
use of NED, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. This work
made use of data supplied by the UK Swift Science Data Centre at the
University of Leicester including the Swift XRT GRB catalog and
light-curve repository (Evans et al. 2007, 2009; Goad et al. 2007). This
research made use of Astropy49 (Robitaille et al. 2013), a
community-developed core Python package for Astronomy. Some of the
results in this paper have been derived using HEALPix (Gorski et al.
2005).
NR 215
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 52
DI 10.1088/0004-637X/806/1/52
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300052
ER
PT J
AU Snowden, SL
Koutroumpa, D
Kuntz, KD
Lallement, R
Puspitarini, L
AF Snowden, S. L.
Koutroumpa, D.
Kuntz, K. D.
Lallement, R.
Puspitarini, L.
TI THE NORTH GALACTIC POLE RIFT AND THE LOCAL HOT BUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: clouds; ISM: magnetic fields; solar neighborhood;
X-rays: diffuse background
ID SOFT-X-RAY; SENSITIVITY HI SURVEY; WIND CHARGE-EXCHANGE; SOLAR-WIND;
INTERSTELLAR-MEDIUM; MOLECULAR CLOUD; URSA-MAJOR; CHANDRA OBSERVATIONS;
ROSAT SURVEY; MAPS
AB The North Galactic Pole Rift (NGPR) is one of the few distinct neutral hydrogen clouds at high Galactic latitudes that have well-defined distances. It is located at the edge of the Local Cavity (LC) and provides an important test case for understanding the Local Hot Bubble (LHB), the presumed location for the hot diffuse plasma responsible for much of the observed 1/4 keV emission originating in the solar neighborhood. Using data from the ROSAT All-Sky Survey and the Planck reddening map, we find the path length within the LC (LHB plus Complex of Local Interstellar Clouds) to be 98 +/- 27 pc, in excellent agreement with the distance to the NGPR of 98 +/- 6 pc. In addition, we examine another 14 directions that are distributed over the sky where the LC wall is apparently optically thick at 1/4 keV. We find that the data in these directions are also consistent with the LHB model and a uniform emissivity plasma filling most of the LC.
C1 [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, LATMOS IPSL,CNRS INSU, F-78280 Guyancourt, France.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lallement, R.] Univ Paris Diderot, CNRS UMR8111, GEPI, Observ Paris, F-92190 Meudon, France.
[Puspitarini, L.] Inst Teknol Bandung, FMIPA, Bosscha Observ, Bandung 40132, Indonesia.
[Puspitarini, L.] Inst Teknol Bandung, FMIPA, Dept Astron, Bandung 40132, Indonesia.
RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU l'Observatoire de Paris-Meudon GEPI; French National Program "Physique
Chimie du Milieu Interstellaire" of the Institut National des Sciences
de l'Univers (INSU); French National Research Agency (ANR) through the
STILISM project
FX S.L.S. would like to thank the l'Observatoire de Paris-Meudon GEPI for
their hospitality and support as this paper is based on work which took
place while he was a Visiting Scientist in 2014 October-November. D.K.
and R.L. would like to acknowledge financial support from the French
National Program "Physique Chimie du Milieu Interstellaire" of the
Institut National des Sciences de l'Univers (INSU). R.L. and L.P.
acknowledge support from the French National Research Agency (ANR)
through the STILISM project. The ROSAT PSPC data used in the MBM 12
analysis were acquired from the HEASARC archive. The OMNI data were
obtained from the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov.
NR 49
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 120
DI 10.1088/0004-637X/806/1/120
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300120
ER
PT J
AU Snowden, SL
Heiles, C
Koutroumpa, D
Kuntz, KD
Lallement, R
McCammon, D
Peek, JEG
AF Snowden, S. L.
Heiles, C.
Koutroumpa, D.
Kuntz, K. D.
Lallement, R.
McCammon, D.
Peek, J. E. G.
TI REVISITING THE LOCAL LEO COLD CLOUD AND REVISED CONSTRAINTS ON THE LOCAL
HOT BUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: clouds; ISM: magnetic fields; solar neighborhood;
X-rays: diffuse background
ID SOFT-X-RAY; WIND CHARGE-EXCHANGE; SOUTHERN GALACTIC HEMISPHERE;
SENSITIVITY HI SURVEY; ALL-SKY SURVEY; INTERSTELLAR-MEDIUM;
PHYSICAL-PROPERTIES; SUPERNOVA REMNANT; MOLECULAR CLOUDS; CROSS-SECTIONS
AB The Local Leo Cold Cloud (LLCC, at a distance of 11-24 pc) was studied in its relation to the Local Hot Bubble (LHB) and the result suggested that much of the observed 1/4 keV emission in that direction originates in front of the cloud. This placed a strong constraint on the distribution of X-ray emission within the LHB and called into question the assumption of a uniform distribution of X-ray emitting plasma within the Local Cavity. However, recent work has quantified the contribution of heliospheric solar wind charge exchange (SWCX) emission to the diffuse X-ray background measured by the ROSAT All-Sky Survey (RASS) at 1/4 keV, and led to the consistency of pressure measurements between the LHB and the local cloud component of the complex of local interstellar clouds (CLICs) surrounding the Sun. In this paper we revisit the LLCC and improve the previous analysis by using higher resolution RASS data, a serendipitous ROSAT pointed observation, a rigorous treatment of the band-averaged X-ray absorption cross section, and models for the heliospheric and magnetospheric SWCX contributions. We find that the foreground emission to the cloud is in excess of the expected heliospheric (interplanetary plus near Earth) SWCX contribution but that it is marginally consistent with the range of possible LHB plasma path lengths between the LLCC and the CLICs given the currently understood plasma emissivity.
C1 [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Heiles, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, LATMOS IPSL,CNRS INSU, F-78280 Guyancourt, France.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lallement, R.] Univ Paris Diderot, CNRS, GEPI, Observ Paris,UMR8111, F-92190 Meudon, France.
[McCammon, D.] Univ Wisconsin, Madison, WI 53706 USA.
[Peek, J. E. G.] Space Telescope Sci Inst, Baltimore, MD 21210 USA.
RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI McCammon, Dan/0000-0001-5170-4567
FU French National Program "Physique Chimie du Milieu Interstellaire" of
the Institut National des Sciences de l'Univers (INSU); l'Observatoire
de Paris-Meudon GEPI
FX S.L.S. would like to thank the l'Observatoire de Paris-Meudon GEPI for
their hospitality and support as much of the analysis in this paper took
place while he was a Visiting Scientist in 2014 October-November. D.K.
and R.L. would like to acknowledge financial support from the French
National Program "Physique Chimie du Milieu Interstellaire" of the
Institut National des Sciences de l'Univers (INSU). The ROSAT PSPC data
used in the LLCC analysis were acquired from the HEASARC archive. The
IMP-8 data were obtained from the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov.
NR 78
TC 4
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 119
DI 10.1088/0004-637X/806/1/119
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300119
ER
PT J
AU Sonnentrucker, P
Wolfire, M
Neufeld, DA
Flagey, N
Gerin, M
Goldsmith, P
Lis, D
Monje, R
AF Sonnentrucker, P.
Wolfire, M.
Neufeld, D. A.
Flagey, N.
Gerin, M.
Goldsmith, P.
Lis, D.
Monje, R.
TI A HERSCHEL/HIFI LEGACY SURVEY OF HF AND H2O IN THE GALAXY: PROBING
DIFFUSE MOLECULAR CLOUD CHEMISTRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; cosmic rays; ISM: abundances; ISM: clouds; ISM: lines
and bands; ISM: molecules
ID STAR-FORMING REGIONS; RAY IONIZATION RATE; FINE-STRUCTURE EXCITATION;
TRANSLUCENT SIGHT LINES; HYDROGEN-FLUORIDE; INTERSTELLAR-MEDIUM;
TRIGONOMETRIC PARALLAXES; GALACTIC-CENTER; G10.6-0.4 W31C; SAGITTARIUS
B2(M)
AB We combine Herschel observations for a total of 12 sources to construct the most uniform survey of HF and H2O in our Galactic disk. Both molecules are detected in absorption along all sight lines. The high spectral resolution of the Heterodyne Instrument for the Far-infrared (HIFI) allows us to compare the HF and H2O distributions in 47 diffuse cloud components sampling the disk. We find that the HF and H2O velocity distributions follow each other almost perfectly and establish that HF and H2O probe the same gas-phase volume. Our observations corroborate theoretical predictions that HF is a sensitive tracer of H-2 in diffuse clouds, down to molecular fractions of only a few percent. Using HF to trace H-2 in our sample, we find that the N(H2O)-to-N(HF) ratio shows a narrow distribution with a median value of 1.51. Our results further suggest that H2O might be used as a tracer of H-2-within a factor of 2.5-in the diffuse interstellar medium (ISM). We show that the measured factor of similar to 2.5 variation around the median is driven by true local variations in the H2O abundance relative to H-2 throughout the disk. The latter variability allows us to test our theoretical understanding of the chemistry of oxygen-bearing molecules in the diffuse gas. We show that both gas-phase and grain-surface chemistry are required to reproduce our H2O observations. This survey thus confirms that grain surface reactions can play a significant role in the chemistry occurring in the diffuse ISM (n(H) <= 1000 cm(-3)).
C1 [Sonnentrucker, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sonnentrucker, P.] European Space Agcy, F-75738 Paris 15, France.
[Wolfire, M.] Univ Maryland, College Pk, MD 20742 USA.
[Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Flagey, N.] Inst Astron, Hilo, HI 96720 USA.
[Gerin, M.; Lis, D.] Univ Paris 06, Sorbonne Univ, Observ Paris, CNRS,UMR 8112,LERMA, Paris, France.
[Gerin, M.; Lis, D.] PSL Res Univ, LERMA, Observ Paris, CNRS,UMR 8112, F-75014 Paris, France.
[Goldsmith, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lis, D.; Monje, R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RP Sonnentrucker, P (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM sonnentr@stsci.edu
FU NASA [NNN12AA01C]; NSF grant [AST-1411827]
FX We thank the referee for very useful comments that improved the
manuscript significantly. We thank David Hollenbach for useful comments
on grain surface chemistry. P.S. acknowledges support for this work from
NASA through award NNN12AA01C issued by JPL/Caltech. M.G.W. was
supported in part by NSF grant AST-1411827. M.G. thanks CNES and
PCMI/INSU for support for the analysis of the Herschel data. This work
was carried out in part at the Jet Propulsion Laboratory, which is
operated for NASA by the California Institute of Technology. HIFI has
been designed and built by a consortium of institutes and university
departments from across Europe, Canada, and the United States under the
leadership of SRON Netherlands, Institute for Space Research, Groningen,
The Netherlands, and with major contributions from Germany, France, and
the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR,
LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth;
Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF;
Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio
Astronomico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden:
Chalmers University of Technology-MC2, RSS, & GARD; Onsala Space
Observatory; Swedish National Space Board, Stockholm
University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA:
Caltech, JPL, NHSC.
NR 72
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 49
DI 10.1088/0004-637X/806/1/49
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300049
ER
PT J
AU Walton, DJ
Middleton, MJ
Rana, V
Miller, JM
Harrison, FA
Fabian, AC
Bachetti, M
Barret, D
Boggs, SE
Christensen, FE
Craig, WW
Fuerst, F
Grefenstette, BW
Hailey, CJ
Madsen, KK
Stern, D
Zhang, W
AF Walton, D. J.
Middleton, M. J.
Rana, V.
Miller, J. M.
Harrison, F. A.
Fabian, A. C.
Bachetti, M.
Barret, D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Fuerst, F.
Grefenstette, B. W.
Hailey, C. J.
Madsen, K. K.
Stern, D.
Zhang, W.
TI NUSTAR, XMM-NEWTON, AND SUZAKU OBSERVATIONS OF THE ULTRALUMINOUS X-RAY
SOURCE HOLMBERG II X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: individual (Holmberg II
X-1)
ID MASS BLACK-HOLES; BROAD-BAND; ACCRETION DISKS; STATE TRANSITIONS; NEARBY
GALAXIES; SPECTRAL STATE; EMISSION-LINE; SOLAR MASSES; ESO 243-49; IX
X-1
AB We present the first broadband 0.3-25.0 keV X-ray observations of the bright ultraluminous X-ray source (ULX) Holmberg II X-1, performed by NuSTAR, XMM-Newton, and Suzaku in 2013 September. The NuSTAR data provide the first observations of Holmberg II X-1 above 10 keV and reveal a very steep high-energy spectrum, similar to other ULXs observed by NuSTAR to date. These observations further demonstrate that ULXs exhibit spectral states that are not typically seen in Galactic black hole binaries. Comparison with other sources implies that Holmberg II X-1 accretes at a high fraction of its Eddington accretion rate and possibly exceeds it. The soft X-ray spectrum (E < 10 keV) appears to be dominated by two blackbody-like emission components, the hotter of which may be associated with an accretion disk. However, all simple disk models under-predict the NuSTAR data above similar to 10 keV and require an additional emission component at the highest energies probed, implying the NuSTAR data does not fall away with a Wien spectrum. We investigate physical origins for such an additional high-energy emission component and favor a scenario in which the excess arises from Compton scattering in a hot corona of electrons with some properties similar to the very high state seen in Galactic binaries. The observed broadband 0.3-25.0 keV luminosity inferred from these epochs is L-X = (8.1 +/- 0.1) x 10(39) erg s(-1), typical for Holmberg II X-1, with the majority of this flux (similar to 90%) emitted below 10 keV.
C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walton, D. J.; Rana, V.; Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.] CALTECH, Space Radiat Lab, Pasadena, CA 91109 USA.
[Middleton, M. J.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 49109 USA.
[Bachetti, M.; Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Bachetti, M.; Barret, D.] 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-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337;
Rana, Vikram/0000-0003-1703-8796
FU French Space Agency (CNES); NASA; ESA; space agency of Japan (JAXA);
space agency of USA (NASA)
FX The authors would like to thank the referee for the positive feedback,
which helped improve the clarity of the final manuscript. M.B. and D.B.
acknowledge financial support from the French Space Agency (CNES). This
research has made use of data obtained with NuSTAR, a project led by
Caltech, funded by NASA and managed by NASA/JPL and has utilized the
NUSTARDAS software package, jointly developed by the ASDC (Italy) and
Caltech (USA). This research has also made use of data obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States, and with Suzaku, a collaborative
mission between the space agencies of Japan (JAXA) and the USA (NASA).
NR 69
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U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 65
DI 10.1088/0004-637X/806/1/65
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300065
ER
PT J
AU Williams, BF
Dalcanton, JJ
Dolphin, AE
Weisz, DR
Lewis, AR
Lang, DT
Bell, EF
Boyer, M
Fouesneau, M
Gilbert, KM
Monachesi, A
Skillman, E
AF Williams, Benjamin F.
Dalcanton, Julianne J.
Dolphin, Andrew E.
Weisz, Daniel R.
Lewis, Alexia R.
Lang, Dustin
Bell, Eric F.
Boyer, Martha
Fouesneau, Morgan
Gilbert, Karoline M.
Monachesi, Antonela
Skillman, Evan
TI A GLOBAL STAR-FORMING EPISODE IN M31 2-4 GYR AGO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: individual (M31); galaxies: interactions
ID LOCAL GROUP GALAXIES; ANDROMEDA GALAXY; FORMATION HISTORY; STELLAR
CONTENT; DWARF GALAXIES; SPIRAL GALAXY; GIANT STREAM; THIN PLANE; OUTER
DISK; MILKY-WAY
AB We have identified a major global enhancement of star formation in the inner M31 disk that occurred between 2-4 Gyr ago, producing similar to 60% of the stellar mass formed in the past 5 Gyr. The presence of this episode in the inner disk was discovered by modeling the optical resolved star color-magnitude diagrams of low extinction regions in the main disk of M31 (3 < R < 20 kpc) as part of the Panchromatic Hubble Andromeda Treasury. This measurement confirms and extends recent measurements of a widespread star formation enhancement of similar age in the outer disk, suggesting that this burst was both massive and global. Following the galaxy-wide burst, the star formation rate of M31 has significantly declined. We briefly discuss possible causes for these features of the M31 evolutionary history, including interactions with M32, M33, and/or a merger.
C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Weisz, Daniel R.; Lewis, Alexia R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85706 USA.
[Lang, Dustin] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Boyer, Martha] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Fouesneau, Morgan] MPIA, Heidelberg, Germany.
[Gilbert, Karoline M.] STScI, Baltimore, MD 21218 USA.
[Monachesi, Antonela] MPA, Garching, Germany.
[Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM ben@astro.washington.edu; jd@astro.washington.edu;
adolphin@raytheon.com; dweisz@astro.washington.edu; dstn@cmu.edu;
ericbell@umich.edu; martha.boyer@nasa.gov; fouesneau@mpia-hd.mpg.de;
kgilbert@stsci.edu; antonela@mpa-garching.mpg.de; skillman@astro.umn.edu
OI Bell, Eric/0000-0002-5564-9873
FU NASA through grant from the Space Telescope Science Institute
[GO-12055]; NASA - Space Telescope Science Institute [HST-HF-51331.01];
NASA [NAS5-26555]
FX Support for this work was provided by NASA through grant GO-12055 from
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. Support for DRW is provided by NASA
through Hubble Fellowship grants HST-HF-51331.01 awarded by the Space
Telescope Science Institute. We thank Amazon cloud services, for
donating some of the computing time necessary to make these
measurements.
NR 61
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 48
DI 10.1088/0004-637X/806/1/48
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300048
ER
PT J
AU Zhang, BB
van Eerten, H
Burrows, DN
Ryan, GS
Evans, PA
Racusin, JL
Troja, E
MacFadyen, A
AF Zhang, Bin-Bin
van Eerten, Hendrik
Burrows, David N.
Ryan, Geoffrey Scott
Evans, Philip A.
Racusin, Judith L.
Troja, Eleonora
MacFadyen, Andrew
TI AN ANALYSIS OF CHANDRA DEEP FOLLOW-UP GAMMA-RAY BURSTS: IMPLICATIONS FOR
OFF-AXIS JETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; methods: numerical
ID AFTERGLOW LIGHT CURVES; SWIFT XRT DATA; BROAD-BAND OBSERVATIONS; X-RAY;
COMPREHENSIVE ANALYSIS; ELECTRON ACCELERATION; COLLISIONLESS SHOCKS;
SPECTRAL PROPERTIES; OPTICAL AFTERGLOW; RELATIVISTIC JET
AB We present a sample of 27 gamma-ray bursts (GRBs) with detailed Swift. light curves supplemented by late-time Chandra. observations. To answer the missing jet-break problem in general, we develop a numerical-simulationbased model that can be directly fit to the data using Monte Carlo methods. Our numerical model takes into account all the factors that can shape a jet break: (i) lateral expansion, (ii) edge effects, and (iii) off-axis effects. Our results provide improved fits to the light curves and constraints on physical parameters. More importantly, our results suggest that off-axis effects are important and must be included in interpretations of GRB jet breaks.
C1 [Zhang, Bin-Bin; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Zhang, Bin-Bin] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Zhang, Bin-Bin] CSIC, IAA, E-18080 Granada, Spain.
[van Eerten, Hendrik] Max Planck Inst Extraterrestrial Phys MPE, D-85741 Garching, Germany.
[van Eerten, Hendrik; Ryan, Geoffrey Scott; MacFadyen, Andrew] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA.
[Evans, Philip A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Racusin, Judith L.; Troja, Eleonora] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Troja, Eleonora] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA.
RP Zhang, BB (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
EM binbin.zhang@uah.edu
RI Zhang, Binbin/C-9035-2013;
OI Zhang, Binbin/0000-0003-2002-116X; Zhang, Binbin/0000-0003-4111-5958;
MacFadyen, Andrew/0000-0002-0106-9013
FU NASA [NAS5-00136, TM3-14005X, NNX13AO93G]; SAO [SV4-74018, AR3-14005X,
GO1-12102X, GO3-14067X]
FX We thank the anonymous referee for detailed and thoughtful comments that
greatly improved the paper. We thank Peter Veres, Peter Meszaros, Kazumi
Kashiyama, Xiao-Hong Zhao, Xue-Wen Liu, Valerie Connaughton, Dirk Grupe,
Derek Fox, Abe Falcone, Leisa Townsley, Eveline Helder, He Gao, Liang
Li, Fangkun Peng, Enwei Liang, Neil Gehrels, and Bing Zhang for helpful
comments and suggestions. We thank Tyson Littenberg and Dan
Foreman-Mackey for discussion on the MCMC method. B.B.Z. thanks Johannes
Buchner and Farhan Feroz for help on the MULTINEST codes. This work was
supported by SAO contract SV4-74018, NASA contract NAS5-00136, and by
SAO grants AR3-14005X, GO1-12102X, and GO3-14067X. H.V.E., G.S.R., and
A.M. acknowledge the support by NASA TM3-14005X and NNX13AO93G. We
acknowledge the use of public data from the Swift and Chandra data
archive. This work made use of data supplied by the UK Swift Science
Data Centre at the University of Leicester.
NR 101
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U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2015
VL 806
IS 1
AR 15
DI 10.1088/0004-637X/806/1/15
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL2XF
UT WOS:000356810300015
ER
PT J
AU Schiemangk, M
Lampmann, K
Dinkelaker, A
Kohfeldt, A
Krutzik, M
Kurbis, C
Sahm, A
Spiessberger, S
Wicht, A
Erbert, G
Trankle, G
Peters, A
AF Schiemangk, Max
Lampmann, Kai
Dinkelaker, Aline
Kohfeldt, Anja
Krutzik, Markus
Kuerbis, Christian
Sahm, Alexander
Spiessberger, Stefan
Wicht, Andreas
Erbert, Goetz
Traenkle, Guenther
Peters, Achim
TI High-power, micro-integrated diode laser modules at 767 and 780 nm for
portable quantum gas experiments
SO APPLIED OPTICS
LA English
DT Article
ID ATOM INTERFEROMETRY; LINEWIDTH
AB We present micro-integrated diode laser modules operating at wavelengths of 767 and 780 nm for cold quantum gas experiments on potassium and rubidium. The master-oscillator-power-amplifier concept provides both narrow linewidth emission and high optical output power. With a linewidth (10 mu s) below 1 MHz and an output power of up to 3W, these modules are specifically suited for quantum optics experiments and feature the robustness required for operation at a drop tower or on-board a sounding rocket. This technology development hence paves the way toward precision quantum optics experiments in space. (C) 2015 Optical Society of America
C1 [Schiemangk, Max; Lampmann, Kai; Dinkelaker, Aline; Krutzik, Markus; Wicht, Andreas; Peters, Achim] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Schiemangk, Max; Lampmann, Kai; Dinkelaker, Aline; Kohfeldt, Anja; Kuerbis, Christian; Sahm, Alexander; Spiessberger, Stefan; Wicht, Andreas; Erbert, Goetz; Traenkle, Guenther; Peters, Achim] Leibniz Inst Hochstfrequenztech, Ferdinand Braun Inst, D-12489 Berlin, Germany.
[Lampmann, Kai] Johannes Gutenberg Univ Mainz, Inst Phys, D-55128 Mainz, Germany.
[Krutzik, Markus] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Schiemangk, M (reprint author), Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
EM max.schiemangk@physik.hu-berlin.de
FU German Space Agency (DLR) [DLR 50WM0940, DLR 50WM1132, DLR 50WM1134, DLR
50WM1240]; European Commission (EC) [250072]; European Union
FX German Space Agency (DLR) (DLR 50WM0940, DLR 50WM1132, DLR 50WM1134, DLR
50WM1240); European Commission (EC) (250072).; The authors thank H.
Ahlers, H. Muntinga, and A. Wenzlawski from the QUANTUS-I team for
providing their experiment for the test of the MOPA module. C. K. and A.
W. acknowledge financial support from the European Union's Seventh
Framework Programme for research, technological development and
demonstration.
NR 22
TC 8
Z9 8
U1 1
U2 10
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 JUN 10
PY 2015
VL 54
IS 17
BP 5332
EP 5338
DI 10.1364/AO.54.005332
PG 7
WC Optics
SC Optics
GA CK3FE
UT WOS:000356101200010
PM 26192832
ER
PT J
AU Brasunas, J
Mamoutkine, A
Gorius, N
AF Brasunas, J.
Mamoutkine, A.
Gorius, N.
TI Identifying sampling comb changes in Fourier transform spectrometers
with significant self-emission and beam splitter absorption
SO APPLIED OPTICS
LA English
DT Article
ID CALIBRATION; MODE
AB For accurate calibration of Fourier transform spectrometers we must constrain or resample the interferogram data to an invariant sampling comb. This can become challenging when instrument self-emission is significant and beam splitter absorption is present. The originally-sampled interferogram center-burst position can move due not only to sampling comb changes, but also to an interaction between the strength of an external target and the so-called anomalous phase (the two ports of the interferometer contribute center-bursts at different locations, and the relative weighting of the two ports varies with the strength of the external target). We present a model of the anomalous phase to enable partitioning of changes in observed center-burst location between sampling comb changes and anomalous phase effects.
C1 [Brasunas, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mamoutkine, A.] Adnet Syst, Greenbelt, MD 20771 USA.
[Gorius, N.] Catholic Univ, Greenbelt, MD 20771 USA.
RP Brasunas, J (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM john.c.brasunas@nasa.gov
NR 13
TC 1
Z9 1
U1 1
U2 7
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JUN 10
PY 2015
VL 54
IS 17
BP 5461
EP 5468
DI 10.1364/AO.54.005461
PG 8
WC Optics
SC Optics
GA CK3FE
UT WOS:000356101200026
PM 26192848
ER
PT J
AU de Leon, J
Takami, M
Karr, JL
Hashimoto, J
Kudo, T
Sitko, M
Mayama, S
Kusakabe, N
Akiyama, E
Liu, HB
Usuda, T
Abe, L
Brandner, W
Brandt, TD
Carson, J
Currie, T
Egner, SE
Feldt, M
Follette, K
Grady, CA
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Ishii, KWHM
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, Y
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Wisniewski, JP
Yamada, T
Takami, H
Tamura, M
AF de Leon, Jerome
Takami, Michihiro
Karr, Jennifer L.
Hashimoto, Jun
Kudo, Tomoyuki
Sitko, Michael
Mayama, Satoshi
Kusakabe, Nobuyuki
Akiyama, Eiji
Liu, Hauyu Baobab
Usuda, Tomonori
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Follette, Katherine
Grady, Carol A.
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
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
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John P.
Yamada, Toru
Takami, Hideki
Tamura, Motohide
TI NEAR-IR HIGH-RESOLUTION IMAGING POLARIMETRY OF THE SU Aur DISK: CLUES
FOR TIDAL TAILS?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE polarization; protoplanetary disks; stars: individual (SU Aur); stars:
pre-main sequence
ID T-TAURI STARS; PROTOPLANETARY DISK; CIRCUMSTELLAR DISK; PROTOSTELLAR
ENVELOPES; STELLAR ENCOUNTERS; ADAPTIVE OPTICS; FORMING REGIONS;
SCATTERED-LIGHT; GIANT PLANETS; YOUNG STARS
AB We present new high-resolution (similar to 0."09) H-band imaging observations of the circumstellar disk around the T Tauri star SU Aur. Our observations with Subaru-HiCIAO have revealed the presence of scattered light as close as 0."15 (similar to 20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of similar to 90 AU, an inclination of similar to 35 degrees from the plane of the sky, and an approximate PA of 15 degrees for the major axis. We find a brightness asymmetry between the northern and southern sides of the disk due to a non-axisymmetric disk structure. We also identify a pair of asymmetric tail structures extending east and west from the disk. The western tail extends at least 2."5 (350 AU) from the star, and is probably associated with a reflection nebula previously observed at optical and near-IR wavelengths. The eastern tail extends at least 1. (140 AU) at the present signal-to-noise. These tails are likely due to an encounter with an unseen brown dwarf, but our results do not exclude the explanation that these tails are outflow cavities or jets.
C1 [de Leon, Jerome; Takami, Michihiro; Karr, Jennifer L.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[de Leon, Jerome; Mayama, Satoshi; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Miura, Kanagawa 2400193, Japan.
[Hashimoto, Jun; Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Hashimoto, Jun; Kusakabe, Nobuyuki; Akiyama, Eiji; Usuda, Tomonori; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Tamura, Motohide] Subaru Telescope, Hilo, HI 96720 USA.
[Sitko, Michael] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06108 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Follette, Katherine] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96402 USA.
[Grady, Carol A.; McElwain, Michael W.] Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
Univ Sternwarte, D-81679 Munich, Germany.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kwon, Jungmi; Takahashi, Yasuhiro; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Higashihiroshima 7398511, Japan.
[Moro-Martin, Amaya] CSIC, CAB, INTA, Dept Astrophys, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takahashi, Yasuhiro] MEXT, Tokyo, Tokyo 1008959, Japan.
[Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Univ, 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 de Leon, J (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM jpdeleon.bsap@gmail.com
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016;
OI Watanabe, Makoto/0000-0002-3656-4081; Feldt, Markus/0000-0002-4188-5242
FU Ministry of Science and Technology (MoST) of Taiwan
[103-2112-M-001-029]; NSF AST [1008440]
FX We thank the Subaru Telescope staff for their support, especially
Michael Lemmen for making our observations successful. We also thank
Drs. Kazushi Sakamoto, Shigehisa Takakuwa, Lihwai Lin, Yoichi Ohyama,
Pin-Gao Gu, and Henry Hsieh for useful discussions. M. T. is supported
from Ministry of Science and Technology (MoST) of Taiwan (Grant No.
103-2112-M-001-029). C.A.G. acknowledges support under NSF AST 1008440.
This research made use of the Simbad database operated at CDS,
Strasbourg, France, and the NASA's Astrophysics Data System Abstract
Service.
NR 42
TC 2
Z9 2
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 10
PY 2015
VL 806
IS 1
AR L10
DI 10.1088/2041-8205/806/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL0LH
UT WOS:000356633700010
ER
PT J
AU Fransson, C
Larsson, J
Migotto, K
Pesce, D
Challis, P
Chevalier, RA
France, K
Kirshner, RP
Leibundgut, B
Lundqvist, P
McCray, R
Spyromilio, J
Taddia, F
Jerkstrand, A
Mattila, S
Smith, N
Sollerman, J
Wheeler, JC
Crotts, A
Garnavich, P
Heng, K
Lawrence, SS
Panagia, N
Pun, CSJ
Sonneborn, G
Sugerman, B
AF Fransson, Claes
Larsson, Josefin
Migotto, Katia
Pesce, Dominic
Challis, Peter
Chevalier, Roger A.
France, Kevin
Kirshner, Robert P.
Leibundgut, Bruno
Lundqvist, Peter
McCray, Richard
Spyromilio, Jason
Taddia, Francesco
Jerkstrand, Anders
Mattila, Seppo
Smith, Nathan
Sollerman, Jesper
Wheeler, J. Craig
Crotts, Arlin
Garnavich, Peter
Heng, Kevin
Lawrence, Stephen S.
Panagia, Nino
Pun, Chun S. J.
Sonneborn, George
Sugerman, Ben
TI THE DESTRUCTION OF THE CIRCUMSTELLAR RING OF SN 1987A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; shock waves; supernovae: individual (SN 1987A)
ID SUPERNOVA 1987A; RADIO REMNANT; SPECTROSCOPY; SIMULATIONS; EVOLUTION;
SN-1987A; NEBULA; EJECTA; SHOCK
AB We present imaging and spectroscopic observations with Hubble Space Telescope and Very Large Telescope of the ring of SN 1987A from 1994 to 2014. After an almost exponential increase of the shocked emission from the hotspots up to day similar to 8000 (similar to 2009), both this and the unshocked emission are now fading. From the radial positions of the hotspots we see an acceleration of these up to 500-1000 km s(-1), consistent with the highest spectroscopic shock velocities from the radiative shocks. In the most recent observations (2013 and 2014), we find several new hotspots outside the inner ring, excited by either X-rays from the shocks or by direct shock interaction. All of these observations indicate that the interaction with the supernova ejecta is now gradually dissolving the hotspots. We predict, based on the observed decay, that the inner ring will be destroyed by similar to 2025.
C1 [Fransson, Claes; Migotto, Katia; Lundqvist, Peter; Taddia, Francesco; Sollerman, Jesper] AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Larsson, Josefin] AlbaNova, KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Pesce, Dominic; Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[France, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Leibundgut, Bruno; Spyromilio, Jason] European So Observ, D-85748 Garching, Germany.
[McCray, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jerkstrand, Anders] Queens Univ, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Mattila, Seppo] Turku Univ, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Mattila, Seppo] Turku Univ, Tuorla Observ, Dept Phys & Astron, FI-21500 Piikkio, Finland.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Crotts, Arlin] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Garnavich, Peter] Univ Notre Dame, Nieuwland Sci 25, Notre Dame, IN 46556 USA.
[Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland.
[Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA.
[Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, Nino] Osserv Astron Capodimonte, INAF NA, I-80131 Naples, Italy.
[Panagia, Nino] Supernova Ltd, Virgin Gorda VG 1150, Virgin Islands, England.
[Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Sugerman, Ben] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA.
RP Fransson, C (reprint author), AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
RI Jerkstrand, Anders/K-9648-2015;
OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman,
Jesper/0000-0003-1546-6615; Lundqvist, Peter/0000-0002-3664-8082;
/0000-0003-0065-2933; Fransson, Claes/0000-0001-8532-3594; Heng,
Kevin/0000-0003-1907-5910
FU Swedish Research Council; Swedish National Space Board, NASA
[NNX12AF90G]; NSF [AST-1109801]; NASA through a grant from the Space
Telescope Science Institute; ESO Programmes [080.D-0727, 082.D-0273,
086.D-0713, 088.D-0638, 090.D-645, 092.D0119, 094.D-0505]
FX We are grateful to the referee for detailed comments. This work was
supported by the Swedish Research Council and the Swedish National Space
Board, NASA grant NNX12AF90G, NSF grant AST-1109801. Support for the HST
observing program was provided by NASA through a grant from the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc. Partially based on
observations collected at the European Southern Observatory, Chile (ESO
Programmes 080.D-0727, 082.D-0273, 086.D-0713, 088.D-0638, 090.D-645,
092.D0119, 094.D-0505).
NR 23
TC 9
Z9 9
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 10
PY 2015
VL 806
IS 1
AR L19
DI 10.1088/2041-8205/806/1/L19
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL0LH
UT WOS:000356633700019
ER
PT J
AU Morales-Juberias, R
Sayanagi, KM
Simon, AA
Fletcher, LN
Cosentino, RG
AF Morales-Juberias, R.
Sayanagi, K. M.
Simon, A. A.
Fletcher, L. N.
Cosentino, R. G.
TI MEANDERING SHALLOW ATMOSPHERIC JET AS A MODEL OF SATURN'S NORTH-POLAR
HEXAGON
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: general;
planets and satellites: physical evolution
ID GULF-STREAM; EQUILIBRIA; STABILITY; EASTWARD; ANNULUS; WAVES
AB The Voyager flybys of Saturn in 1980-1981 revealed a circumpolar Hexagon at similar to 78 degrees north planetographic latitude that has persisted for over 30 Earth years, more than one Saturn year, and has been observed by ground-based telescopes, Hubble Space Telescope and multiple instruments on board the Cassini orbiter. Its average phase speed is very slow with respect to the System III rotation rate, defined by the primary periodicity in the Saturn Kilometric Radiation during the Voyager era. Cloud tracking wind measurements reveal the presence of a prograde jet-stream whose path traces the Hexagon's shape. Previous numerical models have produced large-amplitude, n = 6, wavy structures with westward intrinsic phase propagation (relative to the jet). However, the observed net phase speed has proven to be more difficult to achieve. Here we present numerical simulations showing that instabilities in shallow jets can equilibrate as meanders closely resembling the observed morphology and phase speed of Saturn's northern Hexagon. We also find that the winds at the bottom of the model are as important as the winds at the cloud level in matching the observed Hexagon's characteristics.
C1 [Morales-Juberias, R.; Cosentino, R. G.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Sayanagi, K. M.] Hampton Univ, Atmospher & Planetary Sci Dept, Hampton, VA 23668 USA.
[Simon, A. A.] NASA, GSFC, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Fletcher, L. N.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England.
RP Morales-Juberias, R (reprint author), New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
EM rmjuberias@gmail.com
RI Simon, Amy/C-8020-2012; Fletcher, Leigh/D-6093-2011
OI Simon, Amy/0000-0003-4641-6186; Fletcher, Leigh/0000-0001-5834-9588
FU NASA [NNX14AH47G, NNX12AR38G]; NSF [1212216]; Royal Society Research
Fellowship at the University of Oxford
FX This work was partially supported by NASA PATM grant number NNX14AH47G
to A.S., and NASA OPR grant NNX12AR38G and NSF A&A grant 1212216 to
K.M.S. L.N.F. was supported by a Royal Society Research Fellowship at
the University of Oxford. Computational resources were provided by New
Mexico Tech.
NR 26
TC 0
Z9 0
U1 4
U2 12
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 JUN 10
PY 2015
VL 806
IS 1
AR L18
DI 10.1088/2041-8205/806/1/L18
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL0LH
UT WOS:000356633700018
ER
PT J
AU Scott, JM
Haykowsky, MJ
AF Scott, Jessica M.
Haykowsky, Mark J.
TI Letter by Scott and Haykowsky Regarding Articles, "Can Intensive
Exercise Harm the Heart? The Benefits of Competitive Endurance Training
for Cardiovascular Structure and Function" and "Can Intensive Exercise
Harm the Heart? You Can Get Too Much of a Good Thing"
SO CIRCULATION
LA English
DT Letter
C1 [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
[Haykowsky, Mark J.] Univ Alberta, Edmonton, AB, Canada.
RP Scott, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
NR 6
TC 0
Z9 0
U1 0
U2 1
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 0009-7322
EI 1524-4539
J9 CIRCULATION
JI Circulation
PD JUN 9
PY 2015
VL 131
IS 23
BP E523
EP E523
DI 10.1161/CIRCULATIONAHA.114.013457
PG 1
WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease
SC Cardiovascular System & Cardiology
GA DC5IJ
UT WOS:000369254400002
PM 26056349
ER
PT J
AU Lecoutre, C
Guillaument, R
Marre, S
Garrabos, Y
Beysens, D
Hahn, I
AF Lecoutre, C.
Guillaument, R.
Marre, S.
Garrabos, Y.
Beysens, D.
Hahn, I.
TI Weightless experiments to probe universality of fluid critical behavior
SO PHYSICAL REVIEW E
LA English
DT Article
ID LIQUID CRITICAL-POINT; CRITICAL ISOCHORE; LIGHT-SCATTERING; XENON; HEAT;
SF6
AB Near the critical point of fluids, critical opalescence results in light attenuation, or turbidity increase, that can be used to probe the universality of critical behavior. Turbidity measurements in SF6 under weightlessness conditions on board the International Space Station are performed to appraise such behavior in terms of both temperature and density distances from the critical point. Data are obtained in a temperature range, far (1 K) from and extremely close (a few mu K) to the phase transition, unattainable from previous experiments on Earth. Data are analyzed with renormalization-group matching classical-to-critical crossover models of the universal equation of state. It results that the data in the unexplored region, which is a minute deviant from the critical density value, still show adverse effects for testing the true asymptotic nature of the critical point phenomena.
C1 [Lecoutre, C.; Guillaument, R.; Marre, S.; Garrabos, Y.] CNRS, ICMCB, ESEME, UPR 9048, F-33600 Pessac, France.
[Lecoutre, C.; Guillaument, R.; Marre, S.; Garrabos, Y.] Univ Bordeaux, ICMCB, UPR 9048, F-33600 Pessac, France.
[Beysens, D.] Univ Paris Diderot, Univ Paris 06, CNRS ESPCI, Phys & Mecan Milieux Heterogenes,UMR 7636, F-75005 Paris, France.
[Beysens, D.] CEA Grenoble, Serv Basses Temp, F-38000 Grenoble, France.
[Beysens, D.] Univ Grenoble 1, F-38000 Grenoble, France.
[Hahn, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lecoutre, C (reprint author), CNRS, ICMCB, ESEME, UPR 9048, F-33600 Pessac, France.
EM carole.lecoutre@icmcb.cnrs.fr
RI Lecoutre, Carole/H-3367-2013; Garrabos, Yves/H-5404-2013; Marre,
Samuel/H-3377-2013
FU CNES; NASA
FX We thank the DECLIC CNES-NASA teams, and associated industrial teams,
involved in the ALI-DECLIC project development and achievement and in
particular the NASA and CADMOS teams for operational managing and
control of the facility onboard the ISS. C.L., R.G., S.M., Y.G., and
D.B. are grateful to CNES for financial support. The research of I.H.
was carried out at Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.
NR 23
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Z9 5
U1 0
U2 8
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
EI 1550-2376
J9 PHYS REV E
JI Phys. Rev. E
PD JUN 8
PY 2015
VL 91
IS 6
AR 060101
DI 10.1103/PhysRevE.91.060101
PG 5
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA CJ8BY
UT WOS:000355725400001
PM 26172640
ER
PT J
AU Sola, F
Dynys, FW
AF Sola, F.
Dynys, F. W.
TI Probing the mechanical properties and microstructure of WSi2/SixGe1-x
multiphase thermoelectric material by nanoindentation, electron and
focused ion beam microscopy methods
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE SEM; TEM; FIB; Nanoindentation; Fracture toughness; Thermoelectric
material
ID ELASTIC PROPERTIES; SILICON; GERMANIUM; ALLOY; NANOCOMPOSITES;
INDENTATION; TRANSITION; HARDNESS; STEEL; FILMS
AB Thermoelectric (TE) materials such as silicon germanium (SiGe) alloys have been traditionally used in radioisotope thermoelectric generators (RTG) NASA applications. Beyond traditional RTG applications, we are exploring other applications in the energy harvesting arena. There is still a need to increment the TE figure of merit (ZT) of SiGe based TE alloys and we have been working on ways to improve it by incorporating tungsten di-silicide (WSi2) phases into the matrix by directional solidification (DS) process. Considerable efforts have been focused until now in microstructural engineering methods that lead to ZT improvement by microstructure optimization of TE materials. Although critical for the previous mentioned applications, work pertinent to the mechanical integrity of this type of WSi2/SiGe based TE materials is lacking. In this work, we explored for the first time the local mechanical properties and microstructure of WSi2/SixGe1-x multiphase thermoelectric material by nanoindentation, scanning electron microscopy (SEM), focused ion beam (FIB) and transmission electron microscopy (TEM) methods. We report hardness (H), modulus (E) and fracture toughness (k(c)) data for all phases. We obtained average H (and E) values (in GPa) of 12.94 (464.95) for the WSi2 phase, 19.49 (214.52) for the matrix, 14.95 (142.84) for the Si rich phase, and 13.98 (138.56) for the Ge rich phase respectively; while average k(c) values (in MPa m(0.5)) were 1.37 for theWSi(2), 0.52 for the matrix, 0.36 for the Si rich and 0.24 for the Ge rich phases respectively. FIB serial sectioning and cross-sectional TEM analysis is also included which provided insights on the deformation process below the nanoindentation area. Published by Elsevier B.V.
C1 [Sola, F.; Dynys, F. W.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Sola, F (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM francisco.sola-lopez@nasa.gov
FU NASA
FX This work was supported by the NASA Advanced Thermoelectric Project. The
authors would like to acknowledge Dr. R. Rogers for the XRD work and Ms.
J. Buehler for polishing of the samples.
NR 32
TC 2
Z9 3
U1 2
U2 49
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD JUN 5
PY 2015
VL 633
BP 165
EP 169
DI 10.1016/j.jallcom.2015.01.246
PG 5
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA CD2MF
UT WOS:000350911800026
ER
PT J
AU Arkoosh, MR
Van Gaest, AL
Strickland, SA
Hutchinson, GP
Krupkin, AB
Dietrich, JP
AF Arkoosh, Mary R.
Van Gaest, Ahna L.
Strickland, Stacy A.
Hutchinson, Greg P.
Krupkin, Alex B.
Dietrich, Joseph P.
TI Dietary Exposure to Individual Polybrominated Diphenyl Ether Congeners
BDE-47 and BDE-99 Alters Innate Immunity and Disease Susceptibility in
Juvenile Chinook Salmon
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID PERSISTENT ORGANIC POLLUTANTS; TROUT ONCORHYNCHUS-MYKISS; RESPIRATORY
BURST; RAINBOW-TROUT; VIBRIO-ANGUILLARUM; FLAME RETARDANTS;
GENE-EXPRESSION; THYROID-HORMONE; TELEOST FISH; IN-VITRO
AB Polybrominated diphenyl ethers (PBDEs), used as commercial flame-retardants, are bioaccumulating in threatened Pacific salmon. However, little is known of PBDE effects on critical physiological functions required for optimal health and survival. BDE-47 and BDE-99 are the predominant PBDE congeners found in Chinook salmon collected from the Pacific Northwest. In the present study, both innate immunity (phagocytosis and production of superoxide anion) and pathogen challenge were used to evaluate health and survival in groups of juvenile Chinook salmon exposed orally to either BDE-47 or BDE-99 at environmentally relevant concentrations. Head kidney macrophages from Chinook salmon exposed to BDE-99, but not those exposed to BDE-47, were found to have a reduced ability in vitro to engulf foreign particles. However, both congeners increased the in vitro production of superoxide anion in head kidney macrophages. Salmon exposed to either congener had reduced survival during challenge with the pathogenic marine bacteria Listonella anguillarum. The concentration response curves generated for these end points were nonmonotonic and demonstrated a requirement for using multiple environmentally relevant PBDE concentrations for effect studies. Consequently, predicting risk from toxicity reference values traditionally generated with monotonic concentration responses may underestimate PBDE effect on critical physiological functions required for optimal health and survival in salmon.
C1 [Arkoosh, Mary R.; Dietrich, Joseph P.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Van Gaest, Ahna L.; Strickland, Stacy A.; Hutchinson, Greg P.; Krupkin, Alex B.] NOAA, Frank Orth & Associates, Under Contract Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Arkoosh, MR (reprint author), NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 South East OSU Dr, Newport, OR 97365 USA.
EM mary.arkoosh@noaa.gov
FU National Oceanic and Atmospheric Administration; US Environmental
Protection Agency, Region 10, Puget Sound Science and Technical Studies
Assistance Program [EPA-R10-PS-1004, 13-923270-01]
FX Funds for this work were provided by the National Oceanic and
Atmospheric Administration and the US Environmental Protection Agency,
Region 10, Puget Sound Science and Technical Studies Assistance Program
(EPA-R10-PS-1004, federal grant no. 13-923270-01). We thank Gina Ylitalo
and Lyndal Johnson from NOAA's Northwest Fisheries Science Center as
well as Sandra O'Neill from the Washington Department of Fish and
Wildlife for their thoughtful comments on the study and review of the
manuscript. We thank Carla Stehr for the scanning electron microscopy
photo of teleost macrophages engulfing foreign particles used for the
TOC art.
NR 62
TC 5
Z9 5
U1 13
U2 41
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 JUN 2
PY 2015
VL 49
IS 11
BP 6974
EP 6981
DI 10.1021/acs.est.5b01076
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA CJ8UN
UT WOS:000355779100072
PM 25938634
ER
PT J
AU Chapel, J
Stancliffe, D
Bevacqua, T
Winkler, S
Clapp, B
Rood, T
Gaylor, D
Freesland, D
Krimchansky, A
AF Chapel, Jim
Stancliffe, Devin
Bevacqua, Tim
Winkler, Stephen
Clapp, Brian
Rood, Tim
Gaylor, David
Freesland, Doug
Krimchansky, Alexander
TI Guidance, navigation, and control performance for the GOES-R spacecraft
SO CEAS SPACE JOURNAL
LA English
DT Article
DE Spacecraft attitude control; Spacecraft pointing; Spacecraft jitter; GPS
at GEO
ID ATTITUDE
AB The Geostationary Operational Environmental Satellite-R series (GOES-R) is the first of the next generation geostationary weather satellites. The series represents a dramatic increase in Earth observation capabilities, with 4 times the resolution, 5 times the observation rate, and 3 times the number of spectral bands. GOES-R also provides unprecedented availability, with less than 120 min per year of lost observation time. This paper presents the guidance navigation & control (GN&C) requirements necessary to realize the ambitious pointing, knowledge, and image navigation and registration (INR) objectives of GOES-. Because the suite of instruments is sensitive to disturbances over a broad spectral range, a high-fidelity simulation of the vehicle has been created with modal content over 500 Hz to assess the pointing stability requirements. Simulation results are presented showing acceleration, shock response spectra, and line-of-sight (LOS) responses for various disturbances from 0 to 512 Hz. Simulation results demonstrate excellent performance relative to the pointing and pointing stability requirements, with LOS jitter for the isolated instrument platform of approximately 1 micro-rad. Attitude and attitude rate knowledge are provided directly to the instrument with an accuracy defined by the integrated rate error requirements. The data are used internally for motion compensation. The final piece of the INR performance is orbit knowledge, which GOES- achieves with GPS navigation. Performance results are shown demonstrating compliance with the 50-75 m orbit position accuracy requirements. As presented in this paper, the GN&C performance supports the challenging mission objectives of GOES-R.
C1 [Chapel, Jim; Stancliffe, Devin; Bevacqua, Tim; Winkler, Stephen; Clapp, Brian] Lockheed Martin Space Syst, Denver, CO USA.
[Rood, Tim] Adv Solut Inc, Littleton, CO USA.
[Gaylor, David] Emergent Space Technol, Greenbelt, MD USA.
[Freesland, Doug] ACS Engn, Columbia, MD USA.
[Krimchansky, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Chapel, J (reprint author), Lockheed Martin Space Syst, Denver, CO USA.
EM jim.d.chapel@lmco.com
NR 18
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Z9 5
U1 0
U2 0
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 1868-2502
EI 1868-2510
J9 CEAS Space J
JI CEAS Space J.
PD JUN
PY 2015
VL 7
IS 2
SI SI
BP 87
EP 104
DI 10.1007/s12567-015-0077-1
PG 18
WC Engineering, Aerospace
SC Engineering
GA DG9YI
UT WOS:000372439300003
ER
PT J
AU San Martin, M
Mendeck, GF
Brugarolas, PB
Singh, G
Serricchio, F
Lee, SW
Wong, EC
Essmiller, JC
AF San Martin, Miguel
Mendeck, Gavin F.
Brugarolas, Paul B.
Singh, Gurkirpal
Serricchio, Frederick
Lee, Steven W.
Wong, Edward C.
Essmiller, John C.
TI In-flight experience of the Mars Science Laboratory Guidance,
Navigation, and Control system for Entry, Descent, and Landing
SO CEAS SPACE JOURNAL
LA English
DT Article
DE EDL; GN&C; Mars; NASA; MSL; Curiosity
AB The Mars Science Laboratory (MSL) project successfully landed the rover Curiosity in Gale crater in August 5, 2012, thus demonstrating and validating a series of technical innovations and advances which resulted in a quantum leap in Entry, Descent, and Landing (EDL) performance relative to previous missions. These included the first use at Mars of Entry Guidance to reduce the size of the landing ellipse and the first use of the SkyCrane landing architecture to enable the placement of a 1 ton class rover on the surface of the red planet. Both of these advances required innovations in the design, analysis and testing of the Guidance, Navigation, and Control system. This paper will start with a high-level description of the MSL EDL/GN&C system design and performance requirements, followed by a brief discussion of the risks and uncertainties as they were understood prior to landing, and the actual in-flight GN&C performance as reconstructed from telemetry. Finally, this paper will address areas of improvements for future Mars EDL missions.
C1 [San Martin, Miguel; Brugarolas, Paul B.; Singh, Gurkirpal; Serricchio, Frederick; Lee, Steven W.; Wong, Edward C.; Essmiller, John C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mendeck, Gavin F.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP San Martin, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alejandro.m.sanmartin@jpl.nasa.gov
OI San Martin, Alejandro/0000-0001-6883-3568
NR 17
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 1868-2502
EI 1868-2510
J9 CEAS Space J
JI CEAS Space J.
PD JUN
PY 2015
VL 7
IS 2
SI SI
BP 119
EP 142
DI 10.1007/s12567-015-0091-3
PG 24
WC Engineering, Aerospace
SC Engineering
GA DG9YI
UT WOS:000372439300005
ER
PT J
AU SunSpiral, V
Trimmer, B
AF SunSpiral, Vytas
Trimmer, Barry
TI An Interview with NASA Principal Investigator Vytas SunSpiral: Expert
Opinion on the Advantages and Limitations of Soft Robotics
SO SOFT ROBOTICS
LA English
DT Editorial Material
AB Vytas SunSpiral is an entrepreneurial researcher moving fluidly between leading startups and building research labs to explore cutting edge robotic technologies. During the last 20 years, he has been the founder and CTO of multiple startups and launched a number of robotics projects at NASA. He has served as an advisor and consultant to startups, and he is currently the Principle Investigator of the Dynamic Tensegrity Robotics Lab (DTRL) at NASA Ames Research Center and is a Fellow of the NASA Innovative Advanced Concepts (NIAC) program. Vytas graduated from Stanford University (1998) with a BA in Symbolic Systems and an MS in Computer Science, with a robotics focus in both.
C1 [SunSpiral, Vytas] NASA, Moffett Field, CA USA.
[SunSpiral, Vytas] NASA Innovat Adv Concepts NIAC Program, Moffett Field, CA USA.
RP SunSpiral, V (reprint author), NASA Ames Res Ctr, Intelligent Syst Div, Intelligent Robot Grp, Dynam Tensegr Robot Lab, Moffett Field, CA 94035 USA.
EM vytas.sunspiral@nasa.gov
NR 0
TC 0
Z9 0
U1 3
U2 5
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 2169-5172
EI 2169-5180
J9 SOFT ROBOT
JI Soft Robot.
PD JUN
PY 2015
VL 2
IS 2
BP 51
EP 58
DI 10.1089/soro.2015.28999.btr
PG 8
WC Robotics
SC Robotics
GA CV8XG
UT WOS:000364571000002
ER
PT J
AU Loeffler, MJ
Hudson, RL
AF Loeffler, Mark J.
Hudson, Reggie L.
TI Descent without Modification? The Thermal Chemistry of H2O2 on Europa
and Other Icy Worlds
SO ASTROBIOLOGY
LA English
DT Article
ID WATER-ICE; HYDROGEN-PEROXIDE; CHEMICAL-COMPOSITION; INFRARED SPECTRUM;
CRYSTALLINE WATER; SUBSURFACE OCEAN; SULFURIC-ACID; GAS-PHASE; SURFACE;
SATELLITES
AB The strong oxidant H2O2 is known to exist in solid form on Europa and is suspected to exist on several other Solar System worlds at temperatures below 200 K. However, little is known of the thermal chemistry that H2O2 might induce under these conditions. Here, we report new laboratory results on the reactivity of solid H2O2 with eight different compounds in H2O-rich ices. Using infrared spectroscopy, we monitored compositional changes in ice mixtures during warming. The compounds CH4 (methane), C3H4 (propyne), CH3OH (methanol), and CH3CN (acetonitrile) were unaltered by the presence of H2O2 in ices, showing that exposure to either solid H(2)O(2)or frozen H2O+H2O2 at cryogenic temperatures will not oxidize these organics, much less convert them to CO2. This contrasts strongly with the much greater reactivity of organics with H2O2 at higher temperatures, and particularly in the liquid and gas phases. Of the four inorganic compounds studied, CO, H2S, NH3, and SO2, only the last two reacted in ices containing H2O2, NH3 making NH4+ and SO2 making SO42- by H+ and e(-) transfer, respectively. An important astrobiological conclusion is that formation of surface H2O2 on Europa and that molecule's downward movement with H2O-ice do not necessarily mean that all organics encountered in icy subsurface regions will be destroyed by H2O2 oxidation. Key Words: Europa-Laboratory investigations-Icy moons-Infrared spectroscopy-H2O2 resistance.
C1 [Loeffler, Mark J.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Hudson, RL (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
EM reggie.hudson@nasa.gov
RI Loeffler, Mark/C-9477-2012
FU NASA's Planetary Geology and Geophysics and Outer Planets Research
programs; NASA Astrobiology Institute
FX The support of NASA's Planetary Geology and Geophysics and Outer Planets
Research programs is gratefully acknowledged. The authors particularly
acknowledge support from the NASA Astrobiology Institute through a grant
to the Goddard Center for Astrobiology. Perry Gerakines is thanked for
assistance in day-to-day operations of the equipment in our laboratory.
NR 56
TC 0
Z9 0
U1 5
U2 14
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 JUN 1
PY 2015
VL 15
IS 6
BP 453
EP 461
DI 10.1089/ast.2014.1195
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CV0MM
UT WOS:000363944800005
PM 26060983
ER
PT J
AU Schuerger, AC
Lee, P
AF Schuerger, Andrew C.
Lee, Pascal
TI Microbial Ecology of a Crewed Rover Traverse in the Arctic: Low
Microbial Dispersal and Implications for Planetary Protection on Human
Mars Missions
SO ASTROBIOLOGY
LA English
DT Article
ID ANTARCTIC RESEARCH STATION; SCIENCE ANALYSIS GROUP; SPACECRAFT SURFACES;
BACILLUS-SUBTILIS; UV-IRRADIATION; SURVIVAL; CONTAMINATION;
MICROORGANISMS; REGIONS; ENVIRONMENTS
AB Between April 2009 and July 2011, the NASA Haughton-Mars Project (HMP) led the Northwest Passage Drive Expedition (NWPDX), a multi-staged long-distance crewed rover traverse along the Northwest Passage in the Arctic. In April 2009, the HMP Okarian rover was driven 496km over sea ice along the Northwest Passage, from Kugluktuk to Cambridge Bay, Nunavut, Canada. During the traverse, crew members collected samples from within the rover and from undisturbed snow-covered surfaces around the rover at three locations. The rover samples and snow samples were stored at subzero conditions (-20 degrees C to -1 degrees C) until processed for microbial diversity in labs at the NASA Kennedy Space Center, Florida. The objective was to determine the extent of microbial dispersal away from the rover and onto undisturbed snow. Interior surfaces of the rover were found to be associated with a wide range of bacteria (69 unique taxa) and fungi (16 unique taxa). In contrast, snow samples from the upwind, downwind, uptrack, and downtrack sample sites exterior to the rover were negative for both bacteria and fungi except for two colony-forming units (cfus) recovered from one downwind (1 cfu; site A4) and one uptrack (1 cfu; site B6) sample location. The fungus, Aspergillus fumigatus (GenBank JX517279), and closely related bacteria in the genus Brevibacillus were recovered from both snow (B. agri, GenBank JX517278) and interior rover surfaces. However, it is unknown whether the microorganisms were deposited onto snow surfaces at the time of sample collection (i.e., from the clothing or skin of the human operator) or via airborne dispersal from the rover during the 12-18h layovers at the sites prior to collection. Results support the conclusion that a crewed rover traveling over previously undisturbed terrain may not significantly contaminate the local terrain via airborne dispersal of propagules from the vehicle. Key Words: Planetary protectionContaminationHabitabilityHaughton CraterMars. Astrobiology 15, xxx-xxx.
C1 [Schuerger, Andrew C.] Univ Florida, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
[Lee, Pascal] Mars Inst, Moffett Field, CA USA.
[Lee, Pascal] SETI Inst, Moffett Field, CA USA.
[Lee, Pascal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Schuerger, AC (reprint author), Univ Florida, Space Life Sci Lab, Bldg M6-1025, Kennedy Space Ctr, FL 32899 USA.
EM schuerg@ufl.edu
FU NASA's Planetary Protection Office [NNX12AJ84G, NNX08AQ81A]; NASA's
Human Exploration and Operations Mission Directorate (HEOMD)
[NNX08AO59A]; Mars Institute; SETI Institute; National Aeronautics and
Space Administration (NASA); California Air National Guard; AM General
Corporation; Cornell University; Simon Fraser University; University of
Alberta; National Space Biomedical Research Institute; Canadian Space
Agency; Bombardier, Inc.; First Air, Inc.; Hamilton Sundstrand
Corporation; Nunavut Research Institute; Aboriginal Affairs and Northern
Development Canada; Polar Continental Shelf Project of Natural Resources
Canada; Nunavut community of Kugluktuk; Nunavut community of Cambridge
Bay; Nunavut community of Gjoa Haven; Nunavut community of Resolute Bay;
Nunavut community of Grise Fiord
FX The research was supported by two research grants (NNX12AJ84G and
NNX08AQ81A) from NASA's Planetary Protection Office and through a
Cooperative Agreement (NNX08AO59A) by NASA's Human Exploration and
Operations Mission Directorate (HEOMD). The NASA Haughton-Mars Project
and the Northwest Passage Drive Expedition (NWPDX) were sponsored by the
Mars Institute, the SETI Institute, and the National Aeronautics and
Space Administration (NASA). We would like to thank W.L. Nicholson for
his suggestions on 16S and 18S sequencing protocols and the loan of
specialized equipment for a portion of the lab work described herein.
Thanks are also owed to the many other sponsors and supporters of the
NWPDX expedition including the California Air National Guard; AM General
Corporation; Cornell University; Simon Fraser University; University of
Alberta; the National Space Biomedical Research Institute; the Canadian
Space Agency, Bombardier, Inc.; First Air, Inc.; Hamilton Sundstrand
Corporation; the Nunavut Research Institute; Aboriginal Affairs and
Northern Development Canada; the Polar Continental Shelf Project of
Natural Resources Canada; and the Nunavut communities of Kugluktuk,
Cambridge Bay, Gjoa Haven, Resolute Bay, and Grise Fiord. Pascal Lee
expresses special thanks to NWPDX-2009 field team members John W.
Schutt, Joe Amarualik, Jesse T. Weaver, and Mark Carroll for the
excellent support and enthusiasm during the NWPDX-2009 traverse. Kira
Lorber and Stephen Braham are thanked for logistics and communications
support, respectively.
NR 49
TC 3
Z9 3
U1 3
U2 17
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 JUN 1
PY 2015
VL 15
IS 6
BP 478
EP 491
DI 10.1089/ast.2015.1289
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CV0MM
UT WOS:000363944800007
PM 26060984
ER
PT J
AU Alwood, JS
Shahnazari, M
Chicana, B
Schreurs, AS
Kumar, A
Bartolini, A
Shirazi-Fard, Y
Globus, RK
AF Alwood, Joshua S.
Shahnazari, Mohammad
Chicana, Betsabel
Schreurs, A. S.
Kumar, Akhilesh
Bartolini, Alana
Shirazi-Fard, Yasaman
Globus, Ruth K.
TI Ionizing Radiation Stimulates Expression of Pro-Osteoclastogenic Genes
in Marrow and Skeletal Tissue
SO JOURNAL OF INTERFERON AND CYTOKINE RESEARCH
LA English
DT Article
ID LONG-DURATION SPACEFLIGHT; KAPPA-B LIGAND; BONE-RESORPTION;
MUSCULOSKELETAL DISUSE; RECEPTOR ACTIVATOR; OXIDATIVE STRESS; CANCELLOUS
BONE; MURINE MODEL; T-CELLS; DIFFERENTIATION
AB Exposure to ionizing radiation can cause rapid mineral loss and increase bone-resorbing osteoclasts within metabolically active, cancellous bone tissue leading to structural deficits. To better understand mechanisms involved in rapid, radiation-induced bone loss, we determined the influence of total body irradiation on expression of select cytokines known both to stimulate osteoclastogenesis and contribute to inflammatory bone disease. Adult (16 week), male C57BL/6J mice were exposed to either 2Gy gamma rays (Cs-137, 0.8Gy/min) or heavy ions (Fe-56, 600MeV, 0.50-1.1Gy/min); this dose corresponds to either a single fraction of radiotherapy (typical total dose is 10Gy) or accumulates over long-duration interplanetary missions. Serum, marrow, and mineralized tissue were harvested 4h7 days later. Gamma irradiation caused a prompt (2.6-fold within 4h) and persistent (peaking at 4.1-fold within 1 day) rise in the expression of the obligate osteoclastogenic cytokine, receptor activator of nuclear factor kappa-B ligand (Rankl), within marrow cells over controls. Similarly, Rankl expression peaked in marrow cells within 3 days of iron exposure (9.2-fold). Changes in Rankl expression induced by gamma irradiation preceded and overlapped with a rise in expression of other pro-osteoclastic cytokines in marrow (eg, monocyte chemotactic protein-1 increased by 11.9-fold, and tumor necrosis factor-alpha increased by 1.7-fold over controls). The ratio, Rankl/Opg, in marrow increased by 1.8-fold, a net pro-resorption balance. In the marrow, expression of the antioxidant transcription factor, Nfe2l2, strongly correlated with expression levels of Nfatc1, Csf1, Tnf, and Rankl. Radiation exposure increased a serum marker of bone resorption (tartrate-resistant acid phosphatase) and led to cancellous bone loss (16% decrement after 1 week). We conclude that total body irradiation (gamma or heavy-ion) caused temporal elevations in the concentrations of specific genes expressed within marrow and mineralized tissue related to bone resorption, including select cytokines that lead to osteoclastogenesis and elevated resorption; this is likely to account for rapid and progressive deterioration of cancellous microarchitecture following exposure to ionizing radiation.
C1 [Alwood, Joshua S.; Shahnazari, Mohammad; Chicana, Betsabel; Schreurs, A. S.; Kumar, Akhilesh; Bartolini, Alana; Shirazi-Fard, Yasaman; Globus, Ruth K.] NASA, Ames Res Ctr, Bone & Signaling Lab, Space Biosci Div, Moffett Field, CA 94035 USA.
RP Globus, RK (reprint author), NASA, Ames Res Ctr, Bone & Signaling Lab, Space Biosci Div, Mail Stop 236-7, Moffett Field, CA 94035 USA.
EM ruth.k.globus@nasa.gov
FU National Space Biomedical Research Institute under NASA [MA02501, NCC
9-58]; DOE-NASA - Office of Science (Biological and Environmental
Research), U.S. Department of Energy [DE-SC0001507]; 2 NASA Postdoctoral
Program fellowships from NASA's Space Biology Program
FX This research was supported by the National Space Biomedical Research
Institute grant No. MA02501 under NASA cooperative agreement NCC 9-58
(R.K.G., J.S.A.), a DOE-NASA Interagency Award No. DE-SC0001507,
supported by the Office of Science (Biological and Environmental
Research), U.S. Department of Energy (R.K.G.), and 2 NASA Postdoctoral
Program fellowships from NASA's Space Biology Program (J.S.A., A.K). The
authors thank P. Guida, A. Rusek, L. Loudenslager, and A. Kim of the
NASA Space Radiation Laboratory at BNL for experimental support and S.
Choi and T. Truong for microcomputed tomography support and C. Tahimic
for manuscript review.
NR 46
TC 1
Z9 1
U1 4
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 JUN 1
PY 2015
VL 35
IS 6
BP 480
EP 487
DI 10.1089/jir.2014.0152
PG 8
WC Biochemistry & Molecular Biology; Cell Biology; Immunology
SC Biochemistry & Molecular Biology; Cell Biology; Immunology
GA CU9RR
UT WOS:000363883100008
PM 25734366
ER
PT J
AU Price, H
Baker, J
Naderi, F
AF Price, Hoppy
Baker, John
Naderi, Firouz
TI A Minimal Architecture for Human Journeys to Mars
SO NEW SPACE
LA English
DT Article
AB Proposed architectures for human journeys to Mars need to take note of the two competing constraints of an executable program: the annual NASA human spaceflight budget will likely remain constrained (possibly growing with inflation), and going to Mars and landing on Mars need to happen within the interest horizon of the various stakeholders, including the public. In this article we describe a stepwise approach for human journeys to Mars using a minimal architecture. We refer to this architecture as minimal because it would minimize large new development efforts and rely largely on elements currently being developed or planned by NASA, such as SLS, Orion, a deep space habitat, and a 100-kWe-class SEP tug. In the architecture proposed here, human missions to Mars would begin with a crewed landing on Phobos in 2033, followed by a short-stay landing on Mars in 2039, and continue with a one-year stay in 2043. Each mission campaign would build on previous campaigns, leaving a legacy and new capabilities for those that follow. A first look independent cost assessment by the Aerospace Corporation suggests that this example could plausibly fit within an inflation-adjusted budget. Furthermore, although not considered here, international contributions could offset some of the cost.
C1 [Price, Hoppy; Baker, John; Naderi, Firouz] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Price, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-170S, Pasadena, CA 91109 USA.
EM Humphrey.W.Price@jpl.nasa.gov
NR 2
TC 3
Z9 3
U1 2
U2 6
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 2168-0256
EI 2168-0264
J9 NEW SPACE
JI New Space
PD JUN 1
PY 2015
VL 3
IS 2
BP 73
EP 81
DI 10.1089/space.2015.0018
PG 9
WC Engineering, Aerospace
SC Engineering
GA CV0ID
UT WOS:000363933100002
ER
PT J
AU Lee, JH
Lin, KC
Eklund, D
AF Lee, Jinho
Lin, Kuo-Cheng
Eklund, Dean
TI Challenges in Fuel Injection for High-Speed Propulsion Systems
SO AIAA JOURNAL
LA English
DT Article
ID SUPERSONIC CROSS-FLOWS; INDUCED IODINE FLUORESCENCE; LARGE-EDDY
SIMULATION; LIQUID JETS; TRANSVERSE INJECTION; AEROSPACE PROPULSION;
TURBULENT PRANDTL; SCRAMJET ENGINES; SCHMIDT NUMBERS; PRIMARY BREAKUP
C1 [Lee, Jinho] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lin, Kuo-Cheng] Taitech Inc, Beavercreek, OH 45430 USA.
[Eklund, Dean] US Air Force, Res Lab, Wright Patterson AFB, OH 45433 USA.
RP Lee, JH (reprint author), NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
FU Hypersonic Propulsion Element of Fundamental Hypersonic Program; U.S.
Air Force Research Laboratory's Robust Scramjet Program
FX This work was sponsored by the Hypersonic Propulsion Element of the
Fundamental Hypersonic Program under the leadership of A. Auslander and
R. Gaffney (Associate Principal Investigators) and J. Pittman (Principal
Investigator). The sponsorship of T. Jackson and R. Mercier under the
auspices of the U.S. Air Force Research Laboratory's Robust Scramjet
Program is also gratefully acknowledged.
NR 121
TC 0
Z9 0
U1 2
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JUN
PY 2015
VL 53
IS 6
BP 1405
EP 1423
DI 10.2514/1.J053280
PG 19
WC Engineering, Aerospace
SC Engineering
GA CH9WD
UT WOS:000354386200001
ER
PT J
AU Jones, MG
Watson, WR
Howerton, BM
Busse-Gerstengarbe, S
AF Jones, M. G.
Watson, W. R.
Howerton, B. M.
Busse-Gerstengarbe, S.
TI Effects of Mean Flow Assumption and Harmonic Distortion on Impedance
Eduction Methods
SO AIAA JOURNAL
LA English
DT Article
ID GRAZING FLOW; BOUNDARY-CONDITION; LINER IMPEDANCE; VALIDATION; DUCT
AB This investigation uses methods based on the Pridmore-Brown and convected Helmholtz equations to study the acoustic behavior of a single-layer, conventional liner fabricated by DLR, German Aerospace Center and tested in the NASA Langley Grazing Flow Impedance Tube. Two key assumptions are explored in this investigation. First, a comparison of results achieved with uniform-flow and shear-flow impedance eduction methods is considered. Second, an approach based on the Prony method is used to extend these methods from single-mode to multimode implementations. In addition, a detailed study into the effects of harmonic distortion on the educed impedance is performed, and the results are used to develop guidelines regarding acceptable levels of harmonic distortion.
C1 [Jones, M. G.; Howerton, B. M.] NASA, Langley Res Ctr, Struct Acoust Branch, Res Directorate, Hampton, VA 23681 USA.
[Watson, W. R.] NASA, Langley Res Ctr, Computat AeroSci Branch, Res Directorate, Hampton, VA 23681 USA.
[Busse-Gerstengarbe, S.] Tech Univ Berlin, Inst Fluid Mech & Engn Acoust, D-10623 Berlin, Germany.
RP Jones, MG (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Res Directorate, Hampton, VA 23681 USA.
FU NASA; German Research Foundation [TH 288/35-1]
FX The authors wish to express their appreciation to Carl Gerhold and Chris
Jasinski for their support in the implementation of the multimode
impedance eduction method and to Jason June for his support with
implementation of the shear-flow assumption. This research was funded by
the Fixed Wing Project of NASA's Fundamental Aeronautics Program.
Support for S. Busse-Gerstengarbe was provided by the German Research
Foundation as part of the UNLIMITED Project (TH 288/35-1).
NR 20
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 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JUN
PY 2015
VL 53
IS 6
BP 1503
EP 1514
DI 10.2514/1.J053399
PG 12
WC Engineering, Aerospace
SC Engineering
GA CH9WD
UT WOS:000354386200009
ER
PT J
AU Mankbadi, MR
Georgiadis, NJ
AF Mankbadi, M. R.
Georgiadis, N. J.
TI Examination of Parameters Affecting Large-Eddy Simulations of Flow Past
a Square Cylinder
SO AIAA JOURNAL
LA English
DT Article
C1 [Mankbadi, M. R.; Georgiadis, N. J.] NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, Cleveland, OH 44135 USA.
RP Mankbadi, MR (reprint author), NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
FU Rotary Wing Project; Aeronautical Sciences Project under the Fundamental
Aeronautics Program
FX This work was supported by the Rotary Wing Project and the Aeronautical
Sciences Project under the Fundamental Aeronautics Program. Special
thanks to J. R. DeBonis, D. A. Yoder, and G. E. Welch for their advice.
NR 7
TC 2
Z9 2
U1 1
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JUN
PY 2015
VL 53
IS 6
BP 1706
EP 1711
DI 10.2514/1.J053684
PG 6
WC Engineering, Aerospace
SC Engineering
GA CH9WD
UT WOS:000354386200024
ER
PT J
AU Bouhenni, R
Dunmire, J
Liu, Y
Rafiq, Q
Gothard, D
King, J
Naiman, M
Ansari, R
Edward, DP
AF Bouhenni, Rachida
Dunmire, Jeffrey
Liu, Ying
Rafiq, Qundeel
Gothard, David
King, James
Naiman, Melissa
Ansari, Rafat
Edward, Deepak P.
TI Identification of Molecular Signatures in Vitreous Humor Following Laser
Exposure using Dynamic Light Scattering
SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE
LA English
DT Meeting Abstract
CT Annual Meeting of the
Association-for-Research-in-Vision-and-Ophthalmology (ARVO)
CY MAY 03-07, 2015
CL Denver, CO
SP Assoc Res Vis & Ophthalmol
C1 [Bouhenni, Rachida; Dunmire, Jeffrey] Summa Hlth Syst, Ophthalmol, Akron, OH USA.
[Liu, Ying; Rafiq, Qundeel; Edward, Deepak P.] Johns Hopkins Univ, Baltimore, MD USA.
[Gothard, David] BIOSTATS, Akron, OH USA.
[King, James; Ansari, Rafat] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Naiman, Melissa] Univ Illinois, Chicago, IL USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC
PI ROCKVILLE
PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA
SN 0146-0404
EI 1552-5783
J9 INVEST OPHTH VIS SCI
JI Invest. Ophthalmol. Vis. Sci.
PD JUN
PY 2015
VL 56
IS 7
MA 4630
PG 3
WC Ophthalmology
SC Ophthalmology
GA CT5ZY
UT WOS:000362891103411
ER
PT J
AU Ethier, CR
Feola, A
Raykin, J
Mulugeta, L
Gleason, R
Myers, JG
Nelson, ES
Samuels, B
AF Ethier, C. Ross
Feola, Andrew
Raykin, Julia
Mulugeta, Lealem
Gleason, Rudy
Myers, Jerry G.
Nelson, Emily S.
Samuels, Brian
TI Modeling the Effects of Spaceflight on the Posterior Eye in VIIP
SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE
LA English
DT Meeting Abstract
CT Annual Meeting of the
Association-for-Research-in-Vision-and-Ophthalmology (ARVO)
CY MAY 03-07, 2015
CL Denver, CO
SP Assoc Res Vis & Ophthalmol
C1 [Ethier, C. Ross; Feola, Andrew; Raykin, Julia; Gleason, Rudy] Georgia Inst Technol, Biomed Engn, Atlanta, GA 30332 USA.
[Mulugeta, Lealem] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Myers, Jerry G.; Nelson, Emily S.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Samuels, Brian] Univ Alabama Birmingham, Ophthalmol, Birmingham, AL USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC
PI ROCKVILLE
PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA
SN 0146-0404
EI 1552-5783
J9 INVEST OPHTH VIS SCI
JI Invest. Ophthalmol. Vis. Sci.
PD JUN
PY 2015
VL 56
IS 7
MA 4825
PG 3
WC Ophthalmology
SC Ophthalmology
GA CT5ZY
UT WOS:000362891104183
ER
PT J
AU Parsons-Wingerter, PA
Radhakrishnan, K
Chalam, KV
Grant, MB
AF Parsons-Wingerter, Patricia A.
Radhakrishnan, Krishnan
Chalam, K. V.
Grant, Maria B.
TI VESGEN Analysis of Generational Branching Patterns in Arteries and Veins
for Investigating Diabetic Retinopathy by Spectralis Angiographic
Imaging
SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE
LA English
DT Meeting Abstract
CT Annual Meeting of the
Association-for-Research-in-Vision-and-Ophthalmology (ARVO)
CY MAY 03-07, 2015
CL Denver, CO
SP Assoc Res Vis & Ophthalmol
C1 [Parsons-Wingerter, Patricia A.] NASA, Ames Res Ctr, Space Biosci Res Branch, Moffett Field, CA 94035 USA.
[Radhakrishnan, Krishnan] Univ Kentucky, Internal Med, Lexington, KY USA.
[Chalam, K. V.] Univ Florida, Ophthalmol, Jacksonville, FL USA.
[Grant, Maria B.] Indiana Univ, Glick Eye Inst, Ophthalmol, Indianapolis, IN 46204 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC
PI ROCKVILLE
PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA
SN 0146-0404
EI 1552-5783
J9 INVEST OPHTH VIS SCI
JI Invest. Ophthalmol. Vis. Sci.
PD JUN
PY 2015
VL 56
IS 7
MA 5960
PG 2
WC Ophthalmology
SC Ophthalmology
GA CT5ZY
UT WOS:000362891107029
ER
PT J
AU Youngquist, RC
Nurge, MA
Johnson, WL
Starr, SO
AF Youngquist, Robert C.
Nurge, Mark A.
Johnson, Wesley L.
Starr, Stanley O.
TI Modeling Transmission Effects on Multilayer Insulation
SO JOURNAL OF THERMAL SCIENCE AND ENGINEERING APPLICATIONS
LA English
DT Article
ID REFLECTANCE; ALUMINUM
AB Multilayer insulation (MLI), commonly used in cryogenics, is typically composed of many layers of thin polymer sheets each coated with a thin film of highly reflective metal. The primary purpose of this insulation is to block radiative energy transfer. However, at very low temperatures where blackbody radiation occurs at long wavelengths, some energy may be transmitted through these layers, degrading the performance of the insulation. Traditional modeling techniques assume that the films are opaque and are not easily extended to include radiative transmission through the layers. In order to model the effect of wavelength dependent transmission on the thermal performance of MLI, an L1-norm energy vector is defined and combined with a square energy distribution matrix. The key here is that the energy distribution matrix describes one time step of the radiation-one set of reflections, transmissions, and absorptions-and since this matrix is square, it can be easily raised to a large power, describing the final state of the system quickly. This approach removes the need to track every reflected and transmitted radiation element, but instead determines the eventual location where the thermal radiation energy is deposited. This method can be generalized to model dependence of the reflection and transmission of the radiation on wavelength or angle of propagation, to include thermal conduction effects, and to model transient behavior. The results of this work predict the degree of transmission dependent degradation expected to be seen when using state-of-the-art MLI in low temperature cryogenic systems.
C1 [Youngquist, Robert C.; Nurge, Mark A.; Starr, Stanley O.] NASA, KSC Appl Phys Lab NE L5, Kennedy Space Ctr, FL 32899 USA.
[Johnson, Wesley L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Nurge, MA (reprint author), NASA, KSC Appl Phys Lab NE L5, Kennedy Space Ctr, FL 32899 USA.
EM robert.c.youngquist@nasa.gov; mark.a.nurge@nasa.gov;
wesley.l.johnson@nasa.gov; stanley.o.starr@nasa.gov
FU NASA's Advanced Exploration Systems Program
FX This work was funded by NASA's Advanced Exploration Systems Program.
NR 13
TC 2
Z9 2
U1 3
U2 5
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1948-5085
EI 1948-5093
J9 J THERM SCI ENG APPL
JI J. Therm. Sci. Eng. Appl.
PD JUN
PY 2015
VL 7
IS 2
AR 021007
DI 10.1115/1.4028570
PG 7
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA CU2WP
UT WOS:000363384700007
ER
PT J
AU Zhu, YQ
Toon, OB
Lambert, A
Kinnison, DE
Brakebusch, M
Bardeen, CG
Mills, MJ
English, JM
AF Zhu, Yunqian
Toon, Owen B.
Lambert, Alyn
Kinnison, Douglas E.
Brakebusch, Matthias
Bardeen, Charles G.
Mills, Michael J.
English, Jason M.
TI Development of a Polar Stratospheric Cloud Model within the Community
Earth System Model using constraints on Type I PSCs from the 2010-2011
Arctic winter
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
ID NITRIC-ACID TRIHYDRATE; LARGE HNO3-CONTAINING PARTICLES;
CHEMICAL-TRANSPORT MODEL; OZONE LOSS; ATMOSPHERIC CHEMISTRY;
H2SO4/HNO3/H2O SOLUTIONS; HETEROGENEOUS REACTIONS; TOMOGRAPHIC APPROACH;
CHLORINE ACTIVATION; PHYSICAL PROCESSES
AB Polar stratospheric clouds (PSCs) are critical elements of Arctic and Antarctic ozone depletion. We establish a PSC microphysics model using coupled chemistry, climate, and microphysics models driven by specific dynamics. We explore the microphysical formation and evolution of STS (Supercooled Ternary Solution) and NAT (Nitric Acid Trihydrate). Characteristics of STS particles dominated by thermodynamics compare well with observations. For example, the mass of STS is close to the thermodynamic equilibrium assumption when the particle surface area is >4 mu m(2)/cm(3). We derive a new nucleation rate equation for NAT based on observed denitrification in the 2010-2011 Arctic winter. The homogeneous nucleation scheme leads to supermicron NAT particles as observed. We also find that as the number density of NAT particles increases, the denitrification also increases. Simulations of the PSC lidar backscatter, denitrification, and gas phase species are generally within error bars of the observations. However, the simulations are very sensitive to temperature, which limits our ability to fully constrain some parameters (e.g., denitrification, ozone amount) based on observations.
C1 [Zhu, Yunqian; Toon, Owen B.; Brakebusch, Matthias; English, Jason M.] Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kinnison, Douglas E.; Bardeen, Charles G.; Mills, Michael J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Zhu, YQ (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
EM yunqian.zhu@colorado.edu
RI Mills, Michael/B-5068-2010; English, Jason/E-9365-2015
OI Mills, Michael/0000-0002-8054-1346; English, Jason/0000-0001-9700-6860
FU NASA [NNX09AK71G]; AURA satellite project; National Science Foundation;
National Science Foundation [CNS-0821794]; University of Colorado
Boulder
FX MIPAS data are from the MIPAS2D database (www.isac.cnr.it/similar to
rss/mipas2d.htm). We thank E. Arnone for his help with the MIPAS data.
Data are provided courtesy of the National Centre for Earth Observation
via the NERC Earth Observation Data Centre (NEODC). The work at the
University of Colorado was supported by NASA grant NNX09AK71G, as well
as a grant from the AURA satellite project. Work at the Jet Propulsion
Laboratory, California Institute of Technology, was carried out under a
contract with the National Aeronautics and Space Administration. We
thank Lynn Harvey for her help with the MLS data. We thank Michael Pitts
for his help with the CALIPSO PSC cloud coverage retrieval. We thank
Stephan Borrmann and his group for their help with the PSC size data
from the RECONCILE campaign. This work utilized the Yellowstone and
Janus supercomputer. 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. Janus is supported by the National
Science Foundation (award CNS-0821794) and the University of Colorado
Boulder. The Janus supercomputer is a joint effort of the University of
Colorado Boulder, the University of Colorado Denver and the National
Center for Atmospheric Research.
NR 135
TC 3
Z9 3
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD JUN
PY 2015
VL 7
IS 2
BP 551
EP 585
DI 10.1002/2015MS000427
PG 35
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ7ZH
UT WOS:000360825000010
ER
PT J
AU Borghesi, G
Mastorakos, E
AF Borghesi, Giulio
Mastorakos, Epaminondas
TI Spontaneous ignition of isolated n-heptane droplets at low,
intermediate, and high ambient temperatures from a mixture-fraction
perspective
SO COMBUSTION AND FLAME
LA English
DT Article
DE Single droplet; Detailed numerical simulation; Complex chemistry;
Microgravity; Autoignition
ID DETAILED NUMERICAL SIMULATIONS; CONDITIONAL MOMENT CLOSURE; MICROGRAVITY
EXPERIMENTS; SPRAY COMBUSTION; AUTOIGNITION; FLAMES; METHANOL;
EVAPORATION; CHEMISTRY; TRANSPORT
AB Detailed numerical simulations of isolated n-heptane droplets autoignition have been conducted at pressures of 5 and 10 atm for several values of the initial ambient gas temperature. The ignition modes considered included low-, intermediate-, and high-temperature ignition. The analysis was conducted from a mixture-fraction perspective. For sufficiently low values of the ambient gas temperature, two-stage ignition was observed. Under these conditions, low-temperature reactions played an important role in the transition of the system to a fully burning state. As the initial value of the ambient gas temperature increased, the influence of the low-temperature reactions on the ignition process decreased and eventually became marginal for temperatures above 900 K. Comparisons against homogeneous reactor calculations showed that the ignition location in mixture fraction space could be reasonably predicted for the high-temperature case, whereas discrepancies occurred for the intermediate- and low-temperature ones due to the shift in the maximum reactivity of the system caused by the cool flame appearance. The dependence of the ignition process on the initial droplet diameter was also studied for different values of the initial ambient gas temperature. It was found that, for all cases investigated, a value of the droplet diameter existed for which ignition took the least time to occur. For smaller droplets, the ignition transient was longer and eventually a burning flame did no longer appear when the droplet was initially too small. For the low-temperature case, the minimum ignition delay time was determined by the competition between the quicker ignition of the cool flame and the longer second induction time resulting from the decrease in the droplet size: for the high-temperature case, it was the results of phenomena occurring early during the droplet lifetime. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Borghesi, Giulio] CALTECH, Dept Civil & Mech Engn, Pasadena, CA 91125 USA.
[Mastorakos, Epaminondas] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England.
RP Borghesi, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-130, Pasadena, CA 91109 USA.
EM Giulio.Borghesi@jpl.nasa.gov
OI Mastorakos, Epaminondas/0000-0001-8245-5188
NR 46
TC 4
Z9 4
U1 3
U2 21
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD JUN
PY 2015
VL 162
IS 6
BP 2544
EP 2560
DI 10.1016/j.combustflame.2015.03.003
PG 17
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CQ4RP
UT WOS:000360592600021
ER
PT J
AU Shaver, DJ
Caillouet, CW
AF Shaver, Donna J.
Caillouet, Charles W., Jr.
TI REINTRODUCTION OF KEMP'S RIDLEY (LEPIDOCHELYS KEMPII) SEA TURTLE TO
PADRE ISLAND NATIONAL SEASHORE, TEXAS AND ITS CONNECTION TO
HEAD-STARTING
SO HERPETOLOGICAL CONSERVATION AND BIOLOGY
LA English
DT Article
DE conservation; head-start; Lepidochelys kempii; nesting; satellite
tracking
ID GULF-OF-MEXICO; NORTHWESTERN GULF; HEADSTART PROJECT; RANCHO-NUEVO;
CONSERVATION; MANAGEMENT; RECOVERY; MODELS; COAST; WILD
AB Kemp's Ridley (Lepidochelys kempii) is the most endangered of the sea turtles. Most nesting is on the Gulf of Mexico coastline from Texas, USA, through Veracruz, Mexico, with greatest numbers near Playa de Rancho Nuevo (RN), Tamaulipas, Mexico. The Mexican government began protecting nesters, eggs, and hatchlings at RN in 1966, but annual numbers of nests continued to decline. In January 1978, the U.S. National Park Service (NPS), Fish and Wildlife Service (FWS), and National Marine Fisheries Service (NMFS), the Texas Parks and Wildlife Department (TPWD), and the Instituto Nacional de Pesca (INP) of Mexico implemented a bi-national Kemp's Ridley restoration and enhancement program (KRREP) for the NPS Padre Island National Seashore (PAIS) near Corpus Christi, Texas, and RN. Its planned goals were to reintroduce Kemp's Ridley to PAIS, which included head-starting, and to enhance protection of Kemp's Ridley nesters, eggs, and hatchlings at RN. This paper summarizes collecting, transporting, and incubating eggs, attempted imprinting of eggs and hatchlings, transporting hatchlings, tracking nesters, and documenting nestings in the wild. Through 2014, 20 Padre Island imprinted head-started turtles (n = 69 nests) and 39 RN imprinted head-started turtles (n = 64 nests) were recorded nesting in Texas (n = 125 nests) and near RN (n = 8 nests).
C1 [Shaver, Donna J.] Natl Pk Serv, Padre Isl Natl Seashore, Corpus Christi, TX 78480 USA.
[Caillouet, Charles W., Jr.] Natl Marine Fisheries Serv, Galveston Lab, Galveston, TX 77551 USA.
RP Shaver, DJ (reprint author), Natl Pk Serv, Padre Isl Natl Seashore, POB 181300, Corpus Christi, TX 78480 USA.
EM donna_shaver@nps.gov; waxmanjr@aol.com
FU NPS; NMFS; FWS; TPWD; INP; CONANP; SEMARNAT; Animal Rehabilitation Keep
(ARK); City of Corpus Christi; Friends of Aransas and Matagorda Island
National Wildlife Refuges (FAMI); Gladys Porter Zoo, HEART/Sea Turtle
Restoration Project; National Fish and Wildlife Foundation; National
Park Foundation; Natural Resource Damage Assessment (NRDA); Norcross
Wildlife Foundation; Sea Turtle, Inc.; Shell Oil Company Foundation;
Texas General Land Office; TAMUG; Texas Master Naturalists, Unilever
HPC-USA; U.S. Geological Survey; University of Alabama at Birmingham;
University of Charleston; University of Texas
FX Various components of the work were funded and permitted by NPS, NMFS,
FWS, TPWD, and INP (and its successor agencies including CONANP and
SEMARNAT). Bryan Arroyo, Richard Byles, Kelsey Gocke, Mike Ray, Tom
Shearer, Catherine Yeargan, and others aided with FWS and TPWD
permitting and support. Work by PAIS personnel was authorized under FWS
Permit TE840727-3, TPWD Scientific Permit SPR-0190-122, and NPS
Institutional Animal Care Protocols NPS IACUC 2011-15.; Animal
Rehabilitation Keep (ARK), City of Corpus Christi, Friends of Aransas
and Matagorda Island National Wildlife Refuges (FAMI), Gladys Porter
Zoo, HEART/Sea Turtle Restoration Project, National Fish and Wildlife
Foundation, National Park Foundation, Natural Resource Damage Assessment
(NRDA), Norcross Wildlife Foundation, Sea Turtle, Inc., Shell Oil
Company Foundation, Texas General Land Office, TAMUG, Texas Master
Naturalists, Unilever HPC-USA, U.S. Geological Survey, University of
Alabama at Birmingham, University of Charleston, University of Texas,
and others provided assistance or funding for activities in Texas.
NR 188
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U1 2
U2 17
PU HERPETOLOGICAL CONSERVATION & BIOLOGY
PI CORVALLIS
PA C/O R BRUCE BURY, USGS FOREST & RANGELAND, CORVALLIS, OR 00000 USA
SN 2151-0733
EI 1931-7603
J9 HERPETOL CONSERV BIO
JI Herpetol. Conserv. Biol.
PD JUN
PY 2015
VL 10
IS 1
BP 378
EP 435
PG 58
WC Zoology
SC Zoology
GA CQ1QK
UT WOS:000360373100026
ER
PT J
AU Sundaresan, A
Marriott, K
Mao, J
Bhuiyan, S
Denkins, P
AF Sundaresan, A.
Marriott, K.
Mao, J.
Bhuiyan, S.
Denkins, P.
TI The Effects of Benzofuran-2-Carboxylic Acid Derivatives as
Countermeasures in Immune Modulation and Cancer Cell Inhibition
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Immune suppression; Microgravity; Benzofurans; Countermeasures;
Radiation; Apoptosis
ID INDUCED GENOMIC INSTABILITY; IONIZING-RADIATION; ANTITUMOR-ACTIVITY;
MICROGRAVITY; EXPRESSION; ANALOGS; INCREASES
AB Microgravity and radiation exposure experienced during space flights result in immune system suppression. In long-term spaceflight, the crew is exposed to space radiation, microgravity, infectious agents from other crew members, and microbial contamination, all of which have a significant impact on the body's immune system and may contribute to the development of autoimmune diseases, allergic reactions, and/or cancer initiation. Many studies have revealed strong effects of microgravity on immune cell function, and microgravity is now considered as one of the major causes of immune dysfunction during space flight (Sundaresan, Int. J. Transp. Phenom. 12(1-2), 93-100, 2011; Martinelli et al., IEEE Eng. Biol. Med. 28(4), 85-90, 2009). We screened two newly synthetized derivatives of benzofuran 2-carboxylic acid, KMEG and KM12. The former KMEG was assessed for lymphoproliferative activities while the latter, KM12, was used in an array of cancer cell lines for testing its cancer inhibiting effects. For ground-based studies, synthetic benzofuran-2-carboxylic acid derivatives were assessed for biological effects in several scenarios, which involved exposure to modeled microgravity and radiation, as well as their immune enhancement and anti-cancer effects. Initial findings indicate that the benzofuran-2-carboxylic acid derivatives possibly have immune enhancing and anti-tumor properties in human lymphocytes and cancer cells exposed to analog spaceflight conditions modeled microgravity and gamma-radiation).
C1 [Sundaresan, A.] Texas So Univ, Houston, TX 77004 USA.
[Marriott, K.] Savannah State Univ, Savannah, GA 31404 USA.
[Mao, J.] Tougaloo Coll, Jackson, MS 39174 USA.
[Bhuiyan, S.] Jarvis Christian Coll, Hawkins, TX 75765 USA.
[Denkins, P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Sundaresan, A (reprint author), Texas So Univ, Houston, TX 77004 USA.
EM sundaresana@TSU.EDU
NR 32
TC 0
Z9 0
U1 1
U2 7
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 JUN
PY 2015
VL 27
IS 3
BP 129
EP 140
DI 10.1007/s12217-014-9408-7
PG 12
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA CP0FA
UT WOS:000359550000001
ER
PT J
AU DiLisi, G
Dempsey, R
Rarick, R
Rosenblatt, C
AF DiLisi, Gregory
Dempsey, Robert
Rarick, Richard
Rosenblatt, Charles
TI Using Parabolic Flights to Examine Quantitatively the Stability of
Liquid Bridges under Varying Total Body Force
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Bond number; Liquid bridges; Microgravity; Parabolic flights
ID ARBITRARY VOLUME; MINIMUM VOLUME; EQUAL DISKS; GRAVITY; DYNAMICS;
FIELDS; LIMIT; LONG
AB Liquid bridges were flown aboard a Boeing 727-200 aircraft in a series of parabolic arcs that produced multiple periods of microgravity. During the microgravity portion of each arc, g(eff), the effective total body acceleration due to external forces became negligibly small so that cylindrical liquid bridges could be suspended across two coaxial support posts. Near the bottom of each arc, g(eff) slowly increased to a maximum of 1.84g, causing the liquid bridges to deform and in some cases collapse. Although the physics of liquid bridges subject to varying total body force is well-established and has been analyzed extensively both theoretically and experimentally, specific hardware was designed to vary g(eff) in a precise way that overcomes the gravity-related limitations and high g-jitter associated with parabolic flights. Bridge-stability was examined for axial and lateral orientations with respect to g(eff) by measuring the slenderness ratio as a function of Bond number at the instant of bridge collapse. Results exhibit remarkable agreement with theory as well as with the experimental results obtained in a magnetic levitation-based experiment. The parabolic flight method offers technical originality and provides experimental insights for researchers in the microgravity field. Here we present hardware development, experimental considerations, and results, and demonstrate that parabolic flight is a viable alternative to extant techniques for quantitative experiments on fluids.
C1 [DiLisi, Gregory] John Carroll Univ, University Hts, OH 44118 USA.
[Dempsey, Robert] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Rarick, Richard] Cleveland State Univ, Cleveland, OH 44115 USA.
[Rosenblatt, Charles] Case Western Reserve Univ, Cleveland, OH 44106 USA.
RP DiLisi, G (reprint author), John Carroll Univ, University Hts, OH 44118 USA.
EM gdilisi@jcu.edu
FU National Aeronautics and Space Administration under Reduced Gravity
Student Flight Program
FX This work was supported by the National Aeronautics and Space
Administration under the Reduced Gravity Student Flight Program. The
authors also wish to acknowledge the undergraduate students from John
Carroll University and Baldwin Wallace University who performed several
of the in-flight measurements.
NR 32
TC 0
Z9 0
U1 2
U2 3
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 JUN
PY 2015
VL 27
IS 3
BP 145
EP 153
DI 10.1007/s12217-015-9423-3
PG 9
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA CP0FA
UT WOS:000359550000003
ER
PT J
AU LeNoble, C
Peritz, J
Weber, E
Adaryukov, J
Dodson, C
Svec, L
AF LeNoble, Chelsea
Peritz, Jonathan
Weber, Erica
Adaryukov, James
Dodson, Catherine
Svec, Leedjia
TI The Application of Multipurpose Efficiently Engineered Tabling Outcomes
(MEETO) for Improved Networks
SO NAVAL ENGINEERS JOURNAL
LA English
DT Article
AB From continuous operations (CONOPS) to speed networking events, there are numerous applications within the military environment in which a systematic arrangement of people is required. Shifts must be scheduled to minimize sleep disturbance, teams must be created to maximize diversity, and individuals seek to network with as many new individuals as possible. While planned rotation within groups can improve functions within military operations, there are significant logistical challenges to ensure equitable distribution of personnel, balanced teams, or efficient social networking events. This experiment created and tested different algorithms that sought to solve the challenge of rotating personnel so that an individual would not engage in the same condition more than once for a set period. The successful solution comprised a matrix allowing for multiples of five in systematic rearrangements of stepwise patterns. The solution utilized six rounds of five people per table to achieve the intended result that each person in a group of 100 people meets 24 other people without meeting the same person twice. The algorithm may be adjusted in other situations, for example smaller or larger numbers, even numbers, or unexpected conditions.
C1 [LeNoble, Chelsea] Florida Inst Technol, Melbourne, FL 32901 USA.
[Peritz, Jonathan] Coral Springs Charter Sch, Coral Springs, FL 33065 USA.
[Weber, Erica] Melbourne Cent Catholic High Sch, Melbourne, FL 32901 USA.
[Dodson, Catherine] Michigan State Univ, Social Psychol, E Lansing, MI 48824 USA.
[Adaryukov, James] Satellite High Sch, Satellite Beach, FL 32937 USA.
[Svec, Leedjia] NASA, Houston, TX USA.
RP LeNoble, C (reprint author), Florida Inst Technol, Melbourne, FL 32901 USA.
NR 8
TC 0
Z9 0
U1 1
U2 1
PU AMER SOC NAVAL ENG INC
PI ALEXANDRIA
PA 1452 DUKE STREET, ALEXANDRIA, VA 22314-3458 USA
SN 0028-1425
EI 1559-3584
J9 NAV ENG J
JI Nav. Eng. J.
PD JUN
PY 2015
VL 127
IS 2
BP 101
EP 104
PG 4
WC Engineering, Marine; Engineering, Civil; Oceanography
SC Engineering; Oceanography
GA CO5CV
UT WOS:000359178100005
ER
PT J
AU Alexeyev, SO
Rannu, KA
Dyadina, PI
Latosh, BN
Turyshev, SG
AF Alexeyev, S. O.
Rannu, K. A.
Dyadina, P. I.
Latosh, B. N.
Turyshev, S. G.
TI Observational limits on Gauss-Bonnet and Randall-Sundrum gravities
SO JOURNAL OF EXPERIMENTAL AND THEORETICAL PHYSICS
LA English
DT Article
ID SPHERICALLY SYMMETRIC-SOLUTIONS; EXTENDED EINSTEIN EQUATIONS; DILATONIC
BLACK-HOLES; F R THEORIES; GENERAL-RELATIVITY; HAWKING RADIATION;
BACKGROUND FIELDS; QUANTUM-GRAVITY; STRING GRAVITY; TENSOR
AB We discuss the possibilities of experimental search for the new physics predicted by the Gauss-Bonnet and the Randall-Sundrum theories of gravity. The effective four-dimensional spherically symmetrical solutions of these theories are analyzed. We consider these solutions in the weak-field limit and in the process of the primordial black hole evaporation. We show that the predictions of the discussed models are the same as of general relativity. Hence, current experiments are not applicable for such search, and therefore different methods of observation and higher accuracy are required.
C1 [Alexeyev, S. O.; Rannu, K. A.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia.
[Dyadina, P. I.] Moscow MV Lomonosov State Univ, Dept Phys, Moscow 119991, Russia.
[Latosh, B. N.] Dubna Int Univ, Fac Nat & Engn Sci, Dubna 141980, Moscow Oblast, Russia.
[Latosh, B. N.] Ural Fed Univ, Inst Nat Sci, Dept Phys, Ekaterinburg 620002, Russia.
[Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Alexeyev, SO (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia.
EM salexeyev@gmail.com
RI Latosh, Boris/E-8252-2017
OI Latosh, Boris/0000-0001-7099-0861
FU Federal Agency on Science and Innovations of Russian Federation
[02.740.11.0575]; D. Zimin's "Dynasty" Foundation
FX This paper was supported by the Federal Agency on Science and
Innovations of Russian Federation, state contract 02.740.11.0575. S. A.
and B. L. were also supported by individual grants from D. Zimin's
"Dynasty" Foundation. The authors thank S. Capozziello, M. Smolyakov,
and D. Levkov for the useful discussions on the subject of this work.
This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 84
TC 0
Z9 0
U1 0
U2 1
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 1063-7761
EI 1090-6509
J9 J EXP THEOR PHYS+
JI J. Exp. Theor. Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 966
EP 973
DI 10.1134/S1063776115060011
PG 8
WC Physics, Multidisciplinary
SC Physics
GA CN7YB
UT WOS:000358650800005
ER
PT J
AU Capotondi, A
Wittenberg, AT
Newman, M
Di Lorenzo, E
Yu, JY
Braconnot, P
Cole, J
Dewitte, B
Giese, B
Guilyardi, E
Jin, FF
Karnauskas, K
Kirtman, B
Lee, T
Schneider, N
Xue, Y
Yeh, SW
AF Capotondi, Antonietta
Wittenberg, Andrew T.
Newman, Matthew
Di Lorenzo, Emanuele
Yu, Jin-Yi
Braconnot, Pascale
Cole, Julia
Dewitte, Boris
Giese, Benjamin
Guilyardi, Eric
Jin, Fei-Fei
Karnauskas, Kristopher
Kirtman, Benjamin
Lee, Tong
Schneider, Niklas
Xue, Yan
Yeh, Sang-Wook
TI Understanding ENSO Diversity
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; NINO-SOUTHERN-OSCILLATION; CENTRAL EQUATORIAL
PACIFIC; WESTERLY WIND BURSTS; COUPLED CLIMATE MODELS; TONGUE EL-NINO;
TROPICAL PACIFIC; OCEAN-ATMOSPHERE; DECADAL VARIABILITY; REANALYSIS
PROJECT
AB El Nino-Southern Oscillation (ENSO) is a naturally occurring mode of tropical Pacific variability, with global impacts on society and natural ecosystems. While it has long been known that El Nino events display a diverse range of amplitudes, triggers, spatial patterns, and life cycles, the realization that ENSO's impacts can be highly sensitive to this event-to-event diversity is driving a renewed interest in the subject. This paper surveys our current state of knowledge of ENSO diversity, identifies key gaps in understanding, and outlines some promising future research directions.
C1 [Capotondi, Antonietta; Newman, Matthew] Univ Colorado, Boulder, CO 80309 USA.
[Capotondi, Antonietta; Newman, Matthew] NOAA, ESRL, Boulder, CO 80305 USA.
[Wittenberg, Andrew T.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Di Lorenzo, Emanuele] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Yu, Jin-Yi] Univ Calif Irvine, Irvine, CA USA.
[Braconnot, Pascale] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Cole, Julia] Univ Arizona, Tucson, AZ USA.
[Dewitte, Boris] LEGOS, Toulouse, France.
[Giese, Benjamin] Texas A&M, College Stn, TX USA.
[Guilyardi, Eric] IPSL, LOCEAN, Paris, France.
[Guilyardi, Eric] Univ Reading, Reading, Berks, England.
[Jin, Fei-Fei; Schneider, Niklas] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Karnauskas, Kristopher] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Kirtman, Benjamin] Univ Miami, Miami, FL USA.
[Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Xue, Yan] Climate Predict Ctr, College Pk, MD USA.
[Yeh, Sang-Wook] Hanyang Univ, Ansan, South Korea.
RP Capotondi, A (reprint author), NOAA, ESRL, PSD1, 325 Broadway, Boulder, CO 80305 USA.
EM antonietta.capotondi@noaa.gov
RI Newman, Matthew /F-8336-2010; Wittenberg, Andrew/G-9619-2013; Guilyardi,
Eric/D-4868-2011; Di Lorenzo, Emanuele/E-9107-2012
OI Newman, Matthew /0000-0001-5348-2312; Wittenberg,
Andrew/0000-0003-1680-8963; Guilyardi, Eric/0000-0002-2255-8625; Di
Lorenzo, Emanuele/0000-0002-1935-7363
FU U.S. CLIVAR office; NASA; NOAA; NSF; DOE; National Science Foundation
FX The authors of this paper are members of the U.S. CLIVAR ENSO Diversity
Working Group, sponsored by U.S. CLIVAR. The working group wishes to
acknowledge the U.S. CLIVAR office for its support, and the U.S. CLIVAR
funding agencies, NASA, NOAA, NSF, and DOE, for their sponsorship. The
authors would also like to thank Drs. M. McPhaden and D. Dommenget, as
well as two anonymous reviewers, for their careful readings of the
manuscript, excellent suggestions, and constructive criticism, which
have considerably improved the paper. 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. AC acknowledges support from the National Science
Foundation for this study.
NR 133
TC 63
Z9 64
U1 15
U2 71
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 JUN
PY 2015
VL 96
IS 6
BP 921
EP 938
DI 10.1175/BAMS-D-13-00117.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CN1WZ
UT WOS:000358212700001
ER
PT J
AU Walsh, KJE
Camargo, SJ
Vecchi, GA
Daloz, AS
Elsner, J
Emanuel, K
Horn, M
Lim, YK
Roberts, M
Patricola, C
Scoccimarro, E
Sobel, AH
Strazzo, S
Villarini, G
Wehner, M
Zhao, M
Kossin, JP
Larow, T
Oouchi, K
Schubert, S
Wang, H
Bacmeister, J
Chang, P
Chauvin, F
Jablonowski, C
Kumar, A
Murakami, H
Ose, T
Reed, KA
Saravanan, R
Yamada, Y
Zarzycki, CM
Vidale, PL
Jonas, JA
Henderson, N
AF Walsh, Kevin J. E.
Camargo, Suzana J.
Vecchi, Gabriel A.
Daloz, Anne Sophie
Elsner, James
Emanuel, Kerry
Horn, Michael
Lim, Young-Kwon
Roberts, Malcolm
Patricola, Christina
Scoccimarro, Enrico
Sobel, Adam H.
Strazzo, Sarah
Villarini, Gabriele
Wehner, Michael
Zhao, Ming
Kossin, James P.
LaRow, Tim
Oouchi, Kazuyoshi
Schubert, Siegfried
Wang, Hui
Bacmeister, Julio
Chang, Ping
Chauvin, Fabrice
Jablonowski, Christiane
Kumar, Arun
Murakami, Hiroyuki
Ose, Tomoaki
Reed, Kevin A.
Saravanan, Ramalingam
Yamada, Yohei
Zarzycki, Colin M.
Vidale, Pier Luigi
Jonas, Jeffrey A.
Henderson, Naomi
TI HURRICANES AND CLIMATE The US CLIVAR Working Group on Hurricanes
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID TROPICAL CYCLONE ACTIVITY; GENERAL-CIRCULATION MODELS;
RADIATIVE-CONVECTIVE EQUILIBRIUM; SEA-SURFACE TEMPERATURES; GENESIS
POTENTIAL INDEX; CMIP5 MODELS; FUTURE CHANGES; 20-1ST-CENTURY
PROJECTIONS; MAXIMUM INTENSITY; ATMOSPHERIC MODEL
AB While a quantitative climate theory of tropical cyclone formation remains elusive, considerable progress has been made recently in our ability to simulate tropical cyclone climatologies and to understand the relationship between climate and tropical cyclone formation. Climate models are now able to simulate a realistic rate of global tropical cyclone formation, although simulation of the Atlantic tropical cyclone climatology remains challenging unless horizontal resolutions finer than 50 km are employed. This article summarizes published research from the idealized experiments of the Hurricane Working Group of U.S. Climate and Ocean: Variability, Predictability and Change (CLIVAR). This work, combined with results from other model simulations, has strengthened relationships between tropical cyclone formation rates and climate variables such as midtropospheric vertical velocity, with decreased climatological vertical velocities leading to decreased tropical cyclone formation. Systematic differences are shown between experiments in which only sea surface temperature is increased compared with experiments where only atmospheric carbon dioxide is increased. Experiments where only carbon dioxide is increased are more likely to demonstrate a decrease in tropical cyclone numbers, similar to the decreases simulated by many climate models for a future, warmer climate. Experiments where the two effects are combined also show decreases in numbers, but these tend to be less for models that demonstrate a strong tropical cyclone response to increased sea surface temperatures. Further experiments are proposed that may improve our understanding of the relationship between climate and tropical cyclone formation, including experiments with two-way interaction between the ocean and the atmosphere and variations in atmospheric aerosols.
C1 [Walsh, Kevin J. E.; Horn, Michael] Univ Melbourne, Parkville, Vic 3010, Australia.
[Camargo, Suzana J.; Sobel, Adam H.; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Vecchi, Gabriel A.; Zhao, Ming; Murakami, Hiroyuki] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Daloz, Anne Sophie] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
[Elsner, James; Strazzo, Sarah; LaRow, Tim] Florida State Univ, Tallahassee, FL 32306 USA.
[Emanuel, Kerry] MIT, Cambridge, MA 02139 USA.
[Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Lim, Young-Kwon] Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Lim, Young-Kwon] IM Syst Grp, Greenbelt, MD USA.
[Roberts, Malcolm] Met Off, Exeter, Devon, England.
[Patricola, Christina; Chang, Ping; Saravanan, Ramalingam] Texas A&M Univ, College Stn, TX USA.
[Scoccimarro, Enrico] Ist Nazl Geofis & Vulcanol, Bologna, Italy.
[Scoccimarro, Enrico] Ctr Euromediterraneo Cambiamenti Climat, Bologna, Italy.
[Villarini, Gabriele] Univ Iowa, Iowa City, IA USA.
[Wehner, Michael] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Kossin, James P.] NOAA, NCDC, Asheville, NC USA.
[Oouchi, Kazuyoshi; Yamada, Yohei] JAMSTEC, Yokohama, Kanagawa, Japan.
[Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wang, Hui; Kumar, Arun] NOAA, NCEP, College Pk, MD USA.
[Bacmeister, Julio; Reed, Kevin A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Chauvin, Fabrice] Meteo France, Toulouse, France.
[Zarzycki, Colin M.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Ose, Tomoaki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
[Vidale, Pier Luigi] Univ Reading, Reading, Berks, England.
[Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Jonas, Jeffrey A.] Columbia Univ, New York, NY USA.
RP Walsh, KJE (reprint author), Univ Melbourne, Sch Earth Sci, Parkville, Vic 3010, Australia.
EM kevin.walsh@unimelb.edu.au
RI Vecchi, Gabriel/A-2413-2008; Camargo, Suzana/C-6106-2009; Reed,
Kevin/C-4466-2012; Murakami, Hiroyuki/L-5745-2015; Zarzycki,
Colin/E-5691-2014; Zhao, Ming/C-6928-2014; Jablonowski,
Christiane/I-9068-2012; Kossin, James/C-2022-2016; Chang, Ping
/A-1642-2013; Villarini, Gabriele/F-8069-2016; Sobel, Adam/K-4014-2015;
Patricola, Christina/L-9902-2016
OI Strazzo, Sarah/0000-0003-1332-3135; Vidale, Pier
Luigi/0000-0002-1800-8460; Walsh, Kevin/0000-0002-1860-510X; Vecchi,
Gabriel/0000-0002-5085-224X; Camargo, Suzana/0000-0002-0802-5160; Reed,
Kevin/0000-0003-3741-7080; Jablonowski, Christiane/0000-0003-0407-0092;
Kossin, James/0000-0003-0461-9794; Chang, Ping /0000-0002-9085-0759;
Villarini, Gabriele/0000-0001-9566-2370; Sobel,
Adam/0000-0003-3602-0567; Patricola, Christina/0000-0002-3387-0307
FU NASA; NOAA; NSF; DOE; ARC Centre of Excellence for Climate System
Science [CE110001028]; U.S. DOE [DE-SC0006824, DE-SC0006684,
DE-SC0004966]; NOAA [NA11OAR4310154, NA11OAR4310092]; NSF AGS [1143959];
NASA [NNX09AK34G]; Italian Ministry of Education, Universities and
Research; Italian Ministry of Environment, Land and Sea under the GEMINA
project; Ministry of Education, Culture, Sports, Science and Technology
(MEXT), Japan
FX We wish to take this opportunity to recognize the essential
contributions from participating modeling groups (U.S. DOE-NCAR CAM5.1,
CMCC ECHAM5, CNRM, FSU COAPS, NOAA GFDL HiRAM, NASA GISS-Columbia
University, NASA GSFC GEOS-5, Hadley Centre HadGEM3, JAMSTEC NICAM, MRI
CGCM3, NCEP GFS, and WRF) that ran model experiments and furnished their
data for analysis. We also appreciate the contributions of NOAA GFDL for
hosting the meeting that led to this paper, the U.S. CLIVAR Project
Office and UCAR JOSS for logistics support, and the U.S. CLIVAR funding
agencies-NASA, NOAA, NSF, and DOE for their sponsorship. The Texas
Advanced Computing Center (TACC) at The University of Texas at Austin
and the Texas A&M Supercomputing Facility provided supercomputing
resources used to perform portions of the simulations described in this
paper. Portions of the work described in this paper were funded in part
by the ARC Centre of Excellence for Climate System Science (Grant
CE110001028); the U.S. DOE Grants DE-SC0006824, DE-SC0006684, and
DE-SC0004966; the NOAA Grants NA11OAR4310154 and NA11OAR4310092; NSF AGS
1143959; and NASA Grant NNX09AK34G. E. Scoccimarro received funding from
the Italian Ministry of Education, Universities and Research and the
Italian Ministry of Environment, Land and Sea under the GEMINA project.
The numerical experiments for NICAM and MRI-AGCM were performed on the
Earth Simulator of JAMSTEC under the framework of the KAKUSHIN project
funded by the Ministry of Education, Culture, Sports, Science and
Technology (MEXT), Japan.
NR 126
TC 33
Z9 33
U1 6
U2 31
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 JUN
PY 2015
VL 96
IS 6
BP 997
EP 1017
DI 10.1175/BAMS-D-13-00242.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CN1XE
UT WOS:000358213200002
ER
PT J
AU Holt, B
Johnson, MP
Perkovic-Martin, D
Panzer, B
AF Holt, Benjamin
Johnson, Michael P.
Perkovic-Martin, Dragana
Panzer, Ben
TI Snow depth on Arctic sea ice derived from radar: In situ comparisons and
time series analysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE snow on sea Ice
ID ULTRA-WIDE-BAND; THICKNESS; VARIABILITY; OCEAN
AB The snow radar being flown on NASA's Operation IceBridge, ongoing aircraft campaigns to the Arctic and the Antarctic are providing unique observations of the depth of snow on the sea ice cover. In this paper, we focus on the radar-derived snow depth results from the 2009-2012 Arctic campaigns. We develop and evaluate the use of a distinct snow layer tracker to measure snow depth based on a Support Vector Machine (SVM) supervised learning algorithm. The snow radar is designed to detect both the air-snow and snow-ice interfaces using ultrawideband frequencies from 2 to 8 GHz. The quality, errors, and repeatability of the snow radar snow depth estimates are examined, based on comparisons with in situ data obtained during two separate sea ice field campaigns, the GreenArc 2009 and the CryoVEx 2011 campaigns off Greenland in the Lincoln Sea. Finally, we analyze 4 years (2009-2012) of three annually repeated sea ice flight lines obtained in early spring, located off Greenland and the Canadian Arctic. We examine the annual variations of snow depth differences between perennial and seasonal ice when available. Overall, the snow layer tracker produced consistent, accurate results for snow depths between 0.10 and approximate to 0.60 m. This was confirmed with comparisons with the two data sets from the in situ measurement campaigns as well as with the time series analysis, and is consistent with other published results.
C1 [Holt, Benjamin; Johnson, Michael P.; Perkovic-Martin, Dragana] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Panzer, Ben] Sandia Natl Labs, Albuquerque, NM 87185 USA.
RP Holt, B (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Benjamin.M.Holt@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, and at Kansas University, under contract with
the National Aeronautics and Space Administration. Ben Panzer performed
this work while at the University of Kansas. The authors wish to thank
the following for valuable discussions: Christian Haas (York University)
regarding the CryoVEx field measurements, Ron Kwok (JPL), and Prasad
Gogineni and Carl Leuschen (University of Kansas). We also wish to thank
Jackie Richter-Menge and Bruce Elder (CRREL) as well as Sinead Farrell
(University of Maryland) for providing the GreenArc 2009 data. The snow
radar raw data utilized for this study were produced by CReSIS and made
available, along with the ATM, CAMBOT, and DMS imagery through the
National Snow and Ice Data Center IceBridge data portal
(http://nsidc.org/icebridge/portal/). To identify snow depths for
different sea ice types, we utilized derived sea ice type output data
available from the EUMETSAT Ocean and Sea Ice Processing Centre
(http://saf.met.no/p/ice/#type).
NR 43
TC 3
Z9 3
U1 1
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 JUN
PY 2015
VL 120
IS 6
BP 4260
EP 4287
DI 10.1002/2015JC010815
PG 28
WC Oceanography
SC Oceanography
GA CN0SP
UT WOS:000358124100021
ER
PT J
AU Boardsen, SA
Kim, EH
Raines, JM
Slavin, JA
Gershman, DJ
Anderson, BJ
Korth, H
Sundberg, T
Schriver, D
Travnicek, P
AF Boardsen, S. A.
Kim, E. -H.
Raines, J. M.
Slavin, J. A.
Gershman, D. J.
Anderson, B. J.
Korth, H.
Sundberg, T.
Schriver, D.
Travnicek, P.
TI Interpreting similar to 1Hz magnetic compressional waves in Mercury's
inner magnetosphere in terms of propagating ion-Bernstein waves
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ion-Bernstein mode; ray tracing; Mercury's magnetosphere; planetary loss
cone instability
ID MESSENGERS 1ST FLYBY; ULF WAVES; CYCLOTRON WAVES; PLASMA SHEET; FIELD;
DISTRIBUTIONS; GENERATION; FREQUENCY; MAGNETOMETER; ABSORPTION
AB We show that similar to 1Hz magnetic compressional waves observed in Mercury's inner magnetosphere could be interpreted as ion-Bernstein waves in a moderate proton beta similar to 0.1 plasma. An observation of a proton distribution with a large planetary loss cone is presented, and we show that this type of distribution is highly unstable to the generation of ion-Bernstein waves with low magnetic compression. Ray tracing shows that as these waves propagate back and forth about the magnetic equator; they cycle between a state of low and high magnetic compression. The group velocity decreases during the high-compression state leading to a pileup of compressional wave energy, which could explain the observed dominance of the highly compressional waves. This bimodal nature is due to the complexity of the index of refraction surface in a warm plasma whose upper branch has high growth rate with low compression, and its lower branch has low growth/damping rate with strong compression. Two different cycles are found: one where the compression maximum occurs at the magnetic equator and one where the compression maximum straddles the magnetic equator. The later cycle could explain observations where the maximum in compression straddles the equator. Ray tracing shows that this mode is confined within 12 degrees magnetic latitude which can account for the bulk of the observations. We show that the Doppler shift can account for the difference between the observed and model wave frequency, if the wave vector direction is in opposition to the plasma flow direction. We note that the Wentzel-Kramers-Brillouin approximation breaks down during the pileup of compressional energy and that a study involving full wave solutions is required.
C1 [Boardsen, S. A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Boardsen, S. A.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[Kim, E. -H.] Princeton Univ, Princeton Ctr Heliophys, Princeton, NJ 08544 USA.
[Kim, E. -H.] Princeton Univ, Princeton Plasma Phys Lab, Princeton, NJ 08543 USA.
[Raines, J. M.; Slavin, J. A.; Gershman, D. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Gershman, D. J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Anderson, B. J.; Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Sundberg, T.] Queen Mary Univ London, Sch Phys & Astron, London, England.
[Schriver, D.] Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90024 USA.
[Travnicek, P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Boardsen, SA (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
EM Scott.A.Boardsen@nasa.gov
RI Travnicek, Pavel/G-8608-2014; Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA Planetary Data Analysis Program [NNX10AU26G]; Geoscience
[NNX08AJ78G]; NASA [NNH09AK63I, NNH11AQ46I]; DOE [DEAC02-09CH11466];
NASA Discovery Program [NAS5-97271]; NASA Heliophysics Supporting
Research Program [NNX15AJ68G]
FX We thank K. Ronnmark at Umea University in Sweden for providing us with
the warm plasma instability code WHAMP and the warm plasma ray tracing
code RATRACE. The data used in this study are publicly available at the
Planetary Data System (http://pds.nasa.gov/). This research was
supported by NASA Planetary Data Analysis Program grant NNX10AU26G and
Geoscience grant NNX08AJ78G. The work at the Princeton University was
supported by NASA grants NNH09AK63I and NNH11AQ46I, and DOE contract
DEAC02-09CH11466. The MESSENGER project is supported by the NASA
Discovery Program under contracts NAS5-97271 to the Johns Hopkins
University Applied Physics Laboratory. This work was also supported by
the NASA Heliophysics Supporting Research Program under grant
NNX15AJ68G.
NR 55
TC 5
Z9 5
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4213
EP 4228
DI 10.1002/2014JA020910
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100010
ER
PT J
AU Hwang, J
Choi, EJ
Park, JS
Fok, MC
Lee, DY
Kim, KC
Shin, DK
Usanova, ME
Reeves, GD
AF Hwang, J.
Choi, E. -J.
Park, J. -S.
Fok, M. -C.
Lee, D. -Y.
Kim, K. -C.
Shin, D. -K.
Usanova, M. E.
Reeves, G. D.
TI Comprehensive analysis of the flux dropout during 7-8 November 2008
storm using multisatellite observations and RBE model
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE flux dropout; RBE model; magneopause shadowing; atmospheric
precipitation; geomagnetic storm; radiation belt
ID OUTER RADIATION BELT; PITCH-ANGLE SCATTERING; ION-CYCLOTRON WAVES;
ELECTRON ACCELERATION; INNER MAGNETOSPHERE; MAGNETIC STORMS; CHORUS
WAVES; 30 SEPTEMBER; PHASE-SPACE; DIFFUSION
AB We investigate an electron flux dropout during a weak storm on 7-8 November 2008, with Dst minimum value being - 37 nT. During this period, two clear dropouts were observed on GOES 11>2MeV electrons. We also find a simultaneous dropout in the subrelativistic electrons recorded by Time History of Events and Macroscale Interactions during Substorms probes in the outer radiation belt. Using the Radiation Belt Environment model, we try to reproduce the observed dropout features in both relativistic and subrelativistic electrons. We found that there are local time dependences in the dropout for both observation and simulation in subrelativistic electrons: ( 1) particle loss begins from nightside and propagates into dayside and (2) resupply starts from near dawn magnetic local time and propagates into the dayside following electron drift direction. That resupply of the particles might be caused by substorm injections due to enhanced convection. We found a significant precipitation in hundreds keV electrons during the dropout. We observe electromagnetic ion cyclotron and chorus waves both on the ground and in space. We find the drift shells are opened near the beginning of the first dropout. The dropout in MeV electrons at GEO might therefore be initiated due to the magnetopause shadowing, and the followed dropout in hundreds keV electrons might be the result of the combination of magnetopause shadowing and precipitation loss into the Earth's atmosphere.
C1 [Hwang, J.; Kim, K. -C.] Korea Astron & Space Sci Inst, Taejon, South Korea.
[Hwang, J.] Korea Univ Sci & Technol, Dept Astron & Space Sci, Taejon, South Korea.
[Choi, E. -J.] Korea Adv Inst Sci & Technol, Dept Phys, Taejon 305701, South Korea.
[Park, J. -S.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea.
[Fok, M. -C.] NASA GSFC, Greenbelt, MD USA.
[Lee, D. -Y.; Shin, D. -K.] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju, South Korea.
[Usanova, M. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
RP Hwang, J (reprint author), Korea Astron & Space Sci Inst, Taejon, South Korea.
EM jahwang@kasi.re.kr
OI Reeves, Geoffrey/0000-0002-7985-8098
FU Planetary system research for space exploration project; KASI; NSL
[20110030742]; Canadian Space Agency; NASA [NAS5-02099]
FX This work was supported by "Planetary system research for space
exploration" project and the basic research funding from KASI. This work
at Chungbuk National University was supported by an NSL grant
(20110030742) of the National Research Foundation of Korea. We are
thankful to the THEMIS team
(http://themis.ssl.berkeley.edu/data_retrieval. index); NASA's CDAWeb (
http://cdaweb.gsfc.nasa.gov/), OMNI ( http://omniweb.gsfc.nasa.gov/);
and NOAA's GOES (http://www.goes.noaa.gov/), POES
(ftp://virbo.org/POES), NGDC
http://www.ngdc.noaa.gov/ngdcinfo/onlineaccess.html),and LANL GEO data (
by personal contact to G.D. Reeves) for providing online data access and
data analysis tools. The authors thank I.R. Mann, D.K. Milling, and the
rest of the CARISMA team for the data. CARISMA is operated by the
University of Alberta, funded by the Canadian Space Agency. We
acknowledge NASA contract NAS5-02099 for the use of data from the THEMIS
mission.
NR 55
TC 3
Z9 3
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4298
EP 4312
DI 10.1002/2015JA021085
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100015
ER
PT J
AU Welling, DT
Jordanova, VK
Glocer, A
Toth, G
Liemohn, MW
Weimer, DR
AF Welling, D. T.
Jordanova, V. K.
Glocer, A.
Toth, G.
Liemohn, M. W.
Weimer, D. R.
TI The two-way relationship between ionospheric outflow and the ring
current
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; ring current; ionospheric outflow
ID ALLEN PROBES OBSERVATIONS; SHEET ION COMPOSITION; FIELD-ALIGNED CURRENT;
POLAR WIND; PLASMA SHEET; NEAR-EARTH; INNER MAGNETOSPHERE;
MAGNETIC-FIELD; STORM-TIME; PROTON PRECIPITATION
AB It is now well established that the ionosphere, because it acts as a significant source of plasma, plays a critical role in ring current dynamics. However, because the ring current deposits energy into the ionosphere, the inverse may also be true: the ring current can play a critical role in the dynamics of ionospheric outflow. This study uses a set of coupled, first-principles-based numerical models to test the dependence of ionospheric outflow on ring current-driven region 2 field-aligned currents (FACs). A moderate magnetospheric storm event is modeled with the Space Weather Modeling Framework using a global MHD code (Block Adaptive Tree Solar wind Roe-type Upwind Scheme, BATS-R-US), a polar wind model (Polar Wind Outflow Model), and a bounce-averaged kinetic ring current model (ring current atmosphere interaction model with self-consistent magnetic field, RAM-SCB). Initially, each code is two-way coupled to all others except for RAM-SCB, which receives inputs from the other models but is not allowed to feed back pressure into the MHD model. The simulation is repeated with pressure coupling activated, which drives strong pressure gradients and region 2 FACs in BATS-R-US. It is found that the region 2 FACs increase heavy ion outflow by up to 6 times over the noncoupled results. The additional outflow further energizes the ring current, establishing an ionosphere-magnetosphere mass feedback loop. This study further demonstrates that ionospheric outflow is not merely a plasma source for the magnetosphere but an integral part in the nonlinear ionosphere-magnetosphere-ring current system.
C1 [Welling, D. T.; Toth, G.; Liemohn, M. W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Jordanova, V. K.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Glocer, A.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Weimer, D. R.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA.
RP Welling, DT (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM dwelling@umich.edu
RI Toth, Gabor/B-7977-2013;
OI Toth, Gabor/0000-0002-5654-9823; Jordanova, Vania/0000-0003-0475-8743
FU NSF [AGS 1202984]; NASA [NNH13AV48I, NNH14AX90I, NNX11AO60G,
NNX13AD69G]; Los Alamos National Laboratory Directed Research and
Development (LDRD) Program
FX The authors acknowledge the use of data from the ACE satellite MAG and
SWEPAM instruments provided by NASA GSFC Space Physics Data Facility.
Dst index was obtained via the World Data Center for Geomagnetism,
Kyoto. This work was supported by NSF award AGS 1202984; NASA awards
NNH13AV48I, NNH14AX90I, NNX11AO60G, and NNX13AD69G; and the Los Alamos
National Laboratory Directed Research and Development (LDRD) Program.
Models used in this study can be freely obtained from
http://csem.engin.umich.edu; simulation data can be obtained by
contacting the authors.
NR 114
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U1 1
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 JUN
PY 2015
VL 120
IS 6
BP 4338
EP 4353
DI 10.1002/2015JA021231
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100018
ER
PT J
AU Gershman, DJ
Raines, JM
Slavin, JA
Zurbuchen, TH
Sundberg, T
Boardsen, SA
Anderson, BJ
Korth, H
Solomon, SC
AF Gershman, Daniel J.
Raines, Jim M.
Slavin, James A.
Zurbuchen, Thomas H.
Sundberg, Torbjoern
Boardsen, Scott A.
Anderson, Brian J.
Korth, Haje
Solomon, Sean C.
TI MESSENGER observations of multiscale Kelvin-Helmholtz vortices at
Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Kelvin-Helmholtz; Mercury; MESSENGER; finite gyroradius
ID EARTHS MAGNETOSPHERE; PLANETARY IONS; PLASMA SHEET; SOLAR-WIND;
MAGNETOPAUSE; MAGNETOSHEATH; MAGNETOTAIL; INSTABILITIES; MAGNETOMETER;
ENVIRONMENT
AB Observations by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft in Mercury's magnetotail demonstrate for the first time that Na+ ions exert a dynamic influence on Mercury's magnetospheric system. Na+ ions are shown to contribute up to similar to 30% of the ion thermal pressure required to achieve pressure balance in the premidnight plasma sheet. High concentrations of planetary ions should lead to Na+ dominance of the plasma mass density in these regions. On orbits with northward-oriented interplanetary magnetic field and high (i.e., >1cm(-3)) Na+ concentrations, MESSENGER has often recorded magnetic field fluctuations near the Na+ gyrofrequency associated with the Kelvin-Helmholtz (K-H) instability. These nightside K-H vortices are characteristically different from those observed on Mercury's dayside that have a nearly constant wave frequency of similar to 0.025Hz. Collectively, these observations suggest that large spatial gradients in the hot planetary ion population at Mercury may result in a transition from a fluid description to a kinetic description of vortex formation across the dusk terminator, providing the first set of truly multiscale observations of the K-H instability at any of the diverse magnetospheric environments explored in the solar system.
C1 [Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Sundberg, Torbjoern] Queen Mary Univ London, Sch Phys & Astron, London, England.
[Boardsen, Scott A.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
RP Gershman, DJ (reprint author), NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
EM djgersh@umich.edu
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA Discovery Program [NAS5-97271]; Carnegie Institution of Washington
[NASW-00002]; NASA Postdoctoral Program at Goddard Space Flight Center
FX We thank two anonymous reviewers for their thoughtful comments on an
earlier draft. The data used in this work can be obtained from the
Planetary Data System (http://pds.nasa.gov/). 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. D.J.G. is supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities.
NR 64
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U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4354
EP 4368
DI 10.1002/2014JA020903
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100019
ER
PT J
AU Fatemi, S
Lue, C
Holmstrom, M
Poppe, AR
Wieser, M
Barabash, S
Delory, GT
AF Fatemi, Shahab
Lue, Charles
Holmstrom, Mats
Poppe, Andrew R.
Wieser, Martin
Barabash, Stas
Delory, Gregory T.
TI Solar wind plasma interaction with Gerasimovich lunar magnetic anomaly
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Interaction with lunar crustal fields; Hybrid modeling of plasma
ID MHD SIMULATION; MOON; SURFACE; FIELDS; PROSPECTOR; MAGNETOMETER;
ENVIRONMENT; REGIONS; CAVITY; MODEL
AB We present the results of the first local hybrid simulations (particle ions and fluid electrons) for the solar wind plasma interaction with realistic lunar crustal fields. We use a three-dimensional hybrid model of plasma and an empirical model of the Gerasimovich magnetic anomaly based on Lunar Prospector observations. We examine the effects of low and high solar wind dynamic pressures on this interaction when the Gerasimovich magnetic anomaly is located at nearly 20 degrees solar zenith angle. We find that for low solar wind dynamic pressure, the crustal fields mostly deflect the solar wind plasma, form a plasma void at very close distances to the Moon (below 20km above the surface), and reflect nearly 5% of the solar wind in charged form. In contrast, during high solar wind dynamic pressure, the crustal fields are more compressed, the solar wind is less deflected, and the lunar surface is less shielded from impinging solar wind flux, but the solar wind ion reflection is more locally intensified (up to 25%) compared to low dynamic pressures. The difference is associated with an electrostatic potential that forms over the Gerasimovich magnetic anomaly as well as the effects of solar wind plasma on the crustal fields during low and high dynamic pressures. Finally, we show that an antimoonward Hall electric field is the dominant electric field for similar to 3km altitude and higher, and an ambipolar electric field has a noticeable contribution to the electric field at close distances (<3km) to the Moon.
C1 [Fatemi, Shahab; Poppe, Andrew R.; Delory, Gregory T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fatemi, Shahab; Poppe, Andrew R.; Delory, Gregory T.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
[Lue, Charles; Holmstrom, Mats; Wieser, Martin; Barabash, Stas] Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
[Lue, Charles] Umea Univ, Dept Phys, Umea, Sweden.
RP Fatemi, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM shahab@ssl.berkeley.edu
OI Holmstrom, Mats/0000-0001-5494-5374
FU NASA's Solar System Exploration Research Virtual Institute (SSERVI)
[NNX14AG16A]; SSERVI [SSERVI-2015-026]
FX S. Fatemi, A. R. Poppe, and G. T. Delory gratefully acknowledge support
from NASA's Solar System Exploration Research Virtual Institute
(SSERVI), grant NNX14AG16A. This publication is SSERVI contribution
SSERVI-2015-026. This research was conducted using resources provided by
the Swedish National Infrastructure for Computing (SNIC) at the High
Performance Computing Center North (HPC2N), Umea University, Sweden. The
software used in this work was developed in part by the DOE NNSA ASC-
and DOE Office of Science ASCR-supported Flash Center for Computational
Science at the University of Chicago. The visualization tools we
developed for our model data analysis are based on python Matplotlib and
Mayavi open libraries. The authors thank the International Space Science
Institute (ISSI) Bern, Switzerland, for organizing a meeting when the
topic of this paper was extensively discussed. We thank the teams who
created and provided Wind magnetic field and plasma data used in this
analysis, including K. W. Ogilvie, A. J. Lazarus, and R. Lepping. The
Wind data used for this paper is available at Comprehensive Solar Wind
Laboratory For Long-Term Solar Wind Measurements at NASA website wind.
nasa.gov. Data set name: WIND SWE 92-sec and MFI Magnetic Field.
Selection period is 17 June 2009 between 16: 30 UT and 21: 50 UT.
NR 54
TC 8
Z9 8
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4719
EP 4735
DI 10.1002/2015JA021027
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100048
ER
PT J
AU Dai, L
Takahashi, K
Lysak, R
Wang, C
Wygant, JR
Kletzing, C
Bonnell, J
Cattell, CA
Smith, CW
MacDowall, RJ
Thaller, S
Breneman, A
Tang, XW
Tao, X
Chen, LJ
AF Dai, Lei
Takahashi, Kazue
Lysak, Robert
Wang, Chi
Wygant, John R.
Kletzing, Craig
Bonnell, John
Cattell, Cynthia A.
Smith, Charles W.
MacDowall, Robert J.
Thaller, Scott
Breneman, Aaron
Tang, Xiangwei
Tao, Xin
Chen, Lunjin
TI Storm time occurrence and spatial distribution of Pc4 poloidal ULF waves
in the inner magnetosphere: A Van Allen Probes statistical study
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Pc4 ULF waves; poloidal waves; geomagnetic storm; Van Allen Probe; solar
wind dynamic pressure; ring current
ID GIANT PULSATIONS; MAGNETIC-FIELD; AMPTE CCE; HYDROMAGNETIC-WAVES;
SYNCHRONOUS ORBIT; ALFVEN WAVES; CONE ANGLE; SOLAR-WIND; ACCELERATION;
ELECTRONS
AB Poloidal ULF waves are capable of efficiently interacting with energetic particles in the ring current and the radiation belt. Using Van Allen Probes (Radiation Belt Storm Probes (RBSP)) data from October 2012 to July 2014, we investigate the spatial distribution and storm time occurrence of Pc4 (7-25mHz) poloidal waves in the inner magnetosphere. Pc4 poloidal waves are sorted into two categories: waves with and without significant magnetic compressional components. Two types of poloidal waves have comparable occurrence rates, both of which are much higher during geomagnetic storms. The noncompressional poloidal waves mostly occur in the late recovery phase associated with an increase of Dst toward 0, suggesting that the decay of the ring current provides their free energy source. The occurrence of dayside compressional Pc4 poloidal waves is found correlated with the variation of the solar wind dynamic pressure, indicating their origin in the solar wind. Both compressional and noncompressional waves preferentially occur on the dayside near noon at L similar to 5-6. In addition, compressional poloidal waves are observed at magnetic local time 18-24 on the nightside. The location of the Pc4 poloidal waves relative to the plasmapause is investigated. The RBSP statistical results may shed light on the in-depth investigations of the generation and propagation of Pc4 poloidal waves.
C1 [Dai, Lei; Wang, Chi] Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China.
[Dai, Lei; Lysak, Robert; Wygant, John R.; Cattell, Cynthia A.; Thaller, Scott; Breneman, Aaron; Tang, Xiangwei] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Takahashi, Kazue] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Kletzing, Craig] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bonnell, John] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Smith, Charles W.] Univ New Hampshire, Inst Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA.
[MacDowall, Robert J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Tao, Xin] Univ Sci & Technol China, Dept Geophys & Planetary Sci, Hefei 230026, Peoples R China.
[Chen, Lunjin] Univ Texas Dallas, Dept Phys, Richardson, TX USA.
RP Dai, L (reprint author), Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China.
EM ldai@spaceweather.ac.cn
OI Cattell, Cynthia/0000-0002-3805-320X; Kletzing,
Craig/0000-0002-4136-3348
FU NASA [NNX14AB97G]; NNSFC [41231067]; Specialized Research Fund for State
Key Laboratories of China; APL for the development of RBSP/EFW; JHU/APL
[921647]
FX Work by L.D. and K.T. was supported by NASA grant NNX14AB97G. This work
was supported by NNSFC grant 41231067 and in part by the Specialized
Research Fund for State Key Laboratories of China. Work at UMN was
supported by a contract from APL for the development of RBSP/EFW.EMFISIS
is supported by a JHU/APL contract 921647. The RBSP EMFISIS data are
available at http://emfisis.physics.uiowa.edu/Flight/. The RBSP EFW data
are available at http://rbsp.space.umn.edu/data/rbsp/. The OMNI data are
available at CDAWeb. The Dst data are provided by the World Data Center
for Geomagnetism, Kyoto.
NR 63
TC 12
Z9 13
U1 2
U2 18
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 JUN
PY 2015
VL 120
IS 6
BP 4748
EP 4762
DI 10.1002/2015JA021134
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100050
ER
PT J
AU Chi, PJ
Le, G
AF Chi, P. J.
Le, G.
TI Observations of magnetospheric high-m poloidal waves by ST-5 satellites
in low Earth orbit during geomagnetically quiet times
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE high-m waves; poloidal mode; drift Alfven ballooning mode
ID ALFVEN-BALLOONING MODES; KINETIC-THEORY; PULSATIONS; PLASMAPAUSE
AB The poloidal waves with large azimuthal wave numbers (m similar to 100) in the magnetosphere are known to be generated by drift or drift-bounce resonance with energetic ring current particles, and these waves may play a role in modulating the energetic particles in the inner magnetosphere. When examining the magnetic field data collected by the NASA Space Technology 5 (ST-5) satellites in the low Earth orbit, Le et al. (2011) discovered many wave events with frequencies of 30-200 mHz (in the Pc2 and Pc3 bands), and they proposed that these waves should, in fact, be Doppler-shifted high-m poloidal waves in the magnetosphere with frequencies at only a few millihertz (in the Pc5 band). Using a new method that examines the differences in wave phase detected by the three ST-5 satellites, we confirm that the frequencies in the Earth frame for the poloidal waves observed are mainly between 3 and 5 mHz. Not only were poloidal waves observed frequently by ST-5 in the dayside magnetosphere but they were also occasionally seen in the nightside when the satellites passed through the same L shells. In each wave event, the azimuthal wave number may change with L, but the wave frequency in the Earth frame remains the same. We also find that poloidal waves can last more than 9 h during geomagnetically quiet conditions, suggesting that even a very weak ring current can supply enough energetic particles to excite poloidal waves.
C1 [Chi, P. J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA.
[Le, G.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Chi, PJ (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA.
EM pchi@igpp.ucla.edu
RI Le, Guan/C-9524-2012
OI Le, Guan/0000-0002-9504-5214
NR 22
TC 2
Z9 2
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4776
EP 4783
DI 10.1002/2015JA021145
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100052
ER
PT J
AU Ni, BB
Zou, ZY
Gu, XD
Zhou, C
Thorne, RM
Bortnik, J
Shi, R
Zhao, ZY
Baker, DN
Kanekal, SG
Spence, HE
Reeves, GD
Li, XL
AF Ni, Binbin
Zou, Zhengyang
Gu, Xudong
Zhou, Chen
Thorne, Richard M.
Bortnik, Jacob
Shi, Run
Zhao, Zhengyu
Baker, Daniel N.
Kanekal, Shrikhanth G.
Spence, Harlan E.
Reeves, Geoffrey D.
Li, Xinlin
TI Variability of the pitch angle distribution of radiation belt
ultrarelativistic electrons during and following intense geomagnetic
storms: Van Allen Probes observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE radiation belt ultrarelativistic electrons; pitch angle distribution;
decay time scales; geomagnetic storms; resonant wave-particle
interactions
ID MARCH 2013 STORM; RELATIVISTIC ELECTRONS; EMIC WAVES;
STATISTICAL-ANALYSIS; RESONANT SCATTERING; MAGNETIC STORM; ACCELERATION;
CHORUS; RING; SIMULATIONS
AB Fifteen months of pitch angle resolved Van Allen Probes Relativistic Electron-Proton Telescope (REPT) measurements of differential electron flux are analyzed to investigate the characteristic variability of the pitch angle distribution of radiation belt ultrarelativistic (>2MeV) electrons during storm conditions and during the long-term poststorm decay. By modeling the ultrarelativistic electron pitch angle distribution as sin(n)alpha, where alpha is the equatorial pitch angle, we examine the spatiotemporal variations of the n value. The results show that, in general, n values increase with the level of geomagnetic activity. In principle, ultrarelativistic electrons respond to geomagnetic storms by becoming more peaked at 90 degrees pitch angle with n values of 2-3 as a supportive signature of chorus acceleration outside the plasmasphere. High n values also exist inside the plasmasphere, being localized adjacent to the plasmapause and exhibiting energy dependence, which suggests a significant contribution from electromagnetic ion cyclotron (EMIC) wave scattering. During quiet periods, n values generally evolve to become small, i.e., 0-1. The slow and long-term decays of the ultrarelativistic electrons after geomagnetic storms, while prominent, produce energy and L-shell-dependent decay time scales in association with the solar and geomagnetic activity and wave-particle interaction processes. At lower L shells inside the plasmasphere, the decay time scales tau(d) for electrons at REPT energies are generally larger, varying from tens of days to hundreds of days, which can be mainly attributed to the combined effect of hiss-induced pitch angle scattering and inward radial diffusion. As L shell increases to L similar to 3.5, a narrow region exists (with a width of similar to 0.5L), where the observed ultrarelativistic electrons decay fastest, possibly resulting from efficient EMIC wave scattering. As L shell continues to increase, tau(d) generally becomes larger again, indicating an overall slower loss process by waves at high L shells. Our investigation based upon the sin(n)alpha function fitting and the estimate of decay time scale offers a convenient and useful means to evaluate the underlying physical processes that play a role in driving the acceleration and loss of ultrarelativistic electrons and to assess their relative contributions.
C1 [Ni, Binbin; Zou, Zhengyang; Gu, Xudong; Zhou, Chen; Shi, Run; Zhao, Zhengyu] Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan 430072, Peoples R China.
[Ni, Binbin] Chinese Acad Sci, State Key Lab Space Weather, Beijing, Peoples R China.
[Thorne, Richard M.; Bortnik, Jacob] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Baker, Daniel N.; Li, Xinlin] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Kanekal, Shrikhanth G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Reeves, Geoffrey D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
RP Ni, BB (reprint author), Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan 430072, Peoples R China.
EM bbni@whu.edu.cn
RI Reeves, Geoffrey/E-8101-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; zou, zhengyang/0000-0003-1273-4573
FU NSFC [41204120, 41474141]; Fundamental Research Funds for the Central
Universities [2042014kf0251]; Specialized Research Fund for State Key
Laboratories; JHU/APL under NASA [967399, 921647, NAS5-01072]; ECT
sub-award [13-041]; NASA [NNX11AR64G]
FX This work was supported by the NSFC grants 41204120 and 41474141, the
Fundamental Research Funds for the Central Universities grant
2042014kf0251, and the Project Supported by the Specialized Research
Fund for State Key Laboratories. This work was also supported by JHU/APL
contracts 967399 and 921647 under NASA's prime contract NAS5-01072. The
analysis at UCLA was supported by the ECT sub-award 13-041 and NASA
grant NNX11AR64G. Van Allen Probes REPT data were obtained from
http://www.rbsp-ect.lanl.gov/science/DataDirectories.php.
NR 48
TC 8
Z9 9
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4863
EP 4876
DI 10.1002/2015JA021065
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100058
ER
PT J
AU Lindkvist, J
Holmstrom, M
Khurana, KK
Fatemi, S
Barabash, S
AF Lindkvist, Jesper
Holmstrom, Mats
Khurana, Krishan K.
Fatemi, Shahab
Barabash, Stas
TI Callisto plasma interactions: Hybrid modeling including induction by a
subsurface ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Callisto; plasma interaction; hybrid model; subsurface ocean; Galileo
flyby; magnetosphere
ID MAGNETIC-FIELD; WAVE OBSERVATIONS; EUROPA; MAGNETOSPHERE; SATELLITES;
ABSENCE
AB By using a hybrid plasma solver (ions as particles and electrons as a fluid), we have modeled the interaction between Callisto and Jupiter's magnetosphere for variable ambient plasma parameters. We compared the results with the magnetometer data from flybys (C3, C9, and C10) by the Galileo spacecraft. Modeling the interaction between Callisto and Jupiter's magnetosphere is important to establish the origin of the magnetic field perturbations observed by Galileo and thought to be related to a subsurface ocean. Using typical upstream magnetospheric plasma parameters and a magnetic dipole corresponding to the inductive response inside the moon, we show that the model results agree well with observations for the C3 and C9 flybys, but agrees poorly with the C10 flyby close to Callisto. The study does support the existence of a subsurface ocean at Callisto.
C1 [Lindkvist, Jesper; Holmstrom, Mats; Barabash, Stas] Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
[Lindkvist, Jesper] Umea Univ, Dept Phys, Umea, Sweden.
[Khurana, Krishan K.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Fatemi, Shahab] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fatemi, Shahab] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
RP Lindkvist, J (reprint author), Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
EM jesper@irf.se
OI Holmstrom, Mats/0000-0001-5494-5374
FU Swedish National Space Board (SNSB)
FX This research was conducted using resources provided by the Swedish
National Infrastructure for Computing (SNIC) at the High Performance
Computing Center North (HPC2N), Umea University, Sweden. The software
used in this work was in part developed by the DOE NNSA-ASC OASCR Flash
Center at the University of Chicago. The hybrid solver is part of the
openly available FLASH code and can be downloaded from
http://flash.uchicago.edu/. The simulation results are available from
the corresponding author on request. MAG data from the Galileo orbiter
is publicly available via the NASA Planetary Data System (PDS) archive.
Jesper Lindkvist is funded by the Swedish National Space Board (SNSB).
NR 19
TC 8
Z9 8
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN
PY 2015
VL 120
IS 6
BP 4877
EP 4889
DI 10.1002/2015JA021212
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100059
ER
PT J
AU Connor, HK
Raeder, J
Sibeck, DG
Trattner, KJ
AF Connor, H. K.
Raeder, J.
Sibeck, D. G.
Trattner, K. J.
TI Relation between cusp ion structures and dayside reconnection for four
IMF clock angles: OpenGGCM-LTPT results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE cusp ion dispersions; dayside reconnection; MHD simulation; test
particle simulation
ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE RECONNECTION; MAGNETOSPHERIC
CUSPS; MIDALTITUDE CUSP; PRECIPITATION; SIMULATIONS; CONVECTION; MODEL
AB When, where, and which type of reconnection (antiparallel or component) happens on the dayside magnetopause are long-standing unsolved questions due to insufficient in situ observation of reconnection sites. Previous studies showed that the dispersed ion signatures observed in the magnetospheric cusps depend on the reconnection mechanism, suggesting that cusp ion signatures can be a good tool to investigate the locations and properties of dayside reconnection. We investigate this close relation between cusp signatures and magnetopause reconnection for four different interplanetary magnetic field (IMF) clock angles (CA) using the Open Global Geospace Circulation Model (OpenGGCM) and the Liouville Theorem Particle Tracer(LTPT). OpenGGCM produces dayside reconnection under the resistive MHD theory, and LTPT calculates cusp ion signatures caused by the simulated reconnection. Our model results show that for CA = 0 degrees, antiparallel reconnection at both the northern and southern lobes causes a reverse dispersion in which ion energies increase with increasing latitude. For CA = 60 degrees, unsteady antiparallel reconnection at both the northern and southern lobes causes double reverse dispersions. For CA = 120 degrees, component reconnection near the subsolar point produces a dispersionless signature in the low-latitude cusp, and antiparallel reconnection on the duskside northern magnetopause produces a normal dispersion in the high-latitude cusp in which ion energies decrease with increasing latitude. For CA = 180 degrees, antiparallel reconnection near the subsolar point causes a normal dispersion.
C1 [Connor, H. K.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Trattner, K. J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Connor, HK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM hyunju.k.connor@nasa.gov
FU National Aeronautics and Space Administration [NNX10AL07G]; NSF MRI
program [PHY-1229408]
FX The simulation data of this paper are available upon request. This work
was supported by grant NNX10AL07G from the National Aeronautics and
Space Administration, and an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. Computations were
performed on Trillian, a Cray XE6m-200 super-computer at UNH supported
by the NSF MRI program under grant PHY-1229408.
NR 38
TC 1
Z9 1
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 JUN
PY 2015
VL 120
IS 6
BP 4890
EP 4906
DI 10.1002/2015JA021156
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN1RZ
UT WOS:000358199100060
ER
PT J
AU Qian, XS
Wu, S
Furman, E
Zhang, QM
Su, J
AF Qian, Xiaoshi
Wu, Shan
Furman, Eugene
Zhang, Q. M.
Su, Ji
TI Ferroelectric polymers as multifunctional electroactive materials:
recent advances, potential, and challenges
SO MRS COMMUNICATIONS
LA English
DT Article
ID POLY(VINYLIDENE FLUORIDE-TRIFLUOROETHYLENE) COPOLYMER;
HIGH-DIELECTRIC-CONSTANT; ENHANCED ENERGY-STORAGE; ELECTROCALORIC
REFRIGERATION; ELECTROMECHANICAL PROPERTIES; VINYLIDENE FLUORIDE;
ROOM-TEMPERATURE; WORKING BODY; BEHAVIOR; NANOCOMPOSITES
AB As multifunctional electroactive materials, ferroelectric polymers are unique owing to their exceptionally high dielectric strength (>600 MV/m), high flexibility, and easy and low-temperature fabrication into required shapes. Although polyvinylidene difluoride (PVDF)-based ferroelectric polymers have been known for several decades, recent findings reveal the potential of this class of electroactive polymers (EAPs) to achieve giant electroactive responses by tuning the molecular, nano, and meso-structures. This paper presents these advances, including giant electrocaloric effect, giant electroactuation, and large, hysteresis-free polarization response. New developments in materials benefit applications, such as environmentally benign and potentially highly energy-efficient electrical field controlled solid-state refrigeration, artificial muscles, and high-energy and power density electric energy storage devices. The challenges in developing these materials to realize these applications, and strategies to further improve the responses of EAPs will be also discussed.
C1 [Qian, Xiaoshi; Wu, Shan; Furman, Eugene; Zhang, Q. M.] Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA.
[Qian, Xiaoshi; Wu, Shan; Furman, Eugene; Zhang, Q. M.] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA.
[Su, Ji] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Qian, XS (reprint author), Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA.
EM xyq5004@psu.edu; qxz1@psu.edu
FU U.S. DoE, Office of Basic Energy Sciences, Division of Materials Science
and Engineering [DE-FG02-07ER46410]; Office of Naval Research
[N00014-14-1-0109]
FX The research of ECE in modified ferroelectric PVDF-based polymers was
supported by U.S. DoE, Office of Basic Energy Sciences, Division of
Materials Science and Engineering under Award No. DE-FG02-07ER46410. The
research of PVDF based polymers for capacitor application was supported
by the Office of Naval Research, under grant No. N00014-14-1-0109.
NR 118
TC 1
Z9 1
U1 9
U2 44
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 2159-6859
EI 2159-6867
J9 MRS COMMUN
JI MRS Commun.
PD JUN
PY 2015
VL 5
IS 2
BP 115
EP 129
DI 10.1557/mrc.2015.20
PG 15
WC Materials Science, Multidisciplinary
SC Materials Science
GA CN1AK
UT WOS:000358147300003
ER
PT J
AU AghaKouchak, A
Farahmand, A
Melton, FS
Teixeira, J
Anderson, MC
Wardlow, BD
Hain, CR
AF AghaKouchak, A.
Farahmand, A.
Melton, F. S.
Teixeira, J.
Anderson, M. C.
Wardlow, B. D.
Hain, C. R.
TI Remote sensing of drought: Progress, challenges and opportunities
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
DE drought; remote sensing
ID LAND-SURFACE TEMPERATURE; SNOW WATER EQUIVALENT; MONITORING
METEOROLOGICAL DROUGHT; POLARIZATION DIFFERENCE INDEX; VEGETATION
CONDITION INDEX; PASSIVE MICROWAVE SENSORS; NINO SOUTHERN-OSCILLATION;
EUCALYPTUS-MACULATA HOOK; AMAZON RAIN-FORESTS; SOIL-MOISTURE INDEX
AB This review surveys current and emerging drought monitoring approaches using satellite remote sensing observations from climatological and ecosystem perspectives. We argue that satellite observations not currently used for operational drought monitoring, such as near-surface air relative humidity data from the Atmospheric Infrared Sounder mission, provide opportunities to improve early drought warning. Current and future satellite missions offer opportunities to develop composite and multi-indicator drought models. While there are immense opportunities, there are major challenges including data continuity, unquantified uncertainty, sensor changes, and community acceptability. One of the major limitations of many of the currently available satellite observations is their short length of record. A number of relevant satellite missions and sensors (e.g., the Gravity Recovery and Climate Experiment) provide only a decade of data, which may not be sufficient to study droughts from a climate perspective. However, they still provide valuable information about relevant hydrologic and ecological processes linked to this natural hazard. Therefore, there is a need for models and algorithms that combine multiple data sets and/or assimilate satellite observations into model simulations to generate long-term climate data records. Finally, the study identifies a major gap in indicators for describing drought impacts on the carbon and nitrogen cycle, which are fundamental to assessing drought impacts on ecosystems.
C1 [AghaKouchak, A.; Farahmand, A.] Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA.
[Melton, F. S.] NASA Ames Res Ctr Cooperat Res Earth Sci & Techno, Moffett Field, CA USA.
[Teixeira, J.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Anderson, M. C.] ARS, USDA, Beltsville, MD USA.
[Wardlow, B. D.] Univ Nebraska, Sch Nat Resources, Lincoln, NE USA.
[Hain, C. R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP AghaKouchak, A (reprint author), Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA.
EM amir.a@uci.edu
RI Anderson, Martha/C-1720-2015
OI Anderson, Martha/0000-0003-0748-5525
FU National Aeronautics and Space Administration (NASA) [NNX15AC27G]
FX This study is supported by the National Aeronautics and Space
Administration (NASA) award NNX15AC27G. The input data sets and final
outputs presented in this paper are all freely available through the
Global Integrated Drought Monitoring and Prediction System (GIDMaPS;
http://drought.eng.uci.edu/), and the NOAA/NIDIS Global Vegetation
Health data (http://www.star.nesdis.noaa.gov/smcd/emb/vci/VH/).
NR 329
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U1 26
U2 107
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 JUN
PY 2015
VL 53
IS 2
BP 452
EP 480
DI 10.1002/2014RG000456
PG 29
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CN3JO
UT WOS:000358322200008
ER
PT J
AU Richardson, IG
von Rosenvinge, TT
Cane, HV
AF Richardson, I. G.
von Rosenvinge, T. T.
Cane, H. V.
TI The Properties of Solar Energetic Particle Event-Associated Coronal Mass
Ejections Reported in Different CME Catalogs
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections; Solar energetic particles; STEREO; SOHO
ID ASYMMETRIC CONE MODEL; PEAK INTENSITIES; AUTOMATIC DETECTION; PROTON
EVENTS; HALO CMES; CYCLE 23; EARTH; SHOCK; ACCELERATION; DEPENDENCE
AB We compare estimates of the speed and width of coronal mass ejections (CMEs) in several catalogs for the CMEs associated with similar to 200 solar energetic particle (SEP) events in 2006 - 2013 that included 25 MeV protons. The catalogs used are: CDAW, CACTUS, SEEDS, and CORIMP, all derived from observations by the LASCO coronagraphs on the SOHO spacecraft, the CACTUS catalog derived from the COR2 coronagraphs on the STEREO-A and -B spacecraft, and the DONKI catalog, which uses observations from SOHO and the STEREO spacecraft. We illustrate how, for this set of events, CME parameters can differ considerably in each catalog. The well-known correlation between CME speed and proton event intensity is shown to be similar for most catalogs, but this is largely because it is determined by a few large particle events associated with fast CMEs, and small events associated with slow CMEs. Intermediate particle events "shuffle" in position when speeds from different catalogs are used. Quadrature spacecraft CME speeds do not improve the correlation. CME widths also vary widely between catalogs, and they are influenced by plane-of-the-sky projection and how the width is inferred from the coronagraph images. The high degree of association (similar to 50 %) between the 25 MeV proton events and "full halo" (360 degrees-width) CMEs as defined in the CDAW catalog is removed when other catalogs are considered. Using CME parameters from the quadrature spacecraft, the SEP intensity is correlated with CME width, which is also correlated with CME speed.
C1 [Richardson, I. G.; von Rosenvinge, T. T.] 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.
[Cane, H. V.] Bruny Isl Radio Spectrometer, Bruny Isl, Tas, Australia.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov; tycho.t.vonrosenvinge@nasa.gov;
hcane@utas.edu.au
OI Richardson, Ian/0000-0002-3855-3634
FU NASA
FX We thank the many individuals who have contributed to the development of
the CME catalogs used in this study. The LASCO CME catalog is compiled
at the CDAW Data Center by NASA and The Catholic University of America
in cooperation with the Naval Research Laboratory. The CACTUS CME
catalog is maintained by the Solar Influences Data Analysis Center at
the Royal Observatory of Belgium. SEEDS is compiled at the Space Weather
Laboratory of George Mason University and is supported by the NASA
Living With a Star Program and NASA Applied Information Systems Research
Program. The Institute for Astronomy of the University of Hawaii
produces the CORIMP catalog. DONKI is developed at the Community
Coordinated Modeling Center, NASA Goddard Space Flight Center. SOHO is a
project of international cooperation between ESA and NASA. We thank
Leila Mays for information about the DONKI database. This work was
supported by the NASA Living With a Star Program as part of the
activities of the Focussed Science Team studying the variability of
solar energetic particle events.
NR 47
TC 2
Z9 2
U1 1
U2 8
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 JUN
PY 2015
VL 290
IS 6
BP 1741
EP 1759
DI 10.1007/s11207-015-0701-4
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM9YX
UT WOS:000358068200012
ER
PT J
AU Mays, ML
Taktakishvili, A
Pulkkinen, A
MacNeice, PJ
Rastatter, L
Odstrcil, D
Jian, LK
Richardson, IG
LaSota, JA
Zheng, Y
Kuznetsova, MM
AF Mays, M. L.
Taktakishvili, A.
Pulkkinen, A.
MacNeice, P. J.
Rastaetter, L.
Odstrcil, D.
Jian, L. K.
Richardson, I. G.
LaSota, J. A.
Zheng, Y.
Kuznetsova, M. M.
TI Ensemble Modeling of CMEs Using the WSA-ENLIL plus Cone Model
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections, modeling; Coronal mass ejections,
interplanetary; Coronal mass ejections, forecasting
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENT; 2013 APRIL 11;
SOLAR-WIND; 3-DIMENSIONAL PROPAGATION; INTERPLANETARY SHOCKS; INNER
HELIOSPHERE; WHITE-LIGHT; FORECASTS; EVOLUTION
AB Ensemble modeling of coronal mass ejections (CMEs) provides a probabilistic forecast of CME arrival time that includes an estimation of arrival-time uncertainty from the spread and distribution of predictions and forecast confidence in the likelihood of CME arrival. The real-time ensemble modeling of CME propagation uses the Wang-Sheeley-Arge (WSA)-ENLIL+Cone model installed at the Community Coordinated Modeling Center (CCMC) and executed in real-time at the CCMC/Space Weather Research Center. The current implementation of this ensemble-modeling method evaluates the sensitivity of WSA-ENLIL+Cone model simulations of CME propagation to initial CME parameters. We discuss the results of real-time ensemble simulations for a total of 35 CME events that occurred between January 2013 -aEuro parts per thousand July 2014. For the 17 events where the CME was predicted to arrive at Earth, the mean absolute arrival-time prediction error was 12.3 hours, which is comparable to the errors reported in other studies. For predictions of CME arrival at Earth, the correct-rejection rate is 62 %, the false-alarm rate is 38 %, the correct-alarm ratio is 77 %, and the false-alarm ratio is 23 %. The arrival time was within the range of the ensemble arrival predictions for 8 out of 17 events. The Brier Score for CME arrival-predictions is 0.15 (where a score of 0 on a range of 0 to 1 is a perfect forecast), which indicates that on average, the predicted probability, or likelihood, of CME arrival is fairly accurate. The reliability of ensemble CME-arrival predictions is heavily dependent on the initial distribution of CME input parameters (e.g. speed, direction, and width), particularly the median and spread. Preliminary analysis of the probabilistic forecasts suggests undervariability, indicating that these ensembles do not sample a wide-enough spread in CME input parameters. Prediction errors can also arise from ambient-model parameters, the accuracy of the solar-wind background derived from coronal maps, or other model limitations. Finally, predictions of the K (P) geomagnetic index differ from observed values by less than one for 11 out of 17 of the ensembles and K (P) prediction errors computed from the mean predicted K (P) show a mean absolute error of 1.3.
C1 [Mays, M. L.; Taktakishvili, A.] Catholic Univ Amer, Washington, DC 20064 USA.
[Mays, M. L.; Taktakishvili, A.; Pulkkinen, A.; MacNeice, P. J.; Rastaetter, L.; Odstrcil, D.; Jian, L. K.; Zheng, Y.; Kuznetsova, M. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Jian, L. K.; Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[LaSota, J. A.] Univ Illinois, Champaign, IL USA.
RP Mays, ML (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.
EM m.leila.mays@nasa.gov
RI Jian, Lan/B-4053-2010;
OI Jian, Lan/0000-0002-6849-5527; Richardson, Ian/0000-0002-3855-3634
FU NSF [AGS 1242798, 1321493]
FX The work was carried out as a part of NASA's Game Changing Development
Program Advanced Radiation Protection Integrated Solar Energetic Proton
(ISEP) project. L.K. Jian acknowledges the support of NSF grants AGS
1242798 and 1321493. M.L. Mays thanks T. Nieves-Chinchilla and B.J.
Thompson for useful discussions. We gratefully acknowledge the
participants of the CME Arrival Time Scoreboard
(kauai.ccmc.gsfc.nasa.gov/CMEscoreboard). The ACE and Wind solar-wind
plasma and magnetic-field data were obtained at NASA's CDAWeb
(cdaweb.gsfc.nasa.gov). OMNI data were obtained from NASA's COHOWeb
(omniweb.gsfc.nasa.gov/coho). The Dst geomagnetic index was obtained
from the World Data Center for Geomagnetism in Kyoto, Japan. Estimated
real-time planetary KP indices are from NOAA and the NGDC,
and final definitive KP indices are from the Helmholtz Center
Potsdam GFZ German Research Centre for Geosciences. 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 mission of international cooperation
between the European Space Agency and NASA. The STEREO/SECCHI data are
produced by an international consortium of the NRL, LMSAL and NASA GSFC
(USA), RAL and University of Birmingham (UK), MPS (Germany), CSL
(Belgium), IOTA and IAS (France). Some figure colors are based on
ColorBrewer.org.
NR 69
TC 28
Z9 28
U1 1
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 JUN
PY 2015
VL 290
IS 6
BP 1775
EP 1814
DI 10.1007/s11207-015-0692-1
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM9YX
UT WOS:000358068200014
ER
PT J
AU Aleksi, J
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Biland, A
Blanch, O
Boller, A
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Carmona, E
Carosi, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Da Vela, P
Dazzi, F
De Angelis, A
De Caneva, G
De Lotto, B
Wilhelmi, ED
Mendez, CD
Prester, DD
Dorner, D
Doro, M
Einecke, S
Eisenacher, D
Elsaesser, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Godinovic, N
Munoz, AG
Gozzini, SR
Hadasch, D
Hanabata, Y
Hayashida, M
Herrera, J
Hildebrand, D
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kadenius, V
Kellermann, H
Knoetig, ML
Kodani, K
Konno, Y
Krause, J
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lewandowska, N
Lindfors, E
Lombardi, S
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorenz, E
Lozano, I
Makariev, M
Mallot, K
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Munar-Adrover, P
Nakajima, D
Niedzwiecki, A
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Persic, M
Moroni, PGP
Prandini, E
Puljak, I
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Rugamer, S
Saito, T
Saito, K
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schweizer, T
Sun, S
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Spanier, F
Stamatescu, V
Stamerra, A
Steinbring, T
Steinke, B
Storz, J
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Tibolla, O
Torres, DF
Toyama, T
Treves, A
Uellenbeck, M
Vogler, P
Zanin, R
Archambault, S
Archer, A
Beilicke, M
Benbow, W
Berger, K
Bird, R
Biteau, J
Buckley, JH
Bugaev, V
Cerruti, M
Chen, X
Ciupik, L
Collins-Hughes, E
Cui, W
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fortin, P
Fortson, L
Furniss, A
Galante, N
Gillanders, GH
Griffin, S
Gyuk, G
Hakansson, N
Holder, J
Johnson, CA
Kaaret, P
Kar, P
Kertzman, M
Kieda, D
Lang, MJ
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Ong, RA
Otte, AN
Perkins, JS
Pichel, A
Pohl, M
Popkow, A
Prokoph, H
Pueschel, E
Ragan, K
Reyes, LC
Reynolds, PT
Richards, GT
Roache, E
Rovero, AC
Sembroski, GH
Shahinyan, K
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Wakely, SP
Welsing, R
Wilhelm, A
Williams, DA
Buson, S
Finke, J
Villata, M
Raiteri, C
Aller, HD
Aller, MF
Cesarini, A
Chen, WP
Gurwell, MA
Jorstad, SG
Kimeridze, GN
Koptelova, E
Kurtanidze, OM
Kurtanidze, SO
Lahteenmaki, A
Larionov, VM
Larionova, EG
Lin, HC
McBreen, B
Moody, JW
Morozova, DA
Marscher, AP
Max-Moerbeck, W
Nikolashvili, MG
Perri, M
Readhead, ACS
Richards, JL
Ros, JA
Sadun, AC
Sakamoto, T
Sigua, LA
Smith, PS
Tornikoski, M
Troitsky, IS
Wehrle, AE
Jordan, B
AF Aleksi, J.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Bangale, P.
de Almeida, U. Barres
Barrio, J. A.
Gonzalez, J. Becerra
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Biland, A.
Blanch, O.
Boller, A.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carmona, E.
Carosi, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Caneva, G.
De Lotto, B.
Wilhelmi, E. de Ona
Mendez, C. Delgado
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Eisenacher, D.
Elsaesser, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Lopez, R. J. Garcia
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Godinovic, N.
Munoz, A. Gonzalez
Gozzini, S. R.
Hadasch, D.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hildebrand, D.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kadenius, V.
Kellermann, H.
Knoetig, M. L.
Kodani, K.
Konno, Y.
Krause, J.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lewandowska, N.
Lindfors, E.
Lombardi, S.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorenz, E.
Lozano, I.
Makariev, M.
Mallot, K.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Munar-Adrover, P.
Nakajima, D.
Niedzwiecki, A.
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Persic, M.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Reinthal, R.
Rhode, W.
Ribo, M.
Rico, J.
Garcia, J. Rodriguez
Rugamer, S.
Saito, T.
Saito, K.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schultz, C.
Schweizer, T.
Sun, S.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Spanier, F.
Stamatescu, V.
Stamerra, A.
Steinbring, T.
Steinke, B.
Storz, J.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Tibolla, O.
Torres, D. F.
Toyama, T.
Treves, A.
Uellenbeck, M.
Vogler, P.
Zanin, R.
Archambault, S.
Archer, A.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Biteau, J.
Buckley, J. H.
Bugaev, V.
Cerruti, M.
Chen, X.
Ciupik, L.
Collins-Hughes, E.
Cui, W.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fortin, P.
Fortson, L.
Furniss, A.
Galante, N.
Gillanders, G. H.
Griffin, S.
Gyuk, G.
Hakansson, N.
Holder, J.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kertzman, M.
Kieda, D.
Lang, M. J.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Ong, R. A.
Otte, A. N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Popkow, A.
Prokoph, H.
Pueschel, E.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Rovero, A. C.
Sembroski, G. H.
Shahinyan, K.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Wakely, S. P.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Buson, S.
Finke, J.
Villata, M.
Raiteri, C.
Aller, H. D.
Aller, M. F.
Cesarini, A.
Chen, W. P.
Gurwell, M. A.
Jorstad, S. G.
Kimeridze, G. N.
Koptelova, E.
Kurtanidze, O. M.
Kurtanidze, S. O.
Lahteenmaki, A.
Larionov, V. M.
Larionova, E. G.
Lin, H. C.
McBreen, B.
Moody, J. W.
Morozova, D. A.
Marscher, A. P.
Max-Moerbeck, W.
Nikolashvili, M. G.
Perri, M.
Readhead, A. C. S.
Richards, J. L.
Ros, J. A.
Sadun, A. C.
Sakamoto, T.
Sigua, L. A.
Smith, P. S.
Tornikoski, M.
Troitsky, I. S.
Wehrle, A. E.
Jordan, B.
CA MAGIC Collaboration
VERITAS Collaboration
TI Unprecedented study of the broadband emission of Mrk 421 during flaring
activity in March 2010
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae
objects: individual: Mrk 421; gamma rays: galaxies
ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; GAMMA-RAY OUTBURST;
SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ATMOSPHERIC CHERENKOV
TELESCOPES; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRAL
ENERGY-DISTRIBUTION; SELF-COMPTON MODEL; X-RAY; TEV BLAZARS
AB Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED).
Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail.
Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population.
Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2-10 keV band and the VHE gamma-ray flux above 200 GeV, consistent with the gamma-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE gamma-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 x 10(4) < gamma < 6 x 10(5), where. is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands.
Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low-and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (delta, B and R), in addition to the parameters related to the particle population.
C1 [Aleksi, J.; Blanch, O.; Cortina, J.; Munoz, A. Gonzalez; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Stamatescu, V.] Campus UAB, IFAE, Bellaterra 08193, Spain.
[Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Ist Nazl Fis Nucl, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Zagreb 10000, Croatia.
[Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hose, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Noda, K.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Sun, S.; Steinke, B.; Strzys, M.; Teshima, M.; Toyama, T.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, Madrid 28040, Spain.
[Gonzalez, J. Becerra; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Tescaro, D.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; De Caneva, G.; Garczarczyk, M.; Gozzini, S. R.; Hughes, G.; Mallot, K.; Chen, X.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Boller, A.; Hildebrand, D.; Knoetig, M. L.; Prandini, E.; Vogler, P.] ETH, CH-8093 Zurich, Switzerland.
[Bretz, T.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Rugamer, S.; Spanier, F.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Carmona, E.; Mendez, C. Delgado] CIEMAT, E-28040 Madrid, Spain.
[Wilhelmi, E. de Ona; Hadasch, D.] Inst Space Sci, Barcelona 08193, Spain.
[Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.; Buson, S.] Univ Padua, I-35131 Padua, Italy.
[Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.; Buson, S.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
[Galindo, D.; Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kashiwa, Chiba 2778582, Japan.
[Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland.
[Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, Oulu 90014, Finland.
[Makariev, M.; Maneva, G.; Temnikov, P.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, Barcelona 08193, Spain.
[Torres, D. F.] Inst Space Sci, Barcelona 08193, Spain.
[Treves, A.] Univ Insubria, I-22100 Como, Italy.
[Treves, A.] INFN Milano Bicocca, I-22100 Como, Italy.
[Gonzalez, J. Becerra; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra; Perkins, J. S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra; Perkins, J. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Archambault, S.; Griffin, S.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Collins-Hughes, E.; Pueschel, E.; McBreen, B.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Ciupik, L.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.; Richards, J. L.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Eisch, J. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McArthur, S.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Finke, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Villata, M.; Raiteri, C.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Cesarini, A.] Univ Trent, Dept Phys, I-38050 Trento, Italy.
[Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Jorstad, S. G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Koptelova, E.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Kurtanidze, O. M.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany.
[Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland.
[Larionov, V. M.; Larionova, E. G.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Peetersburg 198504, Russia.
[Larionov, V. M.] Pulkovo Observ, St Petersburg 198504, Russia.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Moody, J. W.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
[Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Perri, M.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Ros, J. A.] Agrp Astron Sabadell, Sabadell Barcelona 08206, Spain.
[Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO 80217 USA.
[Sakamoto, T.] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan.
[Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
RP Paneque, D (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
EM dpaneque@mpp.mpg.de; sysun@mpp.mpg.de; takami@post.kek.jp
RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Temnikov,
Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev,
Martin/M-2122-2016; Torres, Diego/O-9422-2016; Delgado,
Carlos/K-7587-2014; Barrio, Juan/L-3227-2014; Martinez Rodriguez,
Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Lahteenmaki,
Anne/L-5987-2013; Larionov, Valeri/H-1349-2013; Font, Lluis/L-4197-2014;
Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya,
Marcos/L-2304-2014; Morozova, Daria/H-1298-2013; Larionova,
Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad,
Svetlana/H-6913-2013; GAug, Markus/L-2340-2014; Miranda, Jose
Miguel/F-2913-2013; Stamatescu, Victor/C-9945-2016
OI Bonnoli, Giacomo/0000-0003-2464-9077; Antonelli, Lucio
Angelo/0000-0002-5037-9034; Stamerra, Antonio/0000-0002-9430-5264;
Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez,
Josefa/0000-0002-6729-9022; Bird, Ralph/0000-0002-4596-8563; Doro,
Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507; de Ona
Wilhelmi, Emma/0000-0002-5401-0744; LA BARBERA,
ANTONINO/0000-0002-5880-8913; Cesarini, Andrea/0000-0002-8611-8610;
Villata, Massimo/0000-0003-1743-6946; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480;
Perri, Matteo/0000-0003-3613-4409; Persic, Massimo/0000-0003-1853-4900;
Raiteri, Claudia Maria/0000-0003-1784-2784; Temnikov,
Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Delgado,
Carlos/0000-0002-7014-4101; Barrio, Juan/0000-0002-0965-0259; Cortina,
Juan/0000-0003-4576-0452; Pueschel, Elisa/0000-0002-0529-1973; Prada
Moroni, Pier Giorgio/0000-0001-9712-9916; Larionov,
Valeri/0000-0002-4640-4356; Font, Lluis/0000-0003-2109-5961; Contreras
Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya,
Marcos/0000-0002-8791-7908; Morozova, Daria/0000-0002-9407-7804;
Larionova, Elena/0000-0002-2471-6500; Troitskiy,
Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; GAug,
Markus/0000-0001-8442-7877; Miranda, Jose Miguel/0000-0002-1472-9690;
Stamatescu, Victor/0000-0001-9030-7513
FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund
SNF; ERDF under the Spanish MINECO; Japanese JSPS; Japanese MEXT; Centro
de Excelencia Severo Ochoa project of the Spanish Consolider-Ingenio
programme [SEV-2012-0234]; CPAN project of the Spanish
Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the
Spanish Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland
[268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ)
Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG Collaborative
Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW
[745/N-HESS-MAGIC/2010/0]; US Department of Energy Office of Science; US
National Science Foundation; Smithsonian Institution; NSERC in Canada;
Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA
[NNX11AQ03G, NNX08AW31G, NNX11A043G]; Academia Sinica; NSF [AST-0808050,
AST-1109911]; Russian RFBR [12-02-00452]; St. Petersburg University
[6.0.163.2010, 6.38.71.2012]; Georgian National Science Foundation
[GNSF/ST07/4-180]; Shota Rustaveli National Science Foundation
[FR/577/6-320/13]
FX The authors thank the anonymous referee for providing a very detailed
and constructive list of remarks that helped us to improve the
manuscript. The MAGIC collaboration would like to thank the Instituto de
Astrofisica de Canarias for the excellent working conditions at the
Observatorio del Roque de los Muchachos in La Palma. The financial
support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss
National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese
JSPS and MEXT is gratefully acknowledged. This work was also supported
by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN
CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish
Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of
Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and
the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative
Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant
745/N-HESS-MAGIC/2010/0. The VERITAS collaboration acknowledges supports
from the grants from the US Department of Energy Office of Science, the
US National Science Foundation and the Smithsonian Institution, by NSERC
in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by
STFC in the UK. We acknowledge the excellent work of the technical
support staff at the Fred Lawrence Whipple Observatory and at the
collaborating institutions in the construction and operation of the
instrument. The Fermi-LAT collaboration acknowledges generous ongoing
support from a number of agencies and institutes that have supported
both the development and the operation of the LAT as well as scientific
data analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. The research
at Boston University was funded in part by NASA Fermi Guest Investigator
grant NNX11AQ03G. The Submillimeter Array is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica. The OVRO 40-m monitoring program is
supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF
grants AST-0808050 and AST-1109911. The Metsahovi team acknowledges the
support from the Academy of Finland to our observing projects (numbers
212656, 210338, 121148, and others). This work was partly supported by
Russian RFBR grant 12-02-00452 and St. Petersburg University research
grants 6.0.163.2010, 6.38.71.2012. The Abastumani Observatory team
acknowledges financial support by the Georgian National Science
Foundation through grant GNSF/ST07/4-180 and by the Shota Rustaveli
National Science Foundation through the grant FR/577/6-320/13.; We
acknowledge the use of public data from the Swift and RXTE data archive.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A22
DI 10.1051/0004-6361/201424811
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600034
ER
PT J
AU Azulay, R
Guirado, JC
Marcaide, JM
Marti-Vidal, I
Ros, E
Jauncey, DL
Lestrade, JF
Preston, RA
Reynolds, JE
Tognelli, E
Ventura, P
AF Azulay, R.
Guirado, J. C.
Marcaide, J. M.
Marti-Vidal, I.
Ros, E.
Jauncey, D. L.
Lestrade, J. -F.
Preston, R. A.
Reynolds, J. E.
Tognelli, E.
Ventura, P.
TI Dynamical masses of the low-mass stellar binary AB Doradus B
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrometry; binaries: close; stars: fundamental parameters; stars:
pre-main sequence
ID MAIN-SEQUENCE TRACKS; EVOLUTIONARY MODELS; MOVING GROUP; ECLIPSING
BINARY; QUADRUPLE SYSTEM; AGE; STARS; CONSTRAINTS; PHOTOMETRY; DWARFS
AB Context. AB Doradus is the main system of the AB Doradus moving group. It is a quadruple system formed by two widely separated binaries of pre-main-sequence (PMS) stars: AB DorA/C and AB Dor Ba/Bb. The pair AB DorA/C has been extensively studied and its dynamical masses have been determined with high precision, thus making AB DorC a benchmark for calibrating PMS stellar models. If the orbit and dynamical masses of the pair AB Dor Ba/Bb could be determined, they could play a similar role to that of AB DorC in calibrating PMS models, and would also help to better understand the dynamics of the whole AB Doradus system.
Aims. We aim to determine the individual masses of the pair AB Dor Ba/Bb using VLBI observations and archive infrared data as part of a larger program that monitors binary systems in the AB Doradus moving group.
Methods. We observed the system AB Dor B between 2007 and 2013 with the Australian Long Baseline Array (LBA) at a frequency of 8.4 GHz in phase-reference mode.
Results. We detected, for the first time, compact radio emission from both stars in the binary, AB Dor Ba and AB Dor Bb. This result allowed us to determine the orbital parameters of both the relative and absolute orbits and, consequently, their individual dynamical masses: 0 : 28 +/- 0 : 05 M-circle dot and 0 : 25 +/- 0 : 05 M-circle dot, respectively.
Conclusions. Comparisons of the dynamical masses with the prediction of PMS evolutionary models show that the models under-predict the dynamical masses of the binary components Ba and Bb by 10-30% and 10-40%, respectively, although they still agree at the 2 sigma level. Some of the stellar models considered favor an age between 50 and 100 Myr for this system, while others predict older ages. We also discuss the evolutionary status of AB Dor Ba/Bb in terms of an earlier double-double star scenario that might explain the strong radio emission detected in both components.
C1 [Azulay, R.; Guirado, J. C.; Marcaide, J. M.; Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Azulay, R.; Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Guirado, J. C.; Ros, E.] Univ Valencia, Obser Astron, Valencia 46980, Spain.
[Marti-Vidal, I.] Onsala Space Observ, Chalmers Univ Technol, S-43992 Onsala, Sweden.
[Jauncey, D. L.; Reynolds, J. E.] CSIRO Astron & Space Sci, Canberra, ACT 2122, Australia.
[Jauncey, D. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 0200, Australia.
[Lestrade, J. -F.] Observ Paris LERMA, F-75014 Paris, France.
[Preston, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tognelli, E.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy.
[Tognelli, E.] INFN, Sect Pisa, I-56127 Pisa, Italy.
[Ventura, P.] INAF Observ Rome, I-00040 Monte Porzio Catone, RM, Italy.
RP Azulay, R (reprint author), Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, E-46100 Valencia, Spain.
EM Rebecca.Azulay@uv.es
RI Marti-Vidal, Ivan/A-8799-2017;
OI Marti-Vidal, Ivan/0000-0003-3708-9611; Ventura,
Paolo/0000-0002-5026-6400; Ros, Eduardo/0000-0001-9503-4892
FU Spanish MINECO [AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat
Valenciana [PROMETEO/2009/104, PROMETEOII/2014/057]; Commonwealth of
Australia
FX This work has been partially supported by the Spanish MINECO projects
AYA2009-13036-C02-02 and AYA2012-38491-C02-01 and by the Generalitat
Valenciana projects PROMETEO/2009/104 and PROMETEOII/2014/057. The 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. We thank J. Montalban for providing
the PMS models and for the guidance to use them appropriately. The data
used in this study were acquired as part of NASA's Earth Science Data
Systems and archived and distributed by the Crustal Dynamics Data
Information System (CDDIS). This research has made use of the SIMBAD
database, operated at CDS, Strasbourg, France. R.A. acknowledges the
Max-Planck-Institute fur Radioastronomie for its hospitality and
especially J. A. Zensus for support.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A16
DI 10.1051/0004-6361/201525704
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600028
ER
PT J
AU Benisty, M
Juhasz, A
Boccaletti, A
Avenhaus, H
Milli, J
Thalmann, C
Dominik, C
Pinilla, P
Buenzli, E
Pohl, A
Beuzit, JL
Birnstiel, T
de Boer, J
Bonnefoy, M
Chauvin, G
Christiaens, V
Garufi, A
Grady, C
Henning, T
Huelamo, N
Isella, A
Langlois, M
Menard, F
Mouillet, D
Olofsson, J
Pantin, E
Pinte, C
Pueyo, L
AF Benisty, M.
Juhasz, A.
Boccaletti, A.
Avenhaus, H.
Milli, J.
Thalmann, C.
Dominik, C.
Pinilla, P.
Buenzli, E.
Pohl, A.
Beuzit, J. -L.
Birnstiel, T.
de Boer, J.
Bonnefoy, M.
Chauvin, G.
Christiaens, V.
Garufi, A.
Grady, C.
Henning, T.
Huelamo, N.
Isella, A.
Langlois, M.
Menard, F.
Mouillet, D.
Olofsson, J.
Pantin, E.
Pinte, C.
Pueyo, L.
TI Asymmetric features in the protoplanetary disk MWC 758
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: high angular resolution; protoplanetary disks
ID HD 142527; IMAGING POLARIMETRY; TRANSITIONAL DISKS; DUST FILTRATION;
SPIRAL ARMS; GAP EDGES; PLANET; EVOLUTION; VLT/NACO; MWC-758
AB Context. The study of dynamical processes in protoplanetary disks is essential to understand planet formation. In this context, transition disks are prime targets because they are at an advanced stage of disk clearing and may harbor direct signatures of disk evolution.
Aims. We aim to derive new constraints on the structure of the transition disk MWC 758, to detect non-axisymmetric features and understand their origin.
Methods. We obtained infrared polarized intensity observations of the protoplanetary disk MWC 758 with VLT/SPHERE at 1.04 mu m to resolve scattered light at a smaller inner working angle (0.093 '') and a higher angular resolution (0.027 '') than previously achieved.
Results. We observe polarized scattered light within 0.53 '' (148 au) down to the inner working angle (26 au) and detect distinct non-axisymmetric features but no fully depleted cavity. The two small-scale spiral features that were previously detected with HiCIAO are resolved more clearly, and new features are identified, including two that are located at previously inaccessible radii close to the star. We present a model based on the spiral density wave theory with two planetary companions in circular orbits. The best model requires a high disk aspect ratio (H/r similar to 0.20 at the planet locations) to account for the large pitch angles which implies a very warm disk.
Conclusions. Our observations reveal the complex morphology of the disk MWC 758. To understand the origin of the detected features, the combination of high-resolution observations in the submillimeter with ALMA and detailed modeling is needed.
C1 [Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] CNRS, IPAG, F-38000 Grenoble, France.
[Juhasz, A.] Inst Astron, Cambridge CB3 OHA, England.
[Boccaletti, A.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Avenhaus, H.; Christiaens, V.] Univ Chile, Dept Astron, Santiago, Chile.
[Milli, J.; de Boer, J.] ESO, Santiago, Chile.
[Thalmann, C.; Garufi, A.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Dominik, C.] Sterrenkundig Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Pinilla, P.; de Boer, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Buenzli, E.; Pohl, A.; Henning, T.; Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Pohl, A.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Grady, C.] Eureka Sci, Greenbelt, MD 20771 USA.
[Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Huelamo, N.] Ctr Astrobiol INTA CSIC, Villanueva De La Canada 28691, Spain.
[Isella, A.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Langlois, M.] Univ Lyon 1, CNRS, Ecole Normale Super Lyon, Observ Lyon,Ctr Rech Astrophys Lyon,UMR 5574, F-69230 St Genis Laval, France.
[Menard, F.; Pinte, C.] Univ Chile, CNRS INSU, UMI FCA, France UMI 3386, Santiago, Chile.
[Menard, F.; Pinte, C.] Univ Chile, Dept Astron, Santiago, Chile.
[Pantin, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU SAp, F-91191 Gif Sur Yvette, France.
[Pueyo, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Benisty, M (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
EM Myriam.Benisty@obs.ujf-grenoble.fr
RI Huelamo, Nuria/C-3042-2017;
OI Huelamo, Nuria/0000-0002-2711-8143; Buenzli, Esther/0000-0003-3306-1486;
Birnstiel, Tilman/0000-0002-1899-8783
FU "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France;
NASA Origins of Solar Systems program [NNG13PB64P]; NASA Origins of
Solar Systems [NNX12AJ04G]
FX We acknowledge the SVT team at ESO HQ for their help during the
preparation of the OBs and the VLT team for conducting the observations.
We thank C. P. Dullemond, G. Lesur, M. Min, and M. Tauras for fruitful
discussions, and the referee for providing useful comments. M.B.
acknowledges financial support from "Programme National de Physique
Stellaire" (PNPS) of CNRS/INSU, France. C.G. was supported under the
NASA Origins of Solar Systems program on NNG13PB64P. T.B. acknowledges
support from NASA Origins of Solar Systems grant NNX12AJ04G.
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SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR L6
DI 10.1051/0004-6361/201526011
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600007
ER
PT J
AU Couturier-Tamburelli, I
Pietri, N
Gudipati, MS
AF Couturier-Tamburelli, Isabelle
Pietri, Nathalie
Gudipati, Murthy S.
TI Simulation of Titan's atmospheric photochemistry Formation of
non-volatile residue from polar nitrile ices
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: surfaces; ultraviolet: planetary systems;
astrochemistry; planets and satellites: atmospheres
ID ELECTRONICALLY EXCITED-STATES; OPTICAL-CONSTANTS; ABSORPTION-SPECTRA;
AEROSOLS ANALOGS; ACETYLENE; CHEMISTRY; THOLINS; HAZE; MOLECULES; HC5N
AB We studied the photochemistry of frozen ice of a polar Titan's atmospheric molecule cyanodiacetylene (HC5N) to determine the possible contribution of this compound to the lower altitude photochemistry of haze layers found on Titan. We used infrared analysis to examine the residue produced by irradiation of solid HC5N at lambda > 300 nm. The resulting polymer is orange-brown in color. Based on theoretical analysis and the general tendency of HC5N and C4N2 to undergo similar ice photochemistry at longer wavelengths accessible in Titan's lower atmosphere, we conclude that Titan's lower atmosphere is photochemically active in the regions of cloud, ice, and aerosol formation. C4N2 is a symmetric molecule with no net dipole moment whereas, HC5N has a large dipole moment of similar to 4 D. Consequently, though both these molecules have very similar molecular weight and size, their sublimation temperatures are different, HC5N subliming around 170K compared to 160K for C4N2. Based on our studies we conclude that in Titan's atmosphere the cyanoacetylene class of molecules (HCN, HC3N, HC5N, etc.) would condense first followed by the dicyanoacetylenes (C2N2, C4N2, C6N2, etc.), leading to fractionation of different class of molecules. From the fluxes used in the laboratory and depletion of the original HC5N signals, we estimate Titan's haze ice photochemistry involving polar nitriles to be significant and very similar to their non-polar counterparts.
C1 [Couturier-Tamburelli, Isabelle; Pietri, Nathalie] Aix Marseille Univ, CNRS, UMR 7345, PIIM, F-13013 Marseille, France.
[Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Ice Spect Lab, Div Sci, Pasadena, CA 91109 USA.
RP Couturier-Tamburelli, I (reprint author), Aix Marseille Univ, CNRS, UMR 7345, PIIM, F-13013 Marseille, France.
EM isabelle.couturier@univ-amu.fr; gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011
FU French National Program Environnements Planetaires et Origines de la Vie
(EPOV); NASA Astrobiology Institute; Jet Propulsion Laboratory
Director's Research and Development Fund; JPL Research and Technology
Development funding for the infrastructure of the ice spectroscopy
laboratory (ISL); Titan organic aerosol spectroscopy and chemistry
(TOAST) laboratory at JPL; National Aeronautics and Space Administration
FX This work was funded by the French National Program Environnements
Planetaires et Origines de la Vie (EPOV). The JPL part of the work is
partly supported by several of the following funding sources: NASA
Astrobiology Institute team "Titan as a Prebiotic Chemical System", the
Jet Propulsion Laboratory Director's Research and Development Fund, and
the JPL Research and Technology Development funding for the
infrastructure of the ice spectroscopy laboratory (ISL) and Titan
organic aerosol spectroscopy and chemistry (TOAST) laboratory at JPL.
Research carried out at the Jet Propulsion Laboratory, California
Institute of Technology was under a contract with the National
Aeronautics and Space Administration. We thank Mr. Tim Hempel for
helping in preparing the manuscript to be suitable for the A&A format.
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JI Astron. Astrophys.
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PY 2015
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SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600123
ER
PT J
AU Hoyer, D
Rauch, T
Werner, K
Hauschildt, PH
Kruk, JW
AF Hoyer, D.
Rauch, T.
Werner, K.
Hauschildt, P. H.
Kruk, J. W.
TI Search with UVES and X-Shooter for signatures of the low-mass secondary
in the post common-envelope binary AA Doradus
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; binaries: eclipsing; stars: low-mass; stars:
individual: AA Dor; virtual observatory tools
ID WHITE-DWARFS G191-B2B; BALMER LINE PROBLEM; HOT SUBDWARF STARS; SDOB
PRIMARY; STELLAR LABORATORIES; OSCILLATOR-STRENGTHS; BROWN DWARF; LB
3459; ELEMENTAL COMPOSITION; RE 0503-289
AB Context. AA Dor is a close, totally eclipsing, post common-envelope binary with an sdOB-type primary star and an extremely low-mass secondary star, located close to the mass limit of stable central hydrogen burning. Within error limits, it may either be a brown dwarf or a late M-type dwarf.
Aims. We aim to extract the secondary's contribution to the phase-dependent composite spectra. The spectrum and identified lines of the secondary decide on its nature.
Methods. In January 2014, we measured the phase-dependent spectrum of AA Dor with X-Shooter over one complete orbital period. Since the secondary's rotation is presumable synchronized with the orbital period, its surface strictly divides into a day and night side. Therefore, we may obtain the spectrum of its cool side during its transit and of its hot, irradiated side close to its occultation. We developed the Virtual Observatory (VO) tool TLISA to search for weak lines of a faint companion in a binary system. We successfully applied it to the observations of AA Dor.
Results. We identified 53 spectral lines of the secondary in the ultraviolet-blue, visual, and near-infrared X-Shooter spectra that are strongest close to its occultation. We identified 57 (20 additional) lines in available Ultraviolet and Visual Echelle Spectrograph (UVES) spectra from 2001. The lines are mostly from CII-III and OII, typical for a low-mass star that is irradiated and heated by the primary. We verified the orbital period of P = 22 597.033201 +/- 0.00007 s and determined the orbital velocity K-sec = 232.9(-6.5)(+16.6) km s(-1) of the secondary. The mass of the secondary is M-sec = 0.081(-0.010)(+0.018) M-circle dot and, hence, it is not possible to reliably determine a brown dwarf or an M-type dwarf nature.
Conclusions. Although we identified many emission lines of the secondary's irradiated surface, the resolution and signal-to-noise ratio of our UVES and X-Shooter spectra are not good enough to extract a good spectrum of the secondary's nonirradiated hemisphere.
C1 [Hoyer, D.; Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany.
[Hauschildt, P. H.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Kruk, J. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hoyer, D (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany.
EM rauch@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [50 OR 1501, 05 OR 1402]; Federal Ministry
of Education and Research (BMBF) [05 AC 6VTB, 05 AC 11VTB]; ESO Service
[066.D-1800, 092.C-0692]; NASA [NAS5-26555]; NASA Office of Space
Science [NNX09AF08G]
FX D.H. and T.R. are supported by the German Aerospace Center (DLR, grants
50 OR 1501 and 05 OR 1402, respectively). The GAVO project at Tubingen
was supported by the Federal Ministry of Education and Research (BMBF,
grants 05 AC 6VTB, 05 AC 11VTB). The TLISA tool
(http://astro.uni-tuebingen.de/similar to TLISA) used for this paper was
constructed as part of the activities of the German Astrophysical
Virtual Observatory. The UVES and X-Shooter spectra used in this
analysis were obtained as parts of ESO Service Mode runs, programs
066.D-1800 and 092.C-0692, respectively. We thank David Kilkenny for his
help in determining the exact time of the secondary's occultation during
our X-Shooter observations, Roger Wesson who had performed these
observations and successfully covered this critical time, and Travis
Barman who put the irradiated spectrum of the secondary at our disposal.
Some of the data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts. This research has made use of NASA's Astrophysics
Data System and the SIMBAD database, operated at CDS, Strasbourg,
France.
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SN 0004-6361
EI 1432-0746
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JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A125
DI 10.1051/0004-6361/201526229
PG 26
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SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600137
ER
PT J
AU Kennedy, MB
Milligan, RO
Allred, JC
Mathioudakis, M
Keenan, FP
AF Kennedy, Michael B.
Milligan, Ryan O.
Allred, Joel C.
Mathioudakis, Mihalis
Keenan, Francis P.
TI Radiative hydrodynamic modelling and observations of the X-class solar
flare on 2011 March 9
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: atmosphere; Sun: chromosphere; Sun: flares; Sun: X-rays, gamma rays
ID WHITE-LIGHT FLARES; NONTHERMAL ELECTRONS; IMPULSIVE PHASE; ULTRAVIOLET
OBSERVATIONS; SPECTROSCOPIC-IMAGER; CHROMOSPHERIC FLARES; EMISSION
MEASURES; ATOMIC DATABASE; SOURCE SIZES; RAY
AB Aims. We investigated the response of the solar atmosphere to non-thermal electron beam heating using the radiative transfer and hydrodynamics modelling code RADYN. The temporal evolution of the parameters that describe the non-thermal electron energy distribution were derived from hard X-ray observations of a particular flare, and we compared the modelled and observed parameters.
Methods. The evolution of the non-thermal electron beam parameters during the X1.5 solar flare on 2011 March 9 were obtained from analysis of RHESSI X-ray spectra. The RADYN flare model was allowed to evolve for 110 s, after which the electron beam heating was ended, and was then allowed to continue evolving for a further 300 s. The modelled flare parameters were compared to the observed parameters determined from extreme-ultraviolet spectroscopy.
Results. The model produced a hotter and denser flare loop than that observed and also cooled more rapidly, suggesting that additional energy input in the decay phase of the flare is required. In the explosive evaporation phase a region of high-density cool material propagated upward through the corona. This material underwent a rapid increase in temperature as it was unable to radiate away all of the energy deposited across it by the non-thermal electron beam and via thermal conduction. A narrow and high-density (n(e) <= 10(15) cm(-3)) region at the base of the flare transition region was the source of optical line emission in the model atmosphere. The collision-stopping depth of electrons was calculated throughout the evolution of the flare, and it was found that the compression of the lower atmosphere may permit electrons to penetrate farther into a flaring atmosphere compared to a quiet Sun atmosphere.
C1 [Kennedy, Michael B.; 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.; Allred, Joel C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Kennedy, MB (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
EM mkennedy29@qub.ac.uk
FU Northern Ireland Department of Employment and Learning; International
Space Science Institute; Leverhulme Trust [F/00203/X]; NASA [NNX11AQ53G,
NNX14AE07G]; UK STFC; European Community [606862]
FX M.B.K. thanks the Northern Ireland Department of Employment and Learning
for the award of a Ph.D. studentship and acknowledges support from the
International Space Science Institute to attend a team meeting led by L.
Fletcher on "Observations and Modelling of Flare Chromospheres", where
helpful discussions regarding the manuscript took place. 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. M.M. and F.P.K. acknowledge financial support
from the UK STFC. 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). CHIANTI is
a collaborative project involving George Mason University, the
University of Michigan (USA) and the University of Cambridge (UK). Data
are provided courtesy of NASA/SDO and RHESSI, and the EVE, HMI, and
RHESSI science teams. This research has made use of NASA's Astrophysics
Data System. We thank the anonymous referee for their comments that
helped to improve the quality and clarity of the manuscript.
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JI Astron. Astrophys.
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PY 2015
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DI 10.1051/0004-6361/201425144
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SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600084
ER
PT J
AU Maneva, YG
Ofman, L
Vinas, A
AF Maneva, Y. G.
Ofman, L.
Vinas, A.
TI Relative drifts and temperature anisotropies of protons and alpha
particles in the expanding solar wind: 2.5D hybrid simulations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE solar wind; plasmas; turbulence; waves; instabilities; acceleration of
particles
ID ALFVEN-CYCLOTRON WAVES; DIFFERENTIAL FLOW; ALFVEN/CYCLOTRON
FLUCTUATIONS; VELOCITY DISTRIBUTIONS; ULYSSES OBSERVATIONS;
INSTABILITY-DRIVEN; HE++ IONS; PLASMA; CORONA; ACCELERATION
AB Context. We perform 2.5D hybrid simulations to investigate the origin and evolution of relative drift speeds between protons and a particles in the collisionless turbulent low-(beta) over tilde $ solar wind plasma.
Aims. We study the generation of differential streaming by wave-particle interactions and absorption of turbulent wave spectra. Next we focus on the role of the relative drifts for the turbulent heating and acceleration of ions in the collisionless fast solar wind streams.
Methods. The energy source is given by an initial broad-band spectrum of parallel propagating Alfven-cyclotron waves, which coexists with the plasma and is self-consistently coupled to the perpendicular ion bulk velocities. We include the effect of a gradual solar wind expansion, which cools and decelerates the minor ions. We here consider for the first time the combined effect of self-consistently initialized dispersive turbulent Alfvenic spectra with differentially streaming protons and alpha particles in the expanding solar wind outflows within a 2.5D hybrid simulation study.
Results. For differential streaming of V-ap < 0.5V(A), the selected initial wave spectrum accelerates the minor ions in the non-expanding wind. At V-ap = 0.5V(A) the relative drift speed remains nearly steady. For ions that stream below this threshold value, the waves act to increase the magnitude of the relative drift speed. Ions that stream faster than the threshold value become subject to a nonlinear streaming instability, and as the system evolves, their bulk velocities decrease. We find that the solar wind expansion strongly affects the relative drift speed and significantly slows down both ion species for all values of the relative drift speeds considered in this study. The initial nonresonant wave spectra interact with the particles, resulting in preferential and anisotropic heating for the minor ions with a prominent increase of their perpendicular temperature, which overcomes the effect of the double-adiabatic cooling that is due to the solar wind expansion. Finally, the initial parallel spectra undergo a micro-turbulent nonlinear cascade during which oblique waves are generated, whose intensity depends on the value of the relative drift speed.
C1 [Maneva, Y. G.] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, B-3001 Leuven, Belgium.
[Maneva, Y. G.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ofman, L.; Vinas, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Maneva, YG (reprint author), Katholieke Univ Leuven, Ctr Math Plasma Astrophys, B-3001 Leuven, Belgium.
EM yana.maneva@wis.kuleuven.be
FU NASA [NNX10AC56G]; F+ fellowship at KU Leuven under SOLSPANET
[269299]; ESA Prodex [C 90347]; Wind/SWE project
FX This work was supported by NASA, grant NNX10AC56G. Y. G. Maneva would
like to acknowledge the F+ fellowship at KU Leuven,
(FP7/2007-2013) under the grant agreement SOLSPANET (project 269299) and
C 90347 (ESA Prodex) for partial support. A. F. Vinas would like to
acknowledge the Wind/SWE project for partial support. Fruitful
discussions with P. Hunana are highly appreciated.
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JI Astron. Astrophys.
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PY 2015
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SC Astronomy & Astrophysics
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ER
PT J
AU Melin, JB
Bartlett, JG
AF Melin, Jean-Baptiste
Bartlett, James G.
TI Measuring cluster masses with CMB lensing: a statistical approach
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE large-scale structure of Universe; galaxies: clusters: general; cosmic
background radiation; methods: data analysis; gravitational lensing:
weak; methods: statistical
ID GALAXY CLUSTERS; X-RAY; COSMOLOGICAL CONSTRAINTS; SCALING RELATIONS;
SAMPLE; CALIBRATION; PARAMETERS; EVOLUTION; RICHNESS; VELOCITY
AB We present a method for measuring the masses of galaxy clusters using the imprint of their gravitational lensing signal on the cosmic microwave background (CMB) temperature anisotropies. The method first reconstructs the projected gravitational potential with a quadratic estimator and then applies a matched filter to extract cluster mass. The approach is well-suited for statistical analyses that bin clusters according to other mass proxies. We find that current experiments, such as Planck, the South Pole Telescope and the Atacama Cosmology Telescope, can practically implement such a statistical methodology, and that future experiments will reach sensitivities sufficient for individual measurements of massive systems. As illustration, we use simulations of Planck observations to demonstrate that it is possible to constrain the mass scale of a set of 62 massive clusters with prior information from X-ray observations, similar to the published Planck ESZ-XMM sample. We examine the effect of the thermal (tSZ) and kinetic (kSZ) Sunyaev-Zeldovich (SZ) signals, finding that the impact of the kSZ remains small in this context. The stronger tSZ signal, however, must be actively removed from the CMB maps by component separation techniques prior to reconstruction of the gravitational potential. Our study of two such methods highlights the importance of broad frequency coverage for this purpose. A companion paper presents application to the Planck data on the ESZ-XMM sample.
C1 [Melin, Jean-Baptiste] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
[Bartlett, James G.] Univ Paris Diderot, Sorbonne Paris Cite, AstroParticule & Cosmol, APC,CNRS,IN2P3,CEA,lrfu, F-75205 Paris 13, France.
[Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Melin, JB (reprint author), CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
EM jean-baptiste.melin@cea.fr
FU National Aeronautics and Space Administration
FX The authors would like to thank the anonymous referee for useful
comments which helped to clarify some important aspects of this work. A
portion of the research described in this paper was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 59
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A21
DI 10.1051/0004-6361/201424720
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600033
ER
PT J
AU Ryan, EL
Mizuno, DR
Shenoy, SS
Woodward, CE
Carey, SJ
Noriega-Crespo, A
Kraemer, KE
Price, SD
AF Ryan, E. L.
Mizuno, D. R.
Shenoy, S. S.
Woodward, C. E.
Carey, S. J.
Noriega-Crespo, A.
Kraemer, K. E.
Price, S. D.
TI The kilometer-sized Main Belt asteroid population revealed by Spitzer
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE minor planets,asteroids: general; infrared: general
ID NEAR-EARTH ASTEROIDS; DIGITAL SKY SURVEY; MULTIBAND IMAGING PHOTOMETER;
INFRARED-SURVEY-EXPLORER; INNER GALACTIC PLANE; THERMAL INERTIA; ION
IRRADIATION; OBJECTS; MAGNITUDE; DIAMETERS
AB Aims. Multi-epoch Spitzer Space Telescope 24 mu m data is utilized from the MIPSGAL and Taurus Legacy surveys to detect asteroids based on their relative motion.
Methods. Infrared detections are matched to known asteroids and average diameters and albedos are derived using the near Earth asteroid thermal model (NEATM) for 1865 asteroids ranging in size from 0.2 to 169 km. A small subsample of these objects was also detected by IRAS or MSX and the single wavelength albedo and diameter fits derived from these data are within the uncertainties of the IRAS and/or MSX derived albedos and diameters and available occultation diameters, which demonstrates the robustness of our technique.
Results. The mean geometric albedo of the small Main Belt asteroids in this sample is p(V) = 0.134 with a sample standard deviation of 0.106. The albedo distribution of this sample is far more diverse than the IRAS or MSX samples. The cumulative size-frequency distribution of asteroids in the Main Belt at small diameters is directly derived and a 3 sigma deviation from the fitted size-frequency distribution slope is found near 8 km. Completeness limits of the optical and infrared surveys are discussed.
C1 [Ryan, E. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ryan, E. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mizuno, D. R.] Boston Coll, Inst Sci Res, Chestnut Hill, MA USA.
[Shenoy, S. S.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Carey, S. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Noriega-Crespo, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kraemer, K. E.; Price, S. D.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA.
RP Ryan, EL (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM erin.l.ryan@nasa.gov
OI Kraemer, Kathleen/0000-0002-2626-7155
FU National Science Foundation [AST-0706980]; NASA; JPL/Caltech
FX E.L.R. and C.E.W. acknowledge support from National Science Foundation
grant AST-0706980 to conduct this research. This research was supported
by an appointment to the NASA Postdoctoral Program at Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. This work is based, in part, on archival data
obtained with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Support for this work was provided by an award
issued by JPL/Caltech. We thank an anonymous referee for helpful
comments which greatly improved this paper.
NR 59
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A42
DI 10.1051/0004-6361/201321375
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600054
ER
PT J
AU Sandell, G
Mookerjea, B
Gusten, R
Requena-Torres, MA
Riquelme, D
Okada, Y
AF Sandell, G.
Mookerjea, B.
Guesten, R.
Requena-Torres, M. A.
Riquelme, D.
Okada, Y.
TI High spectral and spatial resolution observations of the PDR emission in
the NGC 2023 reflection nebula with SOFIA and APEX
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; submillimeter: ISM; ISM: lines and bands; ISM: individual
objects: NGC 2023; ISM: molecules; photon-dominated region (PDR)
ID MOLECULAR-HYDROGEN EMISSION; CLUMPY PHOTODISSOCIATION REGIONS;
STAR-FORMING REGIONS; MU-M EMISSION; C-II; VIBRATIONAL FLUORESCENCE;
PHYSICAL CONDITIONS; H-2; NGC-2023; HERSCHEL
AB We have mapped the NGC 2023 reflection nebula in [CII] and CO(11-10) with the heterodyne receiver GREAT on SOFIA and obtained slightly smaller maps in (CO)-C-13(3-2), CO(3-2), CO(4-3), CO(6-5), and CO(7-6) with APEX in Chile. We use these data to probe the morphology, kinematics, and physical conditions of the C II region, which is ionized by FUV radiation from the B2 star HD37903. The [CII] emission traces an ellipsoidal shell-like region at a position angle of similar to-50 degrees, and is surrounded by a hot molecular shell. In the southeast, where the C II region expands into a dense, clumpy molecular cloud ridge, we see narrow and strong line emission from high-J CO lines, which comes from a thin, hot molecular shell surrounding the [C II] emission. The [CII] lines are broader and show photo evaporating gas flowing into the C II region. Based on the strength of the [(CII)-C-13] F = 2-1 line, the [CII] line appears to be somewhat optically thick over most of the nebula with an optical depth of a few. We model the physical conditions of the surrounding molecular cloud and the PDR emission using both RADEX and simple PDR models. The temperature of the CO emitting PDR shell is similar to 90-120 K, with densities of 10(5)-10(6) cm(-3), as deduced from RADEX modeling. Our PDR modeling indicates that the PDR layer where [C II] emission dominates has somewhat lower densities, 10(4) to a few times 10(5) cm(-3).
C1 [Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Mookerjea, B.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India.
[Guesten, R.; Requena-Torres, M. A.; Riquelme, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Okada, Y.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Sandell, G (reprint author), NASA, Ames Res Ctr, SOFIA USRA, MS 232-12,Bldg N232,Rm 146,POB 1, Moffett Field, CA 94035 USA.
EM Goran.H.Sandell@nasa.gov; bhaswati@tifr.res.in
FU NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]
FX The NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA) is
jointly operated 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 to the University of Stuttgart.
NR 48
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A41
DI 10.1051/0004-6361/201525881
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600053
ER
PT J
AU Velusamy, T
Langer, WD
Goldsmith, PF
Pineda, JL
AF Velusamy, T.
Langer, W. D.
Goldsmith, P. F.
Pineda, J. L.
TI Internal structure of spiral arms traced with [C II]: Unraveling the
warm ionized medium, H I, and molecular emission lanes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: structure; Galaxy: structure; Galaxy: general; submillimeter: ISM;
ISM: general
ID GALACTIC PLANE SURVEY; MILKY-WAY GALAXY; INTERSTELLAR-MEDIUM; CLOUDS;
GAS; LINES; GHZ
AB Context. The spiral arm tangencies are ideal lines of sight in which to determine the distribution of interstellar gas components in the spiral arms and study the influence of spiral density waves on the interarm gas in the Milky Way. [CII] emission in the tangencies delineates the warm ionized component and the photon-dominated regions and is thus an important probe of spiral arm structure and dynamics.
Aims. We aim to use [C II], Hi, and (CO)-C-12 spectral line maps of the Crux, Norma, and Perseus tangencies to analyze the internal structure of the spiral arms in different gas layers.
Methods. We used [C II] l-V maps along with those for HI and (CO)-C-12 to derive the average spectral line intensity profiles over the longitudinal range of each tangency. Using the V-LSR of the emission features, we located the [CII], HI, and (CO)-C-12 emissions along a cross cut of the spiral arm. We used the [CII] velocity profile to identify the compressed warm ionized medium (WIM) in the spiral arm.
Results. We present a large-scale (similar to 15 degrees) position-velocity map of the Galactic plane in [CII] from l = 326.degrees 6 to 341.degrees 4 observed with Herschel HIFI. In the spectral line profiles at the tangencies, [C II] has two emission peaks, one associated with the compressed WIM and the other the molecular gas photon-dominated regions. When represented as a cut across the inner to outer edge of the spiral arm, the [C II]-WIM peak appears closest to the inner edge while (CO)-C-12 and [C II] associated with molecular gas are at the outermost edge. Hi has broader emission with an intermediate peak located nearer to that of (CO)-C-12.
Conclusions. The velocity-resolved spectral line data of the spiral arm tangencies unravel the internal structure in the arms locating the emission lanes within them. We interpret the excess [Cii] near the tangent velocities as shock compression of the WIM induced by the spiral density waves and as the innermost edge of spiral arms. For the Norma and Perseus arms, we estimate widths of similar to 250 pc in [C II]-WIM and similar to 400 pc in (CO)-C-12 and overall spiral arm widths of similar to 500 pc in [CII] and (CO)-C-12 emissions; in HI the widths are similar to 400 pc and similar to 620 pc for Perseus and Norma, respectively. The electron densities in the WIM are similar to 0.5 cm(-3), about an order of magnitude higher than the average for the disk. The enhanced electron density in the WIM is a result of compression of the WIM by the spiral density wave potential.
C1 [Velusamy, T.; Langer, W. D.; Goldsmith, P. F.; Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Thangasamy.Velusamy@jpl.nasa.gov
RI Goldsmith, Paul/H-3159-2016
FU National Aeronautics and Space Administration
FX We thank the staffs of the ESA Herschel Science Centre and NASA Herschel
Science Center, and the HIFI, Instrument Control Centre (ICC) for their
help with the data reduction routines. In addition, we owe special
thanks to David Teyssier for clarifications regarding the hebCorrection
tool. This work was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2015
VL 578
AR A135
DI 10.1051/0004-6361/201525902
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM2IF
UT WOS:000357502600147
ER
PT J
AU Roman, MO
Stokes, EC
AF Roman, Miguel O.
Stokes, Eleanor C.
TI Holidays in lights: Tracking cultural patterns in demand for energy
services
SO EARTHS FUTURE
LA English
DT Article
DE Energy Use; Climate Change Mitigation; Human Dimensions; Remote Sensing
ID DAY/NIGHT BAND; LOW-CARBON; CONSUMPTION; ELECTRICITY; VEGETATION;
IMAGERY; URBANIZATION; POPULATION; SATURATION; ALGORITHM
AB Successful climate change mitigation will involve not only technological innovation, but also innovation in how we understand the societal and individual behaviors that shape the demand for energy services. Traditionally, individual energy behaviors have been described as a function of utility optimization and behavioral economics, with price restructuring as the dominant policy lever. Previous research at the macro-level has identified economic activity, power generation and technology, and economic role as significant factors that shape energy use. However, most demand models lack basic contextual information on how dominant social phenomenon, the changing demographics of cities, and the sociocultural setting within which people operate, affect energy decisions and use patterns. Here we use high-quality Suomi-NPP VIIRS nighttime environmental products to: (1) observe aggregate human behavior through variations in energy service demand patterns during the Christmas and New Year's season and the Holy Month of Ramadan and (2) demonstrate that patterns in energy behaviors closely track sociocultural boundaries at the country, city, and district level. These findings indicate that energy decision making and demand is a sociocultural process as well as an economic process, often involving a combination of individual price-based incentives and societal-level factors. While nighttime satellite imagery has been used to map regional energy infrastructure distribution, tracking daily dynamic lighting demand at three major scales of urbanization is novel. This methodology can enrich research on the relative importance of drivers of energy demand and conservation behaviors at fine scales. Our initial results demonstrate the importance of seating energy demand frameworks in a social context.
C1 [Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA.
[Stokes, Eleanor C.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
RP Roman, MO (reprint author), NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA.
EM miguel.o.roman@nasa.gov; eleanor.stokes@yale.edu
FU NASA's Office of the Chief Scientist under the Science Innovation Fund
(SIF); NASA's Minority University Research and Education Program
[NASA-NNX13AR88H]
FX The authors would like to thank Peter Ma and Jesse Allen
(NASA/GSFC/SSAI) for their support on the figures; to Virginia Kalb
(NASA/GSFC) and Zhuosen Wang (NASA/GSFC/ORAU) for their advice on the
Suomi-NPP VIIRS Day/Night Band algorithms; and to Adi Grief, Qingling
Zhang, and Karen Seto (YALE/FES) for much useful discussions. The
authors gratefully acknowledge support provided by NASA's Office of the
Chief Scientist under the Science Innovation Fund (SIF); as well as
NASA's Minority University Research and Education Program under grant
NASA-NNX13AR88H.
NR 62
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U1 2
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD JUN
PY 2015
VL 3
IS 6
BP 182
EP 205
DI 10.1002/2014EF000285
PG 24
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA CN0YU
UT WOS:000358142500002
PM 27819010
ER
PT J
AU Hui, HJ
Peslier, AH
Rudnick, RL
Simonetti, A
Neal, CR
AF Hui, Hejiu
Peslier, Anne H.
Rudnick, Roberta L.
Simonetti, Antonio
Neal, Clive R.
TI Plume-cratonic lithosphere interaction recorded by water and other trace
elements in peridotite xenoliths from the Labait volcano, Tanzania
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE Tanzanian craton; nominally anhydrous mineral; Fourier transform
infrared spectroscopy; laser-ablation inductively coupled plasma mass
spectrometry; water; craton; mantle plume
ID EAST-AFRICAN RIFT; NOMINALLY ANHYDROUS MINERALS; DISLOCATION CREEP
REGIME; UPPER-MANTLE MINERALS; MAGMA ASCENT RATES; CONTINENTAL
LITHOSPHERE; GREENSTONE-BELT; HYDROGEN DIFFUSION; NORTHERN TANZANIA;
BASALTIC GLASSES
AB Water and other trace element concentrations in olivine (1-39 ppm H2O), orthopyroxene (10-150 ppm H2O), and clinopyroxene (16-340 ppm H2O) of mantle xenoliths from the Labait volcano, located on the edge of the Tanzanian craton along the eastern branch of the East African Rift, record melting and subsequent refertilization by plume magmas in a stratified lithosphere. These water contents are at the lower end of the range observed in other cratonic mantle lithospheres. Despite correlations between water content and indices of melting in orthopyroxene from the shallow peridotites, and in both olivine and orthopyroxene from the deep peridotites, water concentrations are too high for the peridotites to be simple residues. Instead, the Labait water contents are best explained as reflecting interaction between residual peridotite with a melt having relatively low water content (<1 wt.% H2O). Plume-derived melts are the likely source of water and other trace element enrichments in the Labait peridotites. Only garnet may have undergone addition of water from the host magma as evidenced by water content increasing toward the kelyphite rim in one otherwise homogeneous garnet. Based on modeling of the diffusion profile, magma ascent occurred at 4-28 m/s. In summary, plume-craton interaction appears to result in only moderate water enrichment of the lithosphere.
C1 [Hui, Hejiu] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210008, Jiangsu, Peoples R China.
[Hui, Hejiu; Simonetti, Antonio; Neal, Clive R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
[Hui, Hejiu] USRA Houston, Lunar & Planetary Inst, Houston, TX USA.
[Peslier, Anne H.] NASA Johnson Space Ctr, Houston, TX USA.
[Rudnick, Roberta L.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
RP Hui, HJ (reprint author), Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210008, Jiangsu, Peoples R China.
EM hhui@nju.edu.cn
RI Hui, Hejiu/D-2912-2011; Simonetti, Antonio/E-4187-2016
OI Hui, Hejiu/0000-0003-2733-5794; Simonetti, Antonio/0000-0002-4025-2283
FU NSF [EAR 0802652, EAR 1118335, EAR 9506510]
FX This project was supported by NSF grants EAR 0802652 and EAR 1118335 to
AHP and EAR 9506510 to RLR. We thank Cin-Ty Lee for invaluable
discussions. We are grateful for the comments from two anonymous
reviewers that greatly improved the manuscript and for efficient editing
by T. Becker. Supporting data are provided in the tables and figures,
including those in an SI file.
NR 165
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U1 6
U2 29
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD JUN
PY 2015
VL 16
IS 6
BP 1687
EP 1710
DI 10.1002/2015GC005779
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM9DV
UT WOS:000358007800001
ER
PT J
AU Tian, HQ
Lu, CQ
Yang, J
Banger, K
Huntzinger, DN
Schwalm, CR
Michalak, AM
Cook, R
Ciais, P
Hayes, D
Huang, MY
Ito, A
Jain, AK
Lei, HM
Mao, JF
Pan, SF
Post, WM
Peng, SS
Poulter, B
Ren, W
Ricciuto, D
Schaefer, K
Shi, XY
Tao, B
Wang, WL
Wei, YX
Yang, QC
Zhang, BW
Zeng, N
AF Tian, Hanqin
Lu, Chaoqun
Yang, Jia
Banger, Kamaljit
Huntzinger, Deborah N.
Schwalm, Christopher R.
Michalak, Anna M.
Cook, Robert
Ciais, Philippe
Hayes, Daniel
Huang, Maoyi
Ito, Akihiko
Jain, Atul K.
Lei, Huimin
Mao, Jiafu
Pan, Shufen
Post, Wilfred M.
Peng, Shushi
Poulter, Benjamin
Ren, Wei
Ricciuto, Daniel
Schaefer, Kevin
Shi, Xiaoying
Tao, Bo
Wang, Weile
Wei, Yaxing
Yang, Qichun
Zhang, Bowen
Zeng, Ning
TI Global patterns and controls of soil organic carbon dynamics as
simulated by multiple terrestrial biosphere models: Current status and
future directions
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
DE soil organic carbon (SOC); heterotrophic respiration (Rh); mean
residence time (MRT); soil carbon dynamics model; belowground processes;
uncertainty
ID PROGRAM MULTISCALE SYNTHESIS; EARTH SYSTEM MODELS; LAND-USE CHANGE;
INTERCOMPARISON PROJECT; NITROGEN INTERACTIONS; AGRICULTURAL LAND;
VEGETATION MODEL; CLIMATE-CHANGE; WHITE SPRUCE; TEMPERATURE
AB Soil is the largest organic carbon (C) pool of terrestrial ecosystems, and C loss from soil accounts for a large proportion of land-atmosphere C exchange. Therefore, a small change in soil organic C (SOC) can affect atmospheric carbon dioxide (CO2) concentration and climate change. In the past decades, a wide variety of studies have been conducted to quantify global SOC stocks and soil C exchange with the atmosphere through site measurements, inventories, and empirical/process-based modeling. However, these estimates are highly uncertain, and identifying major driving forces controlling soil C dynamics remains a key research challenge. This study has compiled century-long (1901-2010) estimates of SOC storage and heterotrophic respiration (Rh) from 10 terrestrial biosphere models (TBMs) in the Multi-scale Synthesis and Terrestrial Model Intercomparison Project and two observation-based data sets. The 10 TBM ensemble shows that global SOC estimate ranges from 425 to 2111Pg C (1Pg=10(15)g) with a median value of 1158Pg C in 2010. The models estimate a broad range of Rh from 35 to 69PgCyr(-1) with a median value of 51PgCyr(-1) during 2001-2010. The largest uncertainty in SOC stocks exists in the 40-65 degrees N latitude whereas the largest cross-model divergence in Rh are in the tropics. The modeled SOC change during 1901-2010 ranges from -70Pg C to 86Pg C, but in some models the SOC change has a different sign from the change of total C stock, implying very different contribution of vegetation and soil pools in determining the terrestrial C budget among models. The model ensemble-estimated mean residence time of SOC shows a reduction of 3.4years over the past century, which accelerate C cycling through the land biosphere. All the models agreed that climate and land use changes decreased SOC stocks, while elevated atmospheric CO2 and nitrogen deposition over intact ecosystems increased SOC stockseven though the responses varied significantly among models. Model representations of temperature and moisture sensitivity, nutrient limitation, and land use partially explain the divergent estimates of global SOC stocks and soil C fluxes in this study. In addition, a major source of systematic error in model estimations relates to nonmodeled SOC storage in wetlands and peatlands, as well as to old C storage in deep soil layers.
C1 [Tian, Hanqin; Lu, Chaoqun; Yang, Jia; Banger, Kamaljit; Pan, Shufen; Ren, Wei; Tao, Bo; Yang, Qichun; Zhang, Bowen] Auburn Univ, Int Ctr Climate & Global Change Res, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
[Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
[Huntzinger, Deborah N.; Schwalm, Christopher R.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA.
[Schwalm, Christopher R.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA.
[Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Cook, Robert; Hayes, Daniel; Mao, Jiafu; Post, Wilfred M.; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Cook, Robert; Hayes, Daniel; Mao, Jiafu; Post, Wilfred M.; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA.
[Ciais, Philippe; Peng, Shushi] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Huang, Maoyi] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
[Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Jain, Atul K.] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA.
[Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Schaefer, Kevin] Natl Snow & Ice Data Ctr, Boulder, CO USA.
[Wang, Weile] NASA, Ames Res Ctr, Mountain View, CA USA.
[Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Tian, HQ (reprint author), Auburn Univ, Int Ctr Climate & Global Change Res, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
EM tianhan@auburn.edu; czl0003@auburn.edu
RI Lei, Huimin/H-9596-2015; Tian, Hanqin/A-6484-2012; Peng,
Shushi/J-4779-2014; Ren, Wei/G-8317-2016; Ren, Wei/I-4048-2014; Banger,
Kamaljit/B-3215-2016; Mao, Jiafu/B-9689-2012; Ricciuto,
Daniel/I-3659-2016; Zeng, Ning/A-3130-2008; Yang, Jia/A-6483-2012; Jain,
Atul/D-2851-2016
OI Cook, Robert/0000-0001-7393-7302; Poulter, Benjamin/0000-0002-9493-8600;
Huang, Maoyi/0000-0001-9154-9485; Zhang, Bowen/0000-0002-8370-0509; Lei,
Huimin/0000-0002-1175-2334; Tian, Hanqin/0000-0002-1806-4091; Peng,
Shushi/0000-0001-5098-726X; Ren, Wei/0000-0002-4840-4835; Mao,
Jiafu/0000-0002-2050-7373; Ricciuto, Daniel/0000-0002-3668-3021; Zeng,
Ning/0000-0002-7489-7629; Yang, Jia/0000-0003-2019-9603; Jain,
Atul/0000-0002-4051-3228
FU NASA ROSES [NNX10AG01A, NNH10AN68I]; U.S. Department of Energy (DOE),
Office of Science, Biological and Environmental Research; DOE
[DE-AC05-00OR22725]; U.S. DOE-BER; U.S. DOE-BER through the Subsurface
Biogeochemical Research Program (SBR) as part of the SBR Scientific
Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL);
U.S. DOE by BATTELLE Memorial Institute [DE-AC05-76RLO1830]; NASA
Interdisciplinary Science Program [NNX10AU06G, NNX11AD47G, NNX14AF93G,
NNG04GM39C]; NASA Land Cover/Land Use Change Program [NNX08AL73G]; NASA
Carbon Monitoring System Program [NNX14AO73G]; National Science
Foundation Dynamics of Coupled Natural-Human System Program [1210360];
Decadal and Regional Climate Prediction using Earth System Models
[AGS-1243220]; DOE National Institute for Climate Change Research
[DUKE-UN-07-SC-NICCR-1014]; EPA STAR program [2004-STAR-L1]; U.S.
National Science Foundation [NSF-AGS-12-43071, NSF-EFRI-083598]; USDA
National Institute of Food and Agriculture (NIFA) [2011-68002-30220];
U.S. Department of Energy (DOE) Office of Science [DOE-DE-SC0006706];
NASA Land cover and Land Use Change Program [NNX14AD94G]; Office of
Science of the U.S. Department of Energy [DE-AC02-05CH11231]; National
Science Foundation [OCI-0725070, ACI-1238993]
FX Funding for the Multi-scale Synthesis and Terrestrial Model
Intercomparison Project (MsTMIP; http://nacp.ornl.gov/MsTMIP.shtml) was
provided through NASA ROSES grant NNX10AG01A. Data management support
for preparing, documenting, and distributing model driver and output
data were performed by the Modeling and Synthesis Thematic Data Center
at Oak Ridge National Laboratory (http://nacp.ornl.gov), with funding
through NASA ROSES grant NNH10AN68I. Finalized MsTMIP data products will
be archived at the ORNL DAAC (http://daac.ornl.gov). This is MsTMIP
contribution 4. Acknowledgments for specific MsTMIP participating models
are as follows. (1) Biome-BGC. Biome-BGC code was provided by the
Numerical Terradynamic Simulation Group at University of Montana. The
computational facilities were provided by NASA Earth Exchange at NASA
Ames Research Center. (2) CLM and GTEC. Simulations were supported in
part by the U.S. Department of Energy (DOE), Office of Science,
Biological and Environmental Research. Oak Ridge National Laboratory is
managed by UTBATTELLE for DOE under contract DE-AC05-00OR22725. (3)
CLM4-VIC. This research is supported in part by the U.S. Department of
Energy (DOE), Office of Science, Biological and Environmental Research
(BER) through the Earth System Modeling program and performed using the
Environmental Molecular Sciences Laboratory (EMSL), a national
scientific user facility sponsored by the U.S. DOE-BER and located at
Pacific Northwest National Laboratory (PNNL). Participation of M. Huang
in the MsTMIP synthesis is supported by the U.S. DOE-BER through the
Subsurface Biogeochemical Research Program (SBR) as part of the SBR
Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory
(PNNL). PNNL is operated for the U.S. DOE by BATTELLE Memorial Institute
under contract DE-AC05-76RLO1830. (4) DLEM. The Dynamic Land Ecosystem
Model (DLEM) developed in International Center for Climate and Global
Change Research at Auburn University has been supported by NASA
Interdisciplinary Science Program (NNX10AU06G, NNX11AD47G, NNX14AF93G,
and NNG04GM39C), NASA Land Cover/Land Use Change Program (NNX08AL73G),
NASA Carbon Monitoring System Program (NNX14AO73G), National Science
Foundation Dynamics of Coupled Natural-Human System Program(1210360),
Decadal and Regional Climate Prediction using Earth System Models
(AGS-1243220), DOE National Institute for Climate Change Research
(DUKE-UN-07-SC-NICCR-1014), and EPA STAR program (2004-STAR-L1). (5)
ISAM. The simulations were supported by the U.S. National Science
Foundation (NSF-AGS-12-43071 and NSF-EFRI-083598), the USDA National
Institute of Food and Agriculture (NIFA) (2011-68002-30220), the U.S.
Department of Energy (DOE) Office of Science (DOE-DE-SC0006706), and the
NASA Land cover and Land Use Change Program (NNX14AD94G). ISAM
simulations were carried out at the National Energy Research Scientific
Computing Center (NERSC), which is supported by the Office of Science of
the U.S. Department of Energy under contract DE-AC02-05CH11231, and at
the Blue Waters sustained-petascale computing, University of Illinois at
Urbana-Champaign, which is supported by the National Science Foundation
(awards OCI-0725070 and ACI-1238993) and the state of Illinois. (6)
LPJ-wsl. This work was conducted at LSCE, France, using a modified
version of the LPJ version 3.1 model, originally made available by the
Potsdam Institute for Climate Impact Research. (7) ORCHIDEE-LSCE.
ORCHIDEE is developed at the IPSL institute in France.; The simulations
were performed with the support of the GHG-Europe FP7 grant with
computing facilities provided by LSCE (Laboratoire des Sciences du
Climat et de l'Environnement) or TGCC (Tres Grand Centre de Calcul). (8)
VISIT. VISIT was developed at the National Institute for Environmental
Studies, Japan. This work was mostly conducted during a visiting stay at
Oak Ridge National Laboratory.
NR 66
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U1 18
U2 107
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 JUN
PY 2015
VL 29
IS 6
BP 775
EP 792
DI 10.1002/2014GB005021
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA CM8NE
UT WOS:000357957600004
ER
PT J
AU Wierzchos, K
Cancilla, JC
Torrecilla, JS
Diaz-Rodriguez, P
Davila, AF
Ascaso, C
Nienow, J
McKay, CP
Wierzchos, J
AF Wierzchos, K.
Cancilla, J. C.
Torrecilla, J. S.
Diaz-Rodriguez, P.
Davila, A. F.
Ascaso, C.
Nienow, J.
McKay, C. P.
Wierzchos, J.
TI Application of artificial neural networks as a tool for moisture
prediction in microbially colonized halite in the Atacama Desert
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE Atacama Desert; halite; microbial endolithic communities; artificial
neural network
ID IONIC LIQUIDS; HYPERARID CORE; WATER-CONTENT; WASTE; LIFE
AB The Atacama Desert is the driest and one of the most life-limiting places on Earth. Despite the extreme conditions, microbial endolithic communities have been found inside halite rocks. The presence of these microbial communities is possible due to the hygroscopic properties of evaporitic rocks composed of sodium chloride. It is important to elucidate every possible water source in such a hyperarid environment. Therefore, in the present study, an artificial neural network (ANN) based model has been designed to predict the presence of liquid water on the surface of halite pinnacles. The model predicts the moisture formation using two basic meteorological variables, air temperature, and air relative humidity. ANNs have been successfully employed for the first time as a tool for predicting the appearance of liquid water, a key factor for the endolithic microbial communities living in the driest part of the Atacama Desert. The model developed is able to correctly predict the formation of water on the surface of the halite pinnacles 83% of the cases. We anticipate the future application of this model as an important tool for the prediction of the water availability and therefore potential habitability of lithic substrates in extreme environments on Earth and perhaps elsewhere.
C1 [Wierzchos, K.; Cancilla, J. C.; Torrecilla, J. S.; Diaz-Rodriguez, P.] Univ Complutense Madrid, Dept Chem Engn, Madrid, Spain.
[Davila, A. F.] SETI Inst, Mountain View, CA USA.
[Ascaso, C.; Wierzchos, J.] Museo Nacl Ciencias Nat CSIC, Madrid, Spain.
[Nienow, J.] Valdosta State Univ, Dept Biol, Valdosta, GA USA.
[McKay, C. P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Wierzchos, K (reprint author), Univ Complutense Madrid, Dept Chem Engn, Madrid, Spain.
EM kacperwierzchos@gmail.com
RI Torrecilla, Jose/L-6525-2014
OI Torrecilla, Jose/0000-0003-1209-203X
FU MINECO (Spain) [CGL2013-42509P]; European Union [HEALTH-F4-2011-258868];
NASA [NNX12AD61G]
FX This work was supported by MINECO (Spain) grant CGL2013-42509P, the
European Union Seventh Framework Programme (FP7/2007-2013) under grant
agreement HEALTH-F4-2011-258868, and by grant NNX12AD61G from NASA
Exobiology program. All the data used for this work can be obtained via
email from the corresponding author at kacperwierzchos@gmail.com.
NR 30
TC 0
Z9 0
U1 3
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD JUN
PY 2015
VL 120
IS 6
BP 1018
EP 1026
DI 10.1002/2014JG002837
PG 9
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA CM8LM
UT WOS:000357952400003
ER
PT J
AU MacGregor, JA
Li, JL
Paden, JD
Catania, GA
Clow, GD
Fahnestock, MA
Gogineni, SP
Grimm, RE
Morlighem, M
Nandi, S
Seroussi, H
Stillman, DE
AF MacGregor, Joseph A.
Li, Jilu
Paden, John D.
Catania, Ginny A.
Clow, Gary D.
Fahnestock, Mark A.
Gogineni, S. Prasad
Grimm, Robert E.
Morlighem, Mathieu
Nandi, Soumyaroop
Seroussi, Helene
Stillman, David E.
TI Radar attenuation and temperature within the Greenland Ice Sheet
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID GEOTHERMAL HEAT-FLUX; ECHO SOUNDING DATA; ANTARCTIC ICE; WEST
ANTARCTICA; PENETRATING RADAR; EAST ANTARCTICA; BASAL MELT;
RADIOFREQUENCY ATTENUATION; ELECTRICAL-CONDUCTIVITY; NORTHEAST GREENLAND
AB The flow of ice is temperature-dependent, but direct measurements of englacial temperature are sparse. The dielectric attenuation of radio waves through ice is also temperature-dependent, and radar sounding of ice sheets is sensitive to this attenuation. Here we estimate depth-averaged radar-attenuation rates within the Greenland Ice Sheet from airborne radar-sounding data and its associated radiostratigraphy. Using existing empirical relationships between temperature, chemistry, and radar attenuation, we then infer the depth-averaged englacial temperature. The dated radiostratigraphy permits a correction for the confounding effect of spatially varying ice chemistry. Where radar transects intersect boreholes, radar-inferred temperature is consistently higher than that measured directly. We attribute this discrepancy to the poorly recognized frequency dependence of the radar-attenuation rate and correct for this effect empirically, resulting in a robust relationship between radar-inferred and borehole-measured depth-averaged temperature. Radar-inferred englacial temperature is often lower than modern surface temperature and that of a steady state ice-sheet model, particularly in southern Greenland. This pattern suggests that past changes in surface boundary conditions (temperature and accumulation rate) affect the ice sheet's present temperature structure over a much larger area than previously recognized. This radar-inferred temperature structure provides a new constraint for thermomechanical models of the Greenland Ice Sheet.
C1 [MacGregor, Joseph A.; Catania, Ginny A.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
[Li, Jilu; Paden, John D.; Gogineni, S. Prasad; Nandi, Soumyaroop] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Catania, Ginny A.] Univ Texas Austin, Dept Geol Sci, Austin, TX USA.
[Clow, Gary D.] US Geol Survey, Lakewood, CO 80225 USA.
[Clow, Gary D.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Fahnestock, Mark A.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Grimm, Robert E.; Stillman, David E.] Southwest Res Inst, Dept Space Studies, Boulder, CO USA.
[Morlighem, Mathieu] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP MacGregor, JA (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
EM joemac@ig.utexas.edu
RI Catania, Ginny/B-9787-2008; Morlighem, Mathieu/O-9942-2014;
OI Morlighem, Mathieu/0000-0001-5219-1310; Grimm,
Robert/0000-0002-7588-1194
FU NSF [ARC 1107753, 1108058, ANT 0424589]; NASA [NNX12AB71G]
FX NSF (ARC 1107753 and 1108058; ANT 0424589) and NASA (NNX12AB71G)
supported this work. We thank the organizations (Program for Arctic
Regional Climate Assessment, Center for Remote Sensing of Ice Sheets,
and Operation IceBridge) and innumerable individuals that both supported
and performed the collection and processing of the radar data used in
this study. We thank S. Anandakrishnan, K. Matsuoka, and D.P.
Winebrenner for the inspiration for this work; the Centre for Ice and
Climate for the DEP data; and L.C. Andrews, K. A. Christianson, C.
Grima, J.C. Hiester, N. Holschuh, K. Thirumalai, and D. A. Young for
valuable discussions. We thank Associate Editor J.N. Bassis, D.M.
Schroeder, and an anonymous referee for valuable comments that improved
this manuscript. Echo-intensity data will be archived at the National
Snow and Ice Data Center (NSIDC; http://www.nsidc.org).
NR 90
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U1 2
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD JUN
PY 2015
VL 120
IS 6
BP 983
EP 1008
DI 10.1002/2014JF003418
PG 26
WC Geosciences, Multidisciplinary
SC Geology
GA CM8ZQ
UT WOS:000357994400003
ER
PT J
AU Dow, CF
Kulessa, B
Rutt, IC
Tsai, VC
Pimentel, S
Doyle, SH
van As, D
Lindback, K
Pettersson, R
Jones, GA
Hubbard, A
AF Dow, C. F.
Kulessa, B.
Rutt, I. C.
Tsai, V. C.
Pimentel, S.
Doyle, S. H.
van As, D.
Lindback, K.
Pettersson, R.
Jones, G. A.
Hubbard, A.
TI Modeling of subglacial hydrological development following rapid
supraglacial lake drainage
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE Greenland ice sheet; subglacial hydrology; lake drainage; modeling
ID GREENLAND ICE-SHEET; OUTBURST FLOODS; WEST GREENLAND; OUTLET GLACIER;
SEASONAL-CHANGES; WATER STORAGE; SURFACE MELT; EVOLUTION; SYSTEM; MOTION
AB The rapid drainage of supraglacial lakes injects substantial volumes of water to the bed of the Greenland ice sheet over short timescales. The effect of these water pulses on the development of basal hydrological systems is largely unknown. To address this, we develop a lake drainage model incorporating both (1) a subglacial radial flux element driven by elastic hydraulic jacking and (2) downstream drainage through a linked channelized and distributed system. Here we present the model and examine whether substantial, efficient subglacial channels can form during or following lake drainage events and their effect on the water pressure in the surrounding distributed system. We force the model with field data from a lake drainage site, 70 km from the terminus of Russell Glacier in West Greenland. The model outputs suggest that efficient subglacial channels do not readily form in the vicinity of the lake during rapid drainage and instead water is evacuated primarily by a transient turbulent sheet and the distributed system. Following lake drainage, channels grow but are not large enough to reduce the water pressure in the surrounding distributed system, unless preexisting channels are present throughout the domain. Our results have implications for the analysis of subglacial hydrological systems in regions where rapid lake drainage provides the primary mechanism for surface-to-bed connections.
C1 [Dow, C. F.; Kulessa, B.; Rutt, I. C.; Jones, G. A.] Swansea Univ, Coll Sci, Glaciol Grp, Swansea, W Glam, Wales.
[Dow, C. F.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Tsai, V. C.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
[Pimentel, S.] Trinity Western Univ, Fac Nat & Appl Sci, Dept Math, Langley, BC, Canada.
[Doyle, S. H.; Hubbard, A.] Aberystwyth Univ, Inst Geog & Earth Sci, Aberystwyth, Dyfed, Wales.
[van As, D.] Geol Survey Denmark & Greenland, Copenhagen, Denmark.
[Lindback, K.; Pettersson, R.] Uppsala Univ, Dept Earth Sci, Uppsala, Sweden.
RP Dow, CF (reprint author), Swansea Univ, Coll Sci, Glaciol Grp, Swansea, W Glam, Wales.
EM christine.f.dow@nasa.gov
RI Tsai, Victor/J-8405-2012;
OI Tsai, Victor/0000-0003-1809-6672; Kulessa, Bernd/0000-0002-4830-4949;
Hubbard, Alun/0000-0002-0503-3915
FU NERC [NE/G007195/1]; Greenland Analogue Project; NERC doctoral
scholarship; NASA Postdoctoral Program fellowship at the Goddard Space
Flight Center
FX For further information on the modeling methodology see the supporting
information and/or contact C.F. Dow. This project was funded with NERC
grant NE/G007195/1 and the Greenland Analogue Project. C.F.D. was funded
by a NERC doctoral scholarship and a NASA Postdoctoral Program
fellowship at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities. The authors would like to thank Mauro Werder
and Ian Hewitt for helpful discussions about the modeling approach.
Three anonymous reviewers and the Associate Editor are thanked for their
helpful suggestions that have improved this manuscript.
NR 73
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U1 5
U2 19
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 JUN
PY 2015
VL 120
IS 6
BP 1127
EP 1147
DI 10.1002/2014JF003333
PG 21
WC Geosciences, Multidisciplinary
SC Geology
GA CM8ZQ
UT WOS:000357994400010
PM 26640746
ER
PT J
AU Chemtob, SM
Nickerson, RD
Morris, RV
Agresti, DG
Catalano, JG
AF Chemtob, Steven M.
Nickerson, Ryan D.
Morris, Richard V.
Agresti, David G.
Catalano, Jeffrey G.
TI Synthesis and structural characterization of ferrous trioctahedral
smectites: Implications for clay mineral genesis and detectability on
Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE clay mineralogy; smectite; X-ray diffraction; VNIR; X-ray spectroscopy;
Mars
ID RESOLUTION REFLECTANCE SPECTROSCOPY; HYDROTHERMAL ALTERATION;
MOSSBAUER-SPECTROSCOPY; SILICATE MINERALS; HYDROUS MINERALS; OCTAHEDRAL
SHEET; OXIDATION-STATE; POLARIZED EXAFS; OXYGEN FUGACITY; IRON
AB Widespread detections of phyllosilicates in Noachian terrains on Mars imply a history of near-surface fluid-rock interaction. Ferrous trioctahedral smectites are thermodynamically predicted products of basalt weathering on early Mars, but to date only Fe3+-bearing dioctahedral smectites have been identified from orbital observations. In general, the physicochemical properties of ferrous smectites are poorly studied because they are susceptible to air oxidation. In this study, eight Fe2+-bearing smectites were synthesized from Fe2+-Mg-Al silicate gels at 200 degrees C under anoxic conditions. Samples were characterized by inductively coupled plasma optical emission spectrometry, powder X-ray diffraction, Fe K-edge X-ray absorption spectroscopy (XAS), Mossbauer spectroscopy, and visible/near-infrared (VNIR) reflectance spectroscopy. The range of redox states was Fe3+/sigma Fe=0 to 0.060.01 as determined by both XAS and, for short integration times, Mossbauer. The smectites have 060 distances (d((060))) between 1.53 and 1.56 angstrom, indicating a trioctahedral structure.d((060)) and XAS-derived interatomic Fe-(Fe,Mg,Al) distance scaled with Fe content. Smectite VNIR spectra feature OH/H2O absorption bands at 1.4 and 1.9 mu m, (Fe2+,Mg,Al)(3)-OH stretching bands near 1.4 mu m, and Fe2+Fe2+Fe2+-OH, MgMgMg-OH, AlAl(Mg,Fe2+)-OH, and AlAl-OH combination bands at 2.36 mu m, 2.32 mu m 2.25 mu m, and 2.20 mu m, respectively. The spectra for ferrous saponites are distinct from those for dioctahedral ferric smectites, permitting their differentiation from orbital observations. X-ray diffraction patterns for synthetic high-Mg ferrosaponite and high-Mg ferrian saponite are both consistent with the Sheepbed saponite detected by the chemistry and mineralogy (CheMin) instrument at Gale Crater, Mars, suggesting that anoxic basalt alteration was a viable pathway for clay mineral formation on early Mars.
C1 [Chemtob, Steven M.; Nickerson, Ryan D.; Catalano, Jeffrey G.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Chemtob, Steven M.; Catalano, Jeffrey G.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO USA.
[Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, EIS Directorate, Houston, TX 77058 USA.
[Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
RP Chemtob, SM (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
EM chemtob@levee.wustl.edu
RI Catalano, Jeffrey/A-8322-2013
OI Catalano, Jeffrey/0000-0001-9311-977X
FU NASA [NX11AH09G, NNX14AJ95G]; McDonnell Center for the Space Sciences at
Washington University; National Science Foundation [EAR-1161543]; DOE
Office of Science [DE-AC02-06CH11357]
FX This research was supported by the NASA Mars Fundamental Research
Program under awards NX11AH09G and NNX14AJ95G. Additional support was
provided to S.M.C. by the McDonnell Center for the Space Sciences at
Washington University. Use of the XRD facility at Washington University
is supported by the National Science Foundation under award EAR-1161543.
This research used resources of the Advanced Photon Source, a U.S.
Department of Energy (DOE) Office of Science User Facility operated for
the DOE Office of Science by Argonne National Laboratory under contract
DE-AC02-06CH11357. We thank Chris Gorski for collecting preliminary
Mossbauer spectra on two samples. We thank Qing Ma (5-BM-D), Sungsik Lee
(12-BM-B), and Matt Newville (13-BM-D) for their assistance with XAFS
data collection at the Advanced Photon Source. We thank Abigail Fraeman
for her assistance with VNIR reflectance spectra collection. We thank M.
Darby Dyar and Joseph Michalski for their reviews that greatly improved
the quality of the manuscript. Data sets presented in this manuscript
are available by e-mail requests directed to the corresponding author
(S.M.C.).
NR 84
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U1 3
U2 29
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 JUN
PY 2015
VL 120
IS 6
BP 1119
EP 1140
DI 10.1002/2014JE004763
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM8LB
UT WOS:000357951300005
ER
PT J
AU Wordsworth, RD
Kerber, L
Pierrehumbert, RT
Forget, F
Head, JW
AF Wordsworth, Robin D.
Kerber, Laura
Pierrehumbert, Raymond T.
Forget, Francois
Head, James W.
TI Comparison of "warm and wet" and "cold and icy" scenarios for early Mars
in a 3-D climate model
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE paleoclimate; early Mars; atmospheres; hydrology; valley networks;
astrobiology
ID GENERAL-CIRCULATION MODEL; EARLY MARTIAN CLIMATE; LONG-TERM EVOLUTION;
CO2; CLOUDS; GREENHOUSE; VALLEYS; SURFACE; OCEAN; WATER
AB We use a 3-D general circulation model to compare the primitive Martian hydrological cycle in warm and wet and cold and icy scenarios. In the warm and wet scenario, an anomalously high solar flux or intense greenhouse warming artificially added to the climate model are required to maintain warm conditions and an ice-free northern ocean. Precipitation shows strong surface variations, with high rates around Hellas basin and west of Tharsis but low rates around Margaritifer Sinus (where the observed valley network drainage density is nonetheless high). In the cold and icy scenario, snow migration is a function of both obliquity and surface pressure, and limited episodic melting is possible through combinations of seasonal, volcanic, and impact forcing. At surface pressures above those required to avoid atmospheric collapse (approximate to 0.5bar) and moderate to high obliquity, snow is transported to the equatorial highland regions where the concentration of valley networks is highest. Snow accumulation in the Aeolis quadrangle is high, indicating an ice-free northern ocean is not required to supply water to Gale crater. At lower surface pressures and obliquities, both H2O and CO2 are trapped as ice at the poles and the equatorial regions become extremely dry. The valley network distribution is positively correlated with snow accumulation produced by the cold and icy simulation at 41.8 degrees obliquity but uncorrelated with precipitation produced by the warm and wet simulation. Because our simulations make specific predictions for precipitation patterns under different climate scenarios, they motivate future targeted geological studies.
C1 [Wordsworth, Robin D.] Harvard Univ, Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Wordsworth, Robin D.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Kerber, Laura] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pierrehumbert, Raymond T.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Forget, Francois] Inst Pierre Simon Laplace, Lab Meterol Dynam, Paris, France.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Wordsworth, RD (reprint author), Harvard Univ, Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
EM rwordsworth@seas.harvard.edu
OI Pierrehumbert, Raymond/0000-0002-5887-1197
NR 76
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U1 9
U2 37
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 JUN
PY 2015
VL 120
IS 6
BP 1201
EP 1219
DI 10.1002/2015JE004787
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM8LB
UT WOS:000357951300009
ER
PT J
AU Cook-Hallett, C
Barnes, JW
Kattenhorn, SA
Hurford, T
Radebaugh, J
Stiles, B
Beuthe, M
AF Cook-Hallett, Casey
Barnes, Jason W.
Kattenhorn, Simon A.
Hurford, Terry
Radebaugh, Jani
Stiles, Bryan
Beuthe, Mikael
TI Global contraction/expansion and polar lithospheric thinning on Titan
from patterns of tectonism
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Titan; global stress fields; tectonics
ID CASSINI RADAR; VIMS OBSERVATIONS; GROOVED TERRAIN; DESPUN PLANET; XANADU
REGION; FEATURES; SURFACE; RECONNAISSANCE; ENCELADUS; EVOLUTION
AB We investigate the underlying physical processes that govern the formation and evolution of Titan's tectonic features. This is done by mapping mountain chains and hills using Cassini RADAR data obtained during Titan flybys T3 to T69. Our mapping of mountain chains and hills reveals a global pattern: east-west orientations within 30 degrees of the equator and north-south between 60 degrees latitude and the poles. This result makes Titan one of the few solar system bodies where global processes, rather than regional processes, dominate tectonism. After comparison with five global stress models showing theoretical mountain chain orientations, we suggest that either global contraction coupled with spin-up or global expansion coupled with despinning could explain our observations if coupled with a lithosphere thinner in Titan's polar regions.
C1 [Cook-Hallett, Casey; Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[Cook-Hallett, Casey] North Idaho Coll, Div Nat Sci, Coeur Dalene, ID USA.
[Kattenhorn, Simon A.] Univ Idaho, Dept Geol Sci, Moscow, ID 83843 USA.
[Hurford, Terry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Radebaugh, Jani] Brigham Young Univ, Dept Geol, Provo, UT 84602 USA.
[Stiles, Bryan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Beuthe, Mikael] Royal Observ Belgium, Brussels, Belgium.
RP Cook-Hallett, C (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
EM cook6924@vandals.uidaho.edu
RI Barnes, Jason/B-1284-2009; Hurford, Terry/F-2625-2012
OI Barnes, Jason/0000-0002-7755-3530;
FU NASA [NNX10AQ10G]; PRODEX program; Belgian Federal Science Policy
Office; National Aeronautics and Space Administration
FX Thanks to Alex Patthoff and Emily Martin for discussions and lessons on
ArcGIS. The authors acknowledge support from NASA Outer Planets Research
Program grant NNX10AQ10G. M. Beuthe is supported by the PRODEX program
managed by the European Space Agency and the Belgian Federal Science
Policy Office. The portion of this research carried out by B. Stiles was
done so at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The data to support this article are from the National
Aeronautics and Space Administration (NASA). ArcGIS shapefiles are
available at the following website:r5d4.
barnesos.net/GlobalPatternsofTectonism.
NR 59
TC 6
Z9 6
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JUN
PY 2015
VL 120
IS 6
BP 1220
EP 1236
DI 10.1002/2014JE004645
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM8LB
UT WOS:000357951300010
ER
PT J
AU Nastula, J
Gross, R
AF Nastula, J.
Gross, R.
TI Chandler wobble parameters from SLR and GRACE
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
DE Chandler wobble parameters; SLR; GRACE
ID POLAR MOTION; OCEANIC EXCITATION; GRAVITATIONAL CHANGES;
ANGULAR-MOMENTUM; EARTH ROTATION; SERIES; MODELS; PERIOD
AB The period and quality factor Q of the Chandler wobble are functions of the internal structure and dissipation processes of the Earth. Better estimates of the period and Q of the Chandler wobble can therefore be used to better understand these properties of the Earth. Here the period and Q of the Chandler wobble are estimated by finding those values that minimize the power in the Chandler frequency band of the difference between observed and modeled polar motion excitation functions. The observations of the polar motion excitation functions that we used are derived from both space-geodetic polar motion observations and from satellite laser ranging (SLR) and Gravity Recovery and Climate Experiment (GRACE) observations of the degree-2 coefficients of the Earth's time-varying gravitational field. The models of the polar motion excitation functions that we used are derived from general circulation models of the atmosphere and oceans and from hydrologic models. Our preferred values for the period and Q of the Chandler wobble that we estimated using this approach are 430.90.7 solar days and 127 (56, 255), respectively.
C1 [Nastula, J.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Gross, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nastula, J (reprint author), Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
EM nastula@cbk.waw.pl
FU Ministry of Scientific Research and Information Technology
[2012/05/B/ST10/02132, 2014/13/B/ST10/04975]; National Aeronautics and
Space Administration; Earth Surface and Interior Focus Area of NASA's
Science Mission Directorate
FX J. Nastula was supported by the Ministry of Scientific Research and
Information Technology through projects 2012/05/B/ST10/02132 and
2014/13/B/ST10/04975. J. Nastula thanks Waldemar Popinski for writing
the Multitaper computer procedures used in the numerical computations.
The work of R. Gross described in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. Support
for that work was provided by the Earth Surface and Interior Focus Area
of NASA's Science Mission Directorate. The data series is accessible
from the following: The x, y COMB polar motion data series are available
from: http://keof.jpl.nasa.gov. The Atmospheric Angular Momentum (AAM),
Oceanic Angular Momentum (OAM), and Hydrospheric Angular momentum (HAM)
data series are available from
http://www.gfz-potsdam.de/en/research/organizational-units/departments/d
epartment-1/earth-system-modelling/services/eam/. The Delta
C21 and Delta S21 data series estimated from the
GRACE observations are available from
http:/podaac.jpl.nasa.gov/dataacces. The Delta C21 and Delta
S21 data series denoted as SLR2 are available from
http:/grace.jpl.nasa.gov/data/weekly5x5gravityharmonicsdata/. The Delta
C21 and Delta S21 data series denoted as SLR1 were
made available by M. Cheng and are available from him upon request
(cs21.801110 series, Minkang Cheng, Ph.D Research Scientist, Center for
Space Research, 3925 W. Braker Ln. Ste. 200 Austin, Texas 78759 Phone:
512-471-7818 FAX: 512-232-2443 cheng@csr.utexas.edu.
NR 49
TC 6
Z9 6
U1 2
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD JUN
PY 2015
VL 120
IS 6
BP 4474
EP 4483
DI 10.1002/2014JB011825
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM8ZG
UT WOS:000357993000026
ER
PT J
AU Zwieback, S
Hensley, S
Hajnsek, I
AF Zwieback, Simon
Hensley, Scott
Hajnsek, Irena
TI A Polarimetric First-Order Model of Soil Moisture Effects on the DInSAR
Coherence
SO REMOTE SENSING
LA English
DT Article
DE DInSAR; InSAR; interferometry; electromagnetic model; soil moisture;
deformations; displacement
ID RADAR INTERFEROMETRY; SAR INTERFEROMETRY; PENETRATION; RETRIEVALS;
VEGETATION
AB Changes in soil moisture between two radar acquisitions can impact the observed coherence in differential interferometry: both coherence magnitude || and phase phi are affected. The influence on the latter potentially biases the estimation of deformations. These effects have been found to be variable in magnitude and sign, as well as dependent on polarization, as opposed to predictions by existing models. Such diversity can be explained when the soil is modelled as a half-space with spatially varying dielectric properties and a rough interface. The first-order perturbative solution achieves-upon calibration with airborne L band data-median correlations at HH polarization of 0.77 for the phase phi, of 0.50 for ||, and for the phase triplets of 0.56. The predictions are sensitive to the choice of dielectric mixing model, in particular the absorptive properties; the differences between the mixing models are found to be partially compensatable by varying the relative importance of surface and volume scattering. However, for half of the agricultural fields the Hallikainen mixing model cannot reproduce the observed sensitivities of the phase to soil moisture. In addition, the first-order expansion does not predict any impact on the HV coherence, which is however empirically found to display similar sensitivities to soil moisture as the co-pol channels HH and VV. These results indicate that the first-order solution, while not able to reproduce all observed phenomena, can capture some of the more salient patterns of the effect of soil moisture changes on the HH and VV DInSAR signals. Hence it may prove useful in separating the deformations from the moisture signals, thus yielding improved displacement estimates or new ways for inferring soil moisture.
C1 [Zwieback, Simon; Hajnsek, Irena] ETH, Inst Environm Engn, CH-8093 Zurich, Switzerland.
[Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hajnsek, Irena] German Aerosp Ctr DLR, Microwaves & Radar Inst, D-82230 Wessling, Germany.
RP Zwieback, S (reprint author), ETH, Inst Environm Engn, Stefano Franscini Pl 3, CH-8093 Zurich, Switzerland.
EM zwieback@ifu.baug.ethz.ch; scott.hensley@jpl.nasa.gov;
irena.hajnsek@dlr.de
FU Helmholtz Alliance [HA310]
FX The authors would like to thank the reviewers for their insightful
comments and suggestions. The study has been conducted under the support
of the Helmholtz Alliance HA310 "Remote Sensing and Earth System
Dynamics".
NR 42
TC 6
Z9 6
U1 3
U2 12
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2015
VL 7
IS 6
BP 7571
EP 7596
DI 10.3390/rs70607571
PG 26
WC Remote Sensing
SC Remote Sensing
GA CM3NX
UT WOS:000357590300003
ER
PT J
AU Jung, HC
Jasinski, MF
AF Jung, Hahn Chul
Jasinski, Michael F.
TI Sensitivity of a Floodplain Hydrodynamic Model to Satellite- Based DEM
Scale and Accuracy: Case Study-The Atchafalaya Basin
SO REMOTE SENSING
LA English
DT Article
DE Atchafalaya; digital elevation model; floodplain; hydrodynamic model;
Surface Water and Ocean Topography (SWOT) mission
ID RASTER-BASED MODEL; INUNDATION SIMULATION; MESH RESOLUTION; RIVER-BASIN;
PRONE AREAS; FLOW; REPRESENTATION; DELINEATION; ALTIMETRY; AMAZON
AB The hydrodynamics of low-lying riverine floodplains and wetlands play a critical role in hydrology and ecosystem processes. Because small topographic features affect floodplain storage and flow velocity, a hydrodynamic model setup of these regions imposes more stringent requirements on the input Digital Elevation Model (DEM) compared to upland regions with comparatively high slopes. This current study provides a systematic approach to evaluate the required relative vertical accuracy and spatial resolution of current and future satellite-based altimeters within the context of DEM requirements for 2-D floodplain hydrodynamic models. A case study is presented for the Atchafalaya Basin with a model domain of 1190 km(2). The approach analyzes the sensitivity of modeled floodplain water elevation and velocity to typical satellite-based DEM grid-box scale and vertical error, using a previously calibrated version of the physically-based flood inundation model (LISFLOOD-ACC). Results indicate a trade-off relationship between DEM relative vertical error and grid-box size. Higher resolution models are the most sensitive to vertical accuracy, but the impact diminishes at coarser resolutions because of spatial averaging. The results provide guidance to engineers and scientists when defining the observation scales of future altimetry missions such as the Surface Water and Ocean Topography (SWOT) mission from the perspective of numerical modeling requirements for large floodplains of O[10(3)] km(2) and greater.
C1 [Jung, Hahn Chul] Sci Syst & Applicat Inc SSAI, Lanham, MD 20706 USA.
[Jung, Hahn Chul] NASA, Goddard Space Flight Ctr, Off Appl Sci, Greenbelt, MD 20771 USA.
[Jasinski, Michael F.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
RP Jung, HC (reprint author), Sci Syst & Applicat Inc SSAI, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
EM hahnchul.jung@nasa.gov; michael.f.jasinski@nasa.gov
FU NASA; NASA's Terrestrial Hydrology Program; Goddard Space Flight Center
(GSFC)
FX This research was supported by an appointment to the NASA Postdoctoral
Program (NPP) at the Goddard Space Flight Center (GSFC), administered by
Oak Ridge Associated Universities (ORAU) through a contract with NASA,
and by NASA's Terrestrial Hydrology Program. We gratefully acknowledge
Paul Bates for use of the LISFLOOD-ACC model. LiDAR data were obtained
from the USGS National Geospatial Program and USGS Coastal and Marine
Geology Program archives.
NR 47
TC 2
Z9 2
U1 4
U2 16
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2015
VL 7
IS 6
BP 7938
EP 7958
DI 10.3390/rs70607938
PG 21
WC Remote Sensing
SC Remote Sensing
GA CM3NX
UT WOS:000357590300020
ER
PT J
AU Savani, NP
Vourlidas, A
Szabo, A
Mays, ML
Richardson, IG
Thompson, BJ
Pulkkinen, A
Evans, R
Nieves-Chinchilla, T
AF Savani, N. P.
Vourlidas, A.
Szabo, A.
Mays, M. L.
Richardson, I. G.
Thompson, B. J.
Pulkkinen, A.
Evans, R.
Nieves-Chinchilla, T.
TI Predicting the magnetic vectors within coronal mass ejections arriving
at Earth: 1. Initial architecture
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE CMEs; Bz forecasts
ID STRUCTURED SOLAR-WIND; IN-SITU OBSERVATIONS; CLOUDS; FIELD; FLUX;
EVOLUTION; PROPAGATION; SPACE; CMES; AU
AB The process by which the Sun affects the terrestrial environment on short timescales is predominately driven by the amount of magnetic reconnection between the solar wind and Earth's magnetosphere. Reconnection occurs most efficiently when the solar wind magnetic field has a southward component. The most severe impacts are during the arrival of a coronal mass ejection (CME) when the magnetosphere is both compressed and magnetically connected to the heliospheric environment. Unfortunately, forecasting magnetic vectors within coronal mass ejections remain elusive. Here we report how, by combining a statistically robust helicity rule for a CME's solar origin with a simplified flux rope topology, the magnetic vectors within the Earth-directed segment of a CME can be predicted. In order to test the validity of this proof-of-concept architecture for estimating the magnetic vectors within CMEs, a total of eight CME events (between 2010 and 2014) have been investigated. With a focus on the large false alarm of January 2014, this work highlights the importance of including the early evolutionary effects of a CME for forecasting purposes. The angular rotation in the predicted magnetic field closely follows the broad rotational structure seen within the in situ data. This time-varying field estimate is implemented into a process to quantitatively predict a time-varying Kp index that is described in detail in paper II. Future statistical work, quantifying the uncertainties in this process, may improve the more heuristic approach used by early forecasting systems.
C1 [Savani, N. P.; Vourlidas, A.] Univ Maryland Baltimore Cty, GPHI, Baltimore, MD 21228 USA.
[Savani, N. P.; Szabo, A.; Mays, M. L.; Richardson, I. G.; Thompson, B. J.; Pulkkinen, A.; Nieves-Chinchilla, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mays, M. L.; Nieves-Chinchilla, T.] Catholic Univ Amer, IACS, Washington, DC 20064 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Evans, R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
RP Savani, NP (reprint author), Univ Maryland Baltimore Cty, GPHI, Baltimore, MD 21228 USA.
EM neel.savani02@imperial.ac.uk
RI Nieves-Chinchilla, Teresa/F-3482-2016; Thompson, Barbara/C-9429-2012;
Vourlidas, Angelos/C-8231-2009;
OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890; Vourlidas,
Angelos/0000-0002-8164-5948; Richardson, Ian/0000-0002-3855-3634
FU NASA [NNH14AX40I, S-136361-Y]
FX This work was supported by NASA grant NNH14AX40I and NASA contract
S-136361-Y to NRL. We thank Y.-M. Wang (NRL) for constructive comments
about active region helicity, and M. Stockman (SWPC) and B. Murtagh
(SWPC) for clarifying the forecasting policy and procedures at SWPC. We
thank M. Shankar for his lively debates throughout the process. The OMNI
data were obtained from the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov.
NR 60
TC 13
Z9 13
U1 0
U2 8
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 JUN
PY 2015
VL 13
IS 6
BP 374
EP 385
DI 10.1002/2015SW001171
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CM8NT
UT WOS:000357959400007
ER
PT J
AU Kong, AYY
Rosenzweig, C
Arky, J
AF Kong, Angela Y. Y.
Rosenzweig, Cynthia
Arky, Joshua
TI Nitrogen Dynamics Associated with Organic and Inorganic Inputs to
Substrate Commonly Used on Rooftop Farms
SO HORTSCIENCE
LA English
DT Article
DE compost; leachate; organic matter; potential mineralizable nitrogen;
rooftop farm; urban agriculture
ID MINERALIZABLE NITROGEN; QUALITY PERFORMANCE; MICROBIAL BIOMASS;
SWISS-CHARD; RUNOFF; SOILS; SYSTEMS; ECOSYSTEMS; MANAGEMENT; FERTILIZER
AB Employing rooftops for the cultivation of crops in limited urban space has garnered interest in densely populated cities in the United States, where there is a growing demand for locally sourced vegetable products. Fertility management recommendations for rooftop farming, however, are scant. With insufficient research on nutrient cycling within rooftop farming systems, which tend to use soilless substrates with low organic matter content, the potential tradeoffs between the negative impacts (e.g., nutrient runoff) and the benefits (e.g., increased locally produced vegetables, stormwater retention, etc.) associated with rooftop farms are unclear. The objective of this study was to evaluate the effects of organic and inorganic nitrogen (N) inputs on the N dynamics within substrate typically used on rooftop farms. Substrate without added N inputs (control) was compared with substrates receiving N sources that are both realistic for and/or reflective of amendments currently applied on urban rooftop farms: a synthetic fertilizer (Osmocote (R) 14N-4.2P-11.6K), and three organic N inputs composted poultry manure, municipal green waste (MGW) compost, and vermicompost. Aboveground crop biomass and yields of Beta vulgaris (swiss chard), along with inorganic N availability (ammonium: NH4+ and nitrate: NOD, potentially mineralizable nitrogen (PMN), leachate-inorganic N concentrations, and pH and electrical conductivity (EC) levels were measured during an 8-week greenhouse experiment. Despite differences in carbon-to-nitrogen ratios (C:N), few differences in N cycling and yields were found among the treatments receiving organic N inputs. Crop yields from the synthetic fertilizer and MGW compost treatments were higher than the other organic N input treatments. Inorganic N levels in the synthetic fertilizer treatment decreased from 129 mg N/L at the start of the season to 113 mg N/L at the end of the season, while nearly 10-fold decreases of inorganic N concentrations in the substrate of the control and organic N input treatments from week 0 (79.5-117.8 mg N/L) to week 8 (12.8-16.6 mg N/L) were observed. Greater N availability at critical periods during the season may have promoted greater crop N uptake efficiency and, therefore, higher yields in the system receiving synthetic fertilizer. However, the greatest losses of NH4+ and NO3- via leachate were also measured from this treatment. Our results show that the type of N input influenced plant-available N and yields and that the MGW compost treatment best achieved the balance between higher yields and reduced N losses to potential roof runoff. Furthermore, additional N inputs to these systems, particularly to the treatments receiving organic composts, will likely be necessary if a high N-demanding crop (such as swiss chard) is to be grown in the same substrates for more than 8 weeks. Rooftop farming is an emergent component of urban agriculture; regulations and guidelines for nutrient management of rooftop farms are necessary to optimize productivity and long-term benefits and to minimize negative environmental impacts.
C1 [Kong, Angela Y. Y.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10021 USA.
[Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10021 USA.
[Arky, Joshua] Columbia Univ, Off Acad & Res Programs, Earth Inst, Sustainable Dev, New York, NY 10021 USA.
RP Kong, AYY (reprint author), Columbia Univ, Ctr Climate Syst Res, 545 West 112th St, New York, NY 10021 USA.
EM ak3132@columbia.edu
NR 50
TC 1
Z9 1
U1 5
U2 39
PU AMER SOC HORTICULTURAL SCIENCE
PI ALEXANDRIA
PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA
SN 0018-5345
EI 2327-9834
J9 HORTSCIENCE
JI Hortscience
PD JUN
PY 2015
VL 50
IS 6
BP 806
EP 813
PG 8
WC Horticulture
SC Agriculture
GA CM5YY
UT WOS:000357766100008
ER
PT J
AU Andersson, AJ
Kline, DI
Edmunds, PJ
Archer, SD
Bednarsek, N
Carpenter, RC
Chadsey, M
Goldstein, P
Grottoli, AG
Hurst, TP
King, AL
Kubler, JE
Kuffner, IB
Mackey, KRM
Menge, BA
Paytan, A
Riebesell, U
Schnetzer, A
Warner, ME
Zimmerman, RC
AF Andersson, Andreas J.
Kline, David I.
Edmunds, Peter J.
Archer, Stephen D.
Bednarsek, Nina
Carpenter, Robert C.
Chadsey, Meg
Goldstein, Philip
Grottoli, Andrea G.
Hurst, Thomas P.
King, Andrew L.
Kuebler, Janet E.
Kuffner, Ilsa B.
Mackey, Katherine R. M.
Menge, Bruce A.
Paytan, Adina
Riebesell, Ulf
Schnetzer, Astrid
Warner, Mark E.
Zimmerman, Richard C.
TI Understanding Ocean Acidification Impacts on Organismal to Ecological
Scales
SO OCEANOGRAPHY
LA English
DT Editorial Material
ID CARBON-DIOXIDE; CORAL-REEFS; ANTHROPOGENIC CO2; MARINE ORGANISMS;
CALCIFICATION; PHOTOSYNTHESIS; ECOSYSTEM; PH; METAANALYSIS; MESOCOSM
AB Ocean acidification (OA) research seeks to understand how marine ecosystems and global elemental cycles will respond to changes in seawater carbonate chemistry in combination with other environmental perturbations such as warming, eutrophication, and deoxygenation. Here, we discuss the effectiveness and limitations of current research approaches used to address this goal. A diverse combination of approaches is essential to decipher the consequences of OA to marine organisms, communities, and ecosystems. Consequently, the benefits and limitations of each approach must be considered carefully. Major research challenges involve experimentally addressing the effects of OA in the context of large natural variability in seawater carbonate system parameters and other interactive variables, integrating the results from different research approaches, and scaling results across different temporal and spatial scales.
C1 [Andersson, Andreas J.; Kline, David I.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Edmunds, Peter J.; Carpenter, Robert C.; Kuebler, Janet E.] Calif State Univ Northridge, Northridge, CA 91330 USA.
[Archer, Stephen D.] Bigelow Lab Ocean Sci, East Boothbay, ME USA.
[Bednarsek, Nina] NOAA, Pacific Marine Environm Lab, Newport, OR USA.
[Chadsey, Meg] Washington Sea Grant, Seattle, WA USA.
[Goldstein, Philip] Univ Colorado, Boulder, CO 80309 USA.
[Grottoli, Andrea G.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Hurst, Thomas P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Hatfield Marine Sci Ctr, Newport, OR USA.
[King, Andrew L.] NOAA, Northeast Fisheries Sci Ctr, Silver Spring, MD USA.
[Kuffner, Ilsa B.] US Geol Survey, St Petersburg, FL USA.
[Mackey, Katherine R. M.] Univ Calif Irvine, Earth Syst Sci, Irvine, CA USA.
[Menge, Bruce A.] Oregon State Univ, Integrat Biol, Corvallis, OR 97331 USA.
[Menge, Bruce A.] Oregon State Univ, Marine Biol, Corvallis, OR 97331 USA.
[Paytan, Adina] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Riebesell, Ulf] GEOMAR Helmholtz Ctr Ocean Res, Biol Oceanog, Kiel, Germany.
[Schnetzer, Astrid] N Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
[Warner, Mark E.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE USA.
[Zimmerman, Richard C.] Old Dominion Univ, Earth Ocean & Atmospher Sci, Norfolk, VA USA.
RP Andersson, AJ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM aandersson@ucsd.edu; dkline@ucsd.edu
OI Kuffner, Ilsa/0000-0001-8804-7847
NR 88
TC 12
Z9 12
U1 9
U2 94
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 16
EP 27
PG 12
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700005
ER
PT J
AU Busch, DS
O'Donnell, MJ
Hauri, C
Mach, KJ
Poach, M
Doney, SC
Signorini, SR
AF Busch, D. Shallin
O'Donnell, Michael J.
Hauri, Claudine
Mach, Katharine J.
Poach, Matthew
Doney, Scott C.
Signorini, Sergio R.
TI Understanding, Characterizing, and Communicating Responses to Ocean
Acidification CHALLENGES AND UNCERTAINTIES
SO OCEANOGRAPHY
LA English
DT Article
ID MARINE ORGANISMS; CLIMATE-CHANGE; CORAL-REEFS; ECOSYSTEM; IMPACTS;
SCIENCE; CO2; COMMUNITIES; ADAPTATION; STRESSORS
AB Over the past decade, ocean acidification (OA) has emerged as a major concern in ocean science. The field of OA is based on certainties-update of carbon dioxide into the global ocean alters its carbon chemistry, and many marine organisms, especially calcifiers, are sensitive to this change. However, the field must accommodate uncertainties about the seriousness of these impacts as it synthesizes and draws conclusions from multiple disciplines. There is pressure from stakeholders to expeditiously inform society about the extent to which OA will impact marine ecosystems and the people who depend on them. Ultimately, decisions about actions related to OA require evaluating risks about the likelihood and magnitude of these impacts. As the scientific literature accumulates, some of the uncertainty related to single-species sensitivity to OA is diminishing. Difficulties remain in scaling laboratory results to species and ecosystem responses in nature, though modeling exercises provide useful insight. As recognition of OA grows scientists' ability to communicate the certainties and uncertainties of our knowledge on OA is crucial for interaction with decision makers. In this regard, there are a number of valuable practices that can be drawn from other fields, especially the global climate change community. A generally accepted set of best practices that scientists follow in their discussions of uncertainty would be helpful for the community engaged in ocean acidification.
C1 [Busch, D. Shallin] NOAA, Ocean Acidificat Program, Silver Spring, MD USA.
[Busch, D. Shallin] NOAA, Natl Marine Fisheries Serv, Off Sci & Technol, Silver Spring, MD USA.
[O'Donnell, Michael J.] Calif Ocean Sci Trust, Oakland, CA USA.
[Hauri, Claudine] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
[Hauri, Claudine] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK USA.
[Mach, Katharine J.] Carnegie Inst Sci, IPCC Working Grp Tech Support Unit 2, Dept Global Ecol, Sci, Stanford, CA USA.
[Poach, Matthew] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, NMFS, Highlands, NJ USA.
[Doney, Scott C.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA.
[Signorini, Sergio R.] Sci Applicat Int Corp, Mclean, VA 22102 USA.
[Signorini, Sergio R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Busch, DS (reprint author), NOAA, Ocean Acidificat Program, Seattle, WA 98115 USA.
EM shallin.busch@noaa.gov
RI Doney, Scott/F-9247-2010
OI Doney, Scott/0000-0002-3683-2437
FU NOAA Ocean Acidification Program; National Marine Fisheries Service;
NSF-supported Center for Climate and Energy Decision Making; NASA Ocean
Biology and Biogeochemistry Program
FX We thank the organizers of the 2013 OA Principal Investigators Meeting
for their efforts to build a community of OA researchers and for their
foresight in providing us the venue to develop the themes discussed in
this paper. W. Balch, F. Dobbs, H. Galindo, J. Grear, F. Morel, S.
Palumbi, M. Saito, and C. Zakroff contributed to the initial discussions
around uncertainty. R. Brainard and an anonymous reviewer provided
comments that improved the manuscript The following funding sources
supported our work on this manuscript: NOAA Ocean Acidification Program
and National Marine Fisheries Service (DSB, MP), NSF-supported Center
for Climate and Energy Decision Making (SCD), and NASA Ocean Biology and
Biogeochemistry Program (SS). The content of this manuscript does not
reflect any position of the US Government or of NOAA.
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PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 30
EP 39
DI 10.5670/oceanog.2015.29
PG 10
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700007
ER
PT J
AU Alin, SR
Brainard, RE
Price, NN
Newton, JA
Cohen, A
Peterson, WT
DeCarlo, EH
Shadwick, EH
Noakes, S
Bednarsek, N
AF Alin, Simone R.
Brainard, Russell E.
Price, Nichole N.
Newton, Jan A.
Cohen, Anne
Peterson, William T.
DeCarlo, Eric H.
Shadwick, Elizabeth H.
Noakes, Scott
Bednarsek, Nina
TI Characterizing the Natural System: Toward Sustained, Integrated Coastal
Ocean Acidification Observing Networks to Facilitate Resource Management
and Decision Support
SO OCEANOGRAPHY
LA English
DT Article
ID CONTINENTAL-SHELF; ECOSYSTEMS; SATURATION; PACIFIC; IMPACTS; CARBON
AB Coastal ocean ecosystems have always served human populations they provide food security, livelihoods, coastal protection, and defense. Ocean acidification is a global threat to these ecosystem services, particularly when other local and regional stressors combine with it to jeopardize coastal health. Monitoring efforts call for a coordinated global approach toward sustained, integrated coastal ocean health observing networks to address the region-specific mix of factors while also adhering to global ocean acidification observing network principles to facilitate comparison among regions for increased utility and understanding. Here, we generalize guidelines for scoping and designing regional coastal ocean acidification observing networks and provide examples of existing efforts. While challenging in the early stages of coordinating the design and prioritizing the implementation Of these observing networks, it is essential to actively engage all of the relevant stakeholder groups from the outset, including private industries, public agencies, regulatory bodies, decision makers, and the general public. The long-term sustainability of these critical observing networks will rely on leveraging of resources and the strength of partnerships across the consortium of stakeholders and those implementing coastal ocean health observing networks.
C1 [Alin, Simone R.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Brainard, Russell E.] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI USA.
[Price, Nichole N.] Bigelow Lab Ocean Sci, East Boothbay, ME USA.
[Newton, Jan A.] Univ Washington, Washington Ocean Acidificat Ctr, Seattle, WA 98195 USA.
[Cohen, Anne] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Peterson, William T.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA.
[DeCarlo, Eric H.] Univ Hawaii Manoa, Dept Oceanog, Marine Geol & Geochem Div, Honolulu, HI 96822 USA.
[Shadwick, Elizabeth H.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
[Noakes, Scott] Univ Georgia, Ctr Appl Isotope Studies, Athens, GA 30602 USA.
[Bednarsek, Nina] Univ Washington, Sch Marine & Environm Affairs, Seattle, WA 98195 USA.
RP Alin, SR (reprint author), NOAA, Pacific Marine Environm Lab, 7600 Sand Point Way Ne, Seattle, WA 98115 USA.
EM simone.r.alin@noaa.gov
FU National Science Foundation; National Aeronautics and Space
Administration; National Oceanic and Atmospheric Administration
FX The authors wish to thank the Ocean Carbon and Biogeochemistry Program
and its Ocean Acidification Subcommittee for organizing and hosting the
Second Ocean Acidification Principal Investigators' Meeting, where the
foundation for this article was laid. We also thank the National Science
Foundation, National Aeronautics and Space Administration, and the
National Oceanic and Atmospheric Administration for funding the meeting,
as well as much of the science that informed our productive discussions.
We thank Jon Hare for discussion that particularly improved the
manuscript, as well as Richard Feely, the editors, and two anonymous
reviewers for constructive reviews on earlier versions. Alin thanks
NOAAs Ocean Acidification Program and Pacific Marine Environmental
Laboratory (PMEL contribution number 4267) for supporting her role in
the meeting and paper.
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SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 92
EP 107
DI 10.5670/oceanog.2015.34
PG 16
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700012
ER
PT J
AU Salisbury, J
Vandemark, D
Jonsson, B
Balch, W
Chakraborty, S
Lohrenz, S
Chapron, B
Hales, B
Mannino, A
Mathis, JT
Reul, N
Signorini, SR
Wanninkhof, R
Yates, KK
AF Salisbury, Joseph
Vandemark, Douglas
Joensson, Bror
Balch, William
Chakraborty, Sumit
Lohrenz, Steven
Chapron, Bertrand
Hales, Burke
Mannino, Antonio
Mathis, Jeremy T.
Reul, Nicolas
Signorini, Sergio R.
Wanninkhof, Rik
Yates, Kimberly K.
TI How Can Present and Future Satellite Missions Support Scientific Studies
that Address Ocean Acidification?
SO OCEANOGRAPHY
LA English
DT Article
ID NEURAL-NETWORK TECHNIQUES; SEA-SURFACE TEMPERATURE; CONTINENTAL-SHELF;
UPWELLING SYSTEM; TOTAL ALKALINITY; NORTH-ATLANTIC; RIVER PLUME; CO2;
PHYTOPLANKTON; CARBON
AB Space-based observations offer unique capabilities for studying spatial and temporal dynamics of the upper ocean inorganic carbon cycle and, in turn, supporting research tied to ocean acidification (OA). Satellite sensors measuring sea surface temperature, color, salinity, wind, waves, currents, and sea level enable a fuller understanding of a range of physical, chemical, and biological phenomena that drive regional OA dynamics as well as the potentially varied impacts of carbon cycle change on a broad range of ecosystems. Here, we update and expand on previous work that addresses the benefits of space-based' assets for OA and carbonate system studies. Carbonate chemistry and the key processes controlling surface ocean OA variability are reviewed. Synthesis of present satellite data streams and their utility in this arena are discussed, as are opportunities on the horizon for using new satellite sensors with increased spectral, temporal, and/or spatial resolution. We outline applications that include the ability to track the biochemically dynamic nature of water masses, to map coral reefs at higher resolution, to discern functional phytoplankton groups and their relationships to acid perturbations, and to track processes that contribute to acid variation near the land-ocean interface.
C1 [Salisbury, Joseph; Vandemark, Douglas] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Joensson, Bror] Princeton Univ, Geosci, Princeton, NJ 08544 USA.
[Balch, William] Bigelow Lab Ocean Sci, East Boothbay, ME USA.
[Chakraborty, Sumit; Lohrenz, Steven] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA USA.
[Chapron, Bertrand] IFREMER, Lab Oceanog Spatiale, Plouzane, France.
[Hales, Burke] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Mannino, Antonio] NASA, Goddard Space Flight Ctr, Ocean Ecol Div, Greenbelt, MD 20771 USA.
[Mathis, Jeremy T.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Reul, Nicolas] IFREMER, Lab Oceanog Spatiale, La Seyne Sur Mer, France.
[Signorini, Sergio R.] Sci Applicat Int Corp, Mclean, VA 22102 USA.
[Signorini, Sergio R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wanninkhof, Rik] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Yates, Kimberly K.] US Geol Survey, St Petersburg, FL USA.
RP Salisbury, J (reprint author), Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
EM joe.salisbury@unh.edu
RI Chapron, Bertrand/O-6527-2015; reul, nicolas/C-4895-2009; Mannino,
Antonio/I-3633-2014;
OI Lohrenz, Steven/0000-0003-3811-2975; Reul, Nicolas/0000-0003-4881-2967
FU NASA Ocean Biology & Biogeochemistry program [NNX14AL84G]; NOAA Ocean
Acidification Program and Integrated Ocean Observing System programs,
Northeastern Regional Association of Coastal Ocean Observing Systems
(NERACOOS) [A002004, USM-GR05194-001]; National Oceanic and Atmospheric
Administration (NOAA)'s Ocean Acidification Program; NOAA's Pacific
Marine Environmental Laboratory (PMEL) [4303]; Pathfinder ESA-STSE Ocean
Acidification; National Science Foundation
FX We gratefully acknowledge our sponsors whose grants made this
collaboration possible. The NASA Ocean Biology & Biogeochemistry program
(particularly NNX14AL84G), the NOAA Ocean Acidification Program and
Integrated Ocean Observing System programs, including Northeastern
Regional Association of Coastal Ocean Observing Systems (NERACOOS)
grants A002004 and USM-GR05194-001, Pathfinder ESA-STSE Ocean
Acidification, and the National Science Foundation. Background and
satellite images in Figure 1 are courtesy of NASA, except the GOCI
satellite image, which is courtesy of the Korea Ocean Satellite Research
Center and the SMOS satellite image, which is courtesy of the European
Space Agency. Aquarius is a joint mission shared by NASA and CONAE. We
appreciate the insightful critiques of Frank Muller-Karger, Nick
Hardman-Mountford, and one anonymous reviewer, and thank Amy Ehntholt
and Kristy Donahue for valuable help. References to non-USGS products
and services are provided for information only and do not constitute
endorsement or warranty, expressed or implied, by the US Government, as
to their suitability, content, usefulness, functioning, completeness, or
accuracy. We acknowledge funding support from the National Oceanic and
Atmospheric Administration (NOAA)'s Ocean Acidification Program and
NOAA's Pacific Marine Environmental Laboratory (PMEL contribution number
4303).
NR 90
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PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 108
EP 121
DI 10.5670/oceanog.2015.35
PG 14
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700013
ER
PT J
AU Boehm, AB
Jacobson, MZ
O'Donnell, MJ
Sutula, M
Wakefield, WW
Weisberg, SB
Whiteman, E
AF Boehm, Alexandria B.
Jacobson, Mark Z.
O'Donnell, Michael J.
Sutula, Martha
Wakefield, W. Waldo
Weisberg, Stephen B.
Whiteman, Elizabeth
TI Ocean Acidification Science Needs for Natural Resource Managers of the
North American West Coast
SO OCEANOGRAPHY
LA English
DT Article
ID CALIFORNIA CURRENT SYSTEM; SEAWATER PH; CHEMISTRY; IMPACT;
EUTROPHICATION; ADAPTATION; ORGANISMS; ECOSYSTEM; CO2
AB Natural circulation patterns along the west coast of North America periodically draw subthermocline, low pH waters into shallow coastal areas. The presence of corrosive, low pH waters, caused by ocean acidification (OA), is frequently observed along the North American west coast. Reduction of global atmospheric CO, inputs is the appropriate management focus for decreasing OA, but there are also many management decisions made at regional to local spatial scales that can lessen the exposure to or limit the effects of atmospheric CO,. Here, we describe these local management actions and identify the science needs that would assist local managers in deciding whether, and how best, to address local OA. Science needs are diverse, but three commonalities emerge. First, managers need a comprehensive monitoring program that expands understanding of spatial and temporal OA patterns and how OA changes influence marine ecosystems. Second, they require mechanistic, process-based models that differentiate natural from anthropogenically driven OA patterns and the extent to which local actions would affect OA conditions in context of what is largely a global atmospheric-driven phenomenon. Models present the opportunity to visualize outcomes with and without the changes in management actions included in model scenarios. Third, managers need models that identify which locales are most and least vulnerable to future changes due to OA. Understanding vulnerability will assist managers in better siting facilities (e.g., aquaria) or protecting marine resources. The required monitoring and modeling are all achievable, with much of the necessary research and development already underway. The challenge will be to ensure good and continuing communication between the management community that requires the information and the scientific community that is often hesitant to provide recommendations while uncertainty remains high.
C1 [Boehm, Alexandria B.; Jacobson, Mark Z.] Stanford Univ, Environm & Water Studies Civil & Environm Engn, Stanford, CA 94305 USA.
[O'Donnell, Michael J.; Whiteman, Elizabeth] Calif Ocean Sci Trust, Oakland, CA USA.
[Sutula, Martha] Southern Calif Coastal Water Res Project, Dept Biochem, Costa Mesa, CA USA.
[Wakefield, W. Waldo] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA.
[Weisberg, Stephen B.] Southern Calif Coastal Water Res Project, Costa Mesa, CA USA.
RP Boehm, AB (reprint author), Stanford Univ, Environm & Water Studies Civil & Environm Engn, Stanford, CA 94305 USA.
EM aboehm@stanford.edu
RI Weisberg, Stephen/B-2477-2008
OI Weisberg, Stephen/0000-0002-0655-9425
FU California Ocean Protection Council; California Ocean Science Trust;
Institute of Natural Resources, Oregon
FX This paper is a product of the West Coast Ocean Acidification and
Hypoxia Science Panel. It was developed by a working group that included
panel members and relevant external experts, and it has received input
from the full panel. The Panel is convened by the California Ocean
Science Trust and is supported by the California Ocean Protection
Council, the California Ocean Science Trust, and the Institute of
Natural Resources, Oregon. The authors acknowledge Meg Caldwell, who
provided input to an early version of the manuscript.
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PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 170
EP 181
DI 10.5670/oceanog.2015.40
PG 12
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700018
ER
PT J
AU Gledhill, DK
White, MM
Salisbury, J
Thomas, H
Mlsna, I
Liebman, M
Mook, B
Grear, J
Candelmo, AC
Chambers, RC
Gobler, CJ
Hunt, CW
King, AL
Price, NN
Signorini, SR
Standoff, E
Stymiest, C
Wahle, RA
Waller, JD
Rebuck, ND
Wang, ZHA
Capson, TL
Morrison, JR
Cooley, SR
Doney, SC
AF Gledhill, Dwight K.
White, Meredith M.
Salisbury, Joseph
Thomas, Helmuth
Mlsna, Ivy
Liebman, Matthew
Mook, Bill
Grear, Jason
Candelmo, Allison C.
Chambers, R. Christopher
Gobler, Christopher J.
Hunt, Christopher W.
King, Andrew L.
Price, Nichole N.
Signorini, Sergio R.
Standoff, Esperanza
Stymiest, Cassie
Wahle, Richard A.
Waller, Jesica D.
Rebuck, Nathan D.
Wang, Zhaohui A.
Capson, Todd L.
Morrison, J. Ruairidh
Cooley, Sarah R.
Doney, Scott C.
TI Ocean and Coastal Acidification off New England and Nova Scotia
SO OCEANOGRAPHY
LA English
DT Article
ID ELEVATED CARBON-DIOXIDE; CALANUS-FINMARCHICUS GUNNERUS; COD
GADUS-MORHUA; ARGOPECTEN-IRRADIANS; JUVENILE BIVALVES; SATURATION STATE;
MARINE ORGANISMS; NORTH-ATLANTIC; CLIMATE-CHANGE; UNITED-STATES
AB New England coastal and adjacent Nova Scotia shelf waters have a reduced buffering capacity because of significant freshwater input, making the regions waters potentially more vulnerable to coastal acidification. Nutrient loading and heavy precipitation events further acidify the regions poorly buffered coastal waters. Despite the apparent vulnerability of these waters, and fisheries and maricultures significant dependence on calcifying species, the community lacks the ability to confidently predict how the regions ecosystems will respond to continued ocean and coastal acidification. Here, we discuss ocean and coastal acidification processes specific to New England coastal and Nova Scotia shelf waters and review current understanding of the biological consequences most relevant to the region. We also identify key research and monitoring needs to be addressed and highlight existing capacities that should be leveraged to advance a regional understanding of ocean and coastal acidification.
C1 [Gledhill, Dwight K.] NOAA, Ocean Acidificat Program, Silver Spring, MD 20910 USA.
[White, Meredith M.; Price, Nichole N.; Waller, Jesica D.] Bigelow Lab Ocean Sci, East Boothbay, ME USA.
[Salisbury, Joseph] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Thomas, Helmuth] Dalhousie Univ, Dept Oceanog, Halifax, NS, Canada.
[Mlsna, Ivy] US EPA, Off Water, Oak Ridge Inst Sci Educ, Boston, MA USA.
[Liebman, Matthew] US EPA, Boston, MA USA.
[Mook, Bill] Mook Seafarm Inc, Walpole, ME USA.
[Grear, Jason] US EPA, Populat Ecol Branch, Narragansett, RI USA.
[Candelmo, Allison C.] NOAA, Northeast Fisheries Sci Ctr NEFSC, Sandy Hook, NJ USA.
[Chambers, R. Christopher] NOAA, NEFSC, Sandy Hook, NJ USA.
[Gobler, Christopher J.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Hunt, Christopher W.] Univ New Hampshire, Nat Resources & Earth Syst Sci PhD Program, Durham, NH 03824 USA.
[King, Andrew L.] Norwegian Inst Water Res, Oslo, Norway.
[Signorini, Sergio R.] NASA, Sci Applicat Int Corp, Goddard Space Flight Ctr, Crofton, MD USA.
[Standoff, Esperanza] Univ Maine Cooperat Extens & Sea Grant, Waldoboro, ME USA.
[Stymiest, Cassie] Northeast Reg Assoc Coastal Ocean Observing Syst, Portsmouth, Hants, England.
[Wahle, Richard A.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA.
[Waller, Jesica D.] Univ Maine, Sch Marine Sci, Walpole, ME USA.
[Rebuck, Nathan D.] NOAA, NEFSC, Narragansett, RI USA.
[Wang, Zhaohui A.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA.
[Capson, Todd L.] Sustainable Fisheries Partnership, Washington, DC USA.
[Morrison, J. Ruairidh] NERACOOS, Portsmouth, NH USA.
[Cooley, Sarah R.] Ocean Conservancy, Washington, DC USA.
[Doney, Scott C.] WHOI, Marine Chem & Geochem, Woods Hole, MA USA.
RP Gledhill, DK (reprint author), NOAA, Ocean Acidificat Program, Silver Spring, MD 20910 USA.
EM dwight.gledhill@noaa.gov
RI Doney, Scott/F-9247-2010;
OI Doney, Scott/0000-0002-3683-2437; White, Meredith/0000-0001-8113-9618;
Hunt, Christopher/0000-0001-8061-4560
FU National Oceanic and Atmospheric Administration (NOAA) US Integrated
Ocean Observing System (IOOS) Award [NA11NOS0120034];
Internship/Research Participation Program at the Office of Water, US
Environmental Protection Agency (EPA); NASA [NNX14AL84G NASA-CCS]
FX NECAN thanks the presenters of the NECAN webinar series and participants
at the state-of-science workshop for thoughtful insights. For a complete
listing of participants and contributors, please consult the NECAN
website (http://www.neracoos.org/necan). NECAN is coordinated in part by
NERACOOS (http://www.neracoos.org), with funding from the National
Oceanic and Atmospheric Administration (NOAA) US Integrated Ocean
Observing System (IOOS) Award #NA11NOS0120034. This project was
supported in part by an appointment to the Internship/Research
Participation Program at the Office of Water, US Environmental
Protection Agency (EPA), administered by the Oak Ridge Institute for
Science and Education through an interagency agreement between the US
Department of Energy and the EPA. JS acknowledges support from NASA
grant from NNX14AL84G NASA-CCS. The scientific results and conclusions,
as well as any views or opinions expressed herein, are those of the
authors and do not necessarily reflect the views of any of the federal
agencies with which any of the contributing authors may be affiliated.
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PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2015
VL 28
IS 2
SI SI
BP 182
EP 197
DI 10.5670/oceanog.2015.41
PG 16
WC Oceanography
SC Oceanography
GA CL8NP
UT WOS:000357231700019
ER
PT J
AU Choi, CR
Woo, MH
Dokgo, K
Choi, EJ
Min, KW
Hwang, J
Park, YD
Lee, DY
AF Choi, C. -R.
Woo, M. -H.
Dokgo, K.
Choi, E. -J.
Min, K. -W.
Hwang, J.
Park, Y. -D.
Lee, D. -Y.
TI Pitch-angle diffusion of electrons through growing and propagating along
a magnetic field electromagnetic wave in Earth's radiation belts
SO PHYSICS OF PLASMAS
LA English
DT Article
ID ION-CYCLOTRON WAVES; STOCHASTIC ACCELERATION; PARTICLE INTERACTIONS;
GEOMAGNETIC STORMS; PRECIPITATION; SCATTERING; MAGNETOSPHERE; GROWTH
AB The diffusion of electrons via a linearly polarized, growing electromagnetic (EM) wave propagating along a uniform magnetic field is investigated. The diffusion of electrons that interact with the growing EM wave is investigated through the autocorrelation function of the parallel electron acceleration in several tens of electron gyration timescales, which is a relatively short time compared with the bounce time of electrons between two mirror points in Earth's radiation belts. Furthermore, the pitch-angle diffusion coefficient is derived for the resonant and non-resonant electrons, and the effect of the wave growth on the electron diffusion is discussed. The results can be applied to other problems related to local acceleration or the heating of electrons in space plasmas, such as in the radiation belts. (C) 2015 AIP Publishing LLC.
C1 [Choi, C. -R.; Dokgo, K.; Choi, E. -J.; Min, K. -W.] Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 305701, South Korea.
[Woo, M. -H.] Natl Fus Res Inst, Taejon 305333, South Korea.
[Hwang, J.; Park, Y. -D.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Lee, D. -Y.] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea.
[Choi, E. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Choi, CR (reprint author), Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 305701, South Korea.
EM crchoi@kaist.ac.kr
RI Min, Kyoung Wook/C-1948-2011
FU Korea Astronomy and Space Science Institute (KASI) under an RD program
[2013-1-600-01]; "Planetary system research for space exploration"
project; KASI; National Research Foundation of Korea
[2014M1A3A3A02034585]
FX This research was supported by the Korea Astronomy and Space Science
Institute (KASI) under an R&D program (Project No. 2013-1-600-01)
supervised by the Ministry of Science, ICT and Future Planning (Korea).
This work was also supported by "Planetary system research for space
exploration," project and the basic research funding from KASI. C.-R.
Choi acknowledges the support of the National Research Foundation of
Korea through Grant No. 2014M1A3A3A02034585.
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U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD JUN
PY 2015
VL 22
IS 6
AR 062903
DI 10.1063/1.4923267
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA CM4XN
UT WOS:000357689500052
ER
PT J
AU Yang, JS
Barrila, J
Roland, KL
Kilbourne, J
Ott, CM
Forsyth, RJ
Nickerson, CA
AF Yang, Jiseon
Barrila, Jennifer
Roland, Kenneth L.
Kilbourne, Jacquelyn
Ott, C. Mark
Forsyth, Rebecca J.
Nickerson, Cheryl A.
TI Characterization of the Invasive, Multidrug Resistant Non-typhoidal
Salmonella Strain D23580 in a Murine Model of Infection
SO PLOS NEGLECTED TROPICAL DISEASES
LA English
DT Article
ID ENTERICA SEROVAR TYPHIMURIUM; NONTYPHOIDAL SALMONELLA; SEROTYPE
ENTERITIDIS; ESCHERICHIA-COLI; ACID RESISTANCE; SIGMA-FACTOR; FLAGELLA;
AFRICA; VIRULENCE; ADULTS
AB A distinct pathovar of Salmonella enterica serovar Typhimurium, ST313, has emerged in sub-Saharan Africa as a major cause of fatal bacteremia in young children and HIV-infected adults. D23580, a multidrug resistant clinical isolate of ST313, was previously shown to have undergone genome reduction in a manner that resembles that of the more human-restricted pathogen, Salmonella enterica serovar Typhi. It has since been shown through tissue distribution studies that D23580 is able to establish an invasive infection in chickens. However, it remains unclear whether ST313 can cause lethal disease in a non-human host following a natural course of infection. Herein we report that D23580 causes lethal and invasive disease in a murine model of infection following peroral challenge. The LD50 of D23580 in female BALB/c mice was 4.7 x 10(5) CFU. Tissue distribution studies performed 3 and 5 days post-infection confirmed that D23580 was able to more rapidly colonize the spleen, mesenteric lymph nodes and gall bladder in mice when compared to the well-characterized S. Typhimurium strain SL1344. D23580 exhibited enhanced resistance to acid stress relative to SL1344, which may lend towards increased capability to survive passage through the gastrointestinal tract as well as during its intracellular lifecycle. Interestingly, D23580 also displayed higher swimming motility relative to SL1344, S. Typhi strain Ty2, and the ST313 strain A130. Biochemical tests revealed that D23580 shares many similar metabolic features with SL1344, with several notable differences in the Voges-Proskauer and catalase tests, as well alterations in melibiose, and inositol utilization. These results represent the first full duration infection study using an ST313 strain following the entire natural course of disease progression, and serve as a benchmark for ongoing and future studies into the pathogenesis of D23580.
C1 [Yang, Jiseon; Barrila, Jennifer; Roland, Kenneth L.; Kilbourne, Jacquelyn; Forsyth, Rebecca J.; Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85281 USA.
[Ott, C. Mark] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
[Nickerson, Cheryl A.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA.
RP Yang, JS (reprint author), Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85281 USA.
EM Cheryl.Nickerson@asu.edu
FU NASA [NNX09AH40G]; Graduate Student Facilities Award, School of Life
Sciences, Arizona State University; NIH [R01 AI60557, R21 AI105479]
FX This research was funded by NASA grant NNX09AH40G (CAN), Graduate
Student Facilities Award, School of Life Sciences, Arizona State
University (JY), NIH grants R01 AI60557 and R21 AI105479 (KLR). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
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PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1935-2735
J9 PLOS NEGLECT TROP D
JI Plos Neglect. Trop. Dis.
PD JUN
PY 2015
VL 9
IS 6
AR e0003839
DI 10.1371/journal.pntd.0003839
PG 17
WC Infectious Diseases; Parasitology; Tropical Medicine
SC Infectious Diseases; Parasitology; Tropical Medicine
GA CM0VX
UT WOS:000357398100041
PM 26091096
ER
PT J
AU Acero, F
Ackermann, M
Ajello, M
Albert, A
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Belfiore, A
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bogart, JR
Bonino, R
Bottacini, E
Bregeon, J
Britto, RJ
Bruel, P
Buehler, R
Burnett, TH
Buson, S
Caliandro, GA
Cameron, RA
Caputo, R
Caragiulo, M
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Charles, E
Chaves, RCG
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Cominsky, LR
Conrad, J
Cutini, S
D'Ammando, F
de Angelis, A
DeKlotz, M
de Palma, F
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
Dubois, R
Dumora, D
Favuzzi, C
Fegan, SJ
Ferrara, EC
Finke, J
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guillemot, L
Guiriec, S
Hadasch, D
Harding, AK
Hays, E
Hewitt, JW
Hill, AB
Horan, D
Iafrate, G
Jogler, T
Johannesson, G
Johnson, RP
Johnson, AS
Johnson, TJ
Johnson, WN
Kamae, T
Kataoka, J
Katsuta, J
Kuss, M
La Mura, G
Landriu, D
Larsson, S
Latronico, L
Lemoine-Goumard, M
Li, J
Li, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Massaro, F
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mirabal, N
Mizuno, T
Moiseev, AA
Mongelli, M
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nuss, E
Ohno, M
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Racusin, JL
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Rochester, LS
Romani, RW
Salvetti, D
Sanchez-Conde, M
Parkinson, PMS
Schulz, A
Siskind, EJ
Smith, DA
Spada, F
Spandre, G
Spinelli, P
Stephens, TE
Strong, AW
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, Y
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tibolla, O
Torres, DF
Torresi, E
Tosti, G
Troja, E
Van Klaveren, B
Vianello, G
Winer, BL
Wood, KS
Wood, M
Zimmer, S
AF Acero, F.
Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Belfiore, A.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bogart, J. R.
Bonino, R.
Bottacini, E.
Bregeon, J.
Britto, R. J.
Bruel, P.
Buehler, R.
Burnett, T. H.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caputo, R.
Caragiulo, M.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Charles, E.
Chaves, R. C. G.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Cominsky, L. R.
Conrad, J.
Cutini, S.
D'Ammando, F.
de Angelis, A.
DeKlotz, M.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Dubois, R.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Finke, J.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Hays, E.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Iafrate, G.
Jogler, T.
Johannesson, G.
Johnson, R. P.
Johnson, A. S.
Johnson, T. J.
Johnson, W. N.
Kamae, T.
Kataoka, J.
Katsuta, J.
Kuss, M.
La Mura, G.
Landriu, D.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Massaro, F.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mirabal, N.
Mizuno, T.
Moiseev, A. A.
Mongelli, M.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nuss, E.
Ohno, M.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Racusin, J. L.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Rochester, L. S.
Romani, R. W.
Salvetti, D.
Sanchez-Conde, M.
Parkinson, P. M. Saz
Schulz, A.
Siskind, E. J.
Smith, D. A.
Spada, F.
Spandre, G.
Spinelli, P.
Stephens, T. E.
Strong, A. W.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, Y.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tibolla, O.
Torres, D. F.
Torresi, E.
Tosti, G.
Troja, E.
Van Klaveren, B.
Vianello, G.
Winer, B. L.
Wood, K. S.
Wood, M.
Zimmer, S.
TI FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-rays: general
ID GAMMA-RAY EMISSION; PULSAR WIND NEBULA; ALL-SKY SURVEY; ACTIVE GALACTIC
NUCLEI; PSR B1259-63/LS 2883; SUPERNOVA REMNANT; RADIO-SOURCES;
UNASSOCIATED SOURCES; GLOBULAR-CLUSTERS; WMAP OBSERVATIONS
AB We present the third Fermi Large Area Telescope (LAT) source catalog (3FGL) of sources in the 100 MeV-300 GeV range. Based on the first 4 yr of science data from the Fermi Gamma-ray Space Telescope mission, it is the deepest yet in this energy range. Relative to the Second Fermi LAT catalog, the 3FGL catalog incorporates twice as much data, as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse.-ray emission, a refined procedure for source detection, and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above 4 sigma significance, with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 238 sources are considered as identified based on angular extent or correlated variability (periodic or otherwise) observed at other wavelengths. For 1010 sources we have not found plausible counterparts at other wavelengths. More than 1100 of the identified or associated sources are active galaxies of the blazar class; several other classes of non-blazar active galaxies are also represented in the 3FGL. Pulsars represent the largest Galactic source class. From source counts of Galactic sources we estimate that the contribution of unresolved sources to the Galactic diffuse emission is similar to 3% at 1 GeV.
C1 [Acero, F.; Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Landriu, D.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Van Klaveren, B.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Van Klaveren, B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Caputo, R.; Johnson, R. P.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Caputo, R.; Johnson, R. P.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.; Conrad, J.; Larsson, S.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Desiante, R.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Belfiore, A.; Caraveo, P. A.; Salvetti, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Mongelli, M.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Chaves, R. C. G.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34059 Montpellier, France.
[Britto, R. J.; Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Bruel, P.; Fegan, S. J.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France.
[Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Chekhtman, A.; Johnson, T. J.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Cheung, C. C.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy.
[DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA.
[de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Dumora, D.; Grondin, M. -H.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J. W.; McEnery, J. E.; Mirabal, N.; Moiseev, A. A.; Perkins, J. S.; Racusin, J. L.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Katsuta, J.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Guillemot, L.] Univ Orleans CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France.
Observ Paris, CNRS INSU, Stn Radioastron Nancay, F-18330 Nancay, France.
[Hadasch, D.; La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Hadasch, D.; La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, E-08193 Barcelona, Spain.
[Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Massaro, F.] Yale Univ, Dept Astron, Dept Phys, New Haven, CT 06520 USA.
[Massaro, F.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.; Tanaka, Y.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, 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.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stephens, T. E.] Brigham Young Univ, Harold B Lee Lib, Provo, UT 84602 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Tibolla, O.] Univ Autonoma Chiapas UNACH, MCTP, Tuxtla Gutierrez 29050, Chiapas, Mexico.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Torresi, E.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
RP Acero, F (reprint author), CEA IRFU CNRS Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
EM jean.ballet@cea.fr; tburnett@u.washington.edu;
elisabetta.cavazzuti@asdc.asi.it; digel@stanford.edu
RI Di Venere, Leonardo/C-7619-2017; Bissaldi, Elisabetta/K-7911-2016;
Massaro, Francesco/L-9102-2016; Morselli, Aldo/G-6769-2011; Reimer,
Olaf/A-3117-2013; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
Funk, Stefan/B-7629-2015; 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; Bonino, Raffaella/S-2367-2016
OI Giroletti, Marcello/0000-0002-8657-8852; Baldini,
Luca/0000-0002-9785-7726; TORRESI, ELEONORA/0000-0002-5201-010X; Di
Venere, Leonardo/0000-0003-0703-824X; Stephens,
Thomas/0000-0003-3065-6871; Iafrate, Giulia/0000-0002-6185-8292;
Giordano, Francesco/0000-0002-8651-2394; giommi,
paolo/0000-0002-2265-5003; Bonino, Raffaella/0000-0002-4264-1215;
Caraveo, Patrizia/0000-0003-2478-8018; Hill, Adam/0000-0003-3470-4834;
Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins,
Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094;
Axelsson, Magnus/0000-0003-4378-8785; Bissaldi,
Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850;
Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385;
Torres, Diego/0000-0002-1522-9065; 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;
FU National Aeronautics and Space Administration
FX This work made extensive use of the ATNF pulsar catalog98
(Manchester et al. 2005). This research has made use of the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration, and of archival data,
software, and online services provided by the ASI Science Data Center
(ASDC), operated by the Italian Space Agency.
NR 116
TC 257
Z9 258
U1 20
U2 34
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 JUN
PY 2015
VL 218
IS 2
AR 23
DI 10.1088/0067-0049/218/2/23
PG 41
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7AO
UT WOS:000357122200009
ER
PT J
AU Daly, AM
Bermudez, C
Kolesnikova, L
Alonso, JL
AF Daly, A. M.
Bermudez, C.
Kolesnikova, L.
Alonso, J. L.
TI COMPREHENSIVE ANALYSIS OF PREBIOTIC PROPENAL UP TO 660 GHz
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; ISM: molecules; molecular data; techniques: spectroscopic
ID S-TRANS-ACROLEIN; VIBRATIONALLY EXCITED-STATES; MICROWAVE-SPECTRUM;
LABORATORY CHARACTERIZATION; ASTROPHYSICAL DETECTION;
INTERSTELLAR-MOLECULES; GALACTIC-CENTER; DIPOLE-MOMENT; WAVE SPECTRUM;
CIS-ACROLEIN
AB Since interstellar detection of propenal is only based on two rotational transitions in the centimeter wave region, its high resolution rotational spectrum has been measured up to 660 GHz and fully characterized by assignment of more than 12,000 transitions to provide direct laboratory data to the astronomical community. Spectral assignments and analysis include transitions from the ground state of the trans and cis isomers, three trans-C-13 isotopologues, and ten excited vibrational states of the trans form. Combining new millimeter and submillimeter data with those from the far-infrared region has yielded the most precise set of spectroscopic constants of trans-propenal obtained to date. Newly determined rotational constants, centrifugal distortion constants, vibrational energies, and Coriolis and Fermi interaction constants are given with high accuracy and were used to predict transition frequencies and intensities over a wide frequency range. Results of this work should facilitate astronomers further observation of propenal in the interstellar medium.
C1 [Daly, A. M.; Bermudez, C.; Kolesnikova, L.; Alonso, J. L.] Univ Valladolid, Unidad Asociada CSIC, Labs Espectroscopia & Bioespectroscopia, Area Quim Fis,GEM, E-47011 Valladolid, Spain.
[Daly, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Daly, AM (reprint author), Univ Valladolid, Unidad Asociada CSIC, Labs Espectroscopia & Bioespectroscopia, Area Quim Fis,GEM, Edificio Quifima,Parque Cient UVa, E-47011 Valladolid, Spain.
EM Adam.M.Daly@jpl.nasa.gov
FU Ministerio de Ciencia e Innovacion [CTQ 2013-40717 P, CTQ 2010-19008,
CSD 2009-00038]; Junta de Castilla y Leon [VA070A08, VA175U13];
Minisiterio de Ciencia e Innovacion [BES 2011-047695]
FX This research has been supported by the "Ministerio de Ciencia e
Innovacion" (grant numbers CTQ 2013-40717 P, CTQ 2010-19008 and
CONSOLIDER-Ingenio program "ASTROMOL," CSD 2009-00038) and Junta de
Castilla y Leon (Grants VA070A08 and VA175U13). C.B. wishes to thank the
Minisiterio de Ciencia e Innovacion for an FPI grant (BES 2011-047695).
NR 35
TC 4
Z9 4
U1 0
U2 3
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 JUN
PY 2015
VL 218
IS 2
AR 30
DI 10.1088/0067-0049/218/2/30
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7AO
UT WOS:000357122200016
ER
PT J
AU Kriek, M
Shapley, AE
Reddy, NA
Siana, B
Coil, AL
Mobasher, B
Freeman, WR
de Groot, L
Price, SH
Sanders, R
Shivaei, I
Brammer, GB
Momcheva, IG
Skelton, RE
van Dokkum, PG
Whitaker, KE
Aird, J
Azadi, M
Kassis, M
Bullock, JS
Conroy, C
Dave, R
Keres, D
Krumholz, M
AF Kriek, Mariska
Shapley, Alice E.
Reddy, Naveen A.
Siana, Brian
Coil, Alison L.
Mobasher, Bahram
Freeman, William R.
de Groot, Laura
Price, Sedona H.
Sanders, Ryan
Shivaei, Irene
Brammer, Gabriel B.
Momcheva, Ivelina G.
Skelton, Rosalind E.
van Dokkum, Pieter G.
Whitaker, Katherine E.
Aird, James
Azadi, Mojegan
Kassis, Marc
Bullock, James S.
Conroy, Charlie
Dave, Romeel
Keres, Dusan
Krumholz, Mark
TI THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL
SPECTROSCOPY FOR similar to 1500 H-SELECTED GALAXIES AT 1.37 <= z <= 3.8
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: distances and redshifts; galaxies: evolution; galaxies:
formation; galaxies: high-redshift; surveys
ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; ACTIVE GALACTIC NUCLEI;
EXTRAGALACTIC LEGACY SURVEY; MASS-METALLICITY RELATION; POST-STARBURST
GALAXIES; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; MEDIUM-BAND
SURVEY; QUIESCENT GALAXIES
AB In this paper we present the MOSFIRE Deep Evolution Field (MOSDEF) survey. The MOSDEF survey aims to obtain moderate-resolution (R = 3000-3650) rest-frame optical spectra (similar to 3700-7000 angstrom) for similar to 1500 galaxies at 1.37 <= z <= 3.80 in three well-studied CANDELS fields: AEGIS, COSMOS, and GOODS-N. Targets are selected in three redshift intervals: 1.37 <= z <= 1.70, 2.09 <= z <= 2.61, and 2.95 <= z <= 3.80, down to fixed H-AB (F160W) magnitudes of 24.0, 24.5, and 25.0, respectively, using the photometric and spectroscopic catalogs from the 3D-HST survey. We target both strong nebular emission lines (e.g., [O II] lambda lambda 3727, 3730, H beta, [O III] lambda lambda 4960, 5008, Ha, [N II] lambda lambda 6550, 6585, and [S II] lambda lambda 6718, 6733) and stellar continuum and absorption features (e.g., Balmer lines, Ca-II H and K, Mgb, 4000 angstrom break). Here we present an overview of our survey, the observational strategy, the data reduction and analysis, and the sample characteristics based on spectra obtained during the first 24 nights. To date, we have completed 21 masks, obtaining spectra for 591 galaxies. For similar to 80% of the targets we derive a robust redshift from either emission or absorption lines. In addition, we confirm 55 additional galaxies, which were serendipitously detected. The MOSDEF galaxy sample includes unobscured star-forming, dusty star-forming, and quiescent galaxies and spans a wide range in stellar mass (similar to 10(9)-10(11.5) M-circle dot) and star formation rate (similar to 10(0)-10(3) M-circle dot yr(-1)). The spectroscopically confirmed sample is roughly representative of an H-band limited galaxy sample at these redshifts. With its large sample size, broad diversity in galaxy properties, and wealth of available ancillary data, MOSDEF will transform our understanding of the stellar, gaseous, metal, dust, and black hole content of galaxies during the time when the universe was most active.
C1 [Kriek, Mariska; Price, Sedona H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Shapley, Alice E.; Sanders, Ryan] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Reddy, Naveen A.; Siana, Brian; Mobasher, Bahram; Freeman, William R.; de Groot, Laura; Shivaei, Irene] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Coil, Alison L.; Keres, Dusan] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Momcheva, Ivelina G.; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Skelton, Rosalind E.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Aird, James] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Kassis, Marc] WM Keck Observ, Kamuela, HI 96743 USA.
[Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Conroy, Charlie; Krumholz, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Dave, Romeel] Univ Western Cape, ZA-7535 Cape Town, South Africa.
RP Kriek, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RI Bullock, James/K-1928-2015; Skelton, Rosalind/S-1845-2016
OI Bullock, James/0000-0003-4298-5082; Skelton,
Rosalind/0000-0001-7393-3336
FU NSF AAG [AST-1312780, 1312547, 1312764, 1313171]; NASA through the Space
Telescope Science Institute [AR-13907]; Committee Faculty Research
Grant; Hellmann Fellowship; Alfred P. Sloan Research Fellowship; NSF
CAREER [AST-1055081]; W.M. Keck Foundation; NASA/ESA Hubble Space
Telescope [12177, 12328, 12060-12064, 12440-12445, 13056]; NASA [NAS
5-26555]
FX We thank the MOSFIRE instrument team for building this powerful
instrument and for taking data for us during their commissioning runs.
M. Kriek acknowledges valuable discussions with N. Konidaris about the
reduction of MOSFIRE data and with M. Franx regarding the noise
properties of the data. We thank the referee for a constructive report.
This work would not have been possible without the 3D-HST collaboration,
who provided to us the spectroscopic and photometric catalogs used to
select our targets and to derive stellar population parameters. We are
grateful to I. McLean, K. Kulas, and G. Mace for taking observations for
us in 2013 May and June. We acknowledge support from an NSF AAG
collaborative grant AST-1312780, 1312547, 1312764, and 1313171, and
archival grant AR-13907, provided by NASA through a grant from the Space
Telescope Science Institute. M. Kriek acknowledges support from a
Committee Faculty Research Grant and a Hellmann Fellowship. N.A.R. is
supported by an Alfred P. Sloan Research Fellowship. A.L.C. acknowledges
funding from NSF CAREER grant AST-1055081. The data presented in this
paper were obtained at the W.M. Keck Observatory, which is operated as a
scientific partnership among the California Institute of Technology, the
University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W.M. Keck Foundation. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. This work is
also based on observations made with the NASA/ESA Hubble Space Telescope
(programs 12177, 12328, 12060-12064, 12440-12445, 13056), which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555.
NR 97
TC 45
Z9 45
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2015
VL 218
IS 2
AR 15
DI 10.1088/00647-0049/218/2/15
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7AO
UT WOS:000357122200001
ER
PT J
AU Tyler, RH
Henning, WG
Hamilton, CW
AF Tyler, Robert H.
Henning, Wade G.
Hamilton, Christopher W.
TI TIDAL HEATING IN A MAGMA OCEAN WITHIN JUPITER'S MOON Io
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planets and satellites: dynamical evolution and stability; planets and
satellites: general; planets and satellites: interiors
ID PLANET-PLANET SCATTERING; TERRESTRIAL EXOPLANETS; VISCOELASTIC MODELS;
GIANT PLANETS; CONVECTION; EARTH; FLOW; DISSIPATION; EVOLUTION; GALILEO
AB Active volcanism observed on Io is thought to be driven by the temporally periodic, spatially differential projection of Jupiter's gravitational field over the moon. Previous theoretical estimates of the tidal heat have all treated Io as essentially a solid, with fluids addressed only through adjustment of rheological parameters rather than through appropriate extension of the dynamics. These previous estimates of the tidal response and associated heat generation on Io are therefore incomplete and possibly erroneous because dynamical aspects of the fluid behavior are not permitted in the modeling approach. Here we address this by modeling the partial-melt asthenosphere as a global layer of fluid governed by the Laplace Tidal Equations. Solutions for the tidal response are then compared with solutions obtained following the traditional solid-material approach. It is found that the tidal heat in the solid can match that of the average observed heat flux (nominally 2.25 W m(-2)), though only over a very restricted range of plausible parameters, and that the distribution of the solid tidal heat flux cannot readily explain a longitudinal shift in the observed (inferred) low-latitude heat fluxes. The tidal heat in the fluid reaches that observed over a wider range of plausible parameters, and can also readily provide the longitudinal offset. Finally, expected feedbacks and coupling between the solid/fluid tides are discussed. Most broadly, the results suggest that both solid and fluid tidal-response estimates must be considered in exoplanet studies, particularly where orbital migration under tidal dissipation is addressed.
C1 [Tyler, Robert H.; Henning, Wade G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tyler, Robert H.; Henning, Wade G.] NASA Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Hamilton, Christopher W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Tyler, RH (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM robert.h.tyler@nasa.gov
FU NASA [NNX13AG01G, NNX11AM38G]; NASA; OPR Program [NNX14AR42G]
FX The authors thank Bill Moore for helpful discussions, as well as access
to and training in the use of the TideLab suite of code. R.H.T.
acknowledges support by NASA Outer Planets Research (OPR) Program
(through awards NNX13AG01G, NNX11AM38G). W.G.H. and C.W.H. acknowledge
support of the NASA Post-doctoral Fellowship Program. All authors
acknowledge a new award from the OPR Program (NNX14AR42G) specifically
directed at the topic of this paper.
NR 59
TC 3
Z9 3
U1 2
U2 9
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 JUN
PY 2015
VL 218
IS 2
AR 22
DI 10.1088/0067-0049/218/2/22
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL7AO
UT WOS:000357122200008
ER
PT J
AU Bi, J
Knyazikhin, Y
Choi, SH
Park, T
Barichivich, J
Ciais, P
Fu, R
Ganguly, S
Hall, F
Hilker, T
Huete, A
Jones, M
Kimball, J
Lyapustin, AI
Mottus, M
Nemani, RR
Piao, SL
Poulter, B
Saleska, SR
Saatchi, SS
Xu, L
Zhou, LM
Myneni, RB
AF Bi, Jian
Knyazikhin, Yuri
Choi, Sungho
Park, Taejin
Barichivich, Jonathan
Ciais, Philippe
Fu, Rong
Ganguly, Sangram
Hall, Forrest
Hilker, Thomas
Huete, Alfredo
Jones, Matthew
Kimball, John
Lyapustin, Alexei I.
Mottus, Matti
Nemani, Ramakrishna R.
Piao, Shilong
Poulter, Benjamin
Saleska, Scott R.
Saatchi, Sassan S.
Xu, Liang
Zhou, Liming
Myneni, Ranga B.
TI Sunlight mediated seasonality in canopy structure and photosynthetic
activity of Amazonian rainforests
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE Amazonian rainforests; seasonality; remote sensing; MISR; MODIS
ID LEAF-AREA INDEX; TROPICAL FOREST; DRY SEASON; MODIS; CARBON;
PRODUCTIVITY; VARIABILITY; SENSITIVITY; ALGORITHM; PHENOLOGY
AB Resolving the debate surrounding the nature and controls of seasonal variation in the structure and metabolism of Amazonian rainforests is critical to understanding their response to climate change. In situ studies have observed higher photosynthetic and evapotranspiration rates, increased litterfall and leaf flushing during the Sunlight-rich dry season. Satellite data also indicated higher greenness level, a proven surrogate of photosynthetic carbon fixation, and leaf area during the dry season relative to the wet season. Some recent reports suggest that rainforests display no seasonal variations and the previous results were satellite measurement artefacts. Therefore, here we re-examine several years of data from three sensors on two satellites under a range of sun positions and satellite measurement geometries and document robust evidence for a seasonal cycle in structure and greenness of wet equatorial Amazonian rainforests. This seasonal cycle is concordant with independent observations of solar radiation. Weattribute alternative conclusions to an incomplete study of the seasonal cycle, i. e. the dry season only, and to prognostications based on a biased radiative transfer model. Consequently, evidence of dry season greening in geometry corrected satellite data was ignored and the absence of evidence for seasonal variation in lidar data due to noisy and saturated signals was misinterpreted as evidence of the absence of changes during the dry season. Our results, grounded in the physics of radiative transfer, buttress previous reports of dry season increases in leaf flushing, litterfall, photosynthesis and evapotranspiration in well-hydrated Amazonian rainforests.
C1 [Bi, Jian; Knyazikhin, Yuri; Choi, Sungho; Park, Taejin; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Barichivich, Jonathan] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
[Ciais, Philippe] UVSQ, CEA, CNRS, IPSL,LSCE, F-91191 Gif Sur Yvette, France.
[Fu, Rong] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Ganguly, Sangram] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hall, Forrest] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Huete, Alfredo] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia.
[Jones, Matthew; Kimball, John] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[Lyapustin, Alexei I.] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mottus, Matti] Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland.
[Nemani, Ramakrishna R.] NASA, Adv Supercomp Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Piao, Shilong] Peking Univ, Dept Ecol, Beijing 100871, Peoples R China.
[Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Saleska, Scott R.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
[Saatchi, Sassan S.; Xu, Liang] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA.
[Zhou, Liming] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
RP Bi, J (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
EM jknjazi@bu.edu
RI Myneni, Ranga/F-5129-2012; Mottus, Matti/A-4130-2009; Huete,
Alfredo/C-1294-2008; Zhou, Liming/A-2688-2012;
OI Mottus, Matti/0000-0002-2745-1966; Huete, Alfredo/0000-0003-2809-2376;
Poulter, Benjamin/0000-0002-9493-8600
FU NASA Earth Science Division
FX This study was supported by NASA Earth Science Division.
NR 36
TC 11
Z9 11
U1 4
U2 55
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD JUN
PY 2015
VL 10
IS 6
AR 064014
DI 10.1088/1748-9326/10/6/064014
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CL3FK
UT WOS:000356835600016
ER
PT J
AU Doyle, PM
Jogo, K
Nagashima, K
Krot, AN
Wakita, S
Ciesla, FJ
Hutcheon, ID
AF Doyle, Patricia M.
Jogo, Kaori
Nagashima, Kazuhide
Krot, Alexander N.
Wakita, Shigeru
Ciesla, Fred J.
Hutcheon, Ian D.
TI Early aqueous activity on the ordinary and carbonaceous chondrite parent
bodies recorded by fayalite
SO NATURE COMMUNICATIONS
LA English
DT Article
ID EARLY SOLAR-SYSTEM; OXYGEN-ISOTOPE FRACTIONATION; PROTOPLANETARY DISK;
RATIO ESTIMATION; ORGANIC-MATTER; ASTEROID BELT; CHRONOLOGY; CHONDRULES;
EVOLUTION; ALLENDE
AB Chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric Mn-53-Cr-53 dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first Mn-53-Cr-53 ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2.4(-1.3)(+1.8) Myr after calcium-aluminium-rich inclusions (CAIs), the oldest Solar System solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed 4.2(-0.7)(+0.8) and 5.1(-0.4)(+0.5) Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and Mn-53-Cr-53 ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies similar to 1.8 - 2.5 Myr after CAIs.
C1 [Doyle, Patricia M.; Jogo, Kaori; Nagashima, Kazuhide; Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Doyle, Patricia M.; Jogo, Kaori; Krot, Alexander N.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Wakita, Shigeru] Natl Astron Observ Japan, Ctr Computat Astrophys, Mitaka, Tokyo 1818588, Japan.
[Ciesla, Fred J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Hutcheon, Ian D.] Lawrence Livermore Natl Lab, Glenn Seaborg Inst, Livermore, CA 94551 USA.
RP Doyle, PM (reprint author), Univ Cape Town, Dept Geol Sci, ZA-7701 Rondebosch, South Africa.
EM pdoyle@higp.hawaii.edu; sasha@higp.hawaii.edu
OI Wakita, Shigeru/0000-0002-3161-3454
NR 66
TC 12
Z9 12
U1 5
U2 20
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD JUN
PY 2015
VL 6
AR 7444
DI 10.1038/ncomms8444
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CL7UH
UT WOS:000357176700010
PM 26100451
ER
PT J
AU Sun, T
Socki, RA
Bish, DL
Harvey, RP
Bao, HM
Niles, PB
Cavicchioli, R
Tonui, E
AF Sun, Tao
Socki, Richard A.
Bish, David L.
Harvey, Ralph P.
Bao, Huiming
Niles, Paul B.
Cavicchioli, Ricardo
Tonui, Eric
TI Lost cold Antarctic deserts inferred from unusual sulfate formation and
isotope signatures
SO NATURE COMMUNICATIONS
LA English
DT Article
ID ICE-SHEET; TRANSANTARCTIC MOUNTAINS; ATMOSPHERIC SULFATES; SULFUR
ISOTOPES; VICTORIA LAND; DRY VALLEYS; OXYGEN; REDUCTION; FRACTIONATION;
BACTERIAL
AB The Antarctic ice cap significantly affects global ocean circulation and climate. Continental glaciogenic sedimentary deposits provide direct physical evidence of the glacial history of the Antarctic interior, but these data are sparse. Here we investigate a new indicator of ice sheet evolution: sulfates within the glaciogenic deposits from the Lewis Cliff Ice Tongue of the central Transantarctic Mountains. The sulfates exhibit unique isotope signatures, including delta S-34 up to + 50% for mirabilite evaporites, Delta O-17 up to + 2.3% for dissolved sulfate within contemporary melt-water ponds, and extremely negative delta O-18 as low as -22.2%. The isotopic data imply that the sulfates formed under environmental conditions similar to today's McMurdo Dry Valleys, suggesting that ice-free cold deserts may have existed between the South Pole and the Transantarctic Mountains since the Miocene during periods when the ice sheet size was smaller than today, but with an overall similar to modern global hydrological cycle.
C1 [Sun, Tao; Bao, Huiming] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Sun, Tao; Niles, Paul B.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Socki, Richard A.] NASA, Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
[Bish, David L.] Indiana Univ, Indianapolis, IN 47405 USA.
[Harvey, Ralph P.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Cavicchioli, Ricardo] Univ New S Wales, Sydney, NSW 2052, Australia.
[Tonui, Eric] BP Amer, Upstream Technol, Houston, TX 77079 USA.
RP Sun, T (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
EM tsun9@central.uh.edu
FU NASA's Mars Fundamental Research Program [NNF05GL75G]; National Science
Foundation's Office of Polar Programs, Division of Infrastructure and
Logistics; Economic Development Assistantship from Louisiana State Board
of Regents; NASA Postdoctoral Fellowship; Australian Research Council;
Australian Antarctic Science program
FX We acknowledge funding from NASA's Mars Fundamental Research Program
(grant #NNF05GL75G) to conduct this research. The National Science
Foundation's Office of Polar Programs, Division of Infrastructure and
Logistics provided outstanding field support. T.S. is supported by
Economic Development Assistantship from Louisiana State Board of Regents
and a NASA Postdoctoral Fellowship. The research performed by R.C. is
supported by the Australian Research Council and the Australian
Antarctic Science program. We also thank Michael Kaplan and Sarah
Feakins for helpful discussions.
NR 59
TC 1
Z9 1
U1 4
U2 15
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD JUN
PY 2015
VL 6
AR 7579
DI 10.1038/ncomms8579
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CL7VX
UT WOS:000357181300001
PM 26119082
ER
PT J
AU Du, XM
Cao, DY
Mishra, D
Bernardes, S
Jordan, TR
Madden, M
AF Du, Xiaomin
Cao, Daiyong
Mishra, Deepak
Bernardes, Sergio
Jordan, Thomas R.
Madden, Marguerite
TI Self-Adaptive Gradient-Based Thresholding Method for Coal Fire Detection
Using ASTER Thermal Infrared Data, Part I: Methodology and Decadal
Change Detection
SO REMOTE SENSING
LA English
DT Article
ID LAND-SURFACE-TEMPERATURE; JHARIA COALFIELD; SPONTANEOUS COMBUSTION;
NORTHERN CHINA; TM DATA; EMISSIVITY; INDIA; WUDA; RADIOMETER; RESOLUTION
AB Coal fires that are induced by natural spontaneous combustion or result from human activities occurring on the surface and in underground coal seams destroy coal resources and cause serious environmental degradation. Thermal infrared image data, which directly measure surface temperature, can be an important tool to map coal fires over large areas. As the first of two parts introducing our coal fire detection method, this paper proposes a self-adaptive threshold-based approach for coal fire detection using ASTER thermal infrared data: the self-adaptive gradient-based thresholding method (SAGBT). This method is based on an assumption that the attenuation of temperature along the coal fire's boundaries generates considerable numbers of spots with extremely high gradient values. The SAGBT method applied mathematical morphology thinning to skeletonize the potential high gradient buffers into the extremely high gradient lines, which provides a self-adaptive mechanism to generate thresholds according to the thermal spatial patterns of the images. The final threshold was defined as an average temperature value reading from the high temperature buffers (segmented by 1.0 sigma from the mean) and along a sequence of extremely high gradient lines (thinned from the potential high gradient buffers and segmented within the lower bounds, ranging from 0.5 sigma to 1.5 sigma and with an upper bound of 3.2 sigma, where sigma is the standard deviation), marking the coal fire areas. The SAGBT method used the basic outer boundary of the coal-bearing strata to simply exclude false alarms. The intermediate thresholds reduced the coupling with the temperature and converged by changing the potential high gradient buffers. This simple approach can be economical and accurate in identifying coal fire areas. In addition, it allows for the identification of thresholds using multiple ASTER TIR scenes in a consistent and uniform manner, and supports long-term coal fire change analyses using historical images in local areas. This paper focuses on the introduction of the methodology. Furthermore, an improvement to SAGBT is proposed. In a subsequent paper, subtitled "Part 2, Validation and Sensitivity Analysis," we address satellite-field simultaneous observations and report comparisons between the retrieved thermal anomalies and field measurements in different aspects to prove that the coal fires are separable by the SAGBT method. These comparisons allowed us to estimate the accuracy and biases of the SAGBT method. As an application of the SAGBT, a relationship between coal fires' decadal variation and coal production was also examined. Our work documented a total area increase in the beginning of 2003, which correlates with increased mining activities and the rapid increase of energy consumption in China during the decade (2001-2011). Additionally, a decrease in the total coal fire area is consistent with the nationally sponsored fire suppression efforts during 2007-2008. It demonstrated the applicability of SAGBT method for long-term change detection with multi-temporal images.
C1 [Du, Xiaomin; Cao, Daiyong] China Univ Min & Technol, Sch Geosci & Surveying Engn, Beijing 100083, Peoples R China.
[Du, Xiaomin; Mishra, Deepak; Bernardes, Sergio; Jordan, Thomas R.; Madden, Marguerite] Univ Georgia, Dept Geog, Ctr Geospatial Res, Athens, GA 30602 USA.
[Bernardes, Sergio] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
RP Mishra, D (reprint author), Univ Georgia, Dept Geog, Ctr Geospatial Res, Athens, GA 30602 USA.
EM xiaomin@uga.edu; cdy@cumtb.edu.cn; dmishra@uga.edu;
sergio.bernardes@nasa.gov; tombob@uga.edu; mmadden@uga.edu
FU Strategic Priority Research Program of the Chinese Academy of Sciences,
Carbon Emission from Coal Spontaneous Combustion [XDA05030200]; China
Scholarship Council
FX Funding for this work was provided by a Strategic Priority Research
Program of the Chinese Academy of Sciences, Carbon Emission from Coal
Spontaneous Combustion (Grant No. XDA05030200). The first author's
visiting study at the University of Georgia (UGA) was sponsored by the
China Scholarship Council. We thank Guang Yang and Zhipeng Li for
collection of field data. The authors wish to thank the anonymous
reviewers for their constructive suggestions that improved the paper.
Image acquisition was granted by the Land Processes Distributed Active
Archive Center (LP DAAC) of the National Aeronautics and Space
Administration (NASA), including the tasking of the ASTER orbital sensor
to acquire images during field activities in China. ASTER images were
accessed through the Earth Resources Observation Systems (EROS) Data
Center of the U.S. Geological Survey (USGS). Special thanks to UGA's
international student internship program for facilitating collaboration
between the two institutes.
NR 59
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PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2015
VL 7
IS 6
BP 6576
EP 6610
DI 10.3390/rs70606576
PG 35
WC Remote Sensing
SC Remote Sensing
GA CM3NS
UT WOS:000357589800004
ER
PT J
AU Heidinger, AK
Li, Y
Baum, BA
Holz, RE
Platnick, S
Yang, P
AF Heidinger, Andrew K.
Li, Yue
Baum, Bryan A.
Holz, Robert E.
Platnick, Steven
Yang, Ping
TI Retrieval of Cirrus Cloud Optical Depth under Day and Night Conditions
from MODIS Collection 6 Cloud Property Data
SO REMOTE SENSING
LA English
DT Article
ID PARTICLES; SATELLITE; MODEL
AB This paper presents a technique to generate cirrus optical depth and particle effective size estimates from the cloud emissivities at 8.5, 11 and 12 mu m contained in the Collection-6 (C6) MYD06 cloud product. This technique employs the latest scattering models and scattering radiative transfer approximations to estimate cloud optical depth and particle effective size using efficient analytical formulae. Two scattering models are tested. The first is the same scattering model as that used in the C6 MYD06 solar reflectance products. The second model is an empirical model derived from radiometric consistency. Both models are shown to generate optical depths that compare well to those from constrained CALIPSO retrievals and MYD06. In terms of effective radius retrievals, the results from the radiometric empirical model agree more closely with MYD06 than those from the C6 model. This analysis is applied to AQUA/MODIS data collocated with CALIPSO/CALIOP during January 2010.
C1 [Heidinger, Andrew K.] NOAA Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res, Madison, WI 53706 USA.
[Li, Yue; Baum, Bryan A.; Holz, Robert E.] Univ Wisconsin, SSEC, Madison, WI 53706 USA.
[Platnick, Steven] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Heidinger, AK (reprint author), NOAA Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res, 1225 West Dayton St, Madison, WI 53706 USA.
EM andrew.heidinger@noaa.gov; yue.li@ssec.wisc.edu;
bryan.baum@ssec.wisc.edu; reholz@ssec.wisc.edu;
steven.e.platnick@nasa.gov; pyang@tamu.edu
RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Platnick,
Steven/J-9982-2014; Heidinger, Andrew/F-5591-2010
OI Baum, Bryan/0000-0002-7193-2767; Platnick, Steven/0000-0003-3964-3567;
Heidinger, Andrew/0000-0001-7631-109X
FU NASA [NNX11AR06G]
FX This work was supported by Hal Maring of the NASA ROSES Program. Bryan
Baum and Ping Yang also gratefully acknowledge the support from NASA
grant NNX11AR06G. The NPP Atmospheric PEATE at the University of
Wisconsin provided the data for this paper.
NR 21
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U1 1
U2 9
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2015
VL 7
IS 6
BP 7257
EP 7271
DI 10.3390/rs70607257
PG 15
WC Remote Sensing
SC Remote Sensing
GA CM3NS
UT WOS:000357589800032
ER
PT J
AU Clewley, D
Whitcomb, J
Moghaddam, M
McDonald, K
Chapman, B
Bunting, P
AF Clewley, Daniel
Whitcomb, Jane
Moghaddam, Mahta
McDonald, Kyle
Chapman, Bruce
Bunting, Peter
TI Evaluation of ALOS PALSAR Data for High-Resolution Mapping of Vegetated
Wetlands in Alaska
SO REMOTE SENSING
LA English
DT Article
ID LAND-COVER DATABASE; METHANE EMISSIONS; INVENTORY MAPS; RANDOM FORESTS;
CLIMATE-CHANGE; CLASSIFICATION; SUCCESSION; IMPACTS; PROJECT; EXTENT
AB As the largest natural source of methane, wetlands play an important role in the carbon cycle. High-resolution maps of wetland type and extent are required to quantify wetland responses to climate change. Mapping northern wetlands is particularly important because of a disproportionate increase in temperatures at higher latitudes. Synthetic aperture radar data from a spaceborne platform can be used to map wetland types and dynamics over large areas. Following from earlier work by Whitcomb et al. (2009) using Japanese Earth Resources Satellite (JERS-1) data, we applied the "random forests" classification algorithm to variables from L-band ALOS PALSAR data for 2007, topographic data (e.g., slope, elevation) and locational information (latitude, longitude) to derive a map of vegetated wetlands in Alaska, with a spatial resolution of 50 m. We used the National Wetlands Inventory and National Land Cover Database (for upland areas) to select training and validation data and further validated classification results with an independent dataset that we created. A number of improvements were made to the method of Whitcomb et al. (2009): (1) more consistent training data in upland areas; (2) better distribution of training data across all classes by taking a stratified random sample of all available training pixels; and (3) a more efficient implementation, which allowed classification of the entire state as a single entity (rather than in separate tiles), which eliminated discontinuities at tile boundaries. The overall accuracy for discriminating wetland from upland was 95%, and the accuracy at the level of wetland classes was 85%. The total area of wetlands mapped was 0.59 million km(2), or 36% of the total land area of the state of Alaska. The map will be made available to download from NASA's wetland monitoring website.
C1 [Clewley, Daniel; Whitcomb, Jane; Moghaddam, Mahta] Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
[McDonald, Kyle] CUNY City Coll, New York, NY 10031 USA.
[Chapman, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bunting, Peter] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Ceredigion, Wales.
RP Clewley, D (reprint author), Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
EM daniel.clewley@gmail.com; jbwhitco@usc.edu; mahta@usc.edu;
kmcdonald2@ccny.cuny.edu; bruce.d.chapman@jpl.nasa.gov; pfb@aber.ac.uk
RI Bunting, Pete/B-8678-2013;
OI Bunting, Pete/0000-0002-7435-0148; Clewley, Daniel/0000-0003-1243-3711
FU NASA's Making Earth System Data Records for Use in Research Environments
(MEaSUREs) Program; National Aeronautics and Space Administration
FX This work was supported through NASA's Making Earth System Data Records
for Use in Research Environments (MEaSUREs) Program. This work was
undertaken in part within the framework of the JAXA Kyoto & Carbon
Initiative. ALOS PALSAR data were provided through the Alaska Satellite
Facility. Portions of this work were undertaken at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 61
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U2 13
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2015
VL 7
IS 6
BP 7272
EP 7297
DI 10.3390/rs70607272
PG 26
WC Remote Sensing
SC Remote Sensing
GA CM3NS
UT WOS:000357589800033
ER
PT J
AU Bellini, A
Renzini, A
Anderson, J
Bedin, LR
Piotto, G
Soto, M
Brown, TM
Milone, AP
Sohn, ST
Sweigart, AV
AF Bellini, A.
Renzini, A.
Anderson, J.
Bedin, L. R.
Piotto, G.
Soto, M.
Brown, T. M.
Milone, A. P.
Sohn, S. T.
Sweigart, A. V.
TI UV INSIGHTS INTO THE COMPLEX POPULATIONS OF M87 GLOBULAR CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M87); galaxies: star clusters: general; (Galaxy:)
globular clusters: general; Hertzsprung-Russell and C-M diagrams;
techniques: photometric
ID MULTIPLE STELLAR POPULATIONS; SPACE-TELESCOPE OBSERVATIONS; DOUBLE
MAIN-SEQUENCE; EARLY-TYPE GALAXIES; OMEGA-CENTAURI; ADVANCED CAMERA;
STAR-CLUSTERS; ACS SURVEY; WIDE-FIELD; NGC 6397
AB We have imaged with Hubble Space Telescope WFC3/UVIS the central 2.'7 x 2.'7 region of the giant elliptical galaxy M87, using the ultraviolet filter F275W. In combination with archival ACS/WFC data taken through the F606W and F814W filters, covering the same field, we have constructed integrated-light UV-optical colors and magnitudes for 1460 objects, most of which are believed to be globular clusters (GCs) belonging to M87. The purpose was to ascertain whether the multiple-populations syndrome, ubiquitous among Galactic GCs, also exists among the M87 family of clusters. To achieve this goal, we sought those GCs with exceptionally blue UV-tooptical colors because helium-enriched sub-populations produce a horizontal-branch morphology that is well populated at high effective temperature. For comparison, integrated, synthetic UV-optical and purely optical colors and magnitudes have been constructed for 45 Galactic GCs, starting from individual-star photometry obtained with the same instruments and the same filters. We identify a small group of M87 clusters exhibiting a radial UV-optical color gradient, representing our best candidate GCs hosting multiple populations with extreme helium content. We also find that the central spatial distribution of the bluer GCs is flattened in a direction parallel to the jet, while the distribution of redder GCs is more spherical. We release to the astronomical community our photometric catalog in F275W, F606W, and F814W bands and the high-quality image stacks in the same bands.
C1 [Bellini, A.; Anderson, J.; Soto, M.; Brown, T. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Renzini, A.; Bedin, L. R.; Piotto, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Piotto, G.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Mt Stromlo Observ, I-35122 Padua, Italy.
[Milone, A. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Sohn, S. T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA.
RP Bellini, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM bellini@stsci.edu
OI Piotto, Giampaolo/0000-0002-9937-6387; bedin, luigi/0000-0003-4080-6466;
Brown, Thomas/0000-0002-1793-9968
FU STScI grant [GO-12989, GO-13297]; Australian Research Council
[DP120100475]; Becas Chile de Postdoctorado en el Extranjero project
[74150088]
FX The authors gratefully thank the anonymous referee for his/her useful
suggestions that helped improving the manuscript, and Thomas Puzia for a
critical reading of the manuscript. A. B. and J. A. acknowledge support
from STScI grant GO-12989. A. P. M. acknowledges the financial support
from the Australian Research Council through Discovery Project grant
DP120100475. M. S. acknowledges support from STScI grant GO-13297 and
Becas Chile de Postdoctorado en el Extranjero project 74150088.
NR 63
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 178
DI 10.1088/0004-637X/805/2/178
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400093
ER
PT J
AU Chakraborti, S
Soderberg, A
Chomiuk, L
Kamble, A
Yadav, N
Ray, A
Hurley, K
Margutti, R
Milisavljevic, D
Bietenholz, M
Brunthaler, A
Pignata, G
Pian, E
Mazzali, P
Fransson, C
Bartel, N
Hamuy, M
Levesque, E
MacFadyen, A
Dittmann, J
Krauss, M
Briggs, MS
Connaughton, V
Yamaoka, K
Takahashi, T
Ohno, M
Fukazawa, Y
Tashiro, M
Terada, Y
Murakami, T
Goldsten, J
Barthelmy, S
Gehrels, N
Cummings, J
Krimm, H
Palmer, D
Golenetskii, S
Aptekar, R
Frederiks, D
Svinkin, D
Cline, T
Mitrofanov, IG
Golovin, D
Litvak, ML
Sanin, AB
Boynton, W
Fellows, C
Harshman, K
Enos, H
von Kienlin, A
Rau, A
Zhang, X
Savchenko, V
AF Chakraborti, Sayan
Soderberg, Alicia
Chomiuk, Laura
Kamble, Atish
Yadav, Naveen
Ray, Alak
Hurley, Kevin
Margutti, Raffaella
Milisavljevic, Dan
Bietenholz, Michael
Brunthaler, Andreas
Pignata, Giuliano
Pian, Elena
Mazzali, Paolo
Fransson, Claes
Bartel, Norbert
Hamuy, Mario
Levesque, Emily
MacFadyen, Andrew
Dittmann, Jason
Krauss, Miriam
Briggs, M. S.
Connaughton, V.
Yamaoka, K.
Takahashi, T.
Ohno, M.
Fukazawa, Y.
Tashiro, M.
Terada, Y.
Murakami, T.
Goldsten, J.
Barthelmy, S.
Gehrels, N.
Cummings, J.
Krimm, H.
Palmer, D.
Golenetskii, S.
Aptekar, R.
Frederiks, D.
Svinkin, D.
Cline, T.
Mitrofanov, I. G.
Golovin, D.
Litvak, M. L.
Sanin, A. B.
Boynton, W.
Fellows, C.
Harshman, K.
Enos, H.
von Kienlin, A.
Rau, A.
Zhang, X.
Savchenko, V.
TI A MISSING-LINK IN THE SUPERNOVA-GRB CONNECTION: THE CASE OF SN 2012ap
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; radiation mechanisms: non-thermal; shock
waves; supernovae: individual (SN 2012ap); techniques: interferometric
ID GAMMA-RAY BURSTS; RELATIVISTIC BLAST WAVES; 25 APRIL 1998; EMISSION;
MODEL; SYNCHROTRON
AB Gamma-ray bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly, usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However, supernovae with heavy ejecta can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for a few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. However, the ejecta from SN 2009bb was baryon loaded and in nearly free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than one-sixth of the fluence from GRB 980425. This shows for the first time that central engines in SNe Ic, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs.
C1 [Chakraborti, Sayan; Soderberg, Alicia; Kamble, Atish; Margutti, Raffaella; Milisavljevic, Dan; Dittmann, Jason] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Chakraborti, Sayan] Harvard Univ, Cambridge, MA 02138 USA.
[Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Yadav, Naveen; Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bietenholz, Michael] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada.
[Brunthaler, Andreas] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdrop, South Africa.
[Brunthaler, Andreas] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Pian, Elena] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Mazzali, Paolo] Liverpool John Moores Univ, Liverpool L3 5UX, Merseyside, England.
[Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Fransson, Claes] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile.
[Levesque, Emily] Univ Colorado, C327A, Boulder, CO 80309 USA.
[MacFadyen, Andrew] NYU, New York, NY 10003 USA.
[Krauss, Miriam] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Yamaoka, K.] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648602, Japan.
[Takahashi, T.] ISAS JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohno, M.; Fukazawa, Y.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398526, Japan.
[Tashiro, M.; Terada, Y.] Saitama Univ, Sakura Ku, Saitama, Saitama 3388570, Japan.
[Murakami, T.] Kanazawa Univ, Kanazawa, Ishikawa 9201192, Japan.
[Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Barthelmy, S.; Gehrels, N.; Cummings, J.; Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cummings, J.] UMBC, Dept Phys, Baltimore, MD 21250 USA.
[Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA.
[Palmer, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Golenetskii, S.; Aptekar, R.; Frederiks, D.; Svinkin, D.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Cline, T.] NASA, Goddard Space Flight Ctr, Emeritus, Greenbelt, MD 20771 USA.
[Mitrofanov, I. G.; Golovin, D.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 117997, Russia.
[Boynton, W.; Fellows, C.; Harshman, K.; Enos, H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[von Kienlin, A.; Rau, A.; Zhang, X.] MPE, D-85748 Garching, Germany.
[Savchenko, V.] Observ Paris, F-75205 Paris 13, France.
RP Chakraborti, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
EM schakraborti@fas.harvard.edu
RI Hamuy, Mario/G-7541-2016;
OI Frederiks, Dmitry/0000-0002-1153-6340; MacFadyen,
Andrew/0000-0002-0106-9013; Margutti, Raffaella/0000-0003-4768-7586;
Pian, Elena/0000-0001-8646-4858
FU Science and Technology Facilities Council [ST/L00061X/1]
NR 36
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 JUN 1
PY 2015
VL 805
IS 2
AR 187
DI 10.1088/0004-637X/805/2/187
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400102
ER
PT J
AU Deming, D
Knutson, H
Kammer, J
Fulton, BJ
Ingalls, J
Carey, S
Burrows, A
Fortney, JJ
Todorov, K
Agol, E
Cowan, N
Desert, JM
Fraine, J
Langton, J
Morley, C
Showman, AP
AF Deming, Drake
Knutson, Heather
Kammer, Joshua
Fulton, Benjamin J.
Ingalls, James
Carey, Sean
Burrows, Adam
Fortney, Jonathan J.
Todorov, Kamen
Agol, Eric
Cowan, Nicolas
Desert, Jean-Michel
Fraine, Jonathan
Langton, Jonathan
Morley, Caroline
Showman, Adam P.
TI SPITZER SECONDARY ECLIPSES OF THE DENSE, MODESTLY-IRRADIATED, GIANT
EXOPLANET HAT-P-20b USING PIXEL-LEVEL DECORRELATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; infrared: planetary systems; planetary systems; planets and
satellites: atmospheres
ID HOT JUPITERS; WARM-SPITZER; THERMAL EMISSION; LIGHT CURVES; BROWN DWARF;
HD 209458B; MU-M; ATMOSPHERIC CIRCULATION; TRANSITING PLANET; PHASE
VARIATIONS
AB HAT-P-20b is a giant metal-rich exoplanet orbiting a metal-rich star. We analyze two secondary eclipses of the planet in each of the 3.6 and 4.5 mu m bands of Warm Spitzer. We have developed a simple, powerful, and radically different method to correct the intra-pixel effect for Warm Spitzer data, which we call pixel-level decorrelation ( PLD). PLD corrects the intra-pixel effect very effectively, but without explicitly using-or even measuring-the fluctuations in the apparent position of the stellar image. We illustrate and validate PLD using synthetic and real data and comparing the results to previous analyses. PLD can significantly reduce or eliminate red noise in Spitzer secondary eclipse photometry, even for eclipses that have proven to be intractable using other methods. Our successful PLD analysis of four HAT-P-20b eclipses shows a best-fit blackbody temperature of 1134 +/- 29 K, indicating inefficient longitudinal transfer of heat, but lacking evidence for strong molecular absorption. We find sufficient evidence for variability in the 4.5 mu m band that the eclipses should be monitored at that wavelength by Spitzer, and this planet should be a high priority for James Webb Space Telescope spectroscopy. All four eclipses occur about 35 minutes after orbital phase 0.5, indicating a slightly eccentric orbit. A joint fit of the eclipse and transit times with extant RV data yields e cos omega = 0.01352(-0.00057)(+0.00054) and establishes the small eccentricity of the orbit to high statistical confidence. HAT-P-20b is another excellent candidate for orbital evolution via Kozai migration or other three-body mechanisms.
C1 [Deming, Drake; Fraine, Jonathan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Deming, Drake; Agol, Eric] NASA, Astrobiol Inst, Virtual Planetary Lab, Pasadena, CA 91125 USA.
[Knutson, Heather; Kammer, Joshua] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Fulton, Benjamin J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Ingalls, James; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fortney, Jonathan J.; Morley, Caroline] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Todorov, Kamen] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Cowan, Nicolas] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA.
[Desert, Jean-Michel] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Deming, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ddeming@astro.umd.edu
OI /0000-0002-0802-9145
FU NASA
FX We thank Jasmina Blecic, Patricio Cubillos, and Joseph Harrington for
sending us the digital version of their results, used in Figures 5-7,
and we thank Julie Moses for comments on this paper. This work is based
on observations made with Spitzer, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 56
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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 JUN 1
PY 2015
VL 805
IS 2
AR 132
DI 10.1088/0004-637X/805/2/132
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400047
ER
PT J
AU Kay, C
Opher, M
Evans, RM
AF Kay, C.
Opher, M.
Evans, R. M.
TI GLOBAL TRENDS OF CME DEFLECTIONS BASED ON CME AND SOLAR PARAMETERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: coronal mass ejections (CMEs)
ID CORONAL MASS EJECTIONS; SELF-SIMILAR MAGNETOHYDRODYNAMICS; MAGNETIC-FLUX
ROPE; INTERPLANETARY SPACE; ERUPTING PROMINENCES; MHD SIMULATION;
PROPAGATION; WIND; STEREO; MODEL
AB Accurate space weather forecasting requires. knowledge. of the trajectory of coronal mass ejections (CMEs), including any deflections. close to the Sun or through interplanetary space. Kay et al. introduced ForeCAT, a model of CME deflection resulting from the background solar magnetic field. For a magnetic field solution corresponding to Carrington Rotation (CR) 2029 (declining phase, 2005 April-May), the majority of the CMEs deflected to the Heliospheric Current Sheet, the minimum in magnetic pressure on global scales. Most of the deflection occurred below 4 R-circle dot. Here we extend ForeCAT to include a three-dimensional description of the deflecting CME. We attempt to answer the following questions: (1) do all CMEs deflect to the magnetic minimum? and (2) does most deflection occur within the first few solar radii (4 R-circle dot)? Results for solar minimum and declining-phase CMEs show that not every CME deflects to the magnetic minimum and that typically the majority of the deflection occurs below 10 R-circle dot. Slow, wide, low-mass CMEs in declining-phase solar backgrounds with strong magnetic field and magnetic gradients exhibit the largest deflections. Local gradients related to active regions tend to cause the largest deviations from the deflection predicted by global magnetic gradients, but variations can also be seen for CMEs in the quiet-Sun regions of the declining-phase CR. We show the torques due to differential forces along the CME can cause rotation about the CME's toroidal axis.
C1 [Kay, C.; Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Evans, R. M.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Kay, C (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM ckay@bu.edu
OI Kay, Christina/0000-0002-2827-6012
NR 73
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U1 2
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 JUN 1
PY 2015
VL 805
IS 2
AR 168
DI 10.1088/0004-637X/805/2/168
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400083
ER
PT J
AU Linford, JD
Ribeiro, VARM
Chomiuk, L
Nelson, T
Sokoloski, JL
Rupen, MP
Mukai, K
O'Brien, TJ
Mioduszewski, AJ
Weston, J
AF Linford, J. D.
Ribeiro, V. A. R. M.
Chomiuk, L.
Nelson, T.
Sokoloski, J. L.
Rupen, M. P.
Mukai, K.
O'Brien, T. J.
Mioduszewski, A. J.
Weston, J.
TI THE DISTANCE TO NOVA V959 MON FROM VLA IMAGING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; novae, cataclysmic variables; radio continuum: stars;
stars: individual (V959 Mon); white dwarfs
ID GAMMA-RAY EMISSION; CLASSICAL NOVAE; WHITE-DWARF; MONOCEROTIS 2012; RS
OPHIUCHI; V407 CYGNI; OUTBURST; RADIO; REMNANTS; SHELL
AB Determining reliable distances to classical novae is a challenging but crucial step in deriving their ejected masses and explosion energetics. Here we combine radio expansion measurements from the Karl G. Jansky Very Large Array with velocities derived from optical spectra to estimate an expansion parallax for nova V959 Mon, the first nova discovered through its gamma-ray emission. We spatially resolve the nova at frequencies of 4.5-36.5 GHz in nine different imaging epochs. The first five epochs cover the expansion of the ejecta from 2012 October to 2013 January, while the final four epochs span 2014 February-May. These observations correspond to days 126 through 199 and days 615 through 703 after the first detection of the nova. The images clearly show a non-spherical ejecta geometry. Utilizing ejecta velocities derived from three-dimensional modeling of optical spectroscopy, the radio expansion implies a distance between 0.9 +/- 0.2 and 2.2 +/- 0.4 kpc, with a most probable distance of 1.4 +/- 0.4 kpc. This distance implies a gamma-ray luminosity of 0.6 x 10(35) erg s(-1), which is much less than the prototype gamma-ray-detected nova, V407 Cyg, possibly due to the lack of a red giant companion in the V959 Mon system. V959 Mon also has a much lower gamma-ray luminosity than other classical novae detected in gamma-rays to date, indicating a range of at least a factor of 10 in the gamma-ray luminosities for these explosions.
C1 [Linford, J. D.; Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Ribeiro, V. A. R. M.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Ribeiro, V. A. R. M.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Sokoloski, J. L.; Weston, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Rupen, M. P.] Natl Res Council Canada, Herzberg Inst Astrophys, Penticton, BC, Canada.
[Mukai, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Mukai, K.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA.
[Mukai, K.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[O'Brien, T. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Mioduszewski, A. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Linford, JD (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
EM jlinford@.msu.edu
OI Roberts Machado Ribeiro, Valerio Alipio/0000-0003-3617-4400
FU NASA Fermi Guest Investigator grant [NNH13ZDA001N-FERMI]; Radboud
Excellence Initiative; South Africa SKA Project; NASA [NNX13A091G]; NSF
[AST-1211778]
FX The authors thank the anonymous referee for their constructive (and
extremely pleasant) criticism. The authors thank W. Steffen and N.
Koning for useful discussions on the use of SHAPE, and T. Finzell for
useful discussions on V1324 Sco. J. L. and L. C. were supported in part
by NASA Fermi Guest Investigator grant NNH13ZDA001N-FERMI. V. A. R. M.
R. was supported in part by the Radboud Excellence Initiative and the
South Africa SKA Project. T. N. was supported in part by NASA award
NNX13A091G. J. L. S. and J. W. were funded in part by NSF award
AST-1211778. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. This research made use of APLpy, an
open-source plotting package for Python hosted at
http://aplpy.github.com.
NR 53
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 136
DI 10.1088/0004-637X/805/2/136
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400051
ER
PT J
AU Margutti, R
Guidorzi, C
Lazzati, D
Milisavljevic, D
Kamble, A
Laskar, T
Parrent, J
Gehrels, NC
Soderberg, AM
AF Margutti, R.
Guidorzi, C.
Lazzati, D.
Milisavljevic, D.
Kamble, A.
Laskar, T.
Parrent, J.
Gehrels, N. C.
Soderberg, A. M.
TI DUST IN THE WIND: THE ROLE OF RECENT MASS LOSS IN LONG GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual (GRBs 060218,
100316D, 980425, 130925A); supernovae: general
ID GRB 130925A; RADIO OBSERVATIONS; SCATTERING MODEL; SUPERNOVAE;
AFTERGLOW; EVOLUTION; STARS; TELESCOPE; ENVIRONMENT; EXPLOSIONS
AB We study the late-time (t > 0.5 days) X-ray afterglows of nearby (z < 0.5) long gamma-ray bursts (GRBs) with Swift and identify a population of explosions with slowly decaying, super-soft (photon index Gamma(x) > 3) X-ray emission that is inconsistent with forward shock synchrotron radiation associated with the afterglow. These explosions also show larger-than-average intrinsic absorption (NHx,i > 6 x 10(21) cm(-2)) and prompt gamma-ray emission with extremely long duration (T-90 > 1000 s). The chance association of these three rare properties (i.e., large NHx,i, super-soft Gamma(x), and extreme duration) in the same class of explosions is statistically unlikely. We associate these properties with the turbulent mass-loss history of the progenitor star that enriched and shaped the circumburst medium. We identify a natural connection between NHx,i, Gamma(x), and T-90 in these sources by suggesting that the late-time super-soft X-rays originate from radiation reprocessed by material lost to the environment by the stellar progenitor before exploding (either in the form of a dust echo or as reprocessed radiation from a long-lived GRB remnant), and that the interaction of the explosion's shock/jet with the complex medium is the source of the extremely long prompt emission. However, current observations do not allow us to exclude the possibility that super-soft X-ray emitters originate from peculiar stellar progenitors with large radii that only form in very dusty environments.
C1 [Margutti, R.; Milisavljevic, D.; Kamble, A.; Laskar, T.; Parrent, J.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy.
[Lazzati, D.] Oregon State Univ, Dept Phys, Corvallis, OR 97331 USA.
[Gehrels, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Lazzati, Davide/0000-0002-9190-662X; Margutti,
Raffaella/0000-0003-4768-7586
FU NSF [1066293]; David and Lucile Packard Foundation Fellowship for
Science and Engineering award
FX We thank the referee for helpful comments that improved the quality of
our work. R.M. is grateful to the Aspen Center for Physics and the NSF
Grant #1066293 for hospitality during the completion of this work and
for providing a stimulating environment that inspired this project.
Support for this work was provided by the David and Lucile Packard
Foundation Fellowship for Science and Engineering awarded to A.M.S.
NR 62
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 159
DI 10.1088/0004-637X/805/2/159
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400074
ER
PT J
AU Meyer, ET
Georganopoulos, M
Sparks, WB
Godfrey, L
Lovell, JEJ
Perlman, E
AF Meyer, Eileen T.
Georganopoulos, Markos
Sparks, William B.
Godfrey, Leith
Lovell, James E. J.
Perlman, Eric
TI RULING OUT IC/CMB X-RAYS IN PKS 0637-752 AND THE IMPLICATIONS FOR TEV
EMISSION FROM LARGE-SCALE QUASAR JETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (PKS 0637-752, 3C
273)
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; INVERSE-COMPTON MODEL;
EXTENDED RADIO JETS; 3C 273; CHANDRA OBSERVATIONS; COSMOLOGICAL IMPACT;
EXTRAGALACTIC JETS; SYNCHROTRON; 3C-273
AB The Chandra X-ray observatory has discovered dozens of resolved, kiloparsec-scale jets associated with powerful quasars in which the X-ray fluxes are observed to be much higher than the expected level based on the radio-optical synchrotron spectrum. The most popular explanation for the anomalously high and hard X-ray fluxes is that these jets do not decelerate significantly by the kiloparsec scale, but rather remain highly relativistic (Lorentz factors Gamma similar to 10). By adopting a small angle to the line of sight, the X-rays can thus be explained by inverse Compton upscattering of cosmic microwave background (CMB) photons (IC/CMB), where the observed emission is strongly Doppler boosted. Using over six years of Fermi monitoring data, we show that the expected hard, steady gamma-ray emission implied by the IC/CMB model is not seen in PKS 0637-752, the prototype jet for which this model was first proposed. IC/CMB emission is thus ruled out as the source of the X-rays, joining recent results for the jets in 3C 273 (using the same method) and PKS 1136-135 (using UV polarization). We further show that the Fermi observations give an upper limit of delta < 6.5 for the four brightest X-ray knots of PKS 0637-752, and derive an updated limit of delta < 7.8 for knots A and B1 of 3C 273 (assuming equipartition). Finally, we discuss the fact that high levels of synchrotron X-ray emission in a slow jet will unavoidably lead to a level of angle-integrated TeV emission which exceeds that of the TeV BL Lac class.
C1 [Meyer, Eileen T.; Sparks, William B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meyer, Eileen T.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Godfrey, Leith] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands.
[Lovell, James E. J.] Univ Tasmania, Sch Phys Sci, Hobart, Tas 7001, Australia.
[Perlman, Eric] Florida Inst Technol, Melbourne, FL 32901 USA.
RP Meyer, ET (reprint author), Space Telescope Sci Inst, Baltimore, MD 21218 USA.
EM meyer@stsci.edu
OI Perlman, Eric/0000-0002-3099-1664
FU Fermi Grant [NNX13AO88G]
FX E. T. M. acknowledges Fermi Grant NNX13AO88G.
NR 46
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 154
DI 10.1088/0004-637X/805/2/154
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400069
ER
PT J
AU Miceli, M
Sciortino, S
Troja, E
Orlando, S
AF Miceli, M.
Sciortino, S.
Troja, E.
Orlando, S.
TI SPATIAL DISTRIBUTION OF X-RAY EMITTING EJECTA IN TYCHO'S SNR:
INDICATIONS OF SHOCKED TITANIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Tycho's SNR); ISM: supernova remnants; X-rays:
ISM
ID SUPERNOVA REMNANT W49B; IA SUPERNOVAE; CORE-COLLAPSE; EMISSION;
PROGENITOR; SPECTRUM; MODELS; LINE; SPECTROPOLARIMETRY; NUCLEOSYNTHESIS
AB Young supernova remnants (SNRs) show characteristic ejecta-dominated X-ray emission that allows us to probe the products of explosive nucleosynthesis processes and to ascertain important information about the physics of supernova explosions. Hard X-ray observations have recently revealed the presence of the radioactive decay lines of Ti-44 at similar to 67.9 and similar to 78.4 keV in Tycho's SNR. Here, we analyze a set of XMM-Newton archive observations of Tycho's SNR. We produce equivalent width (EW) maps of the Fe K and Ca XIX emission lines and find indications for a stratification of the abundances of these elements and significant anisotropies. We then perform spatially resolved spectral analysis by identifying five different regions characterized by high/low values of the Fe K EW. We find that the spatial distribution of the Fe K emission is correlated with that of Cr XXII. We also detect the Ti K line complex in the spectra extracted from the two regions with the highest values of Fe and Cr EWs. The Ti line emission remains undetected in regions where Fe and Cr EWs are low. Our results indicate that the post-shock Ti is spatially colocated with other iron-peak nuclei in Tycho's SNR, in agreement with the predictions of multi-D models of SNe Ia.
C1 [Miceli, M.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy.
[Miceli, M.; Sciortino, S.; Orlando, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
[Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Miceli, M (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM miceli@astropa.unipa.it
OI Troja, Eleonora/0000-0002-1869-7817; Miceli, Marco/0000-0003-0876-8391;
Orlando, Salvatore/0000-0003-2836-540X
FU PRIN INAF grant
FX We thank the anonymous referee for comments and suggestions. This paper
was partially funded by the PRIN INAF 2014 grant. M.M. thanks M. Dadina
for discussions about the X-IFU instrumental background.
NR 40
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 120
DI 10.1088/0004-637X/805/2/120
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400035
ER
PT J
AU Plavchan, P
Chen, X
Pohl, G
AF Plavchan, Peter
Chen, Xi
Pohl, Garrett
TI WHAT IS THE MASS OF alpha CEN B b?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: dynamical evolution and stability; planets and
satellites: formation; planets and satellites: individual (alpha
Centauri)
ID TERRESTRIAL PLANET FORMATION; BINARY STAR SYSTEMS; CENTAURI-B; TIDAL
DISSIPATION; STELLAR ACTIVITY; ROTATION; KEPLER; DISCS; CIRCULARIZATION;
COPLANARITY
AB We investigate the possibility of constraining the sin i degeneracy of alpha Cen B b-with orbital period P = 3.24 days; a = 0.042 AU; m sin i = 1.1 M-circle plus-to estimate the true mass of the newly reported terrestrial exoplanet in the nearest stellar system to our Sun. We present detailed numerical simulations of the dynamical stability of the exoplanet in the alpha Cen AB binary system for a range of initial inclinations, eccentricities, and semimajor axes. The system represents a benchmark case for the interplay of the Kozai mechanism with general relativistic and tidal forces. From our simulations, there is only a small boundary in initial inclinations and initial semimajor axes which result in the migration via the Kozai mechanism of alpha Cen B b to its present location. Inside this boundary, the planet orbit is stable for up to 1 Gyr against the Kozai mechanism, and outside this boundary the planet collides with alpha Cen B or is ejected. In our three simulations where the planet migrates in toward the star via the Kozai mechanism, the final inclination is 46 degrees-53 degrees relative to the AB orbital plane, lower than the initial inclination of 75 degrees in each case. We discuss inclination constraints from the formation of alpha Cen B b in situ at its present location, migration in a proto-planetary disk, or migration in resonance with additional planets. We conclude that alpha Cen B b probably has a mass of less than 2.7 M-circle plus, implying a likely terrestrial composition warranting future confirmation.
C1 [Plavchan, Peter; Pohl, Garrett] Dept Phys Astron & Mat Sci, 901 South Natl Ave, Springfield, MO 65897 USA.
[Chen, Xi] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Plavchan, P (reprint author), Dept Phys Astron & Mat Sci, 901 South Natl Ave, Springfield, MO 65897 USA.
EM peterplavchan@missouristate.edu
OI Plavchan, Peter/0000-0002-8864-1667
FU National Aeronautics and Space Administration under Exoplanet
Exploration Program; NASA JPL Research and Technology Development
program; Missouri SpaceGrant Consortium
FX We thank the anonymous referee for a thoughtful review that improved the
clarity and presentation of this manuscript. The authors acknowledge
Thayne Currie, Dave Latham, and David Ciardi for their encouragement in
writing this paper. This research has made use of the NASA Exoplanet
Archive, which is operated by the California Institute of Technology,
under contract with the National Aeronautics and Space Administration
under the Exoplanet Exploration Program. P.P. acknowledges support from
a NASA JPL Research and Technology Development program, and the Missouri
SpaceGrant Consortium.
NR 67
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 174
DI 10.1088/0004-637X/805/2/174
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400089
ER
PT J
AU Sadykov, VM
Dominguez, SV
Kosovichev, AG
Sharykin, IN
Struminsky, AB
Zimovets, I
AF Sadykov, Viacheslav M.
Dominguez, Santiago Vargas
Kosovichev, Alexander G.
Sharykin, Ivan N.
Struminsky, Alexei B.
Zimovets, Ivan
TI PROPERTIES OF CHROMOSPHERIC EVAPORATION AND PLASMA DYNAMICS OF A SOLAR
FLARE FROM IRIS OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; Sun: activity; Sun: atmosphere; Sun: flares; Sun: UV
radiation
ID LOOP RADIATIVE HYDRODYNAMICS; REGION-IMAGING-SPECTROGRAPH; HIGH TIME
RESOLUTION; EXTREME-ULTRAVIOLET; SPECTROSCOPIC OBSERVATIONS; NONTHERMAL
ELECTRONS; HINODE; SPECTROMETER; TRANSPORT; EVENTS
AB The dynamics of hot chromospheric plasma of solar flares is a key to understanding the mechanisms of flare energy release and particle acceleration. A moderate M1.0 class flare of 2014 June 12, (SOL2014-06-12T21:12) was simultaneously observed by NASA's Interface Region Imaging Spectrograph (IRIS) and. other spacecraft, and also by the New Solar Telescope at the BBSO. This paper presents the first part of our investigation focused on analysis of the IRIS data. Our analysis of the IRIS data in different spectral lines reveals a strong redshifted jet-like flow with a speed of similar to 100 km s(-1) of the chromospheric material before the flare. Strong nonthermal emission of the C II k 1334.5 angstrom line, formed in the chromosphere-corona transition region, is observed at the beginning of the impulsive phase in several small (with a size of similar to 1 '') points. It is also found that the C II k line is redshifted across the flaring region before, during, and after the impulsive phase. A peak of integrated emission of the hot (1.1 . 10(7) K) plasma in the Fe XXI 1354.1 angstrom line is detected approximately five minutes after the integrated emission peak of the lower temperature C II k. A strong blueshift of the Fe XXI line across the flaring region corresponds to evaporation flows of the hot chromospheric plasma with a speed of 50 km s-1. Additional analysis of the RHESSI data supports the idea that the upper chromospheric dynamics observed by IRIS has features of "gentle" evaporation driven by heating of the solar chromosphere by accelerated electrons and by a heat flux from the flare energy release site.
C1 [Sadykov, Viacheslav M.; Dominguez, Santiago Vargas; Kosovichev, Alexander G.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Sadykov, Viacheslav M.; Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sadykov, Viacheslav M.; Sharykin, Ivan N.; Struminsky, Alexei B.; Zimovets, Ivan] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Sadykov, Viacheslav M.; Struminsky, Alexei B.] MIPT, Dolgoprudnyi 141700, Moscow Region, Russia.
[Dominguez, Santiago Vargas] Univ Nacl Colombia, Observatorio Astron, Bogota, Colombia.
RP Sadykov, VM (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA.
RI Zimovets, Ivan/E-4431-2017
OI Zimovets, Ivan/0000-0001-6995-3684
FU NASA Ames Research Center; NASA [NNX14AB68G, NNX14AB70G, NNX11AO736];
NSF [AGS-1250818]; RFBR grant [15-32-21078]; NJIT grant
FX The authors acknowledge the Big Bear Solar Observatory (BBSO) observing
and technical team, and the IRIS mission team and the NASA Ames Research
Center for their contributions and support. The authors thank the
referee for very useful comments. The work was partially supported by
NASA grants NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant
AGS-1250818; RFBR grant 15-32-21078; and an NJIT grant.
NR 41
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Z9 8
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 167
DI 10.1088/0004-637X/805/2/167
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400082
ER
PT J
AU Seo, YM
Shirley, YL
Goldsmith, P
Ward-Thompson, D
Kirk, JM
Schmalzl, M
Lee, JE
Friesen, R
Langston, G
Masters, J
Garwood, RW
AF Seo, Young Min
Shirley, Yancy L.
Goldsmith, Paul
Ward-Thompson, Derek
Kirk, Jason M.
Schmalzl, Markus
Lee, Jeong-Eun
Friesen, Rachel
Langston, Glen
Masters, Joe
Garwood, Robert W.
TI AN AMMONIA SPECTRAL MAP OF THE L1495-B218 FILAMENTS IN THE TAURUS
MOLECULAR CLOUD. I. PHYSICAL PROPERTIES OF FILAMENTS AND DENSE CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: molecules; radio lines: ISM; stars: formation
ID GOULD BELT SURVEY; STAR-FORMATION; PRESTELLAR CORES; CO DEPLETION; PIPE
NEBULA; DARK CLOUDS; GRAVITATIONAL COLLAPSE; INTERSTELLAR AMMONIA;
(CO)-O-18 DEPLETION; VLBA DETERMINATION
AB We present deep NH3 observations of the L1495-B218 filaments in the Taurus molecular cloud covering over a 3 degrees angular range using the K-band focal plane array on the 100 m Green Bank Telescope. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed NH3 (1, 1) and (2, 2) with a spectral resolution of 0.038 km s(-1) and a spatial resolution of 31 ''. Most of the ammonia peaks coincide with intensity peaks in dust continuum maps at 350 and 500 mu m. We deduced physical properties by fitting a model to the observed spectra. We find gas kinetic temperatures of 8-15 K, velocity dispersions of 0.05-0.25 km s(-1), and NH3 column densities of 5 x 10(12) to 1 x 10(14) cm(-2). The CSAR algorithm, which is a hybrid of seeded-watershed and binary dendrogram algorithms, identifies a total of 55 NH3 structures, including 39 leaves and 16 branches. The masses of the NH3 sources range from 0.05 to 9.5 M-circle dot. The masses of NH3 leaves are mostly smaller than their corresponding virial mass estimated from their internal and gravitational energies, which suggests that these leaves are gravitationally unbound structures. Nine out of 39 NH3 leaves are gravitationally bound, and seven out of nine gravitationally bound NH3 leaves are associated with star formation. We also found that 12 out of 30 gravitationally unbound leaves are pressure. confined. Our data suggest that a dense core may form as a pressure-confined structure, evolve to a gravitationally bound core, and undergo collapse to form a protostar.
C1 [Seo, Young Min; Shirley, Yancy L.] Univ Arizona, Dept Astron Steward Observ, Tucson, AZ 85721 USA.
[Goldsmith, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ward-Thompson, Derek; Kirk, Jason M.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Schmalzl, Markus] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi Do, South Korea.
[Friesen, Rachel] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Langston, Glen] Natl Sci Fdn, Astron, Arlington, VA 22230 USA.
[Masters, Joe; Garwood, Robert W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Seo, YM (reprint author), Univ Arizona, Dept Astron Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
FU NRAO Observer's Grant [GBT/13A-126]; NSF Grant [AST-1008577,
AST-1410190]
FX We are grateful to the anonymous referee for helpful suggestions. We are
also grateful to A. Hacar and M. Tafalla for providing C18O
data. Y. Seo was support by a NRAO Observer's Grant (GBT/13A-126) and
partially by NSF Grant AST-1008577. Y. Shirley was partially supported
by NSF Grants AST-1008577 and AST-1410190. This work was carried out in
part at the Jet Propulsion Laboratory, which is operated for NASA by the
California Institute of Technology.
NR 97
TC 5
Z9 5
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 185
DI 10.1088/0004-637X/805/2/185
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400100
ER
PT J
AU Tsai, CW
Eisenhardt, PRM
Wu, JW
Stern, D
Assef, RJ
Blain, AW
Bridge, CR
Benford, DJ
Cutri, RM
Griffith, RL
Jarrett, TH
Lonsdale, CJ
Masci, FJ
Moustakas, LA
Petty, SM
Sayers, J
Stanford, SA
Wright, EL
Yan, L
Leisawitz, DT
Liu, FC
Mainzer, AK
McLean, IS
Padgett, DL
Skrutskie, MF
Gelino, CR
Beichman, CA
Juneau, S
AF Tsai, Chao-Wei
Eisenhardt, Peter R. M.
Wu, Jingwen
Stern, Daniel
Assef, Roberto J.
Blain, Andrew W.
Bridge, Carrie R.
Benford, Dominic J.
Cutri, Roc M.
Griffith, Roger L.
Jarrett, Thomas H.
Lonsdale, Carol J.
Masci, Frank J.
Moustakas, Leonidas A.
Petty, Sara M.
Sayers, Jack
Stanford, S. Adam
Wright, Edward L.
Yan, Lin
Leisawitz, David T.
Liu, Fengchuan
Mainzer, Amy K.
McLean, Ian S.
Padgett, Deborah L.
Skrutskie, Michael F.
Gelino, Christopher R.
Beichman, Charles A.
Juneau, Stephanie
TI THE MOST LUMINOUS GALAXIES DISCOVERED BY WISE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; infrared: galaxies; quasars: supermassive black holes
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DUST-OBSCURED
GALAXIES; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ADAPTIVE
OPTICS SYSTEM; STAR-FORMING GALAXIES; INFRARED GALAXIES; DATA RELEASE;
SUBMILLIMETER GALAXIES
AB We present 20 Wide-field Infrared Survey Explorer (WISE)-selected galaxies with bolometric luminosities L-bol > 10(14) L-circle dot, including five with infrared luminosities L-IR equivalent to L(rest 8-1000 mu m) > 10(14) L-circle dot. These "extremely luminous infrared galaxies," or ELIRGs, were discovered using the "W1W2-dropout" selection criteria which requires marginal or non-detections at 3.4 and 4.6 mu m (W1 and W2, respectively) but strong detections at 12 and 22 mu m in the WISE survey. Their spectral energy distributions are dominated by emission at rest-frame 4-10 mu m, suggesting that hot dust with T-d similar to 450 K is responsible for the high luminosities. These galaxies are likely powered by highly obscured active galactic nuclei (AGNs), and there is no evidence suggesting these systems are beamed or lensed. We compare this WISE-selected sample with 116 optically selected quasars that reach the same L-bol level, corresponding to the most luminous unobscured quasars in the literature. We find that the rest-frame 5.8 and 7.8 mu m luminosities of the WISE-selected ELIRGs can be 30%-80% higher than that of the unobscured quasars. The existence of AGNs with L-bol > 10(14) L-circle dot at z > 3 suggests that these supermassive black holes are born with large mass, or have very rapid mass assembly. For black hole seed masses similar to 10(3) M-circle dot, either sustained super-Eddington accretion is needed, or the radiative efficiency must be <15%, implying a black hole with slow spin, possibly due to chaotic accretion.
C1 [Tsai, Chao-Wei; Eisenhardt, Peter R. M.; Stern, Daniel; Moustakas, Leonidas A.; Liu, Fengchuan; Mainzer, Amy K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wu, Jingwen; Wright, Edward L.; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Assef, Roberto J.] Univ Diego Port, Fac Ingn, Nucl Astron, Santiago, Chile.
[Blain, Andrew W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bridge, Carrie R.; Sayers, Jack] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Benford, Dominic J.; Leisawitz, David T.; Padgett, Deborah L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cutri, Roc M.; Masci, Frank J.; Yan, Lin; Gelino, Christopher R.; Beichman, Charles A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Griffith, Roger L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Jarrett, Thomas H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Lonsdale, Carol J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Petty, Sara M.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Juneau, Stephanie] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France.
RP Tsai, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Chao-Wei.Tsai@jpl.nasa.gov
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 [13-ADAP13-0092]; NASA;
W.M. Keck Foundation; NASA Postdoctoral Program at the Jet Propulsion
Laboratory; Gemini-CONICYT [32120009]
FX The authors thank the anonymous referee for the constructive comments
and for encouraging a more thorough discussion of gravitational lensing
in this paper. This publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, and NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology. WISE and NEOWISE are funded by the National Aeronautics and
Space Administration. This work is also based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. 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. Part of this research has made use of the Keck
Observatory Archive (KOA), which is operated by the W. M. Keck
Observatory and the NASA Exoplanet Science Institute (NExScI), under
contract with the National Aeronautics and Space Administration. This
research has made use of the NASA/IPAC Infrared Science Archive and the
NASA/IPAC Extragalactic Database (NED), which are operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contracts with the National Aeronautics and Space Administration. This
material is based upon work supported by the National Aeronautics and
Space Administration under Proposal No. 13-ADAP13-0092 issued through
the Astrophysics Data Analysis Program. C.-W. T. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA. R. J. A. was supported by Gemini-CONICYT grant
number 32120009.
NR 119
TC 29
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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 JUN 1
PY 2015
VL 805
IS 2
AR 90
DI 10.1088/0004-637X/805/2/90
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400005
ER
PT J
AU Walton, DJ
Reynolds, MT
Miller, JM
Reis, RC
Stern, D
Harrison, FA
AF Walton, D. J.
Reynolds, M. T.
Miller, J. M.
Reis, R. C.
Stern, D.
Harrison, F. A.
TI BROAD IRON EMISSION FROM GRAVITATIONALLY LENSED QUASARS OBSERVED BY
CHANDRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; SPINNING BLACK-HOLE;
X-RAY REFLECTION; EMITTING REGIONS; NGC 4151; ACCRETION; EVOLUTION;
LINES; GALAXIES
AB Recent work has demonstrated the potential of gravitationally lensed quasars to extend measurements of black hole spin out to high redshift with the current generation of X-ray observatories. Here we present an analysis of a large sample of 27 lensed quasars in the redshift range 1.0 less than or similar to z less than or similar to 4.5 observed with Chandra, utilizing over 1.6 Ms of total observing time, focusing on the rest-frame iron K emission from these sources. Although the X-ray signal-to-noise ratio (S/N) currently available does not permit the detection of iron emission from the inner accretion disk in individual cases in our sample, we find significant structure in the stacked residuals. In addition to the narrow core, seen almost ubiquitously in local active galactic nuclei (AGNs), we find evidence for an additional underlying broad component from the inner accretion disk, with a clear red wing to the emission profile. Based on simulations, we find the detection of this broader component to be significant at greater than the 3 sigma level. This implies that iron emission from the inner disk is relatively common in the population of lensed quasars, and in turn further demonstrates that, with additional observations, this population represents an opportunity to significantly extend the sample of AGN spin measurements out to high redshift.
C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walton, D. J.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Reynolds, M. T.; Miller, J. M.; Reis, R. C.] Univ Michigan, Dept Astron, Ann Arbor, MI 49109 USA.
RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA
FX The authors would like to thank the reviewer for providing feedback
which helped improve this paper, and Julian Merten for useful
discussions. The work of D.J.W./D.S. was performed at JPL/Caltech, under
contract with NASA.
NR 53
TC 3
Z9 3
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2015
VL 805
IS 2
AR 161
DI 10.1088/0004-637X/805/2/161
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL1PG
UT WOS:000356715400076
ER
PT J
AU Luo, T
Wang, ZE
Ferrare, RA
Hostetler, CA
Yuan, RM
Zhang, DM
AF Luo, Tao
Wang, Zhien
Ferrare, Richard A.
Hostetler, Chris A.
Yuan, Renmin
Zhang, Damao
TI Vertically resolved separation of dust and other aerosol types by a new
lidar depolarization method
SO OPTICS EXPRESS
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; OPTICAL-PROPERTIES; SAHARAN DUST; RETRIEVALS
AB This paper developed a new retrieval framework of external mixing of the dust and non-dust aerosol to predict the lidar ratio of the external mixing aerosols and to separate the contributions of non-spherical aerosols by using different depolarization ratios among dust, sea salt, smoke, and polluted aerosols. The detailed sensitivity tests and case study with the new method showed that reliable dust information could be retrieved even without prior information about the non-dust aerosol types. This new method is suitable for global dust retrievals with satellite observations, which is critical for better understanding global dust transportation and for model improvements. (C)2015 Optical Society of America
C1 [Luo, Tao; Wang, Zhien; Zhang, Damao] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82070 USA.
[Ferrare, Richard A.; Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Luo, Tao; Yuan, Renmin] Univ Sci & Technol China, Sch Earth & Space Sci, Hefei 230031, Anhui, Peoples R China.
RP Wang, ZE (reprint author), Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82070 USA.
EM zwang@uwyo.edu
RI zhang, damao/A-2900-2016; Wang, Zhien/F-4857-2011
OI zhang, damao/0000-0002-3518-292X;
FU NASA grant [NNX13AQ41G]; NASA/JPL
FX The CALIPSO data set was obtained from the NASA Langley Research Center
Atmospheric Science Data Center (eosweb.larc.nasa.gov). The CloudSat
2B-GEOPROF and ECMWF-AUX products were obtained from CloudSat Data
Processing Center (cloudsat.cira.colostate.edu). The HSRL data was
obtained from NASA (science.larc.nasa.gov/hsrl/). This research was
funded by NASA grant NNX13AQ41G and a contract from NASA/JPL.
NR 39
TC 1
Z9 1
U1 9
U2 20
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 JUN 1
PY 2015
VL 23
IS 11
BP 14095
EP 14107
DI 10.1364/OE.23.014095
PG 13
WC Optics
SC Optics
GA CL4DI
UT WOS:000356902400069
PM 26072778
ER
PT J
AU Lin, B
Nehrir, AR
Harrison, FW
Browell, EV
Ismail, S
Obland, MD
Campbell, J
Dobler, J
Meadows, B
Fan, TF
Kooi, S
AF Lin, Bing
Nehrir, Amin R.
Harrison, F. Wallace
Browell, Edward V.
Ismail, Syed
Obland, Michael D.
Campbell, Joel
Dobler, Jeremy
Meadows, Byron
Fan, Tai-Fang
Kooi, Susan
TI Atmospheric CO2 column measurements in cloudy conditions using
intensity-modulated continuous-wave lidar at 1.57 micron
SO OPTICS EXPRESS
LA English
DT Article
ID ABSORPTION
AB This study evaluates the capability of atmospheric CO2 column measurements under cloudy conditions using an airborne intensity-modulated continuous-wave integrated-path-differential-absorption lidar operating in the 1.57-mu m CO2 absorption band. The atmospheric CO2 column amounts from the aircraft to the tops of optically thick cumulus clouds and to the surface in the presence of optically thin clouds are retrieved from lidar data obtained during the summer 2011 and spring 2013 flight campaigns, respectively. For the case of intervening thin cirrus clouds with an average cloud optical depth of about 0.16 over an arid/semi-arid area, the CO2 column measurements from 12.2 km altitude were found to be consistent with the cloud free conditions with a lower precision due to the additional optical attenuation of the thin clouds. The clear sky precision for this flight campaign case was about 0.72% for a 0.1-s integration, which was close to previously reported flight campaign results. For a vegetated area and lidar path lengths of 8 to 12 km, the precision of the measured differential absorption optical depths to the surface was 1.3 - 2.2% for 0.1-s integration. The precision of the CO2 column measurements to thick clouds with reflectance about 1/10 of that of the surface was about a factor of 2 to 3 lower than that to the surface owing to weaker lidar returns from clouds and a smaller CO2 differential absorption optical depth compared to that for the entire column. (C) 2015 Optical Society of America
C1 [Lin, Bing; Nehrir, Amin R.; Harrison, F. Wallace; Ismail, Syed; Obland, Michael D.; Campbell, Joel; Meadows, Byron] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Browell, Edward V.] NASA, Langley Res Ctr, STARSS II Affiliate, Hampton, VA 23681 USA.
[Dobler, Jeremy] Exelis Inc, Ft Wayne, IN 46818 USA.
[Fan, Tai-Fang; Kooi, Susan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Lin, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM bing.lin@nasa.gov
FU NASA ASCENDS Mission Study and NASA Langley Research Center
FX The authors would like to express their appreciation to D. MacDonnell,
D. Garber, D. McGregor, and Y. Hu for their valuable comments and
encouragement. This research was supported by the NASA ASCENDS Mission
Study and NASA Langley Research Center.
NR 12
TC 3
Z9 3
U1 3
U2 11
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 JUN 1
PY 2015
VL 23
IS 11
BP A582
EP A593
PG 12
WC Optics
SC Optics
GA CL4DI
UT WOS:000356902400019
PM 26072883
ER
PT J
AU Jiang, JZ
Hofmann, D
Jarvis, DJ
Fecht, HJ
AF Jiang, Jian-Zhong
Hofmann, Douglas
Jarvis, David John
Fecht, Hans-J.
TI Low-Density High-Strength Bulk Metallic Glasses and Their Composites: A
Review
SO ADVANCED ENGINEERING MATERIALS
LA English
DT Review
ID HIGH MECHANICAL STRENGTH; CA-MG-ZN; SUPERCOOLED LIQUID REGION; AMORPHOUS
MATRIX COMPOSITES; HIGH-TENSILE STRENGTH; MOLD CASTING METHOD; SHAPED
COPPER MOLD; FCC-AL PARTICLES; FORMING ABILITY; THERMAL-STABILITY
AB This review gives an overview of the field of low-density (<6gcm(-3)) bulk metallic glasses/composites and their potential engineering and space applications. The review focuses on four systems, Al-, Mg-, Ca-, and Ti-based metallic glass-forming systems. In the following sections, glass forming ability, mechanical properties, thermal stability, and corrosion resistance of the four metallic glass systems and their composites are presented.
C1 [Fecht, Hans-J.] Univ Ulm, Inst Micro & Nanomat, Fac Engn & Comp Sci, D-89081 Ulm, Germany.
[Jiang, Jian-Zhong] Zhejiang Univ, Dept Mat Sci & Engn, ICNSM, Hangzhou 310027, Zhejiang, Peoples R China.
[Jiang, Jian-Zhong] Zhejiang Univ, Lab New Struct Mat, Hangzhou 310027, Zhejiang, Peoples R China.
[Hofmann, Douglas] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA.
[Jarvis, David John] ESA ESTEC, Noordwijk, Netherlands.
RP Jiang, JZ (reprint author), Zhejiang Univ, Dept Mat Sci & Engn, ICNSM, Hangzhou 310027, Zhejiang, Peoples R China.
EM hans.fecht@uni-ulm.de
FU European Space Agency ESA (AccMet project); European Space Agency ESA
(ThermoLab-ISS); National Key Basic Research Program of China
[2012CB825700]; National Natural Science Foundation of China [51371157,
10979002]; Zhejiang University-Helmholtz Cooperation fund; Fundamental
Research Funds for the Central Universities; Air Force Office of
Scientific Research [RF01152700/PO60020925]
FX The authors gratefully acknowledge the useful discussions with Dr. A.L.
Greer (University of Cambridge UK) and the technical support by Dr. L.
Y. Chen (International Center for New-Structured Materials (ICNSM),
Zhejiang University P. R. China), Dr. B. O. Malomo (Department of
Mechanical Engineering, Obafemi Awolowo University, Ile-Ife, Nigeria),
Dr. R. K. Wunderlich, Dr. K. Bruhne, and Dr. A. Sommer (University of
Ulm). The authors like to thank the funding agencies supporting this
work, in particular the European Space Agency ESA (AccMet project and
ThermoLab-ISS) and the National Key Basic Research Program of China
(2012CB825700), National Natural Science Foundation of China (grants
51371157 and 10979002), Zhejiang University-Helmholtz Cooperation fund
and the Fundamental Research Funds for the Central Universities. D. H.
acknowledges financial support from the Air Force Office of Scientific
Research under Grant No. RF01152700/PO60020925.
NR 177
TC 5
Z9 5
U1 17
U2 91
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1438-1656
EI 1527-2648
J9 ADV ENG MATER
JI Adv. Eng. Mater.
PD JUN
PY 2015
VL 17
IS 6
BP 761
EP 780
DI 10.1002/adem.201400252
PG 20
WC Materials Science, Multidisciplinary
SC Materials Science
GA CK6XQ
UT WOS:000356372500004
ER
PT J
AU Hanisch, RJ
Berriman, GB
Lazio, TJW
Bunn, SE
Evans, J
McGlynn, TA
Plante, R
AF Hanisch, R. J.
Berriman, G. B.
Lazio, T. J. W.
Bunn, S. Emery
Evans, J.
McGlynn, T. A.
Plante, R.
TI The Virtual Astronomical Observatory: Re-engineering access to
astronomical data
SO ASTRONOMY AND COMPUTING
LA English
DT Article
DE Catalogs; Surveys; Virtual observatory tools; Data discovery; Data
access; Applications
ID TOOL; VO; SOFTWARE; SYSTEM; IRIS
AB The US Virtual Astronomical Observatory was a software infrastructure and development project designed both to begin the establishment of an operational Virtual Observatory (VU) and to provide the US coordination with the international VU effort. The concept of the VU is to provide the means by which an astronomer is able to discover, access, and process data seamlessly, regardless of its physical location. This paper describes the origins of the VAO, including the predecessor efforts within the US National Virtual Observatory, and summarizes its main accomplishments. These accomplishments include the development of both scripting toolkits that allow scientists to incorporate VU data directly into their reduction and analysis environments and high-level science applications for data discovery, integration, analysis, and catalog cross-comparison. Working with the international community, and based on the experience from the software development, the VAO was a major contributor to international standards within the International Virtual Observatory Alliance. The VAO also demonstrated how an operational virtual observatory could be deployed, providing a robust operational environment in which VU services worldwide were routinely checked for aliveness and compliance with international standards. Finally, the VAO engaged in community outreach, developing a comprehensive web site with on-line tutorials, announcements, links to both US and internationally developed tools and services, and exhibits and hands-on training at annual meetings of the American Astronomical Society and through summer schools and community days. All digital products of the VAO Project, including software, documentation, and tutorials, are stored in a repository for community access. The enduring legacy of the VAO is an increasing expectation that new telescopes and facilities incorporate VU capabilities during the design of their data management systems. Published by Elsevier B.V.
C1 [Hanisch, R. J.] Virtual Astron Observ, Washington, DC 20036 USA.
[Hanisch, R. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Berriman, G. B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bunn, S. Emery] CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA.
[Evans, J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[McGlynn, T. A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Sci Arch Res Ctr, Greenbelt, MD 20771 USA.
[Plante, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.hanisch@nist.gov; gbb@ipac.caltech.edu;
joseph.lazio@jpl.nasa.gov; janet@cfa.harvard.edu;
thomas.a.mcglynn@nasa.gov; rplante@illinois.edu
FU National Science Foundation [AST-0834235]; NASA [NNX13AC07G];
NASA/HEASARC; National Aeronautics & Space Administration (NASA)
FX The VAO program would not have been possible without the financial
support of the National Science Foundation (AST-0834235) and NASA
(NNX13AC07G to STScI/MAST), and it was supported NASA/HEASARC. Funding
at IPAC has been provided by a grant from the National Aeronautics &
Space Administration (NASA) to the Jet Propulsion Laboratory, operated
by the California Institute of Technology under contract to NASA. We
appreciate the wise guidance of the Board of Directors of the VAO, LLC,
and the VAO Science Council, and we are grateful for feedback from the
astronomical community that helped us improve our science tools and
infrastructure. 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 47
TC 3
Z9 3
U1 1
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2213-1337
EI 2213-1345
J9 ASTRON COMPUT
JI Astron. Comput.
PD JUN
PY 2015
VL 11
SI SI
BP 190
EP 209
DI 10.1016/j.ascom.2015.03.007
PN B
PG 20
WC Astronomy & Astrophysics; Computer Science, Interdisciplinary
Applications
SC Astronomy & Astrophysics; Computer Science
GA CK9FV
UT WOS:000356546900015
ER
PT J
AU Gerakines, PA
Hudson, RL
AF Gerakines, Perry A.
Hudson, Reggie L.
TI INFRARED SPECTRA AND OPTICAL CONSTANTS OF ELUSIVE AMORPHOUS METHANE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: molecules
ID ICES RELEVANT; INTENSITY MEASUREMENTS; INTERSTELLAR ICE; PURE ICES; CH4;
MIXTURES; ETHANE; PLUTO; ION; SPECTROSCOPY
AB New and accurate laboratory results are reported for amorphous methane (CH4) ice near 10 K for the study of the interstellar medium (ISM) and the outer solar system. Near-and mid-infrared (IR) data, including spectra, band strengths, absorption coefficients, and optical constants, are presented for the first time for this seldom-studied amorphous solid. The apparent IR band strength near 1300 cm(-1) (7.69 mu m) for amorphous CH4 is found to be about 33% higher than the value long used by IR astronomers to convert spectral observations of interstellar CH4 into CH4 abundances. Although CH4 is most likely to be found in an amorphous phase in the ISM, a comparison of results from various laboratory groups shows that the earlier CH4 band strength at 1300 cm(-1) (7.69 mu m) was derived from IR spectra of ices that were either partially or entirely crystalline CH4. Applications of the new amorphous-CH4 results are discussed, and all optical constants are made available in electronic form.
C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
EM Reggie.Hudson@NASA.gov
RI Gerakines, Perry/D-2226-2012
OI Gerakines, Perry/0000-0002-9667-5904
FU NASA Astrobiology Institute through the Goddard Center for Astrobiology;
NASA
FX NASA funding through the Outer Planets Research and Cassini Data
Analysis programs is acknowledged. Both authors received partial support
from the NASA Astrobiology Institute through the Goddard Center for
Astrobiology. The experimental assistance of Marla Moore, Mark Loeffler,
and Robert Ferrante is acknowledged.
NR 35
TC 8
Z9 8
U1 3
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 JUN 1
PY 2015
VL 805
IS 2
AR L20
DI 10.1088/2041-8205/805/2/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL0IY
UT WOS:000356626900010
ER
PT J
AU Saito, T
Kurita, M
Okamoto, H
Uchida, I
Parker, D
Balazs, G
AF Saito, Tomomi
Kurita, Masanori
Okamoto, Hitoshi
Uchida, Itaru
Parker, Denise
Balazs, George
TI Tracking Male Loggerhead Turtle Migrations Around Southwestern Japan
Using Satellite Telemetry
SO CHELONIAN CONSERVATION AND BIOLOGY
LA English
DT Article
DE Reptilia; Testudines: Cheloniidae; Caretta caretta; male; migration; sea
surface temperature
ID CENTRAL NORTH PACIFIC; CARETTA-CARETTA; SEA-TURTLES; ADULT FEMALE;
HABITAT USE; OCEAN
AB Three satellite-tagged male loggerhead turtles (Caretta caretta) were released from the coastal waters of Satsuma Peninsula, Kyusyu, southwestern Japan (lat 31 degrees 42'N, long 130 degrees 18'E), and their movements were tracked for up to 449 d. Total distance traveled by the turtles ranged from 1540 to 5519 km. The turtles remained mainly along the coast and islands of the East China Sea and the Sea of Japan, except for spending a brief period of time (1-30 d) in the open ocean. The long-distance movement followed a seasonal pattern, evidently triggered by fluctuations in sea surface temperature.
C1 [Saito, Tomomi; Kurita, Masanori; Okamoto, Hitoshi; Uchida, Itaru] Port Nagoya Publ Aquarium, Minato Ku, Nagoya, Aichi 4550033, Japan.
[Parker, Denise] Joint Inst Marine & Atmospher Res, Newport, OR 97365 USA.
[Balazs, George] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA.
RP Saito, T (reprint author), Kochi Univ, Usa Marine Biol Inst, Tosa, Kochi 7811164, Japan.
EM t-saito@kochi-u.ac.jp; m-kurita@nagoyaminato.or.jp;
h-nakamura@nagoyaminato.or.jp; itsahonuworldinhawaii@hotmail.com;
Denise.Parker@noaa.gov
NR 32
TC 2
Z9 3
U1 7
U2 24
PU CHELONIAN RESEARCH FOUNDATION
PI LUNENBURG
PA 168 GOODRICH ST., LUNENBURG, MA USA
SN 1071-8443
EI 1943-3956
J9 CHELONIAN CONSERV BI
JI Chelonian Conserv. Biol.
PD JUN
PY 2015
VL 14
IS 1
BP 82
EP 87
PG 6
WC Zoology
SC Zoology
GA CK8ZM
UT WOS:000356529000011
ER
PT J
AU Salas, E
Tannenbaum, SI
Kozlowski, SWJ
Miller, CA
Mathieu, JE
Vessey, WB
AF Salas, Eduardo
Tannenbaum, Scott I.
Kozlowski, Steve W. J.
Miller, Christopher A.
Mathieu, John E.
Vessey, William B.
TI Teams in Space Exploration: A New Frontier for the Science of Team
Effectiveness
SO CURRENT DIRECTIONS IN PSYCHOLOGICAL SCIENCE
LA English
DT Article
DE teams; teamwork; team training; team cohesion
ID DYNAMICS; ORGANIZATIONS; PERFORMANCE; MODELS; METAANALYSIS
AB Researchers from a variety of disciplines are currently working with NASA to prepare for human exploration of Mars in the next decades. Such exploration will take scientific discovery to new heights, providing unprecedented information about the geology, atmosphere, and potential for life on Mars, including previous life, current life, and perhaps even our own lives in the future. To make these unparalleled discoveries, however, astronauts will need to undertake a novel and unprecedented journey. Moreover, the mission to Mars will require a team of crew members who will have to endure and sustain team performance requirements never seen before. Multidisciplinary teams of scientists have begun to provide the needed steps to address this challenge. The purpose of this article is (a) to illustrate the kinds of new conceptual frameworks and paradigms needed for teams in space exploration, (b) to delineate promising research paths to ensure that a robust team science can emerge for long-duration space exploration (LDSE), (c) to showcase initial findings and insights from studying astronauts now, and (d) to outline a plan of action for team-effectiveness research in LDSE.
C1 [Salas, Eduardo] Rice Univ, Dept Psychol, Houston, TX 77005 USA.
[Tannenbaum, Scott I.] Grp Org Effectiveness, Albany, NY USA.
[Kozlowski, Steve W. J.] Michigan State Univ, Dept Psychol, E Lansing, MI 48824 USA.
[Miller, Christopher A.] Smart Informat Flow Technol, Minneapolis, MN USA.
[Mathieu, John E.] Univ Connecticut, Dept Management, Storrs, CT USA.
[Vessey, William B.] NASA Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX USA.
RP Salas, E (reprint author), Rice Univ, Dept Psychol, MS-25,Sewall Hall 464, Houston, TX 77005 USA.
EM esalas@ist.ucf.edu
OI KOZLOWSKI, STEVE/0000-0002-5123-3424
NR 60
TC 5
Z9 5
U1 3
U2 19
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0963-7214
EI 1467-8721
J9 CURR DIR PSYCHOL SCI
JI Curr. Dir. Psychol.
PD JUN
PY 2015
VL 24
IS 3
BP 200
EP 207
DI 10.1177/0963721414566448
PG 8
WC Psychology, Multidisciplinary
SC Psychology
GA CK6AH
UT WOS:000356309600007
ER
PT J
AU Chan, C
Albright, S
Gorius, N
Brasunas, J
Jennings, D
Flasar, FM
Carlson, R
Guandique, E
Nixon, C
AF Chan, Cheong
Albright, Shane
Gorius, Nicolas
Brasunas, John
Jennings, Don
Flasar, F. Michael
Carlson, Ronald
Guandique, Ever
Nixon, Conor
TI Electrical interferences observed in the Cassini CIRS spectrometer
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Fourier transform spectrometer; Electrical noise; Engineering;
Spacecraft instrumentation
AB The Composite Infrared Spectrometer (CIRS) carried onboard the Cassini spacecraft has now operated successfully for 17 years, following launch in 1997. Following insertion into Saturnian orbit in July 2004, the instrument has taken data nearly continuously, returning over 100 million interferograms (spectra) to date. Although of generally high quality, and resulting in more than 100 peer-reviewed scientific articles, the spectra are afflicted with several types of instrumental electrical (non-random) noise artifacts. These noise artifacts require either mitigation strategies (prevention), removal from the observed data, or else awareness of the affected spectral areas which must be excluded from scientific analysis. The sources and nature of these varied noise types were not readily identified until after launch. The purpose of this article is to inform users of the noise in the CIRS dataset and to serve as a 'lesson-learned' guide for designers of future instruments.
C1 [Chan, Cheong; Albright, Shane; Gorius, Nicolas; Brasunas, John; Jennings, Don; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Carlson, Ronald; Guandique, Ever; Nixon, Conor] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guandique, Ever] ADNET Syst Inc, Bethesda, MD 20817 USA.
RP Chan, C (reprint author), NASA, Goddard Space Flight Ctr, Sch Aerosp Engn, Atlanta, GA 30332 USA.
EM cheongyuchan@gmail.com; conor.a.nixon@nasa.gov
RI Flasar, F Michael/C-8509-2012; Nixon, Conor/A-8531-2009
OI Nixon, Conor/0000-0001-9540-9121
FU NASA Education office
FX The authors would like to thank the CIRS team for their cooperation and
the NASA Education office for funding the internship.
NR 33
TC 1
Z9 1
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD JUN
PY 2015
VL 39
IS 2
BP 367
EP 386
DI 10.1007/s10686-015-9452-3
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK6VA
UT WOS:000356365200009
ER
PT J
AU Lai, QZ
Wu, LG
She, CL
AF Lai Qiao-zhen
Wu Li-guang
She Chung-lin
TI SEA SURFACE TEMPERATURE RESPONSE TO TYPHOON MORAKOT (2009) AND ITS
INFLUENCE
SO JOURNAL OF TROPICAL METEOROLOGY
LA English
DT Article
DE sea surface temperature; typhoon; ocean response; typhoon track forecast
ID TROPICAL CYCLONE; HURRICANE; MODEL; SIMULATIONS; INTENSITY; PACIFIC;
LAYER
AB While previous studies indicate that typhoons can decrease sea surface temperature (SST) along their tracks, a few studies suggest that the cooling patterns in coastal areas are different from those in the open sea. However, little is known about how the induced cooling coupled with the complex ocean circulation in the coastal areas can affect tropical cyclone track and intensity. The sea surface responses to the land falling process of Typhoon Morakot (2009) are examined observationally and its influences on the activity of the typhoon are numerically simulated with the WRF model. The present study shows that the maximum SST cooling associated with Morakot occurred on the left-hand side of the typhoon track during its landfall. Numerical simulations show that, together with the SST gradients associated with the coastal upwelling and mesoscale oceanic vortices, the resulting SST cooling can cause significant difference in the typhoon track, comparable to the current 24-hour track forecasting error. It is strongly suggested that it is essential to include the non-uniform SST distribution in the coastal areas for further improvement in typhoon track forecast.
C1 [Lai Qiao-zhen] Longyan Meteorol Off Fujian Prov, Longyan 364000, Peoples R China.
[Wu Li-guang] Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China.
[She Chung-lin] NASA, Goddard Space Flight Ctr, UMBC Goddard Earth & Sci Technol Ctr, Greenbelt, MD 20771 USA.
RP Wu, LG (reprint author), Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China.
EM liguang@nuist.edu.cn
FU National Key Technology Research and Development Program of China
[2009CB421503]; New Recruitment Graduate Project of the Fujian Province
Meteorological Bureau [2012G01]
FX Foundation item: National Key Technology Research and Development
Program of China (2009CB421503); New Recruitment Graduate Project of the
Fujian Province Meteorological Bureau (2012G01)
NR 25
TC 0
Z9 0
U1 3
U2 8
PU JOURNAL OF TROPICAL METEOROLOGICAL PRESS
PI GUANGZHOU
PA 6 FU JIN RD, GUANGZHOU, 510080, PEOPLES R CHINA
SN 1006-8775
J9 J TROP METEOROL
JI J. Trop. Meteorol.
PD JUN
PY 2015
VL 21
IS 2
BP 111
EP 120
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK9KA
UT WOS:000356557800002
ER
PT J
AU Kokhanovsky, AA
Davis, AB
Cairns, B
Dubovik, O
Hasekamp, OP
Sano, I
Mukai, S
Rozanov, VV
Litvinov, P
Lapyonok, T
Kolomiets, IS
Oberemok, YA
Savenkov, S
Martin, W
Wasilewski, A
Di Noia, A
Stap, FA
Rietjens, J
Xu, F
Natraj, V
Duan, M
Cheng, T
Munro, R
AF Kokhanovsky, A. A.
Davis, A. B.
Cairns, B.
Dubovik, O.
Hasekamp, O. P.
Sano, I.
Mukai, S.
Rozanov, V. V.
Litvinov, P.
Lapyonok, T.
Kolomiets, I. S.
Oberemok, Y. A.
Savenkov, S.
Martin, W.
Wasilewski, A.
Di Noia, A.
Stap, F. A.
Rietjens, J.
Xu, F.
Natraj, V.
Duan, M.
Cheng, T.
Munro, R.
TI Space-based remote sensing of atmospheric aerosols: The multi-angle
spectro-polarimetric frontier
SO EARTH-SCIENCE REVIEWS
LA English
DT Article
DE Aerosol; Remote sensing; Polarimetry; Optical instrumentation; Radiative
transfer; Climate change
ID VECTOR RADIATIVE-TRANSFER; MARKOV-CHAIN FORMALISM; CLOUD-TOP PRESSURE;
OXYGEN-A-BAND; BIDIRECTIONAL REFLECTANCE MODEL; MOLECULAR LINE
ABSORPTION; SKY RADIANCE MEASUREMENTS; POINT-SPREAD FUNCTION; DISCRETE
RANDOM-MEDIA; OPTICAL-PROPERTIES
AB The review of optical instrumentation, forward modeling, and inverse problem solution for the polarimetric aerosol remote sensing from space is presented. The special emphasis is given to the description of current airborne and satellite imaging polarimeters and also to modern satellite aerosol retrieval algorithms based on the measurements of the Stokes vector of reflected solar light as detected on a satellite. Various underlying surface reflectance models are discussed and evaluated. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Kokhanovsky, A. A.; Munro, R.] EUMETSAT, D-64367 Darmstadt, Germany.
[Davis, A. B.; Xu, F.; Natraj, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cairns, B.; Martin, W.; Wasilewski, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dubovik, O.; Litvinov, P.; Lapyonok, T.] Univ Lille 1, CNRS, Lab Opt Atmospher, Lille, France.
[Hasekamp, O. P.; Di Noia, A.; Stap, F. A.; Rietjens, J.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Sano, I.] Kinki Univ, Fac Sci & Technol, Higashiosaka, Osaka 6778502, Japan.
[Mukai, S.] Kyoto Coll Grad Studies Informat, Sakyo Ku, Kyoto 6068225, Japan.
[Rozanov, V. V.] Univ Bremen, Inst Remote Sensing, D-28359 Bremen, Germany.
[Kolomiets, I. S.; Oberemok, Y. A.; Savenkov, S.] Kiev Taras Shevchenko Univ, Radiophys Dept, UA-01601 Kiev, Ukraine.
[Duan, M.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China.
[Duan, M.; Cheng, T.] Chinese Acad Sci, Inst Remote Sensing & Digital Earth RADI, Beijing, Peoples R China.
[Stap, F. A.] Univ Utrecht, Inst Marine & Atmospher Res, NL-3508 TA Utrecht, Netherlands.
RP Kokhanovsky, AA (reprint author), EUMETSAT, Eumetsat Allee 1, D-64367 Darmstadt, Germany.
EM Alexander.kokhanovsky@eumetsat.int
RI Cheng, Tianhai/H-1113-2013; Kokhanovsky, Alexander/C-6234-2016; Xu,
Feng/G-3673-2013;
OI Cheng, Tianhai/0000-0001-7889-9579; Kokhanovsky,
Alexander/0000-0001-7370-1164; Cairns, Brian/0000-0002-1980-1022; Di
Noia, Antonio/0000-0002-5052-0763
FU International Space Science Institute (ISSI) in Bern (Switzerland);
EUMETSAT; JAXA's Global Change Observation Mission - Climate 1 (GCOM-C1)
[JX-PSPC-40059]; JSPS KAKENHI [25340019]; NASA; ESA; DFG; SRON; CNRS;
Bremen University; Lille University
FX This work was supported financially by the International Space Science
Institute (ISSI) in Bern (Switzerland), by EUMETSAT, by JAXA's Global
Change Observation Mission - Climate 1 (GCOM-C1) project
(JX-PSPC-40059), by JSPS KAKENHI (25340019), and by NASA, ESA, DFG,
SRON, CNRS, as well as Bremen University and Lille University. The
authors extend special thanks to Vladimir Budak, Dave Diner, Mike Garay,
Ya. Ilyushin, Ralph Kahn, Olga Kalashnikova, Rob Levy, Anton Lopatin,
John Martonchik, Michael Mishchenko, Lorraine Remer, Felix Seidel,
Robert Spurr, Knut Stamnes, Didier Tanre, and Elenora Zege for the many
useful discussions related to the topic of this paper, at ISSI and
elsewhere. We thank K. Tanaka and H. Murakami of the JAXA (Japan) for
providing us with detailed information about S-GLI. Part of this
research was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 221
TC 10
Z9 11
U1 8
U2 23
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-8252
EI 1872-6828
J9 EARTH-SCI REV
JI Earth-Sci. Rev.
PD JUN
PY 2015
VL 145
BP 85
EP 116
DI 10.1016/j.earscirev.2015.01.012
PG 32
WC Geosciences, Multidisciplinary
SC Geology
GA CK0HC
UT WOS:000355885300007
ER
PT J
AU Seager, R
Hooks, A
Williams, AP
Cook, B
Nakamura, J
Henderson, N
AF Seager, Richard
Hooks, Allison
Williams, A. Park
Cook, Benjamin
Nakamura, Jennifer
Henderson, Naomi
TI Climatology, Variability, and Trends in the US Vapor Pressure Deficit,
an Important Fire-Related Meteorological Quantity*
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID WESTERN UNITED-STATES; DATA ASSIMILATION SYSTEM; NORTH-AMERICA;
WILDFIRE; DROUGHT; FORESTS; US; TEMPERATURE; MECHANISMS; REANALYSIS
AB Unlike the commonly used relative humidity, vapor pressure deficit (VPD) is an absolute measure of the difference between the water vapor content of the air and its saturation value and an accurate metric of the ability of the atmosphere to extract moisture from the land surface. VPD has been shown to be closely related to variability in burned forest areas in the western United States. Here, the climatology, variability, and trends in VPD across the United States are presented. VPD reaches its climatological maximum in summer in the interior southwest United States because of both high temperatures and low vapor pressure under the influence of the northerly, subsiding eastern flank of the Pacific subtropical anticyclone. Maxima of variance of VPD are identified in the Southwest and southern plains in spring and summer and are to a large extent driven by temperature variance, but vapor pressure variance is also important in the Southwest. La Nina-induced circulation anomalies cause subsiding, northerly flow that drives down actual vapor pressure and increases saturation vapor pressure from fall through spring. High spring and summer VPDs can also be caused by reduced precipitation in preceding months, as measured by Bowen ratio anomalies. Case studies of 2002 (the Rodeo-Chediski and Hayman fires, which occurred in Arizona and Colorado, respectively) and 2007 (the Murphy Complex fire, which occurred in Idaho and Nevada) show very high VPDs caused by antecedent surface drying and subsidence warming and drying of the atmosphere. VPD has increased in the southwest United States since 1961, driven by warming and a drop in actual vapor pressure, but has decreased in the northern plains and Midwest, driven by an increase in actual vapor pressure.
C1 [Seager, Richard; Williams, A. Park; Nakamura, Jennifer; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Hooks, Allison] Columbia Univ, Columbia Coll, New York, NY 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 Rte 9W, Palisades, NY 10964 USA.
EM seager@ldeo.columbia.edu
RI Cook, Benjamin/H-2265-2012; Williams, Park/B-8214-2016
OI Williams, Park/0000-0001-8176-8166
FU NSF [AGS-1243204]; Earth Institute at Columbia University undergraduate
research internship
FX This work was supported by NSF Award AGS-1243204 (Linking Near-term
Future Changes in Weather and Hydroclimate in Western North America to
Adaptation for Ecosystem and Water Management). Author AH was supported
by an Earth Institute at Columbia University undergraduate research
internship. The GLDAS data used in this study were acquired as part of
NASA's Earth-Sun System Division and were archived and distributed by
the Goddard Earth Sciences (GES) Data and Information Services Center
(DISC) Distributed Active Archive Center (DAAC). We thank three
reviewers for their helpful comments and criticisms.
NR 43
TC 9
Z9 9
U1 7
U2 26
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JUN
PY 2015
VL 54
IS 6
BP 1121
EP 1141
DI 10.1175/JAMC-D-14-0321.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK6VY
UT WOS:000356367900001
ER
PT J
AU Leppert, KD
Cecil, DJ
AF Leppert, Kenneth D., II
Cecil, Daniel J.
TI Signatures of Hydrometeor Species from Airborne Passive Microwave Data
for Frequencies 10-183 GHz
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PHYSICAL PRECIPITATION RETRIEVAL; MESOSCALE CONVECTIVE SYSTEMS;
CLOUD-RADIATION MODEL; POLARIMETRIC RADAR; SATELLITE MEASUREMENTS; VIDEO
DISDROMETER; ICE CLOUDS; RAIN; CLASSIFICATION; IDENTIFICATION
AB Passive microwave brightness temperatures (BTs) collected above severe thunderstorms using the Advanced Microwave Precipitation Radiometer and Conical Scanning Millimeter-Wave Imaging Radiometer during the Midlatitude Continental Convective Clouds Experiment are compared with a hydrometeor identification applied to dual-polarimetric Weather Surveillance Radar-1988 Doppler radar data collected at Vance Air Force Base, Oklahoma (KVNX). The goal of this work is to determine the signatures of various hydrometeor species in terms of BTs measured at frequencies used by the Global Precipitation Measurement mission Microwave Imager. Results indicate that hail is associated with an ice-scattering signature at all frequencies examined, including 10.7 GHz. However, it appears that frequencies <= 37.1 GHz are most useful for identifying hail. Low-level (below 2.5 km) hail becomes probable for a BT below 240 K at 19.4 GHz, 170 K at 37.1 GHz, 90 K at 85.5 GHz, 80 K at 89.0 GHz, 100 K at 165.5 GHz, and 100 K at 183.3 +/- 7 GHz. Graupel may be distinguished from hail and profiles without any hydrometeor species by its strong scattering signature at higher frequencies (e.g., 165.5 GHz) and its relative lack of scattering at frequencies <= 19.4 GHz. There is a clearer distinction between profiles that contain liquid precipitation and profiles without any hydrometeors when the liquid is associated above with hail and/or graupel (i.e., a hydrometeor category with a strong scattering signature) than when the liquid is associated with smaller ice. Near-surface precipitation is much more likely for a 19.4-GHz BT < 250 K, 37.1-GHz BT < 240 K, 89.0-GHz BT < 220 K, and 165.5-GHz BT < 140 K.
C1 [Leppert, Kenneth D., II] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
[Cecil, Daniel J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Leppert, KD (reprint author), NSSTC, Rm 4074,320 Sparkman Dr, Huntsville, AL 35805 USA.
EM leppert@nsstc.uah.edu
RI Measurement, Global/C-4698-2015
FU NASA Precipitation Measurement Missions Science Team
FX Funding for this research was generously provided through the NASA
Precipitation Measurement Missions Science Team. The authors thank Dr.
Brenda Dolan for providing the code used for the hydrometeor
identification and her help in running the code. The authors also thank
Dr. Timothy Lang for his helpful suggestions for this work and three
anonymous reviewers for providing thoughtful and helpful suggestions for
improving the manuscript. In addition, the authors gratefully
acknowledge the NASA EOSDIS Global Hydrology Resource Center DAAC for
providing the AMPR, CoSMIR, and KVNX radar data.
NR 36
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PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JUN
PY 2015
VL 54
IS 6
BP 1313
EP 1334
DI 10.1175/JAMC-D-14-0145.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK6VY
UT WOS:000356367900013
ER
PT J
AU Carey, LD
Petersen, WA
AF Carey, Lawrence D.
Petersen, Walter A.
TI Sensitivity of C-Band Polarimetric Radar-Based Drop Size Estimates to
Maximum Diameter
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID DUAL-POLARIZATION RADAR; 2D VIDEO DISDROMETER; SMALL RAINDROP
DISTORTION; AXIS RATIOS; DIFFERENTIAL REFLECTIVITY; LABORATORY
MEASUREMENTS; DISTRIBUTION TRUNCATION; DISTRIBUTION PARAMETERS;
DISTRIBUTION RETRIEVAL; RAINFALL ESTIMATION
AB Estimating raindrop size has been a long-standing objective of polarimetric radar-based precipitation retrieval methods. The relationship between the differential reflectivity Z(dr) and the median volume diameter D-0 is typically derived empirically using raindrop size distribution observations from a disdrometer, a raindrop physical model, and a radar scattering model. Because disdrometers are known to undersample large raindrops, the maximum drop diameter D-max is often an assumed parameter in the rain physical model. C-band Z(dr) is sensitive to resonance scattering at drop diameters larger than 5 mm, which falls in the region of uncertainty for D-max. Prior studies have not accounted for resonance scattering at C band and D-max uncertainty in assessing potential errors in drop size retrievals. As such, a series of experiments are conducted that evaluate the effect of D-max parameterization on the retrieval error of D-0 from a fourth-order polynomial function of C-band Z(dr) by varying the assumed D-max through the range of assumptions found in the literature. Normalized bias errors for estimating D-0 from C-band Z(dr) range from -8% to 15%, depending on the postulated error in D-max. The absolute normalized bias error increases with C-band Z(dr), can reach 10% for Z(dr) as low as 1-1.75 dB, and can increase from there to values as large as 15%-45% for larger Z(dr), which is a larger potential bias error than is found at S and X band. Uncertainty in D-max assumptions and the associated potential D-0 retrieval errors should be noted and accounted for in future C-band polarimetric radar studies.
C1 [Carey, Lawrence D.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Petersen, Walter A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Carey, LD (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM larry.carey@nsstc.uah.edu
FU NASA [NNM05AA22A, NNM11AA01A, NNX13AI89G]
FX This research is funded by Dr. Ramesh Kakar, NASA Precipitation
Measurement Mission (PMM), Dr. Gail Skofronick-Jackson, NASA GPM Project
Scientist, and Dr. Mathew Schwaller, NASA GPM Project Office under the
following NASA Contracts: NNM05AA22A, NNM11AA01A, and NNX13AI89G. We
also acknowledge the late Dr. Arthur Hou, whose leadership as the former
NASA GPM Project Scientist was essential to the success of the GPM
program and the realization of this study. We thank Patrick Gatlin, Matt
Wingo, and Chris Schultz for their careful operation and maintenance of
the 2DVD units at the NSSTC berm in Huntsville over many years. We thank
Dr. V. N. Bringi for the use of the CSU 2DVD data, close collaboration,
scientific leadership in the retrieval of raindrop characteristics from
polarimetric radar, and his insight into this research. We acknowledge
the many members of the NASA PMM DSD Working Group who have provided
ideas, insightful comments, and encouragement during the conduct of this
research, including Mr. Patrick Gatlin, Dr. Ali Tokay, Dr. Merhala
Thurai, and Dr. Chris Williams. Constructive comments from four
anonymous reviewers greatly improved the clarity of the text and
figures.
NR 67
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PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JUN
PY 2015
VL 54
IS 6
BP 1352
EP 1371
DI 10.1175/JAMC-D-14-0079.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK6VY
UT WOS:000356367900015
ER
PT J
AU Rutan, DA
Kato, S
Doelling, DR
Rose, FG
Nguyen, LT
Caldwell, TE
Loeb, NG
AF Rutan, David A.
Kato, Seiji
Doelling, David R.
Rose, Fred G.
Le Trang Nguyen
Caldwell, Thomas E.
Loeb, Norman G.
TI CERES Synoptic Product: Methodology and Validation of Surface Radiant
Flux
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID RESEARCH MOORED ARRAY; ENERGY SYSTEM CERES; DIURNAL-VARIATIONS;
RADIATIVE PROPERTIES; CLEAR SKIES; ISCCP DATA; CLOUD; IRRADIANCE; MODEL;
TOP
AB The Clouds and the Earth's Radiant Energy System Synoptic (SYN1deg), edition 3, product provides climate-quality global 3-hourly 1 degrees x 1 degrees gridded top of atmosphere, in-atmosphere, and surface radiant fluxes. The in-atmosphere surface fluxes are computed hourly using a radiative transfer code based upon inputs from Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS), 3-hourly geostationary (GEO) data, and meteorological assimilation data from the Goddard Earth Observing System. The GEO visible and infrared imager calibration is tied to MODIS to ensure uniform MODIS-like cloud properties across all satellite cloud datasets. Computed surface radiant fluxes are compared to surface observations at 85 globally distributed land (37) and ocean buoy (48) sites as well as several other publicly available global surface radiant flux data products. Computed monthly mean downward fluxes from SYN1deg have a bias (standard deviation) of 3.0 W m(-2) (5.7%) for shortwave and -4.0 W m(-2) (2.9%) for longwave compared to surface observations. The standard deviation between surface downward shortwave flux calculations and observations at the 3-hourly time scale is reduced when the diurnal cycle of cloud changes is explicitly accounted for. The improvement is smaller for surface downward longwave flux owing to an additional sensitivity to boundary layer temperature/humidity, which has a weaker diurnal cycle compared to clouds.
C1 [Rutan, David A.; Rose, Fred G.; Le Trang Nguyen; Caldwell, Thomas E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kato, Seiji; Doelling, David R.; Loeb, Norman G.] SSAI, Hampton, VA USA.
RP Rutan, DA (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.
EM david.a.rutan@nasa.gov
FU NASA CERES project
FX This work was funded by the NASA CERES project. The products and the
validation could not have been accomplished without the help of the
CERES TISA team. Data were obtained from the NASA Langley Research
Center EOSDIS Distributed Active Archive Center. We also wish to
acknowledge the hard work by the many dedicated scientists maintaining
surface instrumentation in diverse climates to obtain high-quality
observations of downwelling shortwave and longwave surface flux. Those
groups are noted in appendix B. We also thank the reviewers, whose close
read of the paper greatly improved the end result.
NR 57
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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 JUN
PY 2015
VL 32
IS 6
BP 1121
EP 1143
DI 10.1175/JTECH-D-14-00165.1
PG 23
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CK6WN
UT WOS:000356369500001
ER
PT J
AU Marvel, K
Zelinka, M
Klein, SA
Bonfils, C
Caldwell, P
Doutriaux, C
Santer, BD
Taylor, KE
AF Marvel, Kate
Zelinka, Mark
Klein, Stephen A.
Bonfils, Celine
Caldwell, Peter
Doutriaux, Charles
Santer, Benjamin D.
Taylor, Karl E.
TI External Influences on Modeled and Observed Cloud Trends
SO JOURNAL OF CLIMATE
LA English
DT Article
ID 20TH-CENTURY TEMPERATURE; ATMOSPHERIC CIRCULATION; GENERAL-CIRCULATION;
FEEDBACK PROCESSES; CLIMATE-CHANGE; TROPICAL BELT; OCEAN; ISCCP;
PACIFIC; CMIP5
AB Understanding the cloud response to external forcing is a major challenge for climate science. This crucial goal is complicated by intermodel differences in simulating present and future cloud cover and by observational uncertainty. This is the first formal detection and attribution study of cloud changes over the satellite era. Presented herein are CMIP5 model-derived fingerprints of externally forced changes to three cloud properties: the latitudes at which the zonally averaged total cloud fraction (CLT) is maximized or minimized, the zonal average CLT at these latitudes, and the height of high clouds at these latitudes. By considering simultaneous changes in all three properties, the authors define a coherent multivariate fingerprint of cloud response to external forcing and use models from phase 5 of CMIP (CMIP5) to calculate the average time to detect these changes. It is found that given perfect satellite cloud observations beginning in 1983, the models indicate that a detectable multivariate signal should have already emerged. A search is then made for signals of external forcing in two observational datasets: ISCCP and PATMOS-x. The datasets are both found to show a poleward migration of the zonal CLT pattern that is incompatible with forced CMIP5 models. Nevertheless, a detectable multivariate signal is predicted by models over the PATMOS-x time period and is indeed present in the dataset. Despite persistent observational uncertainties, these results present a strong case for continued efforts to improve these existing satellite observations, in addition to planning for new missions.
C1 [Marvel, Kate; Zelinka, Mark; Klein, Stephen A.; Bonfils, Celine; Caldwell, Peter; Doutriaux, Charles; Santer, Benjamin D.; Taylor, Karl E.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Marvel, Kate] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Marvel, Kate] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
RP Marvel, K (reprint author), Columbia Univ, NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM katherine.d.marvel@nasa.gov
RI Taylor, Karl/F-7290-2011; Santer, Benjamin/F-9781-2011; Klein,
Stephen/H-4337-2016; Zelinka, Mark/C-4627-2011
OI Taylor, Karl/0000-0002-6491-2135; Klein, Stephen/0000-0002-5476-858X;
Zelinka, Mark/0000-0002-6570-5445
FU Regional and Global Climate Modeling Program of the U.S. Department of
Energy (DOE) Office of Science; DOE Lawrence Livermore National
Laboratory [DE-AC52-07NA27344]; Laboratory Directed Research and
Development award [13-ERD-032]; DOE/OBER Early Career Research Program
[SCW1295]
FX CMIP5 data processing was enabled by the CDAT analysis package. The EOF
analysis was performed using the eofs software package available from
http://ajdawson.github.io/eofs/. This work was supported by the Regional
and Global Climate Modeling Program of the U.S. Department of Energy
(DOE) Office of Science and was performed under the auspices of the DOE
Lawrence Livermore National Laboratory (Contract DE-AC52-07NA27344). KM
was supported by a Laboratory Directed Research and Development award
(13-ERD-032). CB was supported by the DOE/OBER Early Career Research
Program Award SCW1295. 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 A1 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.
NR 66
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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 JUN
PY 2015
VL 28
IS 12
BP 4820
EP 4840
DI 10.1175/JCLI-D-14-00734.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK5RR
UT WOS:000356283900012
ER
PT J
AU Orbe, C
Newman, PA
Waugh, DW
Holzer, M
Oman, LD
Li, F
Polvani, LM
AF Orbe, Clara
Newman, Paul A.
Waugh, Darryn W.
Holzer, Mark
Oman, Luke D.
Li, Feng
Polvani, Lorenzo M.
TI Airmass Origin in the Arctic. Part I: Seasonality
SO JOURNAL OF CLIMATE
LA English
DT Article
ID WARM CONVEYOR BELTS; AIR-POLLUTION; STORM TRACKS; TROPOSPHERIC
TRANSPORT; GLOBAL CLIMATOLOGY; WATER-VAPOR; STRATOSPHERE; ANTICYCLONE;
TROPOPAUSE; EXCHANGE
AB The first climatology of airmass origin in the Arctic is presented in terms of rigorously defined airmass fractions that partition air according to where it last contacted the planetary boundary layer (PBL). Results from a present-day climate integration of the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM) reveal that the majority of air in the Arctic below 700 mb last contacted the PBL poleward of 60 degrees N. By comparison, 62% (+/- 0.8%) of the air above 700 mb originates over Northern Hemisphere midlatitudes (i.e., "midlatitude air"). Seasonal variations in the airmass fractions above 700 mb reveal that during boreal winter air from midlatitudes originates primarily over the oceans, with 26% (+/- 1.9%) last contacting the PBL over the eastern Pacific, 21% (+/- 0.87%) over the Atlantic, and 16% (+/- 1.2%) over the western Pacific. During summer, by comparison, midlatitude air originates primarily over land, overwhelmingly so over Asia [41% (+/- 1.0%)] and, to a lesser extent, over North America [24% (+/- 1.5%)]. Seasonal variations in the airmass fractions are interpreted in terms of changes in the large-scale ventilation of the midlatitude boundary layer and the midlatitude tropospheric jet.
C1 [Orbe, Clara; Newman, Paul A.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Holzer, Mark; Polvani, Lorenzo M.] Univ New S Wales, Sch Math & Stat, Dept Appl Math, Sydney, NSW, Australia.
[Holzer, Mark] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Li, Feng] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Polvani, Lorenzo M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
EM clara.orbe@nasa.gov
RI Oman, Luke/C-2778-2009; Waugh, Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; Waugh, Darryn/0000-0001-7692-2798
FU NASA; ARC [DP120100674]; NSF [AGS-1403676, AGS-1402931]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The authors also
acknowledge support from ARC Grant DP120100674 (M.H.) and NSF Grants
AGS-1403676 (D.W.) and AGS-1402931 (M.H. and L.M.P.).
NR 66
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PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD JUN
PY 2015
VL 28
IS 12
BP 4997
EP 5014
DI 10.1175/JCLI-D-14-00720.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK5RR
UT WOS:000356283900023
ER
PT J
AU Thomas, BF
Vogel, RM
Famiglietti, JS
AF Thomas, Brian F.
Vogel, Richard M.
Famiglietti, James S.
TI Objective hydrograph baseflow recession analysis
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Hydromorphology; Groundwater/surface water interaction; Quantile
regression; Numerical derivative; Linear reservoir; Water withdrawal
ID SMOOTHING NOISY DATA; SPLINE FUNCTIONS; FLOW RECESSION; STREAMFLOW;
HYDROLOGY; WATER; RAINFALL; SYSTEMS; STORAGE; CURVES
AB A streamflow hydrograph recession curve expresses the theoretical relationship between aquifer structure and groundwater outflow to a stream channel. That theoretical relationship is often portrayed empirically using a recession plot defined as a plot of ln(-dQ/dt) versus ln(Q), where Q is streamflow discharge. Such hydrograph recession plots are commonly used to estimate recession parameters, aquifer properties and for evaluating alternative hydrologic hypotheses. We introduce a comprehensive and objective approach to analyze baseflow recessions with innovations including the use of quantile regression, efficient and objective numerical estimation of dQ/dt, inclusion of groundwater withdrawals, and incorporation of seasonal effects. We document that these innovations when all combined, lead to significant improvements, over previous studies, in our ability to discern the theoretical behavior of stream aquifer systems. A case study reveals that our methodology enables us to reject the simple linear reservoir hypothesis of stream aquifer interactions for watersheds in New Jersey and results in improved correlations between low flow statistics and aquifer properties for those same watersheds. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Thomas, Brian F.; Famiglietti, James S.] Univ Calif Irvine, Ctr Hydrol Modeling, Irvine, CA 92697 USA.
[Thomas, Brian F.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thomas, Brian F.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Vogel, Richard M.] Tufts Univ, Dept Civil & Environm Engn, Medford, MA 02155 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
RP Thomas, BF (reprint author), 4800 Oak Grove Dr,Mail Stop 300-329, Pasadena, CA 91109 USA.
EM Brian.F.Thomas@jpl.nasa.gov
RI Vogel, Richard/A-8513-2008
OI Vogel, Richard/0000-0001-9759-0024
FU Tufts Institute for the Environment (TIE); University of California
Office of the President Multicampus Research and Programs Initiative;
National Aeronautics and Space Administration
FX Project support was provided by a fellowship awarded to the first author
by the Tufts Institute for the Environment (TIE); and by the University
of California Office of the President Multicampus Research and Programs
Initiative. A portion of the research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
authors also express their appreciation to Charles Kroll for helpful
comments, two anonymous reviewers and Editor Peter Kitanidis whose
comments contributed to substantial improvements to the original
manuscript.
NR 70
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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 JUN
PY 2015
VL 525
BP 102
EP 112
DI 10.1016/j.jhydrol.2015.03.028
PG 11
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA CK0HF
UT WOS:000355885600008
ER
PT J
AU Li, BL
Rodell, M
Famiglietti, JS
AF Li, Bailing
Rodell, Matthew
Famiglietti, James S.
TI Groundwater variability across temporal and spatial scales in the
central and northeastern US
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Spatial and temporal variability of; groundwater storage anomalies;
Scale dependency of groundwater storage; Groundwater recharge
ID CLIMATE EXPERIMENT GRACE; SOIL-MOISTURE; GRAVITY RECOVERY; WATER;
SURFACE; DEPLETION; RECHARGE; STORAGE; ASSIMILATION; ILLINOIS
AB Depth-to-water measurements from 181 monitoring wells in unconfined or semi-confined aquifers in nine regions of the central and northeastern U.S. were analyzed. Groundwater storage exhibited strong seasonal variations in all regions, with peaks in spring and lows in autumn, and its interannual variability was nearly unbounded, such that the impacts of droughts, floods, and excessive pumping could persist for many years. We found that the spatial variability of groundwater storage anomalies (deviations from the long term mean) increases as a power function of extent scale (square root of area). That relationship, which is linear on a log-log graph, is common to other hydrological variables but had never before been shown with groundwater data. We describe how the derived power function can be used to determine the number of wells needed to estimate regional mean groundwater storage anomalies with a desired level of accuracy, or to assess uncertainty in regional mean estimates from a set number of observations. We found that the spatial variability of groundwater storage anomalies within a region often increases with the absolute value of the regional mean anomaly, the opposite of the relationship between soil moisture spatial variability and mean. Recharge (drainage from the lowest model soil layer) simulated by the Variable Infiltration Capacity (VIC) model was compatible with observed monthly groundwater storage anomalies and month-to-month changes in groundwater storage. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Li, Bailing] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Li, Bailing; Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Famiglietti, James S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA.
RP Li, BL (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM bailing.li@nasa.gov
RI Rodell, Matthew/E-4946-2012
OI Rodell, Matthew/0000-0003-0106-7437
FU NASA's Terrestrial Hydrology Program
FX This research was funded by NASA's Terrestrial Hydrology Program. We
thank the USGS and the Illinois State Water Survey for providing the
groundwater data, David Mocko for providing monthly NLDAS-2 VIC model
output and anonymous reviewers for their comments that have helped
improve the quality of this paper.
NR 42
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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 JUN
PY 2015
VL 525
BP 769
EP 780
DI 10.1016/j.jhydrol.2015.04.033
PG 12
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA CK0HF
UT WOS:000355885600065
ER
PT J
AU Yasuda, T
Iwakiri, WB
Tashiro, MS
Terada, Y
Kouzu, T
Enoto, T
Nakagawa, YE
Bamba, A
Urata, Y
Yamaoka, K
Ohno, M
Shibata, S
Makishima, K
AF Yasuda, Tetsuya
Iwakiri, Wataru B.
Tashiro, Makoto S.
Terada, Yukikatsu
Kouzu, Tomomi
Enoto, Teruaki
Nakagawa, Yujin E.
Bamba, Aya
Urata, Yuji
Yamaoka, Kazutaka
Ohno, Masanori
Shibata, Shinpei
Makishima, Kazuo
TI Sub-MeV band observation of a hard burst from AXP 1E 1547.0-5408 with
the Suzaku Wide-band All-sky Monitor
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE stars: magnetars; X-rays: bursts; X-rays: individual (AXP 1E
1547.0-5408, SGR J1550-5418, PSR J1550-5418)
ID X-RAY-DETECTOR; MAGNETIZED NEUTRON-STARS; SGR J1550-5418 BURSTS;
IN-ORBIT PERFORMANCE; 1998 AUGUST 27; GIANT FLARE; BOARD SUZAKU;
RADIATIVE MECHANISM; SGR-1806-20; SGR-1900+14
AB The 2.1-s anomalous X-ray pulsar 1E 1547.0-5408 exhibited an X-ray outburst on 2009 January 22, emitting a large number of short bursts. The wide-band all-sky monitor (WAM) on-board Suzaku detected at least 254 bursts in the 160 keV-6.2MeV band over the period of January 22 00: 57-17: 02 UT from the direction of 1E 1547.0-5408. One of these bursts, which occurred at 06: 45: 13, produced the brightest fluence in the 0.5-6.2 MeV range, with an averaged 0.16-6.2 MeV flux and extrapolated 25 keV-2 MeV fluence of about 1x10(-5) erg cm(-2) s(-1) and about 3x10(-4) erg cm(-2), respectively. After pile-up corrections, the time-resolved WAM spectra of this burst were well-fitted in the 0.16-6.2 MeV range by two-component models; specifically, a blackbody plus an optically thin thermal bremsstrahlung or a combination of a blackbody and a power-law component with an exponential cut-off. These results are compared with previous works reporting the persistent emission and weaker short bursts followed by the same outburst.
C1 [Yasuda, Tetsuya; Tashiro, Makoto S.; Terada, Yukikatsu; Kouzu, Tomomi] Saitama Univ, Grad Sch Sci & Engn, Saitama, Saitama 3388570, Japan.
[Iwakiri, Wataru B.; Enoto, Teruaki] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan.
[Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nakagawa, Yujin E.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Bamba, Aya] Aoyama Gakuin Univ, Dept Phys & Math, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan.
[Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
[Yamaoka, Kazutaka] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Yamaoka, Kazutaka] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Ohno, Masanori] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Shibata, Shinpei] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan.
[Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
RP Yasuda, T (reprint author), Saitama Univ, Grad Sch Sci & Engn, 255 Shimo Okubo, Saitama, Saitama 3388570, Japan.
EM yasuda@heal.phy.saitama-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU Ministry of Education, Culture, Sports, Science, and Technology (MEXT)
of Japan [24-10233, 23340055, 22340039]; MEXT [22684012]; JSPS
[24540309]
FX This work was supported in part by Grant-in-Aid for the Japan Society
for the Promotion of Science (JSPS) Fellows (No. 24-10233, T.Y.),
Grants-in-Aid for Scientific Research (B) from the Ministry of
Education, Culture, Sports, Science, and Technology (MEXT) of Japan (No.
23340055, Y.T.; No. 22340039, M.S.T.), a Grant-in-Aid for Young
Scientists (A) from MEXT (No. 22684012, A. B.), and JSPS KAKENHI (No.
24540309, Y.E.N.).
NR 51
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD JUN
PY 2015
VL 67
IS 3
AR 41
DI 10.1093/pasj/psv011
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK4GQ
UT WOS:000356182500012
ER
PT J
AU Perrone, JA
Liston, DB
AF Perrone, John A.
Liston, Dorion B.
TI Redundancy reduction explains the expansion of visual direction space
around the cardinal axes
SO VISION RESEARCH
LA English
DT Article
DE Oblique effect; Visual motion; Redundancy reduction; Surround
inhibition; MT; MSTd
ID PURSUIT EYE-MOVEMENTS; AREA MT; MACAQUE MONKEY; ORIENTATION SELECTIVITY;
RECEPTIVE-FIELD; MOTION SENSOR; MT/V5 NEURONS; SELF-MOTION; MST NEURONS;
OWL MONKEY
AB Motion direction discrimination in humans is worse for oblique directions than for the cardinal directions (the oblique effect). For some unknown reason, the human visual system makes systematic errors in the estimation of particular motion directions; a direction displacement near a cardinal axis appears larger than it really is whereas the same displacement near an oblique axis appears to be smaller. Although the perceptual effects are robust and are clearly measurable in smooth pursuit eye movements, all attempts to identify the neural underpinnings for the oblique effect have failed. Here we show that a model of image velocity estimation based on the known properties of neurons in primary visual cortex (V1) and the middle temporal (MT) visual area of the primate brain produces the oblique effect. We also provide an explanation for the unusual asymmetric patterns of inhibition that have been found surrounding MT neurons. These patterns are consistent with a mechanism within the visual system that prevents redundant velocity signals from being passed onto the next motion-integration stage, (dorsal Medial superior temporal, MSTd). We show that model redundancy-reduction mechanisms within the MT-MSTd pathway produce the oblique effect. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Perrone, John A.] Univ Waikato, Sch Psychol, Hamilton 3240, New Zealand.
[Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA.
[Liston, Dorion B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Perrone, JA (reprint author), Univ Waikato, Sch Psychol, Hamilton 3240, New Zealand.
EM jpnz@waikato.ac.nz
FU Marsden Fund Council; Office of Naval Research, USA
FX J.P. and D.L. supported by the Marsden Fund Council from Government
funding, administered by the Royal Society of New Zealand. DL supported
by Office of Naval Research, USA. There is no conflict of interest.
NR 53
TC 0
Z9 0
U1 2
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0042-6989
EI 1878-5646
J9 VISION RES
JI Vision Res.
PD JUN
PY 2015
VL 111
BP 31
EP 42
DI 10.1016/j.visres.2015.03.020
PN A
PG 12
WC Neurosciences; Ophthalmology
SC Neurosciences & Neurology; Ophthalmology
GA CK2FW
UT WOS:000356027200004
PM 25888929
ER
PT J
AU Cunnane, D
Kawamura, JH
Wolak, MA
Acharya, N
Tan, T
Xi, XX
Karasik, BS
AF Cunnane, D.
Kawamura, J. H.
Wolak, M. A.
Acharya, N.
Tan, T.
Xi, X. X.
Karasik, B. S.
TI Characterization of MgB2 Superconducting Hot Electron Bolometers
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article
DE Hot electron bolometers (HEBs); MgB2; superconducting devices; terahertz
mixers
ID THIN-FILMS; MIXERS
AB Hot-Electron Bolometer (HEB) mixers have proven to be the best tool for high-resolution spectroscopy at the Terahertz frequencies. However, the current state of the art NbN mixers suffer from a small intermediate frequency (IF) bandwidth as well as a low operating temperature. MgB2 is a promising material for HEB mixer technology in view of its high critical temperature and fast thermal relaxation allowing for a large IF bandwidth. In this work, we have fabricated and characterized thin-film (similar to 15 nm) MgB2-based spiral antenna-coupled HEB mixers on SiC substrate. We achieved the IF bandwidth greater than 8 GHz at 25 K and the device noise temperature < 4000 K at 9 K using a 600 GHz source. Using temperature dependencies of the radiation power dissipated in the device we have identified the optical loss in the integrated microantenna responsible as a cause of the limited sensitivity of the current mixer devices. From the analysis of the current-voltage (IV) characteristics, we have derived the effective thermal conductance of the mixer device and estimated the required local oscillator power in an optimized device to be similar to 1 mu W.
C1 [Cunnane, D.; Kawamura, J. H.; Karasik, B. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wolak, M. A.; Acharya, N.; Tan, T.; Xi, X. X.] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA.
RP Cunnane, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Daniel.P.Cunnane@jpl.nasa.gov
FU National Space and Aeronautics Administration; NASA Astrophysics
Research and Analysis Program through a contract from JPL; NASA
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Space and
Aeronautics Administration. The work at Temple University was supported
by the NASA Astrophysics Research and Analysis Program through a
contract from JPL. The work of D. Cunnane 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.
NR 20
TC 13
Z9 13
U1 4
U2 20
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1051-8223
EI 1558-2515
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2015
VL 25
IS 3
AR 2300206
DI 10.1109/TASC.2014.2369353
PG 6
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA CJ7IN
UT WOS:000355668500001
ER
PT J
AU McDermott, SP
Bransome, NC
Sutton, SE
Smith, BE
Link, JS
Miller, TJ
AF McDermott, S. P.
Bransome, N. C.
Sutton, S. E.
Smith, B. E.
Link, J. S.
Miller, T. J.
TI Quantifying alosine prey in the diets of marine piscivores in the Gulf
of Maine
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE alewife; demersal fish; Gulf of Maine; river herring; trophic
interaction
ID HUDSON RIVER ESTUARY; ATLANTIC COD; STRIPED BASS; POMATOMUS-SALTATRIX;
TROPHIC ECOLOGY; AGE-0 BLUEFISH; CHESAPEAKE-BAY; DELAWARE BAY;
SALMO-SALAR; FOOD WEBS
AB The objectives of this work were to quantify the spatial and temporal distribution of the occurrence of anadromous fishes (alewife Alosa pseudoharengus, blueback herring Alosa aestivalis and American shad Alosa sapidissima) in the stomachs of demersal fishes in coastal waters of the north-west Atlantic Ocean. Results show that anadromous fishes were detectable and quantifiable in the diets of common marine piscivores for every season sampled. Even though anadromous fishes were not the most abundant prey, they accounted for c. 5-10% of the diet by mass for several marine piscivores. Statistical comparisons of these data with fish diet data from a broad-scale survey of the north-west Atlantic Ocean indicate that the frequency of this trophic interaction was significantly higher within spatially and temporally focused sampling areas of this study than in the broad-scale survey. Odds ratios of anadromous predation were as much as 460 times higher in the targeted sampling as compared with the broad-scale sampling. Analyses indicate that anadromous prey consumption was more concentrated in the near-coastal waters compared with consumption of a similar, but more widely distributed species, the Atlantic herring Clupea harengus. In the context of ecosystem-based fisheries management, the results suggest that even low-frequency feeding events may be locally important, and should be incorporated into ecosystem models. (C) 2015 The Fisheries Society of the British Isles
C1 [McDermott, S. P.] Natl Marine Fisheries Serv, Greater Atlantic Reg Off, Gloucester, MA 01930 USA.
[Bransome, N. C.; Miller, T. J.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA.
[Sutton, S. E.; Smith, B. E.; Link, J. S.] NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Woods Hole, MA 02543 USA.
RP McDermott, SP (reprint author), Natl Marine Fisheries Serv, Greater Atlantic Reg Off, 55 Great Republ Dr, Gloucester, MA 01930 USA.
EM sean.mcdermott@noaa.gov
RI Miller, Thomas/C-2129-2008
OI Miller, Thomas/0000-0001-8427-1614
FU NOAA Fisheries Greater Atlantic Regional Fisheries Office Habitat
Conservation Programme; NOAA Cooperative Institute for North Atlantic
Research [CINAR NA09OAR4320129]; NSF-NOAA CAMEO project [OCE-0961-632]
FX This work was funded through an award from NOAA Fisheries Greater
Atlantic Regional Fisheries Office Habitat Conservation Programme and
via a student fellowship to N.B. from the NOAA Cooperative Institute for
North Atlantic Research (CINAR NA09OAR4320129). T.J.M. is supported in
part by an NSF-NOAA CAMEO project (OCE-0961-632). We thank the crew of
NOAA R.V. Gloria Michelle, staff from NEFSC who assisted with fieldwork,
Maine Department of Marine Resources staff and crew of F.V. Robert
Michael. Also, we thank the many scientists who have contributed to the
NEFSC food habits database, without whom, these analyses would not have
been possible. This is contribution 5000 from the University of Maryland
Center for Environmental Science.
NR 63
TC 2
Z9 2
U1 3
U2 13
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 JUN
PY 2015
VL 86
IS 6
BP 1811
EP 1829
DI 10.1111/jfb.12692
PG 19
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA CJ6UD
UT WOS:000355628700009
PM 25943427
ER
PT J
AU Muller, HSP
Brown, LR
Drouin, BJ
Pearson, JC
Kleiner, I
Sams, RL
Sung, K
Ordu, MH
Lewen, F
AF Mueller, Holger S. P.
Brown, Linda R.
Drouin, Brian J.
Pearson, John C.
Kleiner, Isabelle
Sams, Robert L.
Sung, Keeyoon
Ordu, Matthias H.
Lewen, Frank
TI Rotational spectroscopy as a tool to investigate interactions between
vibrational polyads in symmetric top molecules: Low-lying states v(8) <=
2 of methyl cyanide, CH3CN
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Rotational spectroscopy; Infrared spectroscopy; Vibration-rotation
interaction; Methyl cyanide; Interstellar molecule
ID SPECTRAL-LINE CATALOG; ETHYL CYANIDE; GROUND-STATE; INTERSTELLAR-MEDIUM;
HIGH-RESOLUTION; SAGITTARIUS B2(N); INFRARED-SPECTRUM; COLOGNE DATABASE;
EXCITED-STATES; WAVE SPECTRUM
AB Rotational and rovibrational spectra of methyl cyanide were recorded to analyze interactions in low-lying vibrational states and to construct line lists for radio astronomical observations as well as for infrared spectroscopic investigations of planetary atmospheres. The rotational spectra cover large portions of the 36-1627 GHz region. In the infrared (IR), a spectrum was recorded for this study in the region of 2v(8) around 717 cm(-1) with assignments covering 684-765 cm-1. Additional spectra in the vs region were used to validate the analysis.
Information on the K level structure of CH3CN is almost exclusively obtained from IR spectra, as are basics of the J level structure. The large amount and the high accuracy of the rotational data improves knowledge of the J level structure considerably. Moreover, since these data extend to much higher and K quantum numbers, they allowed us to investigate for the first time in depth local interactions between these states which occur at high K values. In particular, we have detected several interactions between v(8) = 1 and 2. Notably, there is a strong Delta v(8) = +/- 1, Delta K = 0, Delta l = +/- 3 Fermi resonance between v(8) = 1(-1) and v(8) = 2(+2) at K = 14. Pronounced effects in the spectrum are also caused by resonant Delta v(8) = +/- 1, Delta K = -/+ 2, Delta l = +/- 1 interactions between v(8) = 1 and 2 at K = 13, l = 1/K = 11, l = 0 and at K = 15, l = +1/K = 13, l = +2. An equivalent resonant interaction occurs between K = 14 of the ground vibrational state and K = 12, l = +1 of v(8) = 1 for which we present the first detailed account. A preliminary account was given in an earlier study on the ground vibrational state. Similar resonances were found for CH3CCH and, more recently, for CH3NC, warranting comparison of the results. From data pertaining to v(8) = 2, we also investigated rotational interactions with v(4) = 1 as well as Delta v(8) = +/- 1, Delta K = 0, Delta l = +/- 3 Fermi interactions between v(8) = 2 and 3.
We have derived N-2- and self-broadening coefficients for the v(8), 2v(8) - v(8), and 2v(8) bands from previously determined v(4) values. Subsequently, we determined transition moments and intensities for the three IR bands. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Mueller, Holger S. P.; Ordu, Matthias H.; Lewen, Frank] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Brown, Linda R.; Drouin, Brian J.; Pearson, John C.; Sung, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kleiner, Isabelle] Univ Paris Est Creteil & Paris Diderot, LISA, Inst Pierre Simon Laplace, CNRS,UMR 7583, F-94010 Creteil, France.
[Sams, Robert L.] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Muller, HSP (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
EM hspm@ph1.uni-koeln.de
RI Sung, Keeyoon/I-6533-2015;
OI Mueller, Holger/0000-0002-0183-8927
FU Bundesministerium fur Bildung und Forschung (BMBF) [FKZ 50OF0901];
Deutsche Forschungsgemeinschaft (DFG) [SFB 494, SFB 956]; Department of
Energy's Office of Biological and Environmental Research located at the
Pacific Northwest National Laboratory (PNNL); United States Department
of Energy [DE-AC05-76RLO1830]
FX H.S.P.M. is grateful to the Bundesministerium fur Bildung und Forschung
(BMBF) for financial support through project FKZ 50OF0901 (ICC HIFI
Herschel) during part of the present investigation. The measurements in
Koln were supported by the Deutsche Forschungsgemeinschaft (DFG) through
the collaborative research grants SFB 494 initially, and later SFB 956,
project area B3. The portion of this work, which was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, was
performed under contract with the National Aeronautics and Space
Administration. The infrared spectra analyzed in the present study were
recorded at the W.R. Wiley Environmental Molecular Sciences Laboratory,
a national scientific user facility sponsored by the Department of
Energy's Office of Biological and Environmental Research located at the
Pacific Northwest National Laboratory (PNNL). PNNL is operated for the
United States Department of Energy by the Battelle Memorial Institute
under Contract DE-AC05-76RLO1830.
NR 86
TC 7
Z9 7
U1 2
U2 13
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 JUN
PY 2015
VL 312
BP 22
EP 37
DI 10.1016/j.jms.2015.02.009
PG 16
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA CJ6XR
UT WOS:000355639000004
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-18-, and C-13-enriched CO2 in the v(3) region: High
accuracy frequency calibration and spectroscopic constants for
(OCO)-O-16-C-12-O-18, (OCO)-O-18-C-12-O-18, and (OCO)-O-16-C-13-O-16
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE O-18-enriched; C-13-enriched; CO2; FT-IR; Absolute wavenumber accuracy;
Remote sensing
ID SENSITIVITY CAVITY RING; ENRICHED CARBON-DIOXIDE; CONSTRAINED
MULTISPECTRUM ANALYSIS; 4.3 MU-M; INFRARED-SPECTROSCOPY; 7000 CM(-1);
LINE POSITIONS; MOLECULAR-CONSTANTS; ABSORPTION-BANDS; SPEED DEPENDENCE
AB In this report, we extend our Fourier transform infrared (FT-IR) spectroscopy measurements of CO2 in the v(3) region (2200-2450 cm(-1), 65-75 THz) to the O-18-, and C-13-substituted isotopologues, using the JPL Bruker IFS-125HR Fourier Transform Spectrometer (JPL-FTS). High quality (S/N similar to 2000) spectra were obtained separately for each of the 180-, and 13C-isotopically enriched samples. The absolute wavenumber accuracies were better than 3 x 10(-6) cm(-1) (similar to 100 kHz) for strong, isolated transitions, calibrated against the highest accuracy reported CO and (OCO)-O-16-C-12-O-16 (626) frequency measurements. The JPL-FTS performance and calibration procedure is shown to be reliable and consistent, achievable through vigorous maintenance of the optical alignment and regular monitoring of its instrumental line shape function. Effective spectroscopic constant fits of the 00011 <- 00001 fundamental bands for 18012080 (628), (OCO)-O-18-C-12-O-18 (828), and (OCO)-O-16-C-13-O-16 (636) were obtained with RMS residuals of 2.9 x 10(-6) cm(-1), 2.8 x 10(-6) cm(-1), and 2.9 x 10(-6) cm(-1), respectively. The observed bands encompassed 79 lines over the J(max) range of P67/R67, 47 lines over P70/R62, and 60 lines over P70/R70 for 628, 828, and 636, respectively. These results complement our recent work on the O-17-enriched isotopologues (Elliott et al., 2014), providing additional high-quality frequency measurements for atmospheric remote sensing applications. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Elliott, Ben M.; Sung, Keeyoon; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Miller, CE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM benm.elliott@epss.ucla.edu; keeyoon.sung@jpl.nasa.gov;
charles.e.miller@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology
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 2014 California Institute of Technology. Government
sponsorship acknowledged.
NR 37
TC 0
Z9 0
U1 1
U2 13
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 JUN
PY 2015
VL 312
BP 78
EP 86
DI 10.1016/j.jms.2015.02.007
PG 9
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA CJ6XR
UT WOS:000355639000011
ER
PT J
AU Kogut, A
Fixsen, DJ
Hill, RS
AF Kogut, Alan
Fixsen, Dale J.
Hill, Robert S.
TI Polarization properties of a broadband multi-moded concentrator
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND
VISION
LA English
DT Article
ID NONIMAGING CONCENTRATORS; FLUX
AB We present the design and performance of a non-imaging concentrator for use in broadband polarimetry at millimeter through submillimeter wavelengths. A rectangular geometry preserves the input polarization state as the concentrator couples f/2 incident optics to a 2 pi sr detector. Measurements of the co-polar and cross-polar beams in both the few-mode and highly over-moded limits agree with a simple model based on mode truncation. The measured co-polar beam pattern is nearly independent of frequency in both linear polarizations. The cross-polar beam pattern is dominated by a uniform term corresponding to polarization efficiency of 94%. After correcting for efficiency, the remaining cross-polar response is -18 dB.
C1 [Kogut, Alan; Fixsen, Dale J.; Hill, Robert S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Alan.J.Kogut@nasa.gov
NR 14
TC 3
Z9 3
U1 1
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1084-7529
EI 1520-8532
J9 J OPT SOC AM A
JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis.
PD JUN
PY 2015
VL 32
IS 6
BP 1040
EP 1045
DI 10.1364/JOSAA.32.001040
PG 6
WC Optics
SC Optics
GA CJ6VM
UT WOS:000355633300004
PM 26367036
ER
PT J
AU Massey, R
Williams, L
Smit, R
Swinbank, M
Kitching, TD
Harvey, D
Jauzac, M
Israel, H
Clowe, D
Edge, A
Hilton, M
Jullo, E
Leonard, A
Liesenborgs, J
Merten, J
Mohammed, I
Nagai, D
Richard, J
Robertson, A
Saha, P
Santana, R
Stott, J
Tittley, E
AF Massey, Richard
Williams, Liliya
Smit, Renske
Swinbank, Mark
Kitching, Thomas D.
Harvey, David
Jauzac, Mathilde
Israel, Holger
Clowe, Douglas
Edge, Alastair
Hilton, Matt
Jullo, Eric
Leonard, Adrienne
Liesenborgs, Jori
Merten, Julian
Mohammed, Irshad
Nagai, Daisuke
Richard, Johan
Robertson, Andrew
Saha, Prasenjit
Santana, Rebecca
Stott, John
Tittley, Eric
TI The behaviour of dark matter associated with four bright cluster
galaxies in the 10 kpc core of Abell 3827
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astroparticle physics; gravitational lensing: strong; galaxies:
clusters: individual: Abell 3827; dark matter
ID HUBBLE-SPACE-TELESCOPE; LENSING MASS RECONSTRUCTION; STELLAR POPULATION
SYNTHESIS; CHARGE-TRANSFER INEFFICIENCY; PIXEL-BASED CORRECTION;
LARGE-SCALE STRUCTURE; ADVANCED CAMERA; NONPARAMETRIC INVERSION; GENETIC
ALGORITHM; CROSS-SECTION
AB Galaxy cluster Abell 3827 hosts the stellar remnants of four almost equally bright elliptical galaxies within a core of radius 10 kpc. Such corrugation of the stellar distribution is very rare, and suggests recent formation by several simultaneous mergers. We map the distribution of associated dark matter, using new Hubble Space Telescope imaging and Very Large Telescope/Multi-Unit Spectroscopic Explorer integral field spectroscopy of a gravitationally lensed system threaded through the cluster core. We find that each of the central galaxies retains a dark matter halo, but that (at least) one of these is spatially offset from its stars. The best-constrained offset is 1.62(-0.49)(+0.47) kpc, where the 68 per cent confidence limit includes both statistical error and systematic biases in mass modelling. Such offsets are not seen in field galaxies, but are predicted during the long infall to a cluster, if dark matter self-interactions generate an extra drag force. With such a small physical separation, it is difficult to definitively rule out astrophysical effects operating exclusively in dense cluster core environments - but if interpreted solely as evidence for self-interacting dark matter, this offset implies a cross-section sigma(DM)/(m) similar to (1.7 +/- 0.7) x 10(-4) cm(2) g(-1) x (t(infall)/10(9) yr)(-2), where t(infall) is the infall duration.
C1 [Massey, Richard; Jauzac, Mathilde; Israel, Holger] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Massey, Richard; Smit, Renske; Swinbank, Mark; Edge, Alastair; Leonard, Adrienne; Robertson, Andrew; Stott, John] Univ Durham, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Williams, Liliya] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Kitching, Thomas D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Harvey, David] Ecole Polytech Fed Lausanne, Observ Sauverny, CH-1290 Versoix, Switzerland.
[Jauzac, Mathilde; Hilton, Matt] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Clowe, Douglas; Santana, Rebecca] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Jullo, Eric] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Leonard, Adrienne] UCL, London WC1E 6BT, England.
[Liesenborgs, Jori] Univ Hasselt, Expertisectr Digitale Media, B-3590 Diepenbeek, Belgium.
[Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Merten, Julian] CALTECH, Pasadena, CA 91125 USA.
[Mohammed, Irshad; Saha, Prasenjit] Univ Zurich, Inst Phys, CH-8057 Zurich, Switzerland.
[Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Richard, Johan] Univ Lyon 1, Observ Lyon, F-69561 St Genis Laval, France.
[Tittley, Eric] Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
RP Massey, R (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England.
EM r.j.massey@durham.ac.uk
OI Mohammed, Irshad/0000-0003-0784-5447; Robertson,
Andrew/0000-0002-0086-0524; Leonard, Adrienne/0000-0002-5976-0405; Edge,
Alastair/0000-0002-3398-6916; Stott, John/0000-0002-1679-9983
FU Royal Society University Research Fellowships; Science and Technology
Facilities Council [ST/L00075X/1, ST/H005234/1, ST/I001573/1];
Leverhulme Trust [PLP-2011-003]; NASA; NASA [NAS 5-26555]; ESO
Telescopes at the La Silla Paranal Observatory [093.A-0237, 294.A-5014];
BIS National E-infrastructure capital grant [ST/K00042X/1]; STFC capital
grant [ST/H008519/1]; STFC DiRAC Operations grant [ST/K003267/1]; Durham
University
FX The authors are pleased to thank Jay Anderson for advice with CTI
correction for HST/WFC3, Jean-Paul Kneib for advice using LENSTOOL, and
the anonymous referee whose suggestions improved the manuscript. RM and
TDK are supported by Royal Society University Research Fellowships. This
work was supported by the Science and Technology Facilities Council
(grant numbers ST/L00075X/1, ST/H005234/1 and ST/I001573/1) and the
Leverhulme Trust (grant number PLP-2011-003). This research was carried
out in part at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.; Facilities: This paper uses
data from observations GO-12817 (PI: R. Massey) with the NASA/ESA Hubble
Space Telescope, obtained at the Space Telescope Science Institute,
which is operated by AURA Inc, under NASA contract NAS 5-26555. This
paper also uses data from observations made with ESO Telescopes at the
La Silla Paranal Observatory under programmes 093.A-0237 and 294.A-5014
(PI: R. Massey). We thank the Director General for granting
discretionary time, and Paranal Science Operations for running the
observations. The LENSTOOL analysis used the DiRAC Data Centric system
at Durham University, operated by the Institute for Computational
Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk).
This equipment was funded by BIS National E-infrastructure capital grant
ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations
grant ST/K003267/1 and Durham University. DiRAC is part of the National
e-Infrastructure. LLRW would like to acknowledge the Minnesota
Supercomputing Institute, without whose computational support GRALE work
would not have been possible.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
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BP 3393
EP 3406
DI 10.1093/mnras/stv467
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000005
ER
PT J
AU Davis, TA
Rowlands, K
Allison, JR
Shabala, SS
Ting, YS
Lagos, CDP
Kaviraj, S
Bourne, N
Dunne, L
Eales, S
Ivison, RJ
Maddox, S
Smith, DJB
Smith, MWL
Temi, P
AF Davis, Timothy A.
Rowlands, Kate
Allison, James R.
Shabala, Stanislav S.
Ting, Yuan-Sen
Lagos, Claudia del P.
Kaviraj, Sugata
Bourne, Nathan
Dunne, Loretta
Eales, Steve
Ivison, Rob. J.
Maddox, Steve
Smith, Daniel J. B.
Smith, Matthew W. L.
Temi, Pasquale
TI Molecular and atomic gas in dust lane early-type galaxies - I. Low star
formation efficiencies in minor merger remnants
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: molecules; galaxies: elliptical and lenticular, cD; galaxies:
evolution; galaxies: interactions; galaxies: ISM
ID CO-TO-H-2 CONVERSION FACTOR; SCIENCE DEMONSTRATION PHASE;
MASS-METALLICITY RELATION; DIGITAL-SKY-SURVEY; ATLAS(3D) PROJECT;
HERSCHEL-ATLAS; FORMING GALAXIES; ELLIPTIC GALAXIES; SAURON PROJECT;
COLD GAS
AB In this work we present IRAM 30-m telescope observations of a sample of bulge-dominated galaxies with large dust lanes, which have had a recent minor merger. We find these galaxies are very gas rich, with H-2 masses between 4 x 10(8) and 2 x 10(10) M-circle dot. We use these molecular gas masses, combined with atomic gas masses from an accompanying paper, to calculate gas-to-dust and gas-to-stellar-mass ratios. The gas-to-dust ratios of our sample objects vary widely (between approximate to 50 and 750), suggesting many objects have low gas-phase metallicities, and thus that the gas has been accreted through a recent merger with a lower mass companion. We calculate the implied minor companion masses and gas fractions, finding a median predicted stellar mass ratio of approximate to 40:1. The minor companion likely had masses between approximate to 10(7) and 10(10) M-circle dot. The implied merger mass ratios are consistent with the expectation for low-redshift gas-rich mergers from simulations. We then go on to present evidence that (no matter which star formation rate indicator is used) our sample objects have very low star formation efficiencies (star formation rate per unit gas mass), lower even than the early-type galaxies from ATLAS(3D) which already show a suppression. This suggests that minor mergers can actually suppress star formation activity. We discuss mechanisms that could cause such a suppression, include dynamical effects induced by the minor merger.
C1 [Davis, Timothy A.; Lagos, Claudia del P.; Ivison, Rob. J.] European So Observ, D-85748 Garching, Germany.
[Davis, Timothy A.; Kaviraj, Sugata; Smith, Daniel J. B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL1 9AB, Herts, England.
[Rowlands, Kate] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Allison, James R.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Shabala, Stanislav S.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Ting, Yuan-Sen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lagos, Claudia del P.] Univ Western Australia, Int Ctr Radio Astron ICRAR, Crawley, WA 6009, Australia.
[Bourne, Nathan; Dunne, Loretta] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dunne, Loretta; Maddox, Steve] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Eales, Steve; Smith, Matthew W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
RP Davis, TA (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM t.davis4@herts.ac.uk
RI Ivison, R./G-4450-2011;
OI Ivison, R./0000-0001-5118-1313; Smith, Daniel/0000-0001-9708-253X;
Lagos, Claudia/0000-0003-3021-8564; Davis, Timothy/0000-0003-4932-9379;
Maddox, Stephen/0000-0001-5549-195X; Ting, Yuan-Sen/0000-0001-5082-9536
FU Science and Technology Facilities Council Ernest Rutherford Fellowship;
European Research Council Starting Grant SEDmorph; Australian Research
Council [DE130101399]; European Research Council Advanced grant
COSMICISM; European Community [229517, 283393]; INSU/CNRS (France); MPG
(Germany); IGN (Spain); STFC (UK); ARC (Australia); AAO; National
Aeronautics and Space Administration
FX TAD acknowledges support from a Science and Technology Facilities
Council Ernest Rutherford Fellowship, and thanks Maarten Baes,
Gianfranco De Zotti, Ivan Oteo Gomez, Michal Michalowski and Catherine
Vlahakis for comments which improved the paper. KR acknowledges support
from the European Research Council Starting Grant SEDmorph (PI: V.
Wild). SSS thanks the Australian Research Council for an Early Career
Fellowship (DE130101399). LD, RJI and SM acknowledge support from the
European Research Council Advanced grant COSMICISM. The research leading
to these results has received funding from the European Community's
Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No.
229517 and No. 283393 (RadioNet3). This paper is based on observations
carried out with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS
(France), MPG (Germany) and IGN (Spain).; The H-ATLAS is a project with
Herschel, which is an ESA space observatory with science instruments
provided by European-led Principal Investigator consortia and with
important participation from NASA. The H-ATLAS website is
http://www.h-atlas.org/. The GAMA input catalogue is based on data taken
from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky
Survey. Complementary imaging of the GAMA regions is being obtained by a
number of independent survey programs including GALEX MIS, VST KIDS,
VISTA VIKING, WISE, H-ATLAS, GMRT and ASKAP providing UV to radio
coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO
and the participating institutions. The GAMA website is
http://www.gama-survey.org/. 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 research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration.
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JI Mon. Not. Roy. Astron. Soc.
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DI 10.1093/mnras/stv597
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SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000014
ER
PT J
AU Marocco, F
Jones, HRA
Day-Jones, AC
Pinfield, DJ
Lucas, PW
Burningham, B
Zhang, ZH
Smart, RL
Gomes, JI
Smith, L
AF Marocco, F.
Jones, H. R. A.
Day-Jones, A. C.
Pinfield, D. J.
Lucas, P. W.
Burningham, B.
Zhang, Z. H.
Smart, R. L.
Gomes, J. I.
Smith, L.
TI A large spectroscopic sample of L and T dwarfs from UKIDSS LAS: peculiar
objects, binaries, and space density
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: spectroscopic; brown dwarfs; stars: low-mass; stars:
luminosity function, mass function
ID LOW-MASS STARS; DIGITAL SKY SURVEY; VERY-LOW MASS; YOUNG KINEMATIC
GROUPS; PROPER MOTION SURVEY; LARGE-AREA SURVEY; BROWN DWARF; ULTRACOOL
DWARFS; LUMINOSITY-FUNCTION; L/T TRANSITION
AB We present the spectroscopic analysis of a large sample of late-M, L, and T dwarfs from the United Kingdom Deep Infrared Sky Survey. Using the YJHK photometry from the Large Area Survey and the red-optical photometry from the Sloan Digital Sky Survey we selected a sample of 262 brown dwarf candidates and we have followed-up 196 of them using the echelle spectrograph X-shooter on the Very Large Telescope. The large wavelength coverage (0.30-2.48 mu m) and moderate resolution (R similar to 5000-9000) of X-shooter allowed us to identify peculiar objects including 22 blue L dwarfs, 2 blue T dwarfs, and 2 low-gravity M dwarfs. Using a spectral indices-based technique, we identified 27 unresolved binary candidates, for which we have determined the spectral type of the potential components via spectral deconvolution. The spectra allowed us to measure the equivalent width of the prominent absorption features and to compare them to atmospheric models. Cross-correlating the spectra with a radial velocity standard, we measured the radial velocity of our targets, and we determined the distribution of the sample, which is centred at -1.7 +/- 1.2 km s(-1) with a dispersion of 31.5 km s(-1). Using our results, we estimated the space density of field brown dwarfs and compared it with the results of numerical simulations. Depending on the binary fraction, we found that there are (0.85 +/- 0.55) x 10(-3) to (1.00 +/- 0.64) x 10(-3) objects per cubic parsec in the L4-L6.5 range, (0.73 +/- 0.47) x 10(-3) to (0.85 +/- 0.55) x 10(-3) objects per cubic parsec in the L7-T0.5 range, and (0.74 +/- 0.48) x 10(-3) to (0.88 +/- 0.56) x 10(-3) objects per cubic parsec in the T1-T4.5 range. We notice that there seems to be an excess of objects in the L-T transition with respect to the late-T dwarfs, a discrepancy that could be explained assuming a higher binary fraction than expected for the L-T transition, or that objects in the high-mass end and low-mass end of this regime form in different environments, i.e. following different initial mass functions.
C1 [Marocco, F.; Jones, H. R. A.; Day-Jones, A. C.; Pinfield, D. J.; Lucas, P. W.; Burningham, B.; Zhang, Z. H.; Gomes, J. I.; Smith, L.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Burningham, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zhang, Z. H.] IAC, E-38200 Tenerife, Spain.
[Smart, R. L.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy.
RP Marocco, F (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM f.marocco@herts.ac.uk
OI Marocco, Federico/0000-0001-7519-1700; Burningham,
Ben/0000-0003-4600-5627; Smart, Richard/0000-0002-4424-4766
FU European Organisation for Astronomical Research in the Southern
Hemisphere, Chile [086.C-0450, 087.C-0639, 088.C-0048, 091.C-0452];
Marie Curie 7th European Community Framework Programme [247593];
European Science Foundation (ESF) [4641]
FX This research is based on observations collected at the European
Organisation for Astronomical Research in the Southern Hemisphere, Chile
programs 086.C-0450, 087.C-0639, 088.C-0048, and 091.C-0452.; The
authors would like to acknowledge the Marie Curie 7th European Community
Framework Programme grant no. 247593 Interpretation and Parametrization
of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff
Exchange Scheme. FM would like to acknowledge the support received from
the European Science Foundation (ESF) within the framework of the ESF
activity entitled 'Gaia Research for European Astronomy Training',
Exchange Grant number 4641.
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SN 0035-8711
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
IS 4
BP 3651
EP 3692
DI 10.1093/mnras/stv530
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000030
ER
PT J
AU Madura, TI
Clementel, N
Gull, TR
Kruip, CJH
Paardekooper, JP
AF Madura, T. I.
Clementel, N.
Gull, T. R.
Kruip, C. J. H.
Paardekooper, J. -P.
TI 3D printing meets computational astrophysics: deciphering the structure
of eta Carinae's inner colliding winds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; binaries: close; stars: individual: Eta Carinae; stars:
mass-loss; stars: winds, outflows
ID SMOOTHED PARTICLE HYDRODYNAMICS; RADIATIVE-TRANSFER; MASSIVE STARS;
BINARY; SIMULATIONS; SPH; INSTABILITIES; COMPANION; EMISSION; MODELS
AB We present the first 3D prints of output from a supercomputer simulation of a complex astrophysical system, the colliding stellar winds in the massive (greater than or similar to 120 M-circle dot), highly eccentric (e similar to 0.9) binary star system eta Carinae. We demonstrate the methodology used to incorporate 3D interactive figures into a PDF (Portable Document Format) journal publication and the benefits of using 3D visualization and 3D printing as tools to analyse data from multidimensional numerical simulations. Using a consumer-grade 3D printer (MakerBot Replicator 2X), we successfully printed 3D smoothed particle hydrodynamics simulations of eta Carinae's inner (r similar to 110 au) wind-wind collision interface at multiple orbital phases. The 3D prints and visualizations reveal important, previously unknown 'finger-like' structures at orbital phases shortly after periastron (phi similar to 1.045) that protrude radially outwards from the spiral wind-wind collision region. We speculate that these fingers are related to instabilities (e.g. thin-shell, Rayleigh-Taylor) that arise at the interface between the radiatively cooled layer of dense post-shock primary-star wind and the fast (3000 km s(-1)), adiabatic post-shock companion-star wind. The success of our work and easy identification of previously unrecognized physical features highlight the important role 3D printing and interactive graphics can play in the visualization and understanding of complex 3D time-dependent numerical simulations of astrophysical phenomena.
C1 [Madura, T. I.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Clementel, N.; Kruip, C. J. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Paardekooper, J. -P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Paardekooper, J. -P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Madura, TI (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA.
EM thomas.i.madura@nasa.gov
FU NASA
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. We thank Frederic Vogt for
very useful discussions on the incorporation of 3D interactive graphics
into PDFs and 3D printing. We thank an anonymous referee for helpful
comments.
NR 49
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
IS 4
BP 3780
EP 3794
DI 10.1093/mnras/stv422
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000038
ER
PT J
AU Kirk, B
Hilton, M
Cress, C
Crawford, SM
Hughes, JP
Battaglia, N
Bond, JR
Burke, C
Gralla, MB
Hajian, A
Hasselfield, M
Hincks, AD
Infante, L
Kosowsky, A
Marriage, TA
Menanteau, F
Moodley, K
Niemack, MD
Sievers, JL
Sifon, C
Wilson, S
Wollack, EJ
Zunckel, C
AF Kirk, Brian
Hilton, Matt
Cress, Catherine
Crawford, Steven M.
Hughes, John P.
Battaglia, Nicholas
Bond, J. Richard
Burke, Claire
Gralla, Megan B.
Hajian, Amir
Hasselfield, Matthew
Hincks, Adam D.
Infante, Leopoldo
Kosowsky, Arthur
Marriage, Tobias A.
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Sievers, Jonathan L.
Sifon, Cristobal
Wilson, Susan
Wollack, Edward J.
Zunckel, Caroline
TI SALT spectroscopic observations of galaxy clusters detected by ACT and a
type II quasar hosted by a brightest cluster galaxy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual: ACT-CL
J0320.4+0032; quasars: general; cosmology: observations
ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; BLACK-HOLES; DATA RELEASE;
COSMOLOGICAL CONSTRAINTS; VELOCITY DISPERSION; PHYSICAL-PROPERTIES;
SCALING RELATIONS; GALACTIC NUCLEI; REDSHIFT SURVEY
AB We present Southern African Large Telescope follow-up observations of seven massive clusters detected by the Atacama Cosmology Telescope (ACT) on the celestial equator using the Sunyaev-Zel'dovich (SZ) effect. We conducted multi-object spectroscopic observations with the Robert Stobie Spectrograph in order to measure galaxy redshifts in each cluster field, determine the cluster line-of-sight velocity dispersions, and infer the cluster dynamical masses. We find that the clusters, which span the redshift range 0.3 < z < 0.55, range in mass from (5-20) x 10(14) M-circle dot (M-200c). Their masses, given their SZ signals, are similar to those of Southern hemisphere ACT clusters previously observed using Gemini and the VLT. We note that the brightest cluster galaxy in one of the systems studied, ACT-CL J0320.4+0032 at z = 0.38, hosts a type II quasar. Only a handful of such systems are currently known, and therefore ACT-CL J0320.4+0032 may be a rare example of a very massive halo in which quasar-mode feedback is actively taking place.
C1 [Kirk, Brian; Hilton, Matt; Burke, Claire; Moodley, Kavilan; Wilson, Susan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Kirk, Brian; Cress, Catherine] Ctr High Performance Comp, ZA-7700 Cape Town, South Africa.
[Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Cress, Catherine] Univ Western Cape, Dept Phys, ZA-7530 Cape Town, South Africa.
[Crawford, Steven M.] South African Astron Observ, ZA-7935 Cape Town, South Africa.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Battaglia, Nicholas] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Bond, J. Richard; Hajian, Amir] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hasselfield, Matthew] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Sievers, Jonathan L.; Zunckel, Caroline] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kirk, B (reprint author), Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
EM bmarshallk@gmail.com; hiltonm@ukzn.ac.za
RI Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Sievers,
Jonathan/0000-0001-6903-5074; Menanteau, Felipe/0000-0002-1372-2534;
Sifon, Cristobal/0000-0002-8149-1352
FU Rutgers University; National Research Foundation; University of
KwaZulu-Natal; US National Science Foundation [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379, AST-0955810, AST-1312380]; Princeton
University; University of Pennsylvania; Canada Foundation for Innovation
(CFI); Comision Nacional de Investigacion Cientifica y Tecnologica
(CONICYT); CFI under the Compute Canada; Government of Ontario; Ontario
Research Fund - Research Excellence; University of Toronto; Alfred P.
Sloan Foundation; National Science Foundation; US Department of Energy
Office of Science
FX We thank the anonymous referee for a number of suggestions that improved
the quality of this paper. We thank Alastair Edge for useful discussions
about known BCG quasar hosts. This work is based in large part on
observations obtained with the SALT. Funding for SALT is provided in
part by Rutgers University, a founding member of the SALT consortium.
BK, MHi and KM acknowledge financial support from the National Research
Foundation and the University of KwaZulu-Natal. This work was supported
by the US National Science Foundation through awards AST-0408698 and
AST-0965625 for the ACT project, as well as awards PHY-0855887 and
PHY-1214379, along with awards AST-0955810 to AJB and AST-1312380 to AK.
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 (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. Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the US Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration (see the SDSS-III web site for details).
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
IS 4
BP 4010
EP 4026
DI 10.1093/mnras/stv595
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000051
ER
PT J
AU Holwerda, BW
Baldry, IK
Alpaslan, M
Bauer, A
Bland-Hawthorn, J
Brough, S
Brown, MJI
Cluver, ME
Conselice, C
Driver, SP
Hopkins, AM
Jones, DH
Lopez-Sanchez, AR
Loveday, J
Meyer, MJ
Moffett, A
AF Holwerda, B. W.
Baldry, I. K.
Alpaslan, M.
Bauer, A.
Bland-Hawthorn, J.
Brough, S.
Brown, M. J. I.
Cluver, M. E.
Conselice, C.
Driver, S. P.
Hopkins, A. M.
Jones, D. H.
Lopez-Sanchez, A. R.
Loveday, J.
Meyer, M. J.
Moffett, A.
TI Galaxy And Mass Assembly (GAMA) blended spectra catalogue: strong
galaxy-galaxy lens and occulting galaxy pair candidates
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; catalogues; dust, extinction; galaxies:
distances and redshifts; galaxies: statistics
ID DIGITAL-SKY-SURVEY; SPECTROSCOPICALLY SELECTED SAMPLE; BACKLIT SPIRAL
GALAXIES; SYNTHETIC FIELD METHOD; DUST ENERGY-BALANCE; ACS SURVEY;
SEEING GALAXIES; NGC 891; OVERLAPPING GALAXIES; INTERNAL STRUCTURE
AB We present the catalogue of blended galaxy spectra from the Galaxy And Mass Assembly (GAMA) survey. These are cases where light from two galaxies are significantly detected in a single GAMA fibre. Galaxy pairs identified from their blended spectrum fall into two principal classes: they are either strong lenses, a passive galaxy lensing an emission-line galaxy; or occulting galaxies, serendipitous overlaps of two galaxies, of any type. Blended spectra can thus be used to reliably identify strong lenses for follow-up observations (high-resolution imaging) and occulting pairs, especially those that are a late-type partly obscuring an early-type galaxy which are of interest for the study of dust content of spiral and irregular galaxies. The GAMA survey setup and its AUTOZ automated redshift determination were used to identify candidate blended galaxy spectra from the cross-correlation peaks. We identify 280 blended spectra with a minimum velocity separation of 600 km s(-1), of which 104 are lens pair candidates, 71 emission-line-passive pairs, 78 are pairs of emission-line galaxies and 27 are pairs of galaxies with passive spectra. We have visually inspected the candidates in the Sloan Digital Sky Survey (SDSS) and Kilo Degree Survey (KiDS) images. Many blended objects are ellipticals with blue fuzz (Ef in our classification). These latter 'Ef' classifications are candidates for possible strong lenses, massive ellipticals with an emission-line galaxy in one or more lensed images. The GAMA lens and occulting galaxy candidate samples are similar in size to those identified in the entire SDSS. This blended spectrum sample stands as a testament of the power of this highly complete, second-largest spectroscopic survey in existence and offers the possibility to expand e.g. strong gravitational lens surveys.
C1 [Holwerda, B. W.] Leiden Univ, Sterrenwacht Leiden, NL-2333 CA Leiden, Netherlands.
[Baldry, I. K.] Liverpool John Moores Univ, Astrophys Res Inst, IC2, Liverpool L3 5RF, Merseyside, England.
[Alpaslan, M.] NASA, Ames Res Ctr, Mountain View, CA 94034 USA.
[Bauer, A.; Brough, S.; Hopkins, A. M.; Lopez-Sanchez, A. R.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Bland-Hawthorn, J.] Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Cluver, M. E.] Univ Western Cape, Dept Phys, ZA-7530 Bellville, South Africa.
[Conselice, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Driver, S. P.; Meyer, M. J.; Moffett, A.] Univ Western Australia, ICRAR M468, Crawley, WA 6009, Australia.
[Driver, S. P.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Lopez-Sanchez, A. R.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Loveday, J.] Univ Sussex, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
RP Holwerda, BW (reprint author), Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
EM benne.holwerda@gmail.com
RI Driver, Simon/H-9115-2014; Brown, Michael/B-1181-2015;
OI Driver, Simon/0000-0001-9491-7327; Brown, Michael/0000-0002-1207-9137;
Alpaslan, Mehmet/0000-0003-0321-1033; Baldry, Ivan/0000-0003-0719-9385
FU European Space Agency; STFC (UK); ARC (Australia); AAO; Australian
Research Council [FT100100280]; National Aeronautics and Space
Administration
FX The authors thank the referee for his or her comments and suggestions.
The lead author thanks the European Space Agency for the support of the
Research Fellowship programme and the whole GAMA team for a magnificent
observational effort. GAMA is a joint European-Australasian project
based around a spectroscopic campaign using the Anglo-Australian
Telescope. The GAMA input catalogue is based on data taken from the SDSS
and the United Kingdom Infrared Telescope Infrared Deep Sky Survey.
Complementary imaging of the GAMA regions is being obtained by a number
of independent survey programmes including GALEX MIS, VST KiDS, VISTA
VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio
coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO,
and the participating institutions. The GAMA website is
www.gamasurvey.org/. MJIB acknowledges financial support from the
Australian Research Council (FT100100280) This research has made use of
the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research has made use of NASA's Astrophysics Data System.
NR 71
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JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
IS 4
BP 4277
EP 4287
DI 10.1093/mnras/stv589
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000069
ER
PT J
AU Wang, LY
Viero, M
Ross, NP
Asboth, V
Bethermin, M
Bock, J
Clements, D
Conley, A
Cooray, A
Farrah, D
Hajian, A
Han, JX
Lagache, G
Marsden, G
Myers, A
Norberg, P
Oliver, S
Page, M
Symeonidis, M
Schulz, B
Wang, WT
Zemcov, M
AF Wang, Lingyu
Viero, Marco
Ross, Nicholas P.
Asboth, Viktoria
Bethermin, Matthieu
Bock, Jamie
Clements, Dave
Conley, Alex
Cooray, Asantha
Farrah, Duncan
Hajian, Amir
Han, Jiaxin
Lagache, Guilaine
Marsden, Gaelen
Myers, Adam
Norberg, Peder
Oliver, Seb
Page, Mat
Symeonidis, Myrto
Schulz, Bernhard
Wang, Wenting
Zemcov, Mike
TI Co-evolution of black hole growth and star formation from a
cross-correlation analysis between quasars and the cosmic infrared
background
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: haloes; galaxies: high-redshift; quasars:
general; submillimetre: galaxies
ID DIGITAL-SKY-SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; ACTIVE GALACTIC
NUCLEI; BARYON ACOUSTIC-OSCILLATIONS; HERSCHEL-SPIRE INSTRUMENT; 7TH
DATA RELEASE; 9TH DATA RELEASE; 100 MU-M; SDSS-III; LUMINOSITY FUNCTION
AB We present the first cross-correlation measurement between Sloan Digital Sky Survey type 1 quasars and the cosmic infrared background (CIB) measured by Herschel. The quasars cover the redshift range 0.15 < z < 3.5 where most of the CIB originates. We detect the sub-millimetre emission of the quasars, which dominates on small scales, and correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. The mean flux of the Data Release 7 (DR7) quasars (median redshift < z > = 1.4) is 11.1, 7.1 and 3.6 mJy at 250, 350 and 500 mu m, respectively, while the mean flux of the DR9 quasars (< z > = 2.5) is 5.7, 5.0 and 1.8 mJy at 250, 350 and 500 mu m, respectively. Assuming a modified blackbody spectral energy distribution with a power law in the mid-infrared, we infer that the mean infrared luminosity of the DR7 and DR9 quasars is 10(12.4) and 10(12.8) L-circle dot, respectively. The correlated emission arises from DSFGs in the same halo as the quasar (the one-halo term) and DSFGs in separate haloes correlated with the quasar-hosting halo (the two-halo term). Using a simple halo model, we find that most quasars are hosted by central galaxies. The host halo mass scale of the DR7 central and satellite quasars is 10(12.4 +/- 0.9) and 10(13.6 +/- 0.4) M-circle dot, respectively. The host halo mass scale of the DR9 central and satellite quasars is 10(12.3 +/- 0.6) and 10(12.8 +/- 0.4) M-circle dot, respectively. Thus, the halo environment of the central quasars is similar to that of the most actively star-forming galaxies, which supports the view that dusty starburst and quasar activity are evolutionarily linked.
C1 [Wang, Lingyu; Han, Jiaxin; Norberg, Peder; Wang, Wenting] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Viero, Marco; Bock, Jamie; Zemcov, Mike] CALTECH, Pasadena, CA 91125 USA.
[Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Asboth, Viktoria; Marsden, Gaelen] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Bethermin, Matthieu] European So Observ, D-85748 Garching, Germany.
[Bock, Jamie; Schulz, Bernhard; Zemcov, Mike] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clements, Dave] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England.
[Conley, Alex] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Farrah, Duncan] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Hajian, Amir] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Lagache, Guilaine] Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lagache, Guilaine] Univ Paris 11, Paris, France.
[Lagache, Guilaine] CNRS, UMR 8617, F-75700 Paris, France.
[Myers, Adam] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Oliver, Seb; Symeonidis, Myrto] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Page, Mat] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Schulz, Bernhard] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Wang, LY (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
EM lingyu.wang25@gmail.com
OI Bethermin, Matthieu/0000-0002-3915-2015
FU 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); Alfred P. Sloan Foundation; National Science
Foundation; US Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; US Department of Energy Office of Science;
University of Arizona; Brazilian Participation Group; Brookhaven
National Laboratory; Carnegie Mellon University; University of Florida;
French Participation Group; German Participation Group; Harvard
University; Instituto de Astrofisica de Canarias; Michigan State/Notre
Dame/JINA Participation Group; Lawrence Berkeley National Laboratory;
Max Planck Institute for Astrophysics; Max Planck Institute for
Extraterrestrial Physics; New York University; Pennsylvania State
University; Spanish Participation Group; University of Tokyo; University
of Utah; Vanderbilt University; University of Virginia; Yale University
FX LW and PN acknowledge support from an ERC StG grant (DEGAS-259586).;
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).; Funding for the SDSS
and SDSS-II has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the US
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. The SDSS website is
http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research
Consortium for the Participating Institutions. The Participating
Institutions are the American Museum of Natural History, Astrophysical
Institute Potsdam, University of Basel, University of Cambridge, Case
Western Reserve University, University of Chicago, Drexel University,
Fermilab, the Institute for Advanced Study, the Japan Participation
Group, Johns Hopkins University, the Joint Institute for Nuclear
Astrophysics, the Kavli Institute for Particle Astrophysics and
Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences
(LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New
Mexico State University, Ohio State University, University of
Pittsburgh, University of Portsmouth, Princeton University, the United
States Naval Observatory and the University of Washington.; Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation and the US
Department of Energy Office of Science. The SDSS-III website is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, Carnegie Mellon
University, University of Florida, the French Participation Group, the
German Participation Group, Harvard University, the Instituto de
Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington and Yale
University.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2015
VL 449
IS 4
BP 4476
EP 4493
DI 10.1093/mnras/stv559
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2VE
UT WOS:000355342000082
ER
PT J
AU Mamajanov, I
Callahan, MP
Dworkin, JP
Cody, GD
AF Mamajanov, Irena
Callahan, Michael P.
Dworkin, Jason P.
Cody, George D.
TI Prebiotic Alternatives to Proteins: Structure and Function of
Hyperbranched Polyesters
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Article; Proceedings Paper
CT Conference on Origins of Life and Evolution of Biospheres (OLEB)
CY JUL 06-11, 2014
CL Nara, JAPAN
DE Hyperbranched polymer; Polyester; Smart material; Protein; Size
exclusion chromatography
ID MOLECULAR-SIZE DISTRIBUTION; CITRIC-ACID; 3-DIMENSIONAL POLYMERS;
AQUEOUS-SOLUTION; DRUG-DELIVERY; AMINO-ACIDS; CARBONACEOUS METEORITES;
THERMAL SYNTHESIS; PEPTIDE FORMATION; FORMOSE REACTION
AB Proteins are responsible multiple biological functions, such as ligand binding, catalysis, and ion channeling. This functionality is enabled by proteins' three-dimensional structures that require long polypeptides. Since plausibly prebiotic synthesis of functional polypeptides has proven challenging in the laboratory, we propose that these functions may have been initially performed by alternative macromolecular constructs, namely hyperbranched polymers (HBPs), during early stages of chemical evolution. HBPs can be straightforwardly synthesized in one-pot processes, possess globular structures determined by their architecture as opposed to folding in proteins, and have documented ligand binding and catalytic properties. Our initial study focuses on glycerol-citric acid HBPs synthesized via moderate heating in the dry state. The polymerization products consisted of a mixture of isomeric structures of varying molar mass as evidenced by NMR, mass spectrometry and size-exclusion chromatography. Addition of divalent cations during polymerization resulted in increased incorporation of citric acid into the HBPs and the possible formation of cation-oligomer complexes. The chelating properties of citric acid govern the makeup of the resulting polymer, turning the polymerization system into a rudimentary smart material.
C1 [Mamajanov, Irena; Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Callahan, Michael P.; Dworkin, Jason P.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mamajanov, I (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
EM imamajanov@ciw.edu
RI Dworkin, Jason/C-9417-2012
OI Dworkin, Jason/0000-0002-3961-8997
NR 61
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U2 22
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
EI 1573-0875
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD JUN
PY 2015
VL 45
IS 1-2
SI SI
BP 123
EP 137
DI 10.1007/s11084-015-9430-9
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA CJ9KC
UT WOS:000355820100014
PM 25990933
ER
PT J
AU Wei, CY
Pohorille, A
AF Wei, Chenyu
Pohorille, Andrew
TI M2 Proton Channel: Toward a Model of a Primitive Proton Pump
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Article; Proceedings Paper
CT Conference on Origins of Life and Evolution of Biospheres (OLEB)
CY JUL 06-11, 2014
CL Nara, JAPAN
DE Proton pump; Proton transport; Energy transduction; Ion channels;
Membrane proteins
ID INFLUENZA-A VIRUS; F0F1 ATP SYNTHASE; ION-CHANNEL; WEAK ACIDS;
MECHANISM; TRANSPORT; BACTERIORHODOPSIN; SELECTIVITY; ACTIVATION;
LIPOSOMES
AB Transmembrane proton transfer was essential to early cellular systems in order to transduce energy for metabolic functions. The reliable, efficient and controlled generation of proton gradients became possible only with the emergence of active proton pumps. On the basis of features shared by most modern proton pumps we identify the essential mechanistic steps in active proton transport. Further, we discuss the mechanism of action of a small, transmembrane M2 proton channel from influenza A virus as a model for proton transport in protocells. The M2 channel is a 94-residue long, alpha-helical tetramer that is activated at low pH and exhibits high selectivity and directionality. A shorter construct, built of transmembrane fragments that are only 24 amino acids in length, exhibits very similar proton transport properties. Molecular dynamics simulations on the microsecond time-scale carried out for the M2 channel provided atomic level details on the activation of the channel in response to protonation of the histidine residue, His37. The pathway of proton conduction is mediated by His37, which accepts and donates protons at different interconverting conformation states when pH is lower than 6.5. The Val27 and Trp41 gates and the salt bridge between Asp44 and Arg45 further enhance the directionality of proton transport. It is argued that the architecture and the mechanism of action similar to that found in the M2 channel might have been the perfect starting point for evolution towards the earliest proton pumps, indicating that active proton transport could have readily emerged from simple, passive proton channels.
C1 [Wei, Chenyu; Pohorille, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wei, Chenyu; Pohorille, Andrew] UCSF, Dept Pharmaceut Chem, San Francisco, CA 94143 USA.
RP Pohorille, A (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA.
EM Andrew.Pohorille@nasa.gov
NR 42
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
EI 1573-0875
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD JUN
PY 2015
VL 45
IS 1-2
SI SI
BP 241
EP 248
DI 10.1007/s11084-015-9421-x
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA CJ9KC
UT WOS:000355820100025
PM 25777465
ER
PT J
AU Wallis, DD
Miles, DM
Narod, BB
Bennest, JR
Murphy, KR
Mann, IR
Yau, AW
AF Wallis, D. D.
Miles, D. M.
Narod, B. B.
Bennest, J. R.
Murphy, K. R.
Mann, I. R.
Yau, A. W.
TI The CASSIOPE/e-POP Magnetic Field Instrument (MGF)
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetometer; Fluxgate; Satellite; Field-aligned currents
ID ALIGNED CURRENTS; BIRKELAND CURRENTS; MAGNETOMETER DATA; ARRAY
AB Field-aligned currents couple energy between the Earth's magnetosphere and ionosphere and are responsible for driving both micro and macro motions of plasma and neutral atoms in both regimes. These currents are believed to be a contributing energy source for ion acceleration in the polar ionosphere and may be detected via measurements of magnetic gradients along the track of a polar orbiting spacecraft, usually the north-south gradients of the east-west field component. The detection of such gradients does not require observatory class measurements of the geomagnetic field. The Magnetic Field instrument (MGF) measures the local magnetic field onboard the Enhanced Polar Outflow Probe (e-POP) satellite by using two ring-core fluxgate sensors to characterize and remove the stray spacecraft field. The fluxgate sensors have their heritage in the MAGSAT design, are double wound for reduced mass and cross-field dependence, and are mounted on a modest 0.9 m carbon-fiber boom. The MGF samples the magnetic field 160 times per sec (similar to 50 meters) to a resolution of 0.0625 nT and outputs data at 1952 bytes per second including temperature measurements. Its power consumption is 2.2 watts, and its noise level is 7 pT per root Hz at 1 Hz.
C1 [Wallis, D. D.] Magnametrics, Ottawa, ON, Canada.
[Wallis, D. D.; Yau, A. W.] Univ Calgary, Calgary, AB, Canada.
[Miles, D. M.; Mann, I. R.] Univ Alberta, Edmonton, AB, Canada.
[Narod, B. B.] Narod Geophys Ltd, Vancouver, BC, Canada.
[Narod, B. B.] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Bennest, J. R.] Bennest Enterprises Ltd, Summerland, BC, Canada.
[Murphy, K. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miles, DM (reprint author), Univ Alberta, Edmonton, AB, Canada.
EM David.Miles@ualberta.ca
OI Miles, David/0000-0002-4714-5966
FU NSERC; Canadian Space Agency; Canadian NSERC PGSD2 graduate scholarship;
NSERC Industrial Research Chair and Discovery Grant programs
FX We acknowledge the support from the Canadian Space Agency for the
development and operation of the CASSIOPE/e-POP mission. The authors are
grateful for the support and guidance of R. Hum. We thank J. Schmidt of
Minerva Technology Inc. for his contributions to the flight firmware, W.
Lunscher and his team at COM DEV for their technical assistance, and the
technical team at Magellan Aerospace Corporation for the boom
development. K.R. Murphy is supported by an NSERC Postdoctoral
fellowship. D.M. Miles is supported by grants from the Canadian Space
Agency and a Canadian NSERC PGSD2 graduate scholarship. I. R. Mann is
supported by an NSERC Discovery Grant. A. W. Yau is supported by grants
from the Canadian Space Agency and the NSERC Industrial Research Chair
and Discovery Grant programs.
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2015
VL 189
IS 1-4
BP 27
EP 39
DI 10.1007/s11214-014-0105-z
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CK1PU
UT WOS:000355980100004
ER
PT J
AU Bedka, KM
Wang, C
Rogers, R
Carey, LD
Feltz, W
Kanak, J
AF Bedka, Kristopher M.
Wang, Cecilia
Rogers, Ryan
Carey, Lawrence D.
Feltz, Wayne
Kanak, Jan
TI Examining Deep Convective Cloud Evolution Using Total Lightning,
WSR-88D, and GOES-14 Super Rapid Scan Datasets*
SO WEATHER AND FORECASTING
LA English
DT Article
ID SEVERE WEATHER; DETECTION NETWORK; UNITED-STATES; ENHANCED-V; GOES-R;
SATELLITE; TOP
AB The Geostationary Operational Environmental Satellite-14 (GOES-14) Imager operated in 1-min Super Rapid Scan Operations for GOES-R (SRSOR) mode during summer and fall of 2012 to emulate the high temporal resolution sampling of the GOES-R Advanced Baseline Imager (ABI). The current GOES operational scan interval is 15-30 min, which is too coarse to capture details important for severe convective storm forecasting including 1) when indicators of a severe storm such as rapid cloud-top cooling, overshooting tops, and above-anvil cirrus plumes first appear; 2) how satellite-observed cloud tops truly evolve over time; and 3) how satellite cloud-top observations compare with radar and lightning observations at high temporal resolution. In this paper, SRSOR data, radar, and lightning observations are used to analyze five convective storms, four of which were severe, to address these uncertainties. GOES cloud-top cooling, increased lightning flash rates, and peak precipitation echo tops often preceded severe weather, signaling rapid intensification of the storm updraft. Near the time of several severe hail or damaging wind events, GOES cloud-top temperatures and radar echo tops were warming rapidly, which indicated variability in the storm updraft that could have allowed the hail and wind gusts to reach the surface. Above-anvil cirrus plumes were another prominent indicator of impending severe weather. Detailed analysis of storms throughout the 2012 SRSOR period indicates that 57% of the plume-producing storms were severe and 85% of plumes from severe storms appeared before a severe weather report with an average lead time of 18 min, 9 min earlier than what would be observed by GOES operational scanning.
C1 [Bedka, Kristopher M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Wang, Cecilia] Sci Syst & Applicat Inc, Hampton, VA USA.
[Rogers, Ryan; Carey, Lawrence D.] Univ Alabama, Huntsville, AL 35899 USA.
[Feltz, Wayne] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
[Kanak, Jan] Slovak Hydrometeorol Inst, Bratislava, Slovakia.
RP Bedka, KM (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM kristopher.m.bedka@nasa.gov
FU GOES-R Risk Reduction Research (R3) program
FX This research has been supported by the GOES-R Risk Reduction Research
(R3) program. In particular, we thank Dr. Steven Goodman, senior (chief)
scientist, GOES-R System Program, for his guidance and support
throughout this effort. The authors would also like to thank Tim Schmit
(NOAA/NESDIS) and Martin Setvak (CHMI) for their valuable comments on
this work. An additional thank you goes to NOAA/NESDIS for collecting
the GOES-14 SRSOR data.
NR 37
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Z9 11
U1 2
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
EI 1520-0434
J9 WEATHER FORECAST
JI Weather Forecast.
PD JUN
PY 2015
VL 30
IS 3
BP 571
EP 590
DI 10.1175/WAF-D-14-00062.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ7FG
UT WOS:000355659300004
ER
PT J
AU Sasso, JP
Eves, ND
Christensen, JF
Koelwyn, GJ
Scott, J
Jones, LW
AF Sasso, John P.
Eves, Neil D.
Christensen, Jesper F.
Koelwyn, Graeme J.
Scott, Jessica
Jones, Lee W.
TI A framework for prescription in exercise-oncology research
SO JOURNAL OF CACHEXIA SARCOPENIA AND MUSCLE
LA English
DT Editorial Material
ID RANDOMIZED CONTROLLED-TRIAL; OPERABLE BREAST-CANCER; QUALITY-OF-LIFE;
PHYSICAL-ACTIVITY; HEART-RATE; AEROBIC EXERCISE; CLINICAL-TRIALS;
FUTURE-RESEARCH; SURVIVORS; METAANALYSIS
AB The field of exercise-oncology has increased dramatically over the past two decades, with close to 100 published studies investigating the efficacy of structured exercise training interventions in patients with cancer. Of interest, despite considerable differences in study population and primary study end point, the vast majority of studies have tested the efficacy of an exercise prescription that adhered to traditional guidelines consisting of either supervised or home-based endurance (aerobic) training or endurance training combined with resistance training, prescribed at a moderate intensity (50-75% of a predetermined physiological parameter, typically age-predicted heart rate maximum or reserve), for two to three sessions per week, for 10 to 60 min per exercise session, for 12 to 15 weeks. The use of generic exercise prescriptions may, however, be masking the full therapeutic potential of exercise treatment in the oncology setting. Against this background, this opinion paper provides an overview of the fundamental tenets of human exercise physiology known as the principles of training, with specific application of these principles in the design and conduct of clinical trials in exercise-oncology research. We contend that the application of these guidelines will ensure continued progress in the field while optimizing the safety and efficacy of exercise treatment following a cancer diagnosis.
C1 [Sasso, John P.; Jones, Lee W.] Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA.
[Eves, Neil D.] Univ British Columbia Okanagan, Sch Hlth & Exercise Sci, Ctr Heart Lung & Vasc Hlth, Kelowna, BC, Canada.
[Christensen, Jesper F.] Rigshosp, Dept Infect Dis, Ctr Inflammat & Metab, DK-2100 Copenhagen, Denmark.
[Christensen, Jesper F.] Rigshosp, Dept Infect Dis, Ctr Phys Act Res CIM CFAS, DK-2100 Copenhagen, Denmark.
[Koelwyn, Graeme J.] NYU, Sch Med, Sackler Inst Grad Biomed Sci, New York, NY USA.
[Scott, Jessica] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
RP Sasso, JP (reprint author), Mem Sloan Kettering Canc Ctr, 1275 York Ave, New York, NY 10021 USA.
FU NCI NIH HHS [P30 CA008748]
NR 50
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Z9 14
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2190-5991
EI 2190-6009
J9 J CACHEXIA SARCOPENI
JI J. Caxhexia Sarcopenia Muscle
PD JUN
PY 2015
VL 6
IS 2
BP 115
EP 124
DI 10.1002/jcsm.12042
PG 10
WC Medicine, General & Internal
SC General & Internal Medicine
GA CJ2UP
UT WOS:000355340500001
PM 26136187
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI Applied Minds: How Engineers Think.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 1
PY 2015
VL 140
IS 10
BP 130
EP 130
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA CJ3MK
UT WOS:000355387900221
ER
PT J
AU Horz, F
Archer, PD
Niles, PB
Zolensky, ME
Evans, M
AF Hoerz, F.
Archer, P. D., Jr.
Niles, P. B.
Zolensky, M. E.
Evans, M.
TI Devolatilization or melting of carbonates at Meteor Crater, AZ?
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SILICATE LIQUID IMMISCIBILITY; IMPACT-MELT; SHOCK METAMORPHISM;
TERRESTRIAL IMPACT; RIES CRATER; ROCKS; GEOCHEMISTRY; SUEVITE; GLASS;
ARIZONA
AB We have investigated the carbonates in the impact melts and in a monolithic clast of highly shocked Coconino sandstone of Meteor Crater, AZ to evaluate whether melting or devolatilization is the dominant response of carbonates during high-speed meteorite impact. Both melt- and clast-carbonates are calcites that have identical crystal habits and that contain anomalously high SiO2 and Al2O3. Also, both calcite occurrences lack any meteoritic contamination, such as Fe or Ni, which is otherwise abundantly observed in all other impact melts and their crystallization products at Meteor Crater. The carbon and oxygen isotope systematics for both calcite deposits suggest a low temperature environment (<100 degrees C) for their precipitation from an aqueous solution, consistent with caliche. We furthermore subjected bulk melt beads to thermogravimetric analysis and monitored the evolving volatiles with a quadrupole mass spectrometer. CO2 yields were <5wt%, with typical values in the 2wt% range; also total CO2 loss is positively correlated with H2O loss, an indication that most of these volatiles derive from the secondary calcite. Also, transparent glasses, considered the most pristine impact melts, yield 100 wt% element totals by EMPA, suggesting complete loss of CO2. The target dolomite decomposed into MgO, CaO, and CO2; the CO2 escaped and the CaO and MgO combined with SiO2 from coexisting quartz and FeO from the impactor to produce the dominant impact melt at Meteor Crater. Although confined to Meteor Crater, these findings are in stark contrast to Osinski etal. (2008) who proposed that melting of carbonates, rather than devolatilization, is the dominant process during hypervelocity impact into carbonate-bearing targets, including Meteor Crater.
C1 [Hoerz, F.] LZ Technol Inc, Houston, TX 77058 USA.
[Archer, P. D., Jr.] NASA, Johnson Space Ctr, Jacobs, Houston, TX 77058 USA.
[Niles, P. B.; Zolensky, M. E.; Evans, M.] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Evans, M.] Texas A&M Univ, College Stn, TX 77843 USA.
RP Horz, F (reprint author), LZ Technol Inc, 1110 NASA Pkwy, Houston, TX 77058 USA.
EM friedrich.p.horz@nasa.gov
FU NASA's Planetary Geology and Geophysics Program; Mars Fundamental
Research Program; Cosmochemistry Program
FX We thank Anne Peslier (EMPA), Kent D. Ross (SEM), and James Martinez
(EBSD) for their assistance in generating some of the analyses reported
here. The Meteor Crater samples were generously provided from Nininger's
original "impactite" collection by the Center for Meteorite Studies,
ASU, Tempe, AZ (all MCxx samples) and by J. Haggerty, USGS Flagstaff, AZ
(MCH samples), or collected in the field by the senior author (COC5).
Fruitful discussions with M. J. Cintala, D. Mittlefehldt, T. H. See, and
D. Stoffler shaped our thinking. Constructive reviews by Alex Deutsch,
Boris Ivanov, and AE Uwe Reimold lead to a much improved article. This
work was supported by NASA's Planetary Geology and Geophysics (F.H),
Mars Fundamental Research (D. A.), and Cosmochemistry Programs (PBN and
MEZ).
NR 68
TC 6
Z9 6
U1 3
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 JUN
PY 2015
VL 50
IS 6
BP 1050
EP 1070
DI 10.1111/maps.12453
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CJ1WQ
UT WOS:000355276100004
ER
PT J
AU Keil, K
Zucolotto, ME
Krot, AN
Doyle, PM
Telus, M
Krot, TV
Greenwood, RC
Franchi, IA
Wasson, JT
Welten, KC
Caffee, MW
Sears, DWG
Riebe, M
Wieler, R
dos Santos, E
Scorzelli, RB
Gattacceca, J
Lagroix, F
Laubenstein, M
Mendes, JC
Schmitt-Kopplin, P
Harir, M
Moutinho, ALR
AF Keil, Klaus
Zucolotto, Maria E.
Krot, Alexander N.
Doyle, Patricia M.
Telus, Myriam
Krot, Tatiana V.
Greenwood, Richard C.
Franchi, Ian A.
Wasson, John T.
Welten, Kees C.
Caffee, Marc W.
Sears, Derek W. G.
Riebe, My
Wieler, Rainer
dos Santos, Edivaldo
Scorzelli, Rosa B.
Gattacceca, Jerome
Lagroix, France
Laubenstein, Matthias
Mendes, Julio C.
Schmitt-Kopplin, Philippe
Harir, Mourad
Moutinho, Andre L. R.
TI The Vicencia meteorite fall: A new unshocked (S1) weakly metamorphosed
(3.2) LL chondrite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID UNEQUILIBRATED ORDINARY CHONDRITES; STONY METEORITES; ORGANIC-MATTER;
EXPOSURE AGES; NOBLE-GASES; CARBONACEOUS CHONDRITES; COSMOGENIC
NUCLIDES; PRODUCTION-RATES; OXYGEN-ISOTOPE; PARENT-BODY
AB The Vicencia meteorite, a stone of 1.547kg, fell on September 21, 2013, at the village Borracha, near the city of Vicencia, Pernambuco, Brazil. It was recovered immediately after the fall, and our consortium study showed it to be an unshocked (S1) LL3.2 ordinary chondrite. The LL group classification is based on the bulk density (3.13gcm(-3)); the chondrule mean apparent diameter (0.9mm); the bulk oxygen isotopic composition (O-17=3.768 +/- 0.042 parts per thousand, O-18=5.359 +/- 0.042 parts per thousand, O-17=0.981 +/- 0.020 parts per thousand); the content of metallic Fe,Ni (1.8 vol%); the Co content of kamacite (1.73 wt%); the bulk contents of the siderophile elements Ir and Co versus Au; and the ratios of metallic Fe-0/total iron (0.105) versus total Fe/Mg (1.164), and of Ni/Mg (0.057) versus total Fe/Mg. The petrologic type 3.2 classification is indicated by the beautifully developed chondritic texture, the standard deviation (similar to 0.09) versus mean Cr2O3 content (similar to 0.14 wt%) of ferroan olivine, the TL sensitivity and the peak temperature and peak width at half maximum, the cathodoluminescence properties of chondrules, the content of trapped Xe-132(tr) (0.317x10(-8)cm(3)STPg(-1)), and the Raman spectra for organic material in the matrix. The cosmic ray exposure age is similar to 72Ma, which is at the upper end of the age distribution of LL group chondrites. The meteorite is unusual in that it contains relatively large, up to nearly 100m in size, secondary fayalite grains, defined as olivine with Fa(>75), large enough to allow insitu measurement of oxygen and Mn-Cr isotope systematics with SIMS. Its oxygen isotopes plot along a mass-dependent fractionation line with a slope of similar to 0.5 and O-17 of 4.0 +/- 0.3 parts per thousand, and are similar to those of secondary fayalite and magnetite in the unequilibrated chondrites EET 90161, MET 96503, and Ngawi. These data suggest that secondary fayalite in Vicencia was in equilibrium with a fluid with a O-17 of similar to 4 parts per thousand, consistent with the composition of the fluid in equilibrium with secondary magnetite and fayalite in other unequilibrated ordinary chondrites. Secondary fayalite and the chondrule olivine phenocrysts in Vicencia are not in isotopic equilibrium, consistent with low-temperature formation of fayalite during aqueous alteration on the LL parent body. That alteration, as dated by the Mn-53-Cr-53 chronology age of secondary fayalite, took place 4.0-1.1+1.4 Ma after formation of CV CAIs when anchored to the quenched angrite D'Orbigny.
C1 [Keil, Klaus; Krot, Alexander N.; Doyle, Patricia M.; Telus, Myriam; Krot, Tatiana V.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Zucolotto, Maria E.] Museu Nacl UFRJ, Quinta da Boa Vista RJ, BR-20940040 Rio De Janeiro, Brazil.
[Greenwood, Richard C.; Franchi, Ian A.] Open Univ, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Wasson, John T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Wasson, John T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Chem & Biochem, Los Angeles, CA 90095 USA.
[Welten, Kees C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Caffee, Marc W.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Riebe, My; Wieler, Rainer] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland.
[dos Santos, Edivaldo; Scorzelli, Rosa B.] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil.
[Gattacceca, Jerome] Aix Marseille Univ, CNRS, CEREGE 34, F-13545 Aix En Provence, France.
[Lagroix, France] IPGP, Paris, France.
[Laubenstein, Matthias] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, AQ, Italy.
[Mendes, Julio C.] Univ Fed Rio de Janeiro, Dept Geol, Rio de Janeiro, Brazil.
[Schmitt-Kopplin, Philippe; Harir, Mourad] Helmholtz Zentrum Munchen, DES, D-85764 Neuherberg, Germany.
RP Keil, K (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM keil@hawaii.edu
RI Schmitt-Kopplin, Philippe/H-6271-2011; Caffee, Marc/K-7025-2015;
Laubenstein, Matthias/C-4851-2013; Lagroix, France/A-6112-2011;
OI Schmitt-Kopplin, Philippe/0000-0003-0824-2664; Caffee,
Marc/0000-0002-6846-8967; Laubenstein, Matthias/0000-0001-5390-4343;
Lagroix, France/0000-0003-2873-2767; Wasson, John/0000-0002-7253-2300
FU NASA Cosmochemistry Program [NNX10AH76G]; NASA [NNX10AG98G]; Swiss
National Science Foundation; SSERVI
FX The research of ANK, PMD, TVK, MT, and KK was supported in part by grant
NNX10AH76G from the NASA Cosmochemistry Program (A. N. Krot, PI), that
of JTW by NASA grant NNX10AG98G, that of KW by the NASA Cosmochemistry
Program, and that of MR and RW by the Swiss National Science Foundation.
DWGS is grateful to Chris McKay for support and Hazel Sears for
assistance in the laboratory. The TL laboratory is supported by a SSERVI
grant to the FINESSE project (PI: Jennifer Heldmann). We thank Alan
Rubin, Addi Bischoff, and an anonymous reviewer for most valuable and
constructive comments that have improved the manuscript considerably.
"This is Hawai'i Institute of Geophysics and Planetology publication
number 2169 and School of Ocean and Earth Science and Technology
publication number 9424".
NR 66
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U1 2
U2 19
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 JUN
PY 2015
VL 50
IS 6
BP 1089
EP 1111
DI 10.1111/maps.12456
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CJ1WQ
UT WOS:000355276100006
ER
PT J
AU Hall, DK
Crawford, CJ
DiGirolamo, NE
Riggs, GA
Foster, JL
AF Hall, Dorothy K.
Crawford, Christopher J.
DiGirolamo, Nicolo E.
Riggs, George A.
Foster, James L.
TI Detection of earlier snowmelt in the Wind River Range, Wyoming, using
Landsat imagery, 1972-2013
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Wind River Range; Snowmelt; Snow-cover depletion curves; Landsat; MODIS
ID WESTERN UNITED-STATES; NORTH-AMERICA; CONTINENTAL GLACIER; COVER;
SNOWPACK; MODIS; VARIABILITY; STREAMFLOW; USA; PRECIPITATION
AB In the western United States snow has been melting earlier in recent decades due to warmer winter and spring weather. This is particularly noticeable in the Pacific Northwest and coastal areas, yet has been less obvious in locations farther inland. Using the historical Landsat image archive, snow cover was mapped in the Wind River Range (WRR) in northwestern Wyoming, from 1972-2013. The objective of this work was to estimate the temporal change in the rate of snowmelt in the Fremont Lake basin of the WRR for the 42-year study period. Much of the streamflow in Wyoming originates from melting snow in the WRR. Streamflow is a significant contributor to the water resources for the north-central part of the state and has tremendous societal and economic impacts especially during the prolonged drought that is affecting the western U.S. Consistent with the ongoing and severe drought, data from the Pine Creek Above Fremont Lake gauge show a striking reduction in cumulative stream discharge in the 2000s vs. the decades of the 1970s, 1980s and 1990s. Snow-cover depletion curves derived from snow maps created from Landsat imagery were generated for the period 1972-2013. MODerate-Resolution Imaging Spectroradiometer (MODIS)-derived standard snow-cover maps were also used to generate snow-cover depletion curves, from 2000-2013, to provide an accuracy assessment of the Landsat technique. Landsat-derived mean snow-cover depletion curves from 2000-2013 and from the three previous decades, show that snow cover in the Fremont lake basin is melting 16 +/- 10 days earlier, on average, in the 2000s compared to the period from 1972-1999. Increasing spring and summer nighttime air temperature is the likely driver of the earlier snowmelt documented in the Landsat record. (C) 2015 Published by Elsevier Inc.
C1 [Hall, Dorothy K.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Crawford, Christopher J.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[DiGirolamo, Nicolo E.; Riggs, George A.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Foster, James L.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
RP Hall, DK (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
FU NASA through the MODIS Science Team and Earth Observing System Program;
NASA Postdoctoral Program [NNH06CC03B]
FX The research conducted at Goddard Space Flight Center (GSFC) was
supported by NASA through the MODIS Science Team and Earth Observing
System Program. Christopher J. Crawford was funded through a NASA
Postdoctoral Program (NNH06CC03B) appointment at the Goddard Space
Flight Center administrated by Oak Ridge Associated Universities.
Valuable discussions were held with personnel at the Pinedale Ranger
District in Wyoming providing much useful information that inspired this
work.
NR 44
TC 3
Z9 3
U1 5
U2 26
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 JUN 1
PY 2015
VL 162
BP 45
EP 54
DI 10.1016/j.rse.2015.01.032
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CI8WI
UT WOS:000355052000004
ER
PT J
AU Muller, D
Krasemann, H
Brewin, RJW
Brockmann, C
Deschamps, PY
Doerffer, R
Fomferra, N
Franz, BA
Grant, MG
Groom, SB
Melin, F
Platt, T
Regner, P
Sathyendranath, S
Steinmetz, F
Swinton, J
AF Mueller, Dagmar
Krasemann, Hajo
Brewin, Robert J. W.
Brockmann, Carsten
Deschamps, Pierre-Yves
Doerffer, Roland
Fomferra, Norman
Franz, Bryan A.
Grant, Mike G.
Groom, Steve B.
Melin, Frederic
Platt, Trevor
Regner, Peter
Sathyendranath, Shubha
Steinmetz, Francois
Swinton, John
TI The Ocean Colour Climate Change Initiative: II. Spatial and temporal
homogeneity of satellite data retrieval due to systematic effects in
atmospheric correction processors
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE OC-CCI; CCI; Ocean-Colour; Climate Change; Atmospheric correction;
Algorithm comparison; Angular dependency; Systematic error
ID MULTIPLE-SCATTERING; ALGORITHM; AEROSOLS; MERIS; RADIANCE; WATERS
AB The established procedure to access the quality of atmospheric correction processors and their underlying algorithms is the comparison of satellite data products with related in-situ measurements. Although this approach addresses the accuracy of derived geophysical properties in a straight forward fashion, it is also limited in its ability to catch systematic sensor and processor dependent behaviour of satellite products along the scan-line, which might impair the usefulness of the data in spatial analyses.
The Ocean Colour Climate Change Initiative (OC-CCI) aims to create an ocean colour dataset on a global scale to meet the demands of the ecosystem modelling community. The need for products with increasing spatial and temporal resolution that also show as little systematic and random errors as possible, increases. Due to cloud cover, even temporal means can be influenced by along-scanline artefacts if the observations are not balanced and effects cannot be cancelled out mutually.
These effects can arise from a multitude of results which are not easily separated, if at all. Among the sources of artefacts, there are some sensor-specific calibration issues which should lead to similar responses in all processors, as well as processor-specific features which correspond with the individual choices in the algorithms. A set of methods is proposed and applied to MERIS data over two regions of interest in the North Atlantic and the South Pacific Gyre. The normalised water leaving reflectance products of four atmospheric correction processors, which have also been evaluated in match-up analysis, is analysed in order to find and interpret systematic effects across track. These results are summed up with a semi-objective ranking and are used as a complement to the match-up analysis in the decision for the best Atmospheric Correction (AC) processor.
Although the need for discussion remains concerning the absolutes by which to judge an AC processor, this example demonstrates clearly, that relying on the match-up analysis alone can lead to misjudgement (C) 2015 Elsevier Inc All rights reserved.
C1 [Mueller, Dagmar; Krasemann, Hajo; Doerffer, Roland] Helmholtz Zentrum Geesthacht, D-21502 Geesthacht, Germany.
[Brewin, Robert J. W.; Grant, Mike G.; Groom, Steve B.; Platt, Trevor; Sathyendranath, Shubha] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Brockmann, Carsten; Fomferra, Norman] Brockmann Consult, D-21502 Geesthacht, Germany.
[Deschamps, Pierre-Yves; Steinmetz, Francois] HYGEOS, F-59000 Lille, France.
[Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Melin, Frederic] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
[Regner, Peter] European Space Agcy, ESRIN, I-00044 Frascati, Italy.
[Swinton, John] Telespazio VEGA UK Ltd, Luton LU1 3LU, Beds, England.
RP Muller, D (reprint author), Helmholtz Zentrum Geesthacht, Max Planck Str 1, D-21502 Geesthacht, Germany.
EM dagmar.mueller@hzg.de
RI Franz, Bryan/D-6284-2012;
OI Franz, Bryan/0000-0003-0293-2082; Brewin, Robert/0000-0001-5134-8291
NR 20
TC 2
Z9 2
U1 0
U2 10
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 JUN 1
PY 2015
VL 162
BP 257
EP 270
DI 10.1016/j.rse.2015.01.033
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CI8WI
UT WOS:000355052000020
ER
PT J
AU Brewin, RJW
Sathyendranath, S
Muller, D
Brockrnann, C
Deschamps, PY
Devred, E
Doerffer, R
Fomferra, N
Franz, B
Grant, M
Groom, S
Horseman, A
Hu, C
Krasemann, H
Lee, Z
Maritorena, S
Meelin, F
Peters, M
Platt, T
Regner, P
Smyth, T
Steinmetz, F
Swinton, J
Werdell, J
White, GN
AF Brewin, Robert J. W.
Sathyendranath, Shubha
Mueller, Dagmar
Brockrnann, Carsten
Deschamps, Pierre-Yves
Devred, Emmanuel
Doerffer, Roland
Fomferra, Norman
Franz, Bryan
Grant, Mike
Groom, Steve
Horseman, Andrew
Hu, Chuanmin
Krasemann, Hajo
Lee, ZhongPing
Maritorena, Stephane
Melin, Frederic
Peters, Marco
Platt, Trevor
Regner, Peter
Smyth, Tim
Steinmetz, Francois
Swinton, John
Werdell, Jeremy
White, George N., III
TI The Ocean Colour Climate Change Initiative: III. A round-robin
comparison on in-water bio-optical algorithms
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Phytoplankton; Ocean colour; Inherent Optical Properties; Remote
sensing; Chlorophyll-a
ID INHERENT OPTICAL-PROPERTIES; DISSOLVED ORGANIC-MATTER; SATELLITE DATA;
SEMIANALYTICAL MODEL; MULTISENSOR APPROACH; SHALLOW WATERS;
PACIFIC-OCEAN; DATA PRODUCTS; PHYTOPLANKTON; OPTIMIZATION
AB Satellite-derived remote-sensing reflectance (R-rs) can be used for mapping biogeochemically relevant variables, such as the chlorophyll concentration and the Inherent Optical Properties (IOPs) of the water, at global scale for use in climate-change studies. Prior to generating such products, suitable algorithms have to be selected that are appropriate for the purpose. Algorithm selection needs to account for both qualitative and quantitative requirements. In this paper we develop an objective methodology designed to rank the quantitative performance of a suite of bio-optical models. The objective classification is applied using the NASA bio-Optical Marine Algorithm Dataset (NOMAD). Using in situ Rrs as input to the models, the performance of eleven semi-analytical models, as well as five empirical chlorophyll algorithms and an empirical diffuse attenuation coefficient algorithm, is ranked for spectrally-resolved IOPs, chlorophyll concentration and the diffuse attenuation coefficient at 489 nm. The sensitivity of the objective classification and the uncertainty in the ranking are tested using a Monte-Carlo approach (bootstrapping). Results indicate that the performance of the semi-analytical models varies depending on the product and wavelength of interest. For chlorophyll retrieval, empirical algorithms perform better than semi-analytical models, in general. The performance of these empirical models reflects either their immunity to scale errors or instrument noise in R data, or simply that the data used for model parameterisation were not independent of NOMAD. Nonetheless, uncertainty in the classification suggests that the performance of some semi-analytical algorithms at retrieving chlorophyll is comparable with the empirical algorithms. For phytoplankton absorption at 443 nm, some semi-analytical models also perform with similar accuracy to an empirical model: We discuss the potential biases, limitations and uncertainty in the approach, as well as additional qualitative considerations for algorithm selection for climate-change studies. Our classification has the potential to be routinely implemented, such that the performance of emerging algorithms can be compared with existing algorithms as they become available. In the long-term, such an approach will further aid algorithm development for ocean-colour studies. (C) 2013 Elsevier Inc All rights reserved.
C1 [Brewin, Robert J. W.; Sathyendranath, Shubha; Grant, Mike; Groom, Steve; Horseman, Andrew; Platt, Trevor; Smyth, Tim] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Brewin, Robert J. W.; Sathyendranath, Shubha] Plymouth Marine Lab, Natl Ctr Earth Observat, Plymouth PL1 3DH, Devon, England.
[Mueller, Dagmar; Doerffer, Roland; Krasemann, Hajo] Helmholtz Zentrum Geesthacht, D-21502 Geesthacht, Germany.
[Brockrnann, Carsten; Fomferra, Norman; Peters, Marco] Brockmann Consult, D-21502 Geesthacht, Germany.
[Deschamps, Pierre-Yves; Steinmetz, Francois] HYGEOS, F-59000 Lille, France.
[Devred, Emmanuel] Univ Laval, Quebec City, PQ G1V 0A6, Canada.
[Franz, Bryan; Werdell, Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hu, Chuanmin] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Lee, ZhongPing] Univ Massachusetts, Coll Sci & Math, Boston, MA 02125 USA.
[Maritorena, Stephane] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Melin, Frederic] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
[Regner, Peter] European Space Agcy, ESRIN, I-00044 Frascati, Italy.
[Swinton, John] Telespazio VEGA UK Ltd, Luton LU1 3LU, Beds, England.
[White, George N., III] Bedford Inst Oceanog, Ocean Sci Div, Dartmouth, NS B2Y 4A2, Canada.
RP Brewin, RJW (reprint author), Plymouth Marine Lab, Prospect Pl, Plymouth PL1 3DH, Devon, England.
EM robr@pml.ac.uk
OI Brewin, Robert/0000-0001-5134-8291
FU NASA SIMBIOS Program [NRA-96-MTPE-04, NRA-99-OES-09]; UK National Centre
for Earth Observation
FX NOMAD data were contributed by participants in the NASA SIMBIOS Program
(NRA-96-MTPE-04 and NRA-99-OES-09) and by voluntary contributors. A
cruise name accompanies each data record. Cruise details, including
contributors' names, are available online
(http://seabass.gsfc.nasa.gov/seabasscgi/nomad.cgi) using the General
Search and Cruise Search utilities to facilitate communication,
collaboration, and acknowledgement. NASA should be commended for the
development of the NOMAD dataset and for on-going in situ activities.
This work is a contribution to the Ocean Colour Climate Change
Initiative of the European Space Agency and was supported by the UK
National Centre for Earth Observation.
NR 72
TC 21
Z9 21
U1 3
U2 30
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JUN 1
PY 2015
VL 162
BP 271
EP 294
DI 10.1016/j.rse.2013.09.016
PG 24
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CI8WI
UT WOS:000355052000021
ER
PT J
AU Laeng, A
Hubert, D
Verhoelst, T
von Clarmann, T
Dinelli, BM
Dudhia, A
Raspollini, P
Stiller, G
Grabowski, U
Keppens, A
Kiefer, M
Sofieva, V
Froidevaux, L
Walker, KA
Lambert, JC
Zehner, C
AF Laeng, A.
Hubert, D.
Verhoelst, T.
von Clarmann, T.
Dinelli, B. M.
Dudhia, A.
Raspollini, P.
Stiller, G.
Grabowski, U.
Keppens, A.
Kiefer, M.
Sofieva, V.
Froidevaux, L.
Walker, K. A.
Lambert, J. -C.
Zehner, C.
TI The ozone climate change initiative: Comparison of four Level-2
processors for the Michelson Interferometer for Passive Atmospheric
Sounding (MIPAS)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MIPAS; Ozone
ID LIMB EMISSION-SPECTRA; MIPAS/ENVISAT MEASUREMENTS; TOMOGRAPHIC
RETRIEVAL; REGULARIZATION METHOD; RADIATIVE-TRANSFER; VERTICAL PROFILES;
AURA SATELLITE; TECHNICAL NOTE; EOS MLS; VALIDATION
AB The MIPAS spectrometer onboard the Envisat platform observed infrared emission from the Earth's limb between 2002 and 2012. It recorded high-resolution spectra during day and night, from pole to pole and between 6 and 70 km altitude in the nominal measurement mode or up to 170 km in special measurement modes, producing daily more than 1000 vertical profiles of various trace gases. The operational Level-2 data are processed by ESA/DLR but there exist three other, independent research Level-2 processors that are hosted by ISAC-CNR/University of Bologna, Oxford University, and KIT IMK/IAA. All four Level-2 processors rely on the same Level-1b data provided by ESA but their retrieval schemes differ. As part of ESA's Ozone Climate Change Initiative project, an intercomparison of the four MIPAS processors took place, in which vertical ozone profiles retrieved by these four processors from MIPAS nominal mode measurements were compared for 2007 and 2008. We present the results of this comparison exercise, which consisted of five parts: an information content study of the vertical averaging kernels, an intercomparison of zonal seasonal means and spreads, a determination of biases through comparison to ozonesonde and lidar measurements, a comparison to other satellite records (bias estimation and precision assessment with respect to ACE-FTS and Aura-MLS data), and a geophysical validation of the provided error bars using MIPAS MIPAS collocations.
The four processors demonstrate similar performance. All processors use the same Level-1b data from ESA, apply global fits, and use microwindows instead of the full spectrum. The main differences in the processing schemes include the choice of microwindows, the regularization approach, the treatment of negative retrieved values, and the cloud detection threshold. The different regularization schemes lead to a different trade-off between noise and resolution, but without a clear average advantage for any particular data set. The vertical resolution is typically 3-5 km and the single profile precision is about 2-3%. In the middle and upper stratosphere, at 25-45 km, all four MIPAS processors clearly show a high bias of 2 to 5% relative to all reference instruments. The similarity of the structure and magnitude of the bias among the MIPAS data sets indicates that the bias is most likely linked to the use of microwindows of the MIPAS AB band. The satellite intercomparisons show furthermore that for the KIT dataset, the onset of the high bias starts at a somewhat higher altitude (only above 35 km) than for the other three datasets. This is likely due to the more restrictive use of the AB band by the KIT processor, which comes at the cost of a coarser vertical resolution near the ozone volume mixing ratio (vmr) peak. In the troposphere, the Level-2 algorithms that suppress negative ozone values in the iterative retrieval process produce a larger positive bias than the algorithm that does not follow such a strategy. Our main conclusion is that the four MIPAS processors are more similar to each other than to any other reference instrument. This indicates that the observed biases are very likely instrument-related. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Laeng, A.; von Clarmann, T.; Stiller, G.; Grabowski, U.; Kiefer, M.] Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany.
[Hubert, D.; Verhoelst, T.; Keppens, A.; Lambert, J. -C.] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Dinelli, B. M.] CNR, ISAC, I-40126 Bologna, Italy.
[Dudhia, A.] Univ Oxford, Oxford OX1 2JD, England.
[Raspollini, P.] CNR, IFAC, Florence, Italy.
[Sofieva, V.] Finnish Meteorol Inst, Helsinki, Finland.
[Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Walker, K. A.] Univ Toronto, Toronto, ON M5S 1A1, Canada.
[Zehner, C.] ESA, ESRIN, Frascati, Italy.
RP Laeng, A (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany.
EM alexandra.laeng@kit.edu
RI Sofieva, Viktoria/E-1958-2014;
OI Sofieva, Viktoria/0000-0002-9192-2208; Dinelli, Bianca
Maria/0000-0002-1218-0008; Hubert, Daan/0000-0002-4365-865X
FU Canadian Space Agency; National Aeronautics and Space Administration
FX This work was performed in the frame of European Space Agency (ESA)
project Ozone_cci. All four MIPAS teams acknowledge ESA for providing
MIPAS Lib data. The ACE mission is supported primarily by the Canadian
Space Agency. Work at the Jet Propulsion Laboratory was performed under
contract with the National Aeronautics and Space Administration.
NR 73
TC 5
Z9 5
U1 2
U2 13
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JUN 1
PY 2015
VL 162
BP 316
EP 343
DI 10.1016/j.rse.2014.12.013
PG 28
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CI8WI
UT WOS:000355052000023
ER
PT J
AU Buchwitz, M
Reuter, M
Schneising, O
Boesch, H
Guerlet, S
Dils, B
Aben, I
Armante, R
Bergamaschi, P
Blumenstock, T
Bovensmann, H
Brunner, D
Buchmann, B
Burrows, JP
Butz, A
Chedin, A
Chevallier, F
Crevoisier, CD
Deutscher, NM
Frankenberg, C
Hase, F
Hasekamp, OP
Heymann, J
Kaminski, T
Laeng, A
Lichtenberg, G
De Maziere, M
Noel, S
Notholt, J
Orphal, J
Popp, C
Parker, R
Scholze, M
Sussmann, R
Stiller, GP
Warneke, T
Zehner, C
Bril, A
Crisp, D
Griffith, DWT
Kuze, A
O'Dell, C
Oshchepkov, S
Sherlock, V
Suto, H
Wennberg, P
Wunch, D
Yokota, T
Yoshida, Y
AF Buchwitz, M.
Reuter, M.
Schneising, O.
Boesch, H.
Guerlet, S.
Dils, B.
Aben, I.
Armante, R.
Bergamaschi, P.
Blumenstock, T.
Bovensmann, H.
Brunner, D.
Buchmann, B.
Burrows, J. P.
Butz, A.
Chedin, A.
Chevallier, F.
Crevoisier, C. D.
Deutscher, N. M.
Frankenberg, C.
Hase, F.
Hasekamp, O. P.
Heymann, J.
Kaminski, T.
Laeng, A.
Lichtenberg, G.
De Maziere, M.
Noel, S.
Notholt, J.
Orphal, J.
Popp, C.
Parker, R.
Scholze, M.
Sussmann, R.
Stiller, G. P.
Warneke, T.
Zehner, C.
Bril, A.
Crisp, D.
Griffith, D. W. T.
Kuze, A.
O'Dell, C.
Oshchepkov, S.
Sherlock, V.
Suto, H.
Wennberg, P.
Wunch, D.
Yokota, T.
Yoshida, Y.
TI The Greenhouse Gas Climate Change Initiative (GHG-CCI): Comparison and
quality assessment of near-surface-sensitive satellite-derived CO2 and
CH4 global data sets
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE SCIAMACHY; GOSAT; Greenhouse gases; Carbon dioxide; Methane; Climate
change
ID COLUMN OBSERVING NETWORK; HYPERSPECTRAL INFRARED OBSERVATIONS;
ATMOSPHERIC CO2; RETRIEVAL ALGORITHM; CARBON-DIOXIDE; METHANE EMISSIONS;
SOLAR OCCULTATION; THIN CLOUDS; 1ST YEAR; PART 1
AB The GHG-CCI project is one of several projects of the European Space Agency's (ESA) Climate Change Initiative (CCI). The goal of the CCI is to generate and deliver data sets of various satellite-derived Essential Climate Variables (ECVs) in line with GCOS (Global Climate Observing System) requirements. The "ECV Greenhouse Gases" (ECV GHG) is the global distribution of important climate relevant gases - atmospheric CO2 and CH4 - with a quality sufficient to obtain information on regional CO2 and CH4 sources and sinks. Two satellite instruments deliver the main input data for GHG-CCI: SCIAMACHY/ENVISAT and TANSO-FTS/GOSAT. The first order priority goal of GHG-CCI is the further development of retrieval algorithms for near-surface-sensitive column-averaged dry air mole fractions of CO2 and CH4, denoted XCO2 and XCH4, to meet the demanding user requirements. GHG-CCI focuses on four core data products: XCO2 from SCIAMACHY and TANSO and XCH4 from the same two sensors. For each of the four core data products at least two candidate retrieval algorithms have been independently further developed and the corresponding data products have been quality-assessed and inter-compared. This activity is referred to as "Round Robin" (RR) activity within the CCI. The main goal of the RR was to identify for each of the four core products which algorithms should be used to generate the Climate Research Data Package (CRDP). The CRDP will essentially be the first version of the ECV GHG. This manuscript gives an overview of the GHG-CCI RR and related activities. This comprises the establishment of the user requirements, the improvement of the candidate retrieval algorithms and comparisons with ground-based observations and models. The manuscript summarizes the final RR algorithm selection decision and its justification. Comparison with ground-based Total Carbon Column Observing Network (TCCON) data indicates that the "breakthrough" single measurement precision requirement has been met for SCIAMACHY and TANSO XCO2 (<3 ppm) and TANSO XCH4 (<17 ppb). The achieved relative accuracy for XCH4 is 3-15 ppb for SCIAMACHY and 2-8 ppb for TANSO depending on algorithm and time period. Meeting the 0.5 ppm systematic error requirement for XCO2 remains a challenge: approximately 1 ppm has been achieved at the validation sites but also larger differences have been found in regions remote from TCCON. More research is needed to identify the causes for the observed differences. In this context GHG-CCI suggests taking advantage of the ensemble of existing data products, for example, via the EnseMble Median Algorithm (EMMA). (C) 2013 Elsevier Inc All rights reserved.
C1 [Buchwitz, M.; Reuter, M.; Schneising, O.; Bovensmann, H.; Burrows, J. P.; Deutscher, N. M.; Heymann, J.; Noel, S.; Notholt, J.; Warneke, T.] Univ Bremen, Inst Environm Phys IUP, D-28334 Bremen, Germany.
[Boesch, H.] Univ Leicester, Leicester, Leics, England.
[Guerlet, S.; Aben, I.; Hasekamp, O. P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Dils, B.; De Maziere, M.] Belgian Inst Space Aeron BIRA, Brussels, Belgium.
[Lichtenberg, G.] Deutsch Zentrum Luft & Raumfahrt DLR, Oberpfaffenhofen, Germany.
[Armante, R.; Chedin, A.; Crevoisier, C. D.] Meteorol Dynam Lab, Palaiseau, France.
[Blumenstock, T.; Butz, A.; Hase, F.; Laeng, A.; Orphal, J.; Sussmann, R.; Stiller, G. P.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany.
[Blumenstock, T.; Butz, A.; Hase, F.; Laeng, A.; Orphal, J.; Sussmann, R.; Stiller, G. P.] Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany.
[Brunner, D.; Buchmann, B.; Popp, C.] Swiss Fed Labs Mat Sci & Technol Empa, Dubendorf, Switzerland.
[Chevallier, F.] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Bergamaschi, P.] European Commiss Joint Res Ctr EC JRC, Inst Environm & Sustainabil, Air & Climate Unit, Ispra, Italy.
[Frankenberg, C.; Crisp, D.] Jet Prop Lab, Pasadena, CA USA.
[Kaminski, T.; Scholze, M.] FastOpt GmbH, Hamburg, Germany.
[Scholze, M.] Univ Bristol, Bristol, Avon, England.
[Zehner, C.] European Space Agcy, ESRIN, Frascati, Italy.
[Bril, A.; Oshchepkov, S.; Yokota, T.; Yoshida, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Deutscher, N. M.; Griffith, D. W. T.] Univ Wollongong, Wollongong, NSW, Australia.
[Kuze, A.; Suto, H.] Japan Aerosp Explorat Agcy JAXA, Tsukuba, Ibaraki, Japan.
[O'Dell, C.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Sherlock, V.] Natl Inst Water & Atmospher Res NIWA, Lauder, New Zealand.
[Wennberg, P.; Wunch, D.] CALTECH, Pasadena, CA 91125 USA.
RP Buchwitz, M (reprint author), Univ Bremen, Inst Environm Phys IUP, FB1,Otto Hahn Allee 1, D-28334 Bremen, Germany.
EM Michael.Buchwitz@iup.physik.uni-bremen.de
RI Deutscher, Nicholas/E-3683-2015; Brunner, Dominik/A-1255-2009; Butz,
Andre/A-7024-2013; Boesch, Hartmut/G-6021-2012; Chevallier,
Frederic/E-9608-2016; Scholze, Marko/N-4573-2014; Reuter,
Maximilian/L-3752-2014; KUZE, AKIHIKO/J-2074-2016; Bovensmann,
Heinrich/P-4135-2016; Sussmann, Ralf/K-3999-2012; Frankenberg,
Christian/A-2944-2013; Notholt, Justus/P-4520-2016; Burrows,
John/B-6199-2014
OI Deutscher, Nicholas/0000-0002-2906-2577; Brunner,
Dominik/0000-0002-4007-6902; Butz, Andre/0000-0003-0593-1608;
Chevallier, Frederic/0000-0002-4327-3813; Scholze,
Marko/0000-0002-3474-5938; Reuter, Maximilian/0000-0001-9141-3895; KUZE,
AKIHIKO/0000-0001-5415-3377; Bovensmann, Heinrich/0000-0001-8882-4108;
Frankenberg, Christian/0000-0002-0546-5857; Notholt,
Justus/0000-0002-3324-885X; Burrows, John/0000-0002-6821-5580
FU ESA/ESRIN (GHG-CCI); EU (MACC-II) [283576]; DLR (SADOS); State of
Bremen; University of Bremen; NASA [NNX11AG01G, NAG5-12247,
NNG05-GD07G]; NASA Orbiting Carbon Observatory Program; DOE ARM program;
Australian Research Council [DP0879468, LP0562346]; EU project IMECC; EU
project GEOmon; Senate of Bremen
FX This work was primarily funded by ESA/ESRIN (GHG-CCI) but also received
funding from EU FP7 (grant agreement No. 283576, MACC-II), DLR (SADOS),
and the State and the University of Bremen. We thank the members of the
GOSAT Project (JAM, NIES, and Ministry of the Environment (MoE), Japan)
for providing GOSAT Level 1B and Level 2 data products (GOSAT RA1 PI
project CONSCIGO). The ACOS v2.9 data were produced by the ACOS/OCO-2
project at the Jet Propulsion Laboratory, California Institute of
Technology, and obtained from the ACOS/OCO-2 data archive maintained at
the NASA Goddard Earth Science Data and Information Services Center. We
thank NOAA for making available the CarbonTracker CO2 fields.
We also thank TCCON and related funding organizations (NASA grants
NNX11AG01G, NAG5-12247, NNG05-GD07G, NASA Orbiting Carbon Observatory
Program, DOE ARM program, the Australian Research Council, DP0879468 and
LP0562346, the EU projects IMECC and GEOmon, the Senate of Bremen). Last
but not least we would like to thank the two referees for helpful
comments.
NR 72
TC 20
Z9 20
U1 10
U2 80
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 JUN 1
PY 2015
VL 162
BP 344
EP 362
DI 10.1016/j.rse.2013.04.024
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CI8WI
UT WOS:000355052000024
ER
PT J
AU Gates, M
Stich, S
McDonald, M
Muirhead, B
Mazanek, D
Abell, P
Lopez, P
AF Gates, Michele
Stich, Steve
McDonald, Mark
Muirhead, Brian
Mazanek, Dan
Abell, Paul
Lopez, Pedro
TI The Asteroid Redirect Mission and sustainable human exploration
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Asteroid Redirect Mission; Human Space Exploration; Human exploration
AB We present the importance of the Asteroid Redirect Mission (ARM) in the context of the Global Exploration Roadmap and NASA's strategy for sustainable human exploration. We also provide status toward baseline of the ARM, including evolution of concept development based on internal NASA analysis and risk reduction, as well as external inputs received. This includes development of mission concept options, key trade studies, and analysis of drivers for both the robotic and crewed mission segments. Published by Elsevier Ltd. on behalf of IAA.
C1 [Gates, Michele] NASA Headquarters, Washington, DC 20546 USA.
[Stich, Steve; McDonald, Mark; Abell, Paul; Lopez, Pedro] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA.
[Muirhead, Brian] NASA, Jet Prop Lab, Washington, DC USA.
[Mazanek, Dan] NASA, Langley Res Ctr, Washington, DC USA.
RP Gates, M (reprint author), NASA Headquarters, Washington, DC 20546 USA.
EM michele.m.gates@nasa.gov; j.s.stich@nasa.gov; mark.a.mcdonald@nasa.gov;
brian.k.muirhead@nasa.gov; daniel.d.mazanek@nasa.gov;
paul.a.abell@nasa.gov; pedro.lopez-1@nasa.gov
NR 7
TC 2
Z9 2
U1 1
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 JUN-JUL
PY 2015
VL 111
BP 29
EP 36
DI 10.1016/j.actaastro.2015.01.025
PG 8
WC Engineering, Aerospace
SC Engineering
GA CI2NY
UT WOS:000354585500003
ER
PT J
AU Summerer, L
Wilcox, RE
Bechtel, R
Harbison, S
AF Summerer, L.
Wilcox, R. E.
Bechtel, R.
Harbison, S.
TI The International Safety Framework for nuclear power source applications
in outer space-Useful and substantial guidance
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Nuclear power sources; Safety; Safety framework; COPUOS; STSC
AB In 2009, the International Safety Framework for Nuclear Power Source Applications in Outer Space was adopted, following a multi-year process that involved all major space faring nations under the auspices of a partnership between the UN Committee on the Peaceful Uses of Outer Space and the International Atomic Energy Agency. The Safety Framework reflects an international consensus on best practices to achieve safety. Following the 1992 UN Principles Relevant to the Use of Nuclear Power Sources in Outer Space, it is the second attempt by the international community to draft guidance promoting the safety of applications of nuclear power sources in space missions.
NPS applications in space have unique safety considerations compared with terrestrial applications. Mission launch and outer space operational requirements impose size, mass and other space environment limitations not present for many terrestrial nuclear facilities. Potential accident conditions could expose nuclear power sources to extreme physical conditions.
The Safety Framework is structured to provide guidance for both the programmatic and technical aspects of safety. In addition to sections containing specific guidance for governments and for management, it contains technical guidance pertinent to the design, development and all mission phases of space NPS applications.
All sections of the Safety Framework contain elements directly relevant to engineers and space mission designers for missions involving space nuclear power sources. The challenge for organisations and engineers involved in the design and development processes of space nuclear power sources and applications is to implement the guidance provided in the Safety Framework by integrating it into the existing standard space mission infrastructure of design, development and operational requirements, practices and processes. This adds complexity to the standard space mission and launch approval processes.
The Safety Framework is deliberately generic to remain relevantly independent of technological progress, of national organisational setups and of space mission types. Implementing its guidance therefore leaves room for interpretation and adaptation. Relying on reported practices, we analyse the guidance particularly relevant to engineers and space mission designers. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Summerer, L.] European Space Agcy, Adv Concepts Team, NL-2201 AZ Noordwijk, Netherlands.
[Wilcox, R. E.] CALTECH, Jet Prop Lab, Project Support Off, Pasadena, CA 91109 USA.
[Bechtel, R.] US DOE, Off Space & Def Power Syst, Washington, DC 20585 USA.
[Harbison, S.] COPUOS STSC, NPS Working Grp, Vienna, Austria.
RP Summerer, L (reprint author), European Space Agcy, Adv Concepts Team, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
EM leopold.summerer@esa.int; rwilcox@jpl.nasa.gov;
ryan.bechtel@nuclear.energy.gov; SHarb67909@aol.com
OI Summerer, Leopold/0000-0001-7742-5216
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX The paper has greatly benefited from information shared within the
2010-2015 work-plan of the Working Group on Space Nuclear Power Sources
in Outer Space within the Scientific and Technical Subcommittee of the
Committee on the Peaceful Uses of Outer Space. The views expressed in
the paper are those of the authors and do not necessarily reflect the
view of any entities with which the authors may be affiliated. Part of
this work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 27
TC 1
Z9 1
U1 2
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 JUN-JUL
PY 2015
VL 111
BP 89
EP 101
DI 10.1016/j.actaastro.2015.02.007
PG 13
WC Engineering, Aerospace
SC Engineering
GA CI2NY
UT WOS:000354585500009
ER
PT J
AU Boll, NJ
Salazar, D
Stelter, CJ
Landis, GA
Colozza, AJ
AF Boll, Nathan J.
Salazar, Denise
Stelter, Christopher J.
Landis, Geoffrey A.
Colozza, Anthony J.
TI Venus high temperature atmospheric dropsonde and extreme-environment
seismometer (HADES)
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Venus; Lander; Geology; Atmosphere; Seismometer; High-temperature
ID FLUX RADIOMETER EXPERIMENT; PIONEER VENUS; MAGNETOMETER; ORBITER
AB The atmospheric composition and geologic structure of Venus have been identified by the US National Research Council's Decadal Survey for Planetary Science as priority targets for scientific exploration; however, the high temperature and pressure at the surface, along with the highly corrosive chemistry of the Venus atmosphere, present significant obstacles to spacecraft design that have severely limited past and proposed landed missions. Following the methodology of the NASA Innovative Advanced Concepts (NIAC) proposal regime and the Collaborative Modeling and Parametric Assessment of Space Systems (COMPASS) design protocol, this paper presents a conceptual study and initial feasibility analysis for a Discovery-class Venus lander capable of an extended-duration mission at ambient temperature and pressure, incorporating emerging technologies within the field of high temperature electronics in combination with novel configurations of proven, high Technology Readiness Level (TRL) systems. Radioisotope Thermal Power (RTG) systems and silicon carbide (SiC) communications and data handling are examined in detail, and various high-temperature instruments are proposed, including a seismometer and an advanced photodiode imager. The study combines this technological analysis with proposals for a descent instrument package and a relay orbiter to demonstrate the viability of an integrated atmospheric and in-situ geologic exploratory mission that differs from previous proposals by greatly reducing the mass, power requirements, and cost, while achieving important scientific goals. Published by Elsevier Ltd. on behalf of IAA.
C1 [Boll, Nathan J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Salazar, Denise] Univ Texas Austin, Austin, TX 78712 USA.
[Stelter, Christopher J.] NASA, Langley Res Ctr, Washington, DC USA.
[Landis, Geoffrey A.; Colozza, Anthony J.] NASA, John H Glenn Res Ctr, Washington, DC USA.
RP Boll, NJ (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM njboll@umich.edu; denise.salazar.1210@gmail.com;
christopherstelter@gmail.com; geoffrey.landis@nasa.gov;
anthony.j.colozza@nasa.gov
NR 39
TC 1
Z9 1
U1 2
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD JUN-JUL
PY 2015
VL 111
BP 146
EP 159
DI 10.1016/j.actaastro.2015.02.008
PG 14
WC Engineering, Aerospace
SC Engineering
GA CI2NY
UT WOS:000354585500013
ER
PT J
AU Barshi, I
AF Barshi, Immanuel
TI From Healy's Training Principles to Training Specifications: The Case of
the Comprehensive LOFT
SO AMERICAN JOURNAL OF PSYCHOLOGY
LA English
DT Article
ID LEARNING CURRICULA; MEDICAL-EDUCATION; INSTRUCTION; CHALLENGE; SCHOOL
AB Alice Healy has dedicated much of her work to questions of skill acquisition, retention, and transfer. In the process, she has come to identify numerous training principles that have been shown to promote the acquisition, retention, and transfer of knowledge and skills in laboratory studies. The goal of this article is to translate some of the training principles offered by Healy and her colleagues (Healy, Schneider, & Bourne, 2012) into real-world, practical training specifications for the particular context of pilot training at the airline level. The training approach described here suggests structuring all of airline pilot training as line-oriented flight training (LOFT), where the notion of "line" refers to the air-line drawn on a map between a departure airport and a destination airport.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Barshi, I (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA.
EM Immanuel.Barshi@nasa.gov
NR 37
TC 0
Z9 0
U1 2
U2 3
PU UNIV ILLINOIS PRESS
PI CHAMPAIGN
PA 1325 S OAK ST, CHAMPAIGN, IL 61820-6903 USA
SN 0002-9556
EI 1939-8298
J9 AM J PSYCHOL
JI Am. J. Psychol.
PD SUM
PY 2015
VL 128
IS 2
BP 219
EP 227
PG 9
WC Psychology, Multidisciplinary
SC Psychology
GA CI4WF
UT WOS:000354753900008
PM 26255441
ER
PT J
AU Lim, YK
AF Lim, Young-Kwon
TI The East Atlantic/West Russia (EA/WR) teleconnection in the North
Atlantic: climate impact and relation to Rossby wave propagation
SO CLIMATE DYNAMICS
LA English
DT Article
DE Teleconnection; EA/WR; Climate impact; Rossby wave; Stationary wave
model
ID ATMOSPHERIC CIRCULATION; GEOPOTENTIAL HEIGHT; HEMISPHERE WINTER; DECADAL
TRENDS; OSCILLATION; PATTERNS; PRECIPITATION; VARIABILITY; FREQUENCY;
BLOCKING
AB Large-scale winter teleconnection of the East Atlantic/West Russia (EA/WR) over the Atlantic and surrounding regions is examined in order to quantify its impacts on temperature and precipitation and identify the physical mechanisms responsible for its existence. A rotated empirical orthogonal function analysis of the upper-tropospheric monthly height field captures successfully the EA/WR pattern and its interannual variation, with the North Atlantic Oscillation (NAO) as the first mode. EA/WR's climate impact extends from eastern North America to Eurasia. The positive (negative) EA/WR produces positive (negative) temperature anomalies over the eastern US, western Europe and Russia east of Caspian Sea, with negative (positive) anomalies over eastern Canada, eastern Europe including Ural Mountains, northeastern Africa and the Middle East. These anomalies are largely explained by lower-tropospheric temperature advections. Positive (negative) precipitation anomalies are found over the mid-latitude Atlantic and central Russia around similar to 60 degrees anomaly is dominant. Eastern Canada and western Europe including the Mediterranean region are characterized by negative (positive) precipitation anomalies. The EA/WR is found to be closely associated with Rossby wave propagation. Wave activity fluxes show that it is strongly tied to large-scale stationary waves. Furthermore, a stationary wave model (SWM) forced with vorticity transients in the mid-latitude Atlantic (similar to 40 degrees N) or diabatic heat source over the subtropical Atlantic near the Caribbean Sea produces well-organized EA/WR-like wave patterns, respectively. Sensitivity tests with the SWM indicate enhancement of EA/WR-like blocking over west of Scandinavia when the mean state is modified to have a positive NAO component that enhances upper-level westerlies between 40 and 60 degrees N.
C1 NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, IM Syst Grp,Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Lim, YK (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, IM Syst Grp,Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM Young-Kwon.Lim@nasa.gov
NR 35
TC 9
Z9 9
U1 2
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JUN
PY 2015
VL 44
IS 11-12
BP 3211
EP 3222
DI 10.1007/s00382-014-2381-4
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI4GH
UT WOS:000354705700019
ER
PT J
AU Wild, M
Folini, D
Hakuba, MZ
Schar, C
Seneviratne, SI
Kato, S
Rutan, D
Ammann, C
Wood, EF
Konig-Langlo, G
AF Wild, Martin
Folini, Doris
Hakuba, Maria Z.
Schaer, Christoph
Seneviratne, Sonia I.
Kato, Seiji
Rutan, David
Ammann, Christof
Wood, Eric F.
Koenig-Langlo, Gert
TI The energy balance over land and oceans: an assessment based on direct
observations and CMIP5 climate models
SO CLIMATE DYNAMICS
LA English
DT Article
DE Global energy balance; Radiation budget; Global climate models; Surface
and satellite observations; CMIP5
ID GENERAL-CIRCULATION MODELS; DOWNWARD LONGWAVE RADIATION; ANNUAL CYCLE;
SATELLITE-OBSERVATIONS; OBSERVING SYSTEM; SURFACE; BUDGET; ATMOSPHERE;
SHORTWAVE; TRANSPORTS
AB The energy budgets over land and oceans are still afflicted with considerable uncertainties, despite their key importance for terrestrial and maritime climates. We evaluate these budgets as represented in 43 CMIP5 climate models with direct observations from both surface and space and identify substantial biases, particularly in the surface fluxes of downward solar and thermal radiation. These flux biases in the various models are then linearly related to their respective land and ocean means to infer best estimates for present day downward solar and thermal radiation over land and oceans. Over land, where most direct observations are available to constrain the surface fluxes, we obtain 184 and 306 Wm(-2) for solar and thermal downward radiation, respectively. Over oceans, with weaker observational constraints, corresponding estimates are around 185 and 356 Wm(-2). Considering additionallysurface albedo and emissivity, we infer a surface absorbed solar and net thermal radiation of 136 and -66 Wm(-2) over land, and 170 and -53 Wm(-2) over oceans, respectively. The surface net radiation is thus estimated at 70 Wm(-2) over land and 117 Wm(-2) over oceans, which may impose additional constraints on the poorly known sensible/latent heat flux magnitudes, estimated here near 32/38 Wm(-2) over land, and 16/100 Wm(-2) over oceans. Estimated uncertainties are on the order of 10 and 5 Wm(-2) for most surface and TOA fluxes, respectively. By combining these surface budgets with satellite-determined TOA budgets we quantify the atmospheric energy budgets as residuals (including ocean to land transports), and revisit the global mean energy balance.
C1 [Wild, Martin; Folini, Doris; Hakuba, Maria Z.; Schaer, Christoph; Seneviratne, Sonia I.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Kato, Seiji; Rutan, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Ammann, Christof] Res Stn Agroscope, Climate & Air Pollut Grp, CH-8046 Zurich, Switzerland.
[Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Koenig-Langlo, Gert] Alfred Wegener Inst, D-27570 Bremerhaven, Germany.
RP Wild, M (reprint author), Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM martin.wild@env.ethz.ch
RI Seneviratne, Sonia/G-8761-2011; Schar, Christoph/A-1033-2008; Wild,
Martin/J-8977-2012; Konig-Langlo, Gert/K-5048-2012
OI Seneviratne, Sonia/0000-0001-9528-2917; Schar,
Christoph/0000-0002-4171-1613; Konig-Langlo, Gert/0000-0002-6100-4107
FU Swiss National Science Foundation [135395]; National Centre for
Competence in Climate Research (NCCR Climate) of the Swiss National
Science Foundation as part of the NCCR Project HyClim; Office of
Science, U.S. Department of Energy
FX This study got support from the Swiss National Science Foundation Grant
No. 135395 "Towards an improved understanding of the global energy
balance: absorption of solar radiation" and from the National Centre for
Competence in Climate Research (NCCR Climate) of the Swiss National
Science Foundation as part of the NCCR Project HyClim. We highly
appreciate the valuable review comments of Dr. Kevin Trenberth on this
manuscript. We are grateful to Prof. Atsumu Ohmura for numerous
discussions and for his leadership in the establishment of GEBA and
BSRN. We would like to thank Dr. Guido Mueller for processing the BSRN
data, Dr. Urs Beyerle and Prof. Reto Knutti for their efforts to
download the immense CMIP5 dataset and Dr. Gabriela Schaepmann-Strub for
advice on the albedo issues. We highly acknowledge Barbara Schar for the
design of the global energy balance figures, and an anonymous reviewer
for useful comments. We acknowledge the international modeling groups
for providing their data for analysis, the Program for Climate Model
Diagnosis and Intercomparison (PCMDI) for collecting and archiving the
model data, the JSC/CLIVAR Working Group on Coupled Modeling (WGCM) and
their Coupled Model Intercomparison Project (CMIP) and Climate
Simulation Panel for organizing the model data analysis activity, and
the IPCC WG1 TSU for technical support. The IPCC Data Archive at
Lawrence Livermore National Laboratory is supported by the Office of
Science, U.S. Department of Energy.
NR 74
TC 33
Z9 33
U1 5
U2 45
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JUN
PY 2015
VL 44
IS 11-12
BP 3393
EP 3429
DI 10.1007/s00382-014-2430-z
PG 37
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI4GH
UT WOS:000354705700029
ER
PT J
AU Obaza, A
Hoffman, R
Clausing, R
AF Obaza, A.
Hoffman, R.
Clausing, R.
TI Long-term stability of eelgrass fish assemblages in two highly developed
coastal estuaries
SO FISHERIES MANAGEMENT AND ECOLOGY
LA English
DT Article
DE eelgrass; estuary; fish assemblage; stability; urbanisation
ID SOUTHERN-CALIFORNIA; DIEL VARIATION; ENVIRONMENTAL-INFLUENCES; HABITAT
UTILIZATION; COMMUNITY ECOLOGY; SHALLOW SEAGRASS; NURSERY FUNCTION;
ZOSTERA-MARINA; PREDATION RISK; CLIMATE-CHANGE
AB Changes in fish assemblages were tracked in representative eelgrass (Zostera marina L.) beds within two estuaries on the urbanised coast of southern California, USA, San Diego Bay and Mission Bay, from 1987 to 2010. Assemblages were sampled twice yearly (spring and summer) at day and night using beach seines. Assemblage stability was examined over time along with changes in assemblage structure across time of day and season, including the influence of temporally variable abiotic variables. Only the occasionally occurring fish, those present in <70% of samples, in Mission Bay appeared to be shifting to a new assemblage. Although season and sampling time significantly affected assemblages, correlations with abiotic factors were low. Given the long history of urban development of these estuaries, community shifts may have occurred prior to the onset of sampling, giving the appearance of stability. Alternatively, eelgrass habitat may be providing a refuge from long-term disturbances.
C1 [Obaza, A.] Ocean Associates Inc, Arlington, VA USA.
[Obaza, A.] Natl Marine Fisheries Serv, West Coast Reg Off, Long Beach, CA 90802 USA.
[Hoffman, R.] Natl Marine Fisheries Serv, Southwest Reg Off, Long Beach, CA 90802 USA.
[Clausing, R.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
RP Obaza, A (reprint author), Natl Marine Fisheries Serv, West Coast Reg Off, 501 West Ocean Blvd,Suite 4200, Long Beach, CA 90802 USA.
EM Adam.Obaza@noaa.gov
NR 88
TC 2
Z9 2
U1 1
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0969-997X
EI 1365-2400
J9 FISHERIES MANAG ECOL
JI Fisheries Manag. Ecol.
PD JUN
PY 2015
VL 22
IS 3
BP 224
EP 238
DI 10.1111/fme.12119
PG 15
WC Fisheries
SC Fisheries
GA CI1GR
UT WOS:000354492100004
ER
PT J
AU Stevenazzi, S
Masetti, M
Nghiem, SV
Sorichetta, A
AF Stevenazzi, Stefania
Masetti, Marco
Nghiem, Son V.
Sorichetta, Alessandro
TI Groundwater vulnerability maps derived from a time-dependent method
using satellite scatterometer data
SO HYDROGEOLOGY JOURNAL
LA English
DT Article
DE Vulnerability mapping; Urban areas; Remote sensing; Nitrate; Italy
ID UNITED-STATES; AQUIFER SUSCEPTIBILITY; NITRATE CONTAMINATION;
PROBABILITY; AUSTRALIA; AREAS; WATER; GIS
AB Introducing the time variable in groundwater vulnerability assessment is an innovative approach to study the evolution of contamination by non-point sources and to forecast future trends. This requires a determination of the relationship between temporal changes in groundwater contamination and in land use. Such effort will enable breakthrough advances in mapping hazardous areas, and in assessing the efficacy of land-use planning for groundwater protection. Through a Bayesian spatial statistical approach, time-dependent vulnerability maps are derived by using hydrogeological variables together with three different time-dependent datasets: population density, high-resolution urban survey, and satellite QuikSCAT (QSCAT) data processed with the innovative dense sampling method (DSM). This approach is demonstrated extensively over the Po Plain in Lombardy region (northern Italy). Calibrated and validated maps show physically consistent relations between the hydrogeological variables and nitrate trends. The results indicate that changes of urban nitrate sources are strongly related to groundwater deterioration. Among the different datasets, QSCAT-DSM is proven to be the most efficient dataset to represent urban nitrate sources of contamination, with major advantages: a worldwide coverage, a continuous decadal data collection, and an adequate resolution without spatial gaps. This study presents a successful approach that, for the first time, allows the inclusion of the time dimension in groundwater vulnerability assessment by using innovative satellite remote sensing data for quantitative statistical analyses of groundwater quality changes.
C1 [Stevenazzi, Stefania; Masetti, Marco] Univ Milan, Dipartimento Sci Terra A Desio, I-20133 Milan, Italy.
[Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sorichetta, Alessandro] Univ Southampton, Geog & Environm, Southampton SO17 1BJ, Hants, England.
RP Stevenazzi, S (reprint author), Univ Milan, Dipartimento Sci Terra A Desio, Via Luigi Mangiagalli 34, I-20133 Milan, Italy.
EM stefania.stevenazzi@unimi.it; marco.masetti@unimi.it;
son.v.nghiem@jpl.nasa.gov; A.Sorichetta@soton.ac.uk
RI Masetti, Marco/N-6823-2013
FU National Aeronautics and Space Administration (NASA) Land-Cover and
Land-Use Change (LCLUC) Program; Bill & Melinda Gates Foundation
[OPP1106427, 1032350]
FX The research carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, was supported by the National
Aeronautics and Space Administration (NASA) Land-Cover and Land-Use
Change (LCLUC) Program. We thank Gregory Neumann of JPL for processing
satellite QSCAT-DSM data. The research carried out at the Department of
Geography and Environment, University of Southampton (UK), was done in
the framework of the WorldPop Project (www.worldpop.org.uk) and
supported by funding from the Bill & Melinda Gates Foundation
(OPP1106427, 1032350).
NR 51
TC 4
Z9 4
U1 2
U2 18
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1431-2174
EI 1435-0157
J9 HYDROGEOL J
JI Hydrogeol. J.
PD JUN
PY 2015
VL 23
IS 4
BP 631
EP 647
DI 10.1007/s10040-015-1236-3
PG 17
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA CI3AW
UT WOS:000354620800003
ER
PT J
AU Petropoulos, GP
Ireland, G
Cass, A
Srivastava, PK
AF Petropoulos, George P.
Ireland, Gareth
Cass, Alexander
Srivastava, Prashant K.
TI Performance Assessment of the SEVIRI Evapotranspiration Operational
Product: Results Over Diverse Mediterranean Ecosystems
SO IEEE SENSORS JOURNAL
LA English
DT Article
DE Evapotranspiration; Earth Observation; operational products; SEVIRI;
validation; Europe
ID LAND-SURFACE MODEL; ENERGY-BALANCE CLOSURE; EDDY-COVARIANCE; VEGETATION
INDEX; SOIL-MOISTURE; VALIDATION; MODIS; SATELLITE; AFRICA; ALGORITHM
AB Evapotranspiration (ET) is an important variable in weather systems and hydrometeorological modeling. In this paper, an extensive validation was carried out on the spinning enhanced visible and infrared imager (SEVIRI) ET operational product, evaluating its accuracy at selected European sites. Validation was performed through comparisons with in-situ eddy covariance measurements belonging to the CarboEurope IP network. Comparisons were performed for selected cloud-free days with a satisfactory energy balance ratio in 2011. A total of nine sites covering six land covers were used in validating the ET retrieval accuracy from the operational product. A series of statistical metrics was computed to evaluate the agreement, which also included explored the variability of site characteristics and influence of land cover on ET performances. Overall, a good agreement was reported between the satellite-derived ET estimates and the ground measurements (d-index = 0.755, root mean square deviation (RMSD) = 0.107 mm h(-1)). A minor negative bias of -0.015 mm h(-1) suggested only slight underestimation of the in-situ data. In terms of land cover, the highest agreement in ET was reported for the olive orchards and open shrubland sites (d-index = 0.893/0.867, RMSD = 0.041/0.050 mm h(-1)). A systematic ET underestimation by SEVIRI was found for all land cover types. Results of this study are largely in agreement to previous analogous validation studies of the product. Our findings support the potential value of the SEVIRI ET product for regional to mesoscale studies and practical applications. The latter is of particular importance for water limiting environments such as those found in the Mediterranean basin, as accurate information on ET rates can provide tremendous support in sustainable water resource management as well as policy and decision making.
C1 [Petropoulos, George P.; Ireland, Gareth; Cass, Alexander] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3FL, Dyfed, Wales.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Petropoulos, GP (reprint author), Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3FL, Dyfed, Wales.
EM petropoulos.george@gmail.com; gai2@aber.ac.uk; alc32@aber.ac.uk;
prashant.k.srivastava@nasa.gov
RI Petropoulos, George/F-2384-2013
OI Petropoulos, George/0000-0003-1442-1423
FU European Commission Marie Curie Re-Integration Gran TRANSFORM-EO; High
Performance Computing Facilities of Wales PREMIER-EO projects
FX The work of G. Petropoulos's contribution was supported by the European
Commission Marie Curie Re-Integration Gran TRANSFORM-EO and the High
Performance Computing Facilities of Wales PREMIER-EO projects. The
associate editor coordinating the review of this paper and approving it
for publication was Prof. Octavian Postolache. (Corresponding author:
George P. Petropoulos.)
NR 41
TC 5
Z9 5
U1 2
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1530-437X
EI 1558-1748
J9 IEEE SENS J
JI IEEE Sens. J.
PD JUN
PY 2015
VL 15
IS 6
BP 3412
EP 3423
DI 10.1109/JSEN.2015.2390031
PG 12
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Physics, Applied
SC Engineering; Instruments & Instrumentation; Physics
GA CI7OV
UT WOS:000354954500010
ER
PT J
AU Stevenson, A
Cray, JA
Williams, JP
Santos, R
Sahay, R
Neuenkirchen, N
McClure, CD
Grant, IR
Houghton, JDR
Quinn, JP
Timson, DJ
Patil, SV
Singhal, RS
Anton, J
Dijksterhuis, J
Hocking, AD
Lievens, B
Rangel, DEN
Voytek, MA
Gunde-Cimerman, N
Oren, A
Timmis, KN
McGenity, TJ
Hallsworth, JE
AF Stevenson, Andrew
Cray, Jonathan A.
Williams, Jim P.
Santos, Ricardo
Sahay, Richa
Neuenkirchen, Nils
McClure, Colin D.
Grant, Irene R.
Houghton, Jonathan D. R.
Quinn, John P.
Timson, David J.
Patil, Satish V.
Singhal, Rekha S.
Anton, Josefa
Dijksterhuis, Jan
Hocking, Ailsa D.
Lievens, Bart
Rangel, Drauzio E. N.
Voytek, Mary A.
Gunde-Cimerman, Nina
Oren, Aharon
Timmis, Kenneth N.
McGenity, Terry J.
Hallsworth, John E.
TI Is there a common water-activity limit for the three domains of life?
SO ISME JOURNAL
LA English
DT Article
ID EXTREMELY HALOPHILIC BACTERIUM; SP-NOV.; GEN. NOV.; XEROPHILIC FUNGI;
SALINIBACTER-RUBER; TETRAGENOCOCCUS-HALOPHILUS; ENTOMOPATHOGENIC FUNGI;
TEMPERATURE RELATIONS; EMENDED DESCRIPTION; COMPATIBLE SOLUTES
AB Archaea and Bacteria constitute a majority of life systems on Earth but have long been considered inferior to Eukarya in terms of solute tolerance. Whereas the most halophilic prokaryotes are known for an ability to multiply at saturated NaCl (water activity (a(w)) 0.755) some xerophilic fungi can germinate, usually at high-sugar concentrations, at values as low as 0.650-0.605 a(w). Here, we present evidence that halophilic prokayotes can grow down to water activities of <0.755 for Halanaerobium lacusrosei (0.748), Halobacterium strain 004.1 (0.728), Halobacterium sp. NRC-1 and Halococcus morrhuae (0.717), Haloquadratum walsbyi (0.709), Halococcus salifodinae (0.693), Halobacterium noricense (0.687), Natrinema pallidum (0.681) and haloarchaeal strains GN-2 and GN-5 (0.635 a(w)). Furthermore, extrapolation of growth curves (prone to giving conservative estimates) indicated theoretical minima down to 0.611 a(w) for extreme, obligately halophilic Archaea and Bacteria. These were compared with minima for the most solute-tolerant Bacteria in high-sugar (or other non-saline) media (Mycobacterium spp., Tetragenococcus halophilus, Saccharibacter floricola, Staphylococcus aureus and so on) and eukaryotic microbes in saline (Wallemia spp., Basipetospora halophila, Dunaliella spp. and so on) and high-sugar substrates (for example, Xeromyces bisporus, Zygosaccharomyces rouxii, Aspergillus and Eurotium spp.). We also manipulated the balance of chaotropic and kosmotropic stressors for the extreme, xerophilic fungi Aspergillus penicilloides and X. bisporus and, via this approach, their established water-activity limits for mycelial growth (similar to 0.65) were reduced to 0.640. Furthermore, extrapolations indicated theoretical limits of 0.632 and 0.636 aw for A. penicilloides and X. bisporus, respectively. Collectively, these findings suggest that there is a common water-activity limit that is determined by physicochemical constraints for the three domains of life.
C1 [Stevenson, Andrew; Cray, Jonathan A.; Williams, Jim P.; Santos, Ricardo; McClure, Colin D.; Grant, Irene R.; Houghton, Jonathan D. R.; Quinn, John P.; Timson, David J.; Hallsworth, John E.] Queens Univ Belfast, Sch Biol Sci, MBC, Inst Global Food Secur, Belfast BT9 7BL, Antrim, North Ireland.
[Santos, Ricardo] Inst Super Tecn, Lab Anal, Lisbon, Portugal.
[Sahay, Richa; Neuenkirchen, Nils; Timmis, Kenneth N.; McGenity, Terry J.; Hallsworth, John E.] Univ Essex, Sch Biol Sci, Colchester CO4 3SQ, Essex, England.
[Patil, Satish V.] North Maharashtra Univ, Sch Life Sci, Jalgaon, Maharashtra, India.
[Singhal, Rekha S.] Inst Chem Technol, Dept Food Engn & Technol, Mumbai, Maharashtra, India.
[Anton, Josefa] Univ Alicante, Dept Physiol Genet & Microbiol, E-03080 Alicante, Spain.
[Dijksterhuis, Jan] CBS Fungal Biodivers Ctr, Utrecht, Netherlands.
[Hocking, Ailsa D.] CSIRO Food & Nutr, N Ryde, NSW, Australia.
[Lievens, Bart] Scientia Terrae Res Inst, Microbial Ecol & Biorat Control, St Katelijne Waver, Belgium.
[Rangel, Drauzio E. N.] Univ Vale Paraiba, Inst Pesquisa Desenvolvimento, Sao Jose dos Campos, SP, Brazil.
[Voytek, Mary A.] NASA Headquarters, Washington, DC USA.
[Gunde-Cimerman, Nina] Univ Ljubljana, Biotech Fac, Ljubljana, Slovenia.
[Oren, Aharon] Hebrew Univ Jerusalem, Alexander Silberman Inst Life Sci, Dept Plant & Environm Sci, Jerusalem, Israel.
[Timmis, Kenneth N.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Microbiol, D-38106 Braunschweig, Germany.
RP Hallsworth, JE (reprint author), Queens Univ Belfast, Sch Biol Sci, 97 Lisburn Rd, Belfast BT9 7BL, Antrim, North Ireland.
EM j.hallsworth@qub.ac.uk
RI Rangel, Drauzio/C-2711-2012; Hallsworth, John/K-7876-2013;
OI Rangel, Drauzio/0000-0001-7188-100X; McGenity,
Terence/0000-0002-1497-8822; Timson, David/0000-0002-0985-8818
FU Research (Northern Ireland); Enterprise Directorate of Queen's
University Belfast; Department of Agriculture and Rural Development
(Northern Ireland); Department for Employment and Learning (Northern
Ireland); Biotechnology and Biological Sciences Research Council (BBSRC,
UK) [BBF/003471/1, BBF/00351X/1]; Beaufort Marine Research Award for
Marine Biodiscovery; Marine Institute, Ireland; State of Sao Paulo
Research Foundation (FAPESP) [2010/06374-1]
FX We are grateful to Peter N Golyshin and Olga V Golyshina (Bangor
University, UK), Barbara J Javor (Southwest Fisheries Science Center,
USA) and Tom L Kieft (New Mexico Tech., USA) for fruitful discussions,
and to Helga Stan-Lotter (University of Salzburg, Austria) for providing
Halobacterium sp. NRC-1. Funding was received from the Research
(Northern Ireland) and Enterprise Directorate of Queen's University
Belfast; Department of Agriculture and Rural Development and the
Department for Employment and Learning (Northern Ireland); Biotechnology
and Biological Sciences Research Council (BBSRC, UK) Projects
BBF/003471/1 and BBF/00351X/1; and the Beaufort Marine Research Award
for Marine Biodiscovery that is carried out under the Sea Change
Strategy and the Strategy for Science Technology and Innovation
(2006-2013), with the support of the Marine Institute, Ireland. This
work was also supported by the State of Sao Paulo Research Foundation
(FAPESP) via a grant awarded to Drauzio EN Rangel (#2010/06374-1).
NR 147
TC 33
Z9 33
U1 11
U2 64
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1751-7362
EI 1751-7370
J9 ISME J
JI ISME J.
PD JUN
PY 2015
VL 9
IS 6
BP 1333
EP 1351
DI 10.1038/ismej.2014.219
PG 19
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA CI5HR
UT WOS:000354786700006
PM 25500507
ER
PT J
AU Lievens, H
Al Bitar, A
Verhoest, NEC
Cabot, F
De Lannoy, GJM
Drusch, M
Dumedah, G
Franssen, HJH
Kerr, Y
Tomer, SK
Martens, B
Merlin, O
Pan, M
van den Berg, MJ
Vereecken, H
Walker, JP
Wood, EF
Pauwels, VRN
AF Lievens, H.
Al Bitar, A.
Verhoest, N. E. C.
Cabot, F.
De Lannoy, G. J. M.
Drusch, M.
Dumedah, G.
Franssen, H-J. Hendricks
Kerr, Y.
Tomer, S. K.
Martens, B.
Merlin, O.
Pan, M.
van den Berg, M. J.
Vereecken, H.
Walker, J. P.
Wood, E. F.
Pauwels, V. R. N.
TI Optimization of a Radiative Transfer Forward Operator for Simulating
SMOS Brightness Temperatures over the Upper Mississippi Basin
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SURFACE SOIL-MOISTURE; ASSIMILATION SYSTEM NLDAS; INTEGRATED FORECAST
SYSTEM; BAND MICROWAVE EMISSION; TRANSFER MODEL; DISCHARGE PREDICTIONS;
RETRIEVAL ALGORITHM; GLOBAL SIMULATION; UNITED-STATES; LAND
AB The Soil Moisture Ocean Salinity (SMOS) satellite mission routinely provides global multiangular observations of brightness temperature TB at both horizontal and vertical polarization with a 3-day repeat period. The assimilation of such data into a land surface model (LSM) may improve the skill of operational flood forecasts through an improved estimation of soil moisture SM. To accommodate for the direct assimilation of the SMOS TB data, the LSM needs to be coupled with a radiative transfer model (RTM), serving as a forward operator for the simulation of multiangular and multipolarization top of the atmosphere TBs. This study investigates the use of the Variable Infiltration Capacity model coupled with the Community Microwave Emission Modelling Platform for simulating SMOS TB observations over the upper Mississippi basin, United States. For a period of 2 years (2010-11), a comparison between SMOS TBs and simulations with literature-based RTM parameters reveals a basin-averaged bias of 30 K. Therefore, time series of SMOS TB observations are used to investigate ways for mitigating these large biases. Specifically, the study demonstrates the impact of the LSM soil moisture climatology in the magnitude of TB biases. After cumulative distribution function matching the SM climatology of the LSM to SMOS retrievals, the average bias decreases from 30 K to less than 5 K. Further improvements can be made through calibration of RTM parameters related to the modeling of surface roughness and vegetation. Consequently, it can be concluded that SM rescaling and RTM optimization are efficient means for mitigating biases and form a necessary preparatory step for data assimilation.
C1 [Lievens, H.; Verhoest, N. E. C.; Martens, B.; van den Berg, M. J.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Al Bitar, A.; Cabot, F.; Kerr, Y.; Tomer, S. K.; Merlin, O.] Ctr Etud Spatiales Biosphere, Toulouse, France.
[De Lannoy, G. J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Drusch, M.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Dumedah, G.; Walker, J. P.; Pauwels, V. R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia.
[Franssen, H-J. Hendricks; Vereecken, H.] Forschungszentrum Julich, D-52425 Julich, Germany.
[Pan, M.; Wood, E. F.] Princeton Univ, Land Surface Hydrol Grp, Princeton, NJ 08544 USA.
RP Lievens, H (reprint author), Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium.
EM hans.lievens@ugent.be
RI Verhoest, Niko/C-9726-2010; Pan, Ming/B-6841-2011;
OI Verhoest, Niko/0000-0003-4116-8881; Pan, Ming/0000-0003-3350-8719;
Hendricks-Franssen, Harrie-Jan/0000-0002-0004-8114; Pauwels,
Valentijn/0000-0002-1290-9313; Martens, Brecht/0000-0002-7368-7953; Al
Bitar, Ahmad/0000-0002-1756-1096
FU Belgian Science Policy (BELSPO) [SR/00/302]; CNES Terre, Ocean, Surfaces
continentales, Atmosphere (TOSCA) program; Australian Research Council
FX The work has been performed in the framework of the ESA-STSE project
"SMOS + Hydrology Study" and was partly funded through project SR/00/302
(Hydras+) financed by the Belgian Science Policy (BELSPO), and the CNES
Terre, Ocean, Surfaces continentales, Atmosphere (TOSCA) program.
Furthermore, we would like to acknowledge the Julich Supercomputing
Center for granting computation time on JUROPA. Hans Lievens is a
postdoctoral research fellow of the Research Foundation Flanders (FWO).
Valentijn Pauwels is currently a Future Fellow funded by the Australian
Research Council.
NR 74
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U1 4
U2 14
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 JUN
PY 2015
VL 16
IS 3
BP 1109
EP 1134
DI 10.1175/JHM-D-14-0052.1
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9YI
UT WOS:000355126500010
ER
PT J
AU Lawston, PM
Santanello, JA
Zaitchik, BF
Rodell, M
AF Lawston, Patricia M.
Santanello, Joseph A., Jr.
Zaitchik, Benjamin F.
Rodell, Matthew
TI Impact of Irrigation Methods on Land Surface Model Spinup and
Initialization of WRF Forecasts
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SOUTHERN GREAT-PLAINS; ATMOSPHERIC RESPONSE; UNITED-STATES; WATER;
PRECIPITATION; FLUXES; TEMPERATURE; CLIMATE; AGRICULTURE; FRAMEWORK
AB In the United States, irrigation represents the largest consumptive use of freshwater and accounts for approximately one-third of total water usage. Irrigation impacts soil moisture and can ultimately influence clouds and precipitation through land-planetary boundary layer (PBL) coupling processes. This study utilizes NASA's Land Information System (LIS) and the NASA Unified Weather Research and Forecasting Model (NU-WRF) framework to investigate the effects of drip, flood, and sprinkler irrigation methods on land-atmosphere interactions, including land-PBL coupling and feedbacks at the local scale. To initialize 2-day, 1-km WRF forecasts over the central Great Plains in a drier-than-normal (2006) and a wetter-than-normal year (2008), 5-yr irrigated LIS spinups were used. The offline and coupled simulation results show that regional irrigation impacts are sensitive to time, space, and method and that irrigation cools and moistens the surface over and downwind of irrigated areas, ultimately resulting in both positive and negative feedbacks on the PBL depending on the time of day and background climate conditions. Furthermore, the results portray the importance of both irrigation method physics and correct representation of several key components of land surface models, including accurate and timely land-cover and crop-type classification, phenology (greenness), and soil moisture anomalies (through a land surface model spinup) in coupled prediction models.
C1 [Lawston, Patricia M.] Univ Delaware, Dept Geog, Newark, DE 19716 USA.
[Lawston, Patricia M.; Santanello, Joseph A., Jr.; Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Lawston, PM (reprint author), Univ Delaware, Dept Geog, 216 Pearson Hall, Newark, DE 19716 USA.
EM pmlawsto@udel.edu
RI Rodell, Matthew/E-4946-2012; Santanello, Joseph/D-4438-2012
OI Rodell, Matthew/0000-0003-0106-7437; Santanello,
Joseph/0000-0002-0807-6590
FU NASA Energy and Water Cycle Study (NEWS); LIS-WRF and LVT
FX Much of this work was conducted as part of the NASA GSFC Intern Program
and supported by the NASA Energy and Water Cycle Study (NEWS). Many
thanks to the LIS team, especially Sujay Kumar, for providing feedback
and support with LIS-WRF and LVT, and to Hiroko Beaudoing, Kristi
Arsenault, and Eric Hunt for sharing their knowledge of irrigation and
land-cover datasets. The MET analysis included data from the Research
Data Archive (RDA; available via http://rda.ucar.edu/datasets/ds337.0),
which is maintained by the Computational and Information Systems
Laboratory (CISL) at the National Center for Atmospheric Research
(NCAR).
NR 57
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U1 0
U2 14
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 JUN
PY 2015
VL 16
IS 3
BP 1135
EP 1154
DI 10.1175/JHM-D-14-0203.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9YI
UT WOS:000355126500011
ER
PT J
AU Demir, I
Conover, H
Krajewski, WF
Seo, BC
Goska, R
He, YB
McEniry, MF
Graves, SJ
Petersen, W
AF Demir, Ibrahim
Conover, Helen
Krajewski, Witold F.
Seo, Bong-Chul
Goska, Radoslaw
He, Yubin
McEniry, Michael F.
Graves, Sara J.
Petersen, Walter
TI Data-Enabled Field Experiment Planning, Management, and Research Using
Cyberinfrastructure
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID RADAR-RAINFALL; BEAM BLOCKAGE; UNIDATA; ACCESS; FLOOD; GIS
AB In the spring of 2013, NASA conducted a field campaign known as Iowa Flood Studies (IFloodS) as part of the Ground Validation (GV) program for the Global Precipitation Measurement (GPM) mission. The purpose of IFloodS was to enhance the understanding of flood-related, space-based observations of precipitation processes in events that transpire worldwide. NASA used a number of scientific instruments such as ground-based weather radars, rain and soil moisture gauges, stream gauges, and disdrometers to monitor rainfall events in Iowa. This article presents the cyberinfrastructure tools and systems that supported the planning, reporting, and management of the field campaign and that allow these data and models to be accessed, evaluated, and shared for research. The authors describe the collaborative informatics tools, which are suitable for the network design, that were used to select the locations in which to place the instruments. How the authors used information technology tools for instrument monitoring, data acquisition, and visualizations after deploying the instruments and how they used a different set of tools to support data analysis and modeling after the campaign are also explained. All data collected during the campaign are available through the Global Hydrology Resource Center (GHRC), a NASA Distributed Active Archive Center (DAAC).
C1 [Demir, Ibrahim; Krajewski, Witold F.; Seo, Bong-Chul; Goska, Radoslaw] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA USA.
[Conover, Helen; He, Yubin; McEniry, Michael F.; Graves, Sara J.] Univ Alabama, Informat Technol & Syst Ctr, Huntsville, AL 35899 USA.
[Petersen, Walter] NASA, Goddard Space Flight Ctr, Off Field Support, Wallops Isl, VA 23337 USA.
RP Demir, I (reprint author), IIHR Hydrosci & Engn, Iowa Flood Ctr, 207 C Maxwell Stanley Hydraul Lab, Iowa City, IA 52242 USA.
EM ibrahim-demir@uiowa.edu
RI Measurement, Global/C-4698-2015
FU NASA's Cooperative Agreement [NNM11AA01A, NNX13AD83G, NNX13AG94G]; Iowa
Flood Center; National Science Foundation [1327830]; NASA GPM program;
Precipitation Measurement Mission program
FX Funding for this work was provided by NASA's Cooperative Agreement
NNM11AA01A and Grants NNX13AD83G and NNX13AG94G, the Iowa Flood Center,
and the National Science Foundation Award 1327830. We also gratefully
acknowledge funding and management support from the NASA GPM and
Precipitation Measurement Mission programs.
NR 27
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U1 0
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JUN
PY 2015
VL 16
IS 3
BP 1155
EP 1170
DI 10.1175/JHM-D-14-0163.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9YI
UT WOS:000355126500012
ER
PT J
AU Bringi, VN
Tolstoy, L
Thurai, M
Petersen, WA
AF Bringi, V. N.
Tolstoy, L.
Thurai, M.
Petersen, W. A.
TI Estimation of Spatial Correlation of Drop Size Distribution Parameters
and Rain Rate Using NASA's S-Band Polarimetric Radar and 2D Video
Disdrometer Network: Two Case Studies from MC3E
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SMALL-SCALE RAINFALL; DIFFERENT CLIMATIC REGIMES; DUAL-POLARIZED RADAR;
PRECIPITATION RADAR; VARIABILITY; VALIDATION; PROFILER; EVENTS; HAIL
AB Polarimetric radar data obtained at high spatial and temporal resolutions offer a distinct advantage in estimating the spatial correlation function of drop size distribution (DSD) parameters and rain rate compared with a fixed gauge-disdrometer network. On two days during the 2011 Midlatitude Continental Convective Clouds Experiment (MC3E) campaign in Oklahoma, NASA's S-band polarimetric radar (NPOL) performed repeated PPI scans every 40 s over six 2D video disdrometer (2DVD) sites, located 20-30 km from the radar. The two cases were 1) a rapidly evolving multicell rain event (with large drops) and 2) a long-duration stratiform rain event. From the time series at each polar pixel, the Pearson correlation coefficient is computed as a function of distance along each radial in the PPI scan. Azimuthal dependence is found, especially for the highly convective event. A pseudo-1D spatial correlation is computed that is fitted to a modified-exponential function with two parameters (decorrelation distance R-0 and shape F). The first event showed significantly higher spatial variability in rain rate (shorter decorrelation distance R-0 = 3.4 km) compared with the second event with R-0 = 10.2 km. Further, for the second event, the spatial correlation of the DSD parameters and rain rate from radar showed good agreement with 2DVD-based spatial correlations over distances ranging from 1.5 to 7 km. The NPOL also performed repeated RHI scans every 40 s along one azimuth centered over the 2DVD network. Vertical correlations of the DSD parameters as well as the rainwater content were determined below the melting level, with the first event showing more variability compared with the second event.
C1 [Bringi, V. N.; Tolstoy, L.; Thurai, M.] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
[Petersen, W. A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Bringi, VN (reprint author), Colorado State Univ, Dept Elect & Comp Engn, Campus Mail 1373, Ft Collins, CO 80523 USA.
EM bringi@engr.colostate.edu
RI Measurement, Global/C-4698-2015
FU NASA GPM program offices
FX We thank the NPOL scientists and technicians as well as the disdrometer
field technicians during MC3E for collecting the data used in this
study. We would also like to thank Dr. R. Kakar of the NASA
Precipitation Measurement Mission and Dr. A. Hou and Dr. M. Schwaller of
the NASA GPM program offices for providing funding for this study. The
S-band profiler data shown in Figs. 2b and 2d were provided by Dr. C. R.
Williams.
NR 39
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U1 0
U2 4
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 JUN
PY 2015
VL 16
IS 3
BP 1207
EP 1221
DI 10.1175/JHM-D-14-0204.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9YI
UT WOS:000355126500015
ER
PT J
AU Best, MJ
Abramowitz, G
Johnson, HR
Pitman, AJ
Balsamo, G
Boone, A
Cuntz, M
Decharme, B
Dirmeyer, PA
Dong, J
Ek, M
Guo, Z
Haverd, V
Van den Hurk, BJJ
Nearing, GS
Pak, B
Peters-Lidard, C
Santanello, JA
Stevens, L
Vuichard, N
AF Best, M. J.
Abramowitz, G.
Johnson, H. R.
Pitman, A. J.
Balsamo, G.
Boone, A.
Cuntz, M.
Decharme, B.
Dirmeyer, P. A.
Dong, J.
Ek, M.
Guo, Z.
Haverd, V.
Van den Hurk, B. J. J.
Nearing, G. S.
Pak, B.
Peters-Lidard, C.
Santanello, J. A., Jr.
Stevens, L.
Vuichard, N.
TI The Plumbing of Land Surface Models: Benchmarking Model Performance
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID ATMOSPHERE COUPLING EXPERIMENT; SOIL WETNESS PROJECT; PARAMETERIZATION
SCHEMES; CLIMATE MODELS; PHASE; HYDROLOGY; MOISTURE; SYSTEM; IMPACT;
ENERGY
AB The Protocol for the Analysis of Land Surface Models (PALS) Land Surface Model Benchmarking Evaluation Project (PLUMBER) was designed to be a land surface model (LSM) benchmarking intercomparison. Unlike the traditional methods of LSM evaluation or comparison, benchmarking uses a fundamentally different approach in that it sets expectations of performance in a range of metrics a priori-before model simulations are performed. This can lead to very different conclusions about LSM performance. For this study, both simple physically based models and empirical relationships were used as the benchmarks. Simulations were performed with 13 LSMs using atmospheric forcing for 20 sites, and then model performance relative to these benchmarks was examined. Results show that even for commonly used statistical metrics, the LSMs' performance varies considerably when compared to the different benchmarks. All models outperform the simple physically based benchmarks, but for sensible heat flux the LSMs are themselves outperformed by an out-of-sample linear regression against downward shortwave radiation. While moisture information is clearly central to latent heat flux prediction, the LSMs are still outperformed by a three-variable nonlinear regression that uses instantaneous atmospheric humidity and temperature in addition to downward shortwave radiation. These results highlight the limitations of the prevailing paradigm of LSM evaluation that simply compares an LSM to observations and to other LSMs without a mechanism to objectively quantify the expectations of performance. The authors conclude that their results challenge the conceptual view of energy partitioning at the land surface.
C1 [Best, M. J.; Johnson, H. R.] Met Off, Exeter EX1 3PB, Devon, England.
[Abramowitz, G.; Pitman, A. J.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia.
[Balsamo, G.] ECMWF, Reading, Berks, England.
[Boone, A.; Decharme, B.] Meteo France, CNRM GAME, Toulouse, France.
[Cuntz, M.] UFZ Helmholtz Ctr Environm Res, Leipzig, Germany.
[Dirmeyer, P. A.; Guo, Z.] George Mason Univ, Ctr Ocean Land Atmosphere Studies, Fairfax, VA 22030 USA.
[Dong, J.; Ek, M.] NOAA, NCEP, EMC, College Pk, MD USA.
[Haverd, V.] CSIRO, Oceans & Atmosphere Flagship, Canberra, ACT, Australia.
[Van den Hurk, B. J. J.] KNMI, De Bilt, Netherlands.
[Nearing, G. S.; Peters-Lidard, C.; Santanello, J. A., Jr.] NASA GSFC, Hydrol Sci Lab, Greenbelt, MD USA.
[Pak, B.; Stevens, L.] CSIRO, Oceans & Atmosphere Flagship, Aspendale, Vic, Australia.
[Vuichard, N.] CEA CNRS UVSQ, IPSL LSCE, UMR 8212, Lab Sci Climat & Environm, Gif Sur Yvette, France.
RP Best, MJ (reprint author), Met Off, Fitzroy Rd, Exeter EX1 3PB, Devon, England.
EM martin.best@metoffice.gov.uk
RI Pitman, Andrew/A-7353-2011; haverd, vanessa/G-8683-2011; Santanello,
Joseph/D-4438-2012; Dirmeyer, Paul/B-6553-2016; Vuichard,
Nicolas/A-6629-2011; Peters-Lidard, Christa/E-1429-2012; Stevens,
Lauren/I-4183-2016;
OI Pitman, Andrew/0000-0003-0604-3274; Santanello,
Joseph/0000-0002-0807-6590; Dirmeyer, Paul/0000-0003-3158-1752;
Peters-Lidard, Christa/0000-0003-1255-2876; Best,
Martin/0000-0003-4468-876X
FU Joint DECC/Defra Met Office Hadley Centre Climate Programme [CA01101];
Australian Research Council Centre of Excellence for Climate System
Science [CE110001028]; 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; Tuscia University;
Universite Laval and Environment Canada; U.S. Department of Energy
FX M. Best and H. Johnson were supported by the Joint DECC/Defra Met Office
Hadley Centre Climate Programme (CA01101). We acknowledge the support of
the Australian Research Council Centre of Excellence for Climate System
Science (CE110001028). This work used eddy covariance data acquired by
the FLUXNET community and in particular by the following networks:
AmeriFlux [U.S. Department of Energy, Biological and Environmental
Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and
DE-FG02-04ER63911)], AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP,
CarboItaly, CarboMont, ChinaFlux, FLUXNET-Canada (supported by CFCAS,
NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA,
NECC, OzFlux, TCOS-Siberia, and USCCC. We acknowledge the financial
support to the eddy covariance data harmonization provided by
CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for
Biogeochemistry, the National Science Foundation, Tuscia University,
Universite Laval and Environment Canada, and the U.S. Department of
Energy and the database development and technical support from Berkeley
Water Center; Lawrence Berkeley National Laboratory; Microsoft Research
eScience; Oak Ridge National Laboratory; University of California,
Berkeley; and University of Virginia.
NR 52
TC 27
Z9 27
U1 5
U2 35
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 JUN
PY 2015
VL 16
IS 3
BP 1425
EP 1442
DI 10.1175/JHM-D-14-0158.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9YI
UT WOS:000355126500028
ER
PT J
AU Owusu-Danquah, JS
Saleeb, AF
Dhakal, B
Padula, SA
AF Owusu-Danquah, J. S.
Saleeb, A. F.
Dhakal, B.
Padula, S. A., II
TI A Comparative Study of Ni49.9Ti50.1 and Ni50.3Ti29.7Hf20 Tube Actuators
(vol 24, pg 1726, 2015)
SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE
LA English
DT Correction
C1 [Owusu-Danquah, J. S.; Saleeb, A. F.; Dhakal, B.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Saleeb, AF (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA.
EM saleeb@uakron.edu
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1059-9495
EI 1544-1024
J9 J MATER ENG PERFORM
JI J. Mater. Eng. Perform.
PD JUN
PY 2015
VL 24
IS 6
SI SI
BP 2577
EP 2577
DI 10.1007/s11665-015-1500-7
PG 1
WC Materials Science, Multidisciplinary
SC Materials Science
GA CI6SF
UT WOS:000354890800050
ER
PT J
AU Mader, TH
Gibson, CR
Lee, AG
Patel, NB
Hart, SF
Pettit, DR
AF Mader, Thomas H.
Gibson, C. Robert
Lee, Andrew G.
Patel, Nimesh B.
Hart, Steven F.
Pettit, Donald R.
TI Unilateral Loss of Spontaneous Venous Pulsations in an Astronaut
SO JOURNAL OF NEURO-OPHTHALMOLOGY
LA English
DT Letter
ID DURATION SPACE-FLIGHT; OPTIC DISC EDEMA
C1 [Mader, Thomas H.] US Army, Cooper Landing, AK 99572 USA.
[Gibson, C. Robert] Coastal Eye Associates, Webster, TX USA.
[Lee, Andrew G.] Methodist Hosp, Dept Ophthalmol, Houston, TX 77030 USA.
[Patel, Nimesh B.] Univ Houston, Univ Eye Inst, Houston, TX USA.
[Hart, Steven F.] NASA, Johnson Space Ctr, Space Med, Houston, TX USA.
[Pettit, Donald R.] NASA, Johnson Space Ctr, Houston, TX USA.
RP Mader, TH (reprint author), US Army, Cooper Landing, AK 99572 USA.
NR 5
TC 3
Z9 3
U1 0
U2 0
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1070-8022
EI 1536-5166
J9 J NEURO-OPHTHALMOL
JI J. Neuro-Ophthal.
PD JUN
PY 2015
VL 35
IS 2
BP 226
EP 227
PG 2
WC Clinical Neurology; Ophthalmology
SC Neurosciences & Neurology; Ophthalmology
GA CI7ZO
UT WOS:000354986600029
PM 25756457
ER
PT J
AU Jiang, B
Woodell, GA
Jobson, DJ
AF Jiang, Bo
Woodell, Glenn A.
Jobson, Daniel J.
TI Novel multi-scale retinex with color restoration on graphics processing
unit
SO JOURNAL OF REAL-TIME IMAGE PROCESSING
LA English
DT Article
DE Multi-scale Retinex; Image enhancement; Autolevels; Real time; GPU
ID IMAGE-ENHANCEMENT; VISION; GPU
AB The multi-scale retinex with color restoration (MSRCR) was developed as a general-purpose image enhancement algorithm that provides simultaneous dynamic range compression, local lightness/contrast enhancement, and good color rendition, and has been successfully used for a wide variety of imagery from diverse fields. While the MSRCR performs good enhancement in most images, the output image can sometimes be further visually optimized during our experiments. An improved MSRCR+Autolevels (AL) algorithm is presented, which can eliminate the impact of a small number of outliers in the histogram of the image and further improve the contrast of an image. New extension significantly improves the visual performance of the MSRCR algorithm. However, the MSRCR+AL containing a large number of complex calculations is computationally expensive, limiting real-time applications. In this paper, a parallel application of the MSRCR+AL algorithm on a graphics processing unit (GPU) is presented. For the various configurations in our test, the GPU-accelerated MSRCR+AL shows a scalable speedup as the resolution of an image increases. The up to 45x speedup (1,024 x 1,024) over the single-threaded CPU counterpart shows a promising direction of using the GPU-based MSRCR+AL in large-scale, time-critical applications. We also achieved 17 frames per second in video processing (1,280 x 720).
C1 [Jiang, Bo] NIA, Hampton, VA 23666 USA.
[Woodell, Glenn A.; Jobson, Daniel J.] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23665 USA.
RP Jiang, B (reprint author), NIA, 100 Explorat Way, Hampton, VA 23666 USA.
EM bjiang07@gmail.com
FU NASA [NNL09AA00A]
FX The authors wish to thank the NASA Aviation Safety Program, External
Hazards Sensing and Mitigation for the funding which made this work
possible. In particular, Dr. Jiang was funded by NASA Grant#NNL09AA00A
to the National Institute of Aerospace.
NR 37
TC 2
Z9 3
U1 2
U2 20
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1861-8200
EI 1861-8219
J9 J REAL-TIME IMAGE PR
JI J. Real-Time Image Process.
PD JUN
PY 2015
VL 10
IS 2
SI SI
BP 239
EP 253
DI 10.1007/s11554-014-0399-9
PG 15
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic; Imaging Science & Photographic Technology
SC Computer Science; Engineering; Imaging Science & Photographic Technology
GA CI4JU
UT WOS:000354715300005
ER
PT J
AU Jiang, X
Olsen, ET
Pagano, TS
Su, H
Yung, YL
AF Jiang, Xun
Olsen, Edward T.
Pagano, Thomas S.
Su, Hui
Yung, Yuk L.
TI Modulation of Midtropospheric CO2 by the South Atlantic Walker
Circulation*
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID ATMOSPHERIC CARBON-DIOXIDE; MAUNA-LOA; EL-NINO; OSCILLATION;
VARIABILITY; CLIMATE; REANALYSIS; MISSION; MODEL; CYCLE
AB Midtropospheric CO2 data from the Atmospheric Infrared Sounder (AIRS) are used in this study to explore the variability of CO2 over the South Atlantic Ocean. It was found that the area-averaged CO2 over the South Atlantic Ocean is less than that over South America by about 1 ppm during December-March. This CO2 contrast is due to the large-scale vertical circulation over this region. During December-March, there is sinking motion over the South Atlantic Ocean. The sinking motion brings high-altitude air with a slightly lower concentration of CO2 to the midtroposphere. Meanwhile, air rising over South America brings near-surface air with a higher concentration of CO2 to the midtroposphere. As a result, the AIRS midtropospheric CO2 concentration is lower over the South Atlantic Ocean than over South America during December-March. The detrended AIRS midtropospheric CO2 difference correlates well with the inverted and detrended 400-hPa vertical pressure velocity difference between the South Atlantic and South America. Results obtained from this study demonstrate the strong impact of large-scale circulation on the vertical distribution of CO2 in the free troposphere and suggest that midtropospheric CO2 measurements can be used as an innovative observational constraint on the simulation of large-scale circulations in climate models.
C1 [Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA.
[Olsen, Edward T.; Pagano, Thomas S.; Su, Hui] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Jiang, X (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 4800 Calhoun Rd, Houston, TX 77004 USA.
EM xjiang7@uh.edu
FU AIRS project; OCO-2 project; NASA [NNX13AC04G]; Caltech; National
Aeronautics and Space Administration
FX We thank two anonymous reviewers for helpful comments. XJ and YLY were
supported by the AIRS project, OCO-2 project, and NASA Grant NNX13AC04G
to UH and Caltech. 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 39
TC 1
Z9 1
U1 0
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JUN
PY 2015
VL 72
IS 6
BP 2241
EP 2247
DI 10.1175/JAS-D-14-0340.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9RW
UT WOS:000355108500003
ER
PT J
AU Chao, WC
AF Chao, Winston C.
TI Correction of Excessive Precipitation over Steep and High Mountains in a
GCM: A Simple Method of Parameterizing the Thermal Effects of Subgrid
Topographic Variation
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID MODEL
AB The excessive precipitation over steep and high mountains (EPSM) in GCMs and mesoscale models is due to a lack of parameterization of the thermal effects of subgrid-scale topographic variation. These thermal effects drive subgrid-scale heated-slope-induced vertical circulations (SHVC). SHVC provide a ventilation effect of removing heat from the boundary layer of resolvable-scale mountain slopes and depositing it higher up. The lack of SHVC parameterization is the cause of EPSM. The author has previously proposed a method of parameterizing SHVC, here termed SHVC.1. Although this has been successful in avoiding EPSM, the drawback is that it suppresses convective-type precipitation in the regions where it is applied.
In this article, the author proposes a new method of parameterizing SHVC, here termed SHVC.2. In SHVC.2, the potential temperature and mixing ratio of the boundary layer are changed when used as input to the cumulus parameterization scheme over mountainous regions. This allows the cumulus parameterization to assume the additional function of SHVC parameterization. SHVC.2 has been tested in NASA Goddard's GEOS-5 GCM. It achieves the primary goal of avoiding EPSM while also avoiding the suppression of convective-type precipitation in the regions where it is applied.
C1 [Chao, Winston C.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Chao, WC (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 610-1, Greenbelt, MD 20771 USA.
EM winston.c.chao@nasa.gov
FU NASA [WBS 432938.11.01.04.01.06, WBS 802678.02.17.01.25]
FX Help from Larry Takacs, Matt Thompson, Joe Stassi, Danifan Barahona, and
Purnendu Chakraborty of NASA GSFC GMAO in using the GEOS-5 GCM and
programming advices is gratefully acknowledged. Discussion with Max
Suarez was useful. Jim Gass provided graphics support. This work was
supported by NASA under WBS 432938.11.01.04.01.06 and WBS
802678.02.17.01.25. Computing resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Studies (NCCS) at the Goddard Space Flight Center.
Maharaj Bhat of NASA/NCCS helped with setting up the Fortran code for
the Student's t test.
NR 16
TC 1
Z9 1
U1 1
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JUN
PY 2015
VL 72
IS 6
BP 2366
EP 2378
DI 10.1175/JAS-D-14-0336.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9RW
UT WOS:000355108500011
ER
PT J
AU Zhang, GJ
Fan, JW
Xu, KM
AF Zhang, Guang J.
Fan, Jiwen
Xu, Kuan-Man
TI Comments on "A Unified Representation of Deep Moist Convection in
Numerical Modeling of the Atmosphere. Part I"
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Editorial Material
C1 [Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Fan, Jiwen] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Zhang, GJ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, CASPO, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM gzhang@ucsd.edu
RI Fan, Jiwen/E-9138-2011; Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
NR 3
TC 2
Z9 2
U1 0
U2 6
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 JUN
PY 2015
VL 72
IS 6
BP 2562
EP 2565
DI 10.1175/JAS-D-14-0246.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CI9RW
UT WOS:000355108500022
ER
PT J
AU Frederick, MA
Banks, DW
Garzon, GA
Matisheck, JR
AF Frederick, M. A.
Banks, D. W.
Garzon, G. A.
Matisheck, J. R.
TI Flight tests of a supersonic natural laminar flow airfoil
SO MEASUREMENT SCIENCE AND TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 16th International Symposium on Flow Visualization (ISFV)
CY JUL 24-27, 2014
CL Okinawa, JAPAN
DE supersonic natural laminar flow; boundary layer transition; boundary
layer; laminar flow; infrared thermography; flight test; airfoil
AB A flight test campaign of a supersonic natural laminar flow airfoil has been recently completed. The test surface was an 80 inch (203 cm) chord and 40 inch (102 cm) span article mounted on the centerline store location of an F-15B airplane. The test article was designed with a leading edge sweep of effectively 0 degrees to minimize boundary layer crossflow. The test article surface was coated with an insulating material to avoid significant heat transfer to and from the test article structure to maintain a quasi-adiabatic wall. An aircraft-mounted infrared camera system was used to determine boundary layer transition and the extent of laminar flow. The tests were flown up to Mach 2.0 and chord Reynolds numbers in excess of 30 million. The objectives of the tests were to determine the extent of laminar flow at high Reynolds numbers and to determine the sensitivity of the flow to disturbances. Both discrete (trip dots) and 2D disturbances (forward-facing steps) were tested. A series of oblique shocks, of yet unknown origin, appeared on the surface, which generated sufficient crossflow to affect transition. Despite the unwanted crossflow, the airfoil performed well. The results indicate that the sensitivity of the flow to the disturbances, which can translate into manufacturing tolerances, was similar to that of subsonic natural laminar flow wings.
C1 [Frederick, M. A.; Banks, D. W.] NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA.
[Garzon, G. A.; Matisheck, J. R.] Aerion Corp, Reno, NV 89502 USA.
RP Frederick, MA (reprint author), NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA.
EM mike.frederick-1@nasa.gov
FU NASA High Speed Fundamental Aeronautics Project; Aerion Corporation
FX Funding for this research was provided by the NASA High Speed
Fundamental Aeronautics Project and the Aerion Corporation.
NR 15
TC 0
Z9 0
U1 1
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-0233
EI 1361-6501
J9 MEAS SCI TECHNOL
JI Meas. Sci. Technol.
PD JUN
PY 2015
VL 26
IS 6
AR 064003
DI 10.1088/0957-0233/26/6/064003
PG 18
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CI4VR
UT WOS:000354752500004
ER
PT J
AU Roundy, JK
Yuan, X
Schaake, J
Wood, EF
AF Roundy, Joshua K.
Yuan, Xing
Schaake, John
Wood, Eric F.
TI A Framework for Diagnosing Seasonal Prediction through Canonical Event
Analysis
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID CLIMATE FORECAST SYSTEM; UNITED-STATES; PRECIPITATION; DROUGHT; FLOODS
AB Hydrologic extremes in the form of flood and drought have large impacts on society that can be reduced through preparations made possible by seasonal prediction. However, the skill of seasonal predictions from global climate models is uncertain, which severely limits their practical use. In the past, the skill assessment has been limited to a single temporal or spatial resolution for a short hindcast period, which is prone to sampling errors, and noise that leads to uncertainty. In this work a framework that uses "canonical" forecast events, or averages in space-time, to provide a more certain assessment of when and where models are skillful is developed. This framework is demonstrated by using NCEP's Climate Forecast System, version 2, hindcast dataset for precipitation and temperature over the contiguous United States (CONUS). As part of the canonical event analyses, the probabilistic predictability metric (PPM) is used to define spatial and seasonal variability of forecast skill and its attribution to El Nino-Southern Oscillation (ENSO) over the CONUS. The PPM indicates that there are clear seasonal and spatial patterns of model skill that provide a better understanding of when and where to have confidence in model predictions as compared to a skill metric based on a single temporal and spatial scale. Furthermore, the canonical event analysis also facilitates the attribution of spatiotemporal variations of precipitation predictive skill to the antecedent ENSO conditions. This work illustrates the importance of using canonical event analysis to diagnose seasonal predictions and discusses its extensions for model development.
C1 [Roundy, Joshua K.; Yuan, Xing; Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
RP Roundy, JK (reprint author), NASA, Goddard Space Flight Ctr, Bldg 33,Room G209, Greenbelt, MD 20771 USA.
EM joshua.roundy@nasa.gov
RI Yuan, Xing/G-8392-2011; Roundy, Joshua/H-9377-2016
OI Yuan, Xing/0000-0001-6983-7368; Roundy, Joshua/0000-0003-0328-3248
FU NASA Earth and Space Science Fellowship [NNX08AU28H]; NOAA Climate
Program Office [NA10OAR4310246, NA12OAR4310090]
FX J. K. Roundy was supported through NASA Earth and Space Science
Fellowship NNX08AU28H (Understanding Hydrologic Sensitivity and
Land-Atmosphere Coupling through Space-Based Remote Sensing), and
through support from the NOAA Climate Program Office (Grants
NA10OAR4310246 and NA12OAR4310090). The support for this research is
gratefully acknowledged. We would also like to thank the three anonymous
reviewers for their helpful comments.
NR 25
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 JUN
PY 2015
VL 143
IS 6
BP 2404
EP 2418
DI 10.1175/MWR-D-14-00190.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ0TL
UT WOS:000355190900023
ER
PT J
AU Lamsal, LN
Duncan, BN
Yoshida, Y
Krotkov, NA
Pickering, KE
Streets, DG
Lu, ZF
AF Lamsal, Lok N.
Duncan, Bryan N.
Yoshida, Yasuko
Krotkov, Nickolay A.
Pickering, Kenneth E.
Streets, David G.
Lu, Zifeng
TI U.S. NO2 trends (2005-2013): EPA Air Quality System (AQS) data versus
improved observations from the Ozone Monitoring Instrument (OMI)
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Nitrogen dioxide; Troposphere; Air quality; Trend; Aura OMI
ID TROPOSPHERIC NITROGEN-DIOXIDE; UNITED-STATES; SATELLITE RETRIEVALS;
ECONOMIC RECESSION; COLUMN RETRIEVAL; POWER-PLANTS; INTEX-B; EMISSIONS;
SPACE; INVENTORY
AB Emissions of nitrogen oxides (NOx) and, subsequently, atmospheric levels of nitrogen dioxide (NO2) have decreased over the U.S. due to a combination of environmental policies and technological change. Consequently, NO2 levels have decreased by 30-40% in the last decade. We quantify NO2 trends (2005 -2013) over the U.S. using surface measurements from the U.S. Environmental Protection Agency (EPA) Air Quality System (AQS) and an improved tropospheric NO2 vertical column density (VCD) data product from the Ozone Monitoring Instrument (OMI) on the Aura satellite. We demonstrate that the current OMI NO2 algorithm is of sufficient maturity to allow a favorable correspondence of trends and variations in OMI and AQS data. Our trend model accounts for the non-linear dependence of NO2 concentration on emissions associated with the seasonal variation of the chemical lifetime, including the change in the amplitude of the seasonal cycle associated with the significant change in NOx emissions that occurred over the last decade. The direct relationship between observations and emissions becomes more robust when one accounts for these non-linear dependencies. We improve the OMI NO2 standard retrieval algorithm and, subsequently, the data product by using monthly vertical concentration profiles, a required algorithm input, from a high-resolution chemistry and transport model (CTM) simulation with varying emissions (2005-2013). The impact of neglecting the time-dependence of the profiles leads to errors in trend estimation, particularly in regions where emissions have changed substantially. For example, trends calculated from retrievals based on time-dependent profiles offer 18% more instances of significant trends and up to 15% larger total NO2 reduction versus the results based on profiles for 2005. Using a CTM, we explore the theoretical relation of the trends estimated from NO2 VCDs to those estimated from ground-level concentrations. The model-simulated trends in VCDs strongly correlate with those estimated from surface concentrations (r = 0.83, N = 355). We then explore the observed correspondence of trends estimated from OMI and AQS data. We find a significant, but slightly weaker, correspondence (i.e., r = 0.68, N = 208) than predicted by the model and discuss some of the important factors affecting the relationship, including known problems (e.g., NOz interferents) associated with the AQS data. This significant correspondence gives confidence in trend and surface concentration estimates from OMI VCDs for locations, such as the majority of the U.S. and globe, that are not covered by surface monitoring networks. Using our improved trend model and our enhanced OMI data product, we find that both OMI and AQS data show substantial downward trends from 2005 to 2013, with an average reduction of 38% for each over the U.S. The annual reduction rates inferred from OMI and AQS measurements are larger (-4.8 +/- 1.9%/yr, -3.7 +/- 1.5%/yr) from 2005 to 2008 than 2010 to 2013 (-1.2 +/- 1.2%/yr, -2.1 +/- 1.4%/yr). We quantify NO2 trends for major U.S. cities and power plants; the latter suggest larger negative trend (-4.0 +/- 1.5%/yr) between 2005 and 2008 and smaller or insignificant changes (-0.5 +/- 1.2%/yr) during 2010-2013. (C) 2015 The Authors. Published by Elsevier Ltd.
C1 [Lamsal, Lok N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Lamsal, Lok N.; Duncan, Bryan N.; Yoshida, Yasuko; Krotkov, Nickolay A.; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Streets, David G.; Lu, Zifeng] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA.
RP Lamsal, LN (reprint author), NASA, GESTAR USRA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lok.lamsal@nasa.gov
RI Krotkov, Nickolay/E-1541-2012; Pickering, Kenneth/E-6274-2012; Duncan,
Bryan/A-5962-2011
OI Krotkov, Nickolay/0000-0001-6170-6750;
FU NASA Air Quality Applied Science Team (AQAST); NASA's Earth Science
Directorate Atmospheric Composition Programs
FX Heather Simon, Paul Miller, and two anonymous reviewers provided helpful
comments that improved this manuscript. This work was supported by the
NASA Air Quality Applied Science Team (AQAST) and NASA's Earth Science
Directorate Atmospheric Composition Programs.
NR 89
TC 21
Z9 22
U1 11
U2 76
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 JUN
PY 2015
VL 110
BP 130
EP 143
DI 10.1016/j.atmosenv.2015.03.055
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CI2QG
UT WOS:000354591500015
ER
PT J
AU Streit, K
Bennett, SA
Van Dover, CL
Coleman, M
AF Streit, Kathrin
Bennett, Sarah A.
Van Dover, Cindy L.
Coleman, Max
TI Sources of organic carbon for Rimicaris hybisae: Tracing individual
fatty acids at two hydrothermal vent fields in the Mid-Cayman rise
SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS
LA English
DT Article
DE Chemosynthetic carbon source; Photosynthetic carbon source; Hydrothermal
vent chemistry; Piccard; Von Damm; Ectosymbionts
ID DEEP-SEA VENT; EXOCULATA; COMMUNITY; SHRIMPS; FRACTIONATION;
BIOSYNTHESIS; BIOLOGY; LIPIDS; RIDGE; LIFE
AB Hydrothermal vents harbor ecosystems mostly decoupled from organic carbon synthesized with the energy of sunlight (photosynthetic carbon source) but fueled instead by oxidation of reduced compounds to generate a chemosynthetic carbon source. Our study aimed to disentangle photosynthetic and chemosynthetic organic carbon sources for the shrimp species Rimicaris hybisae, a primary consumer presumed to obtain its organic carbon mainly from ectosymbiotic chemoautotrophic bacteria living on its gill cover membrane. To provide ectosymbionts with ideal conditions for chemosynthesis, these shrimp live in dense clusters around vent chimneys; they are, however, also found sparsely distributed adjacent to diffuse vent flows, where they might depend on alternative food sources. Densely and sparsely distributed shrimp were sampled and dissected into abdominal tissue and gill cover membrane, covered with ectosymbiotic bacteria, at two hydrothermal vent fields in the Mid-Cayman rise that differ in vent chemistry. Fatty acids (FA) were extracted from shrimp tissues and their carbon isotopic compositions assessed. The FA data indicate that adult R. hybisae predominantly rely on bacteria for their organic carbon needs. Their FA composition is dominated by common bacterial FA of the n7 family (similar to 41%). Bacterial FA of the n4 FA family are also abundant and found to constitute good biomarkers for gill ectosymbionts. Sparsely distributed shrimp contain fractions of n4 FA in gill cover membranes similar to 4% lower than densely packed ones (similar to 18%) and much higher fractions of photosynthetic FA in abdominal tissues, similar to 4% more (compared with 1.6%), suggesting replacement of ectosymbionts along with exoskeletons (molt), while they take up alternative diets of partly photosynthetic organic carbon. Abdominal tissues also contain photosynthetic FA from a second source taken up presumably during an early dispersal phase and still present to c. 3% in adult shrimp. The contribution of photosynthetic carbon to the FA pool of adult R. hybisae is, however, overall small (max. 8%). Significant differences in carbon isotopic values of chemosynthetically derived FA between vent fields suggest that different dominant C fixation pathways are being used. (C) 2015 Published by Elsevier Ltd.
C1 [Streit, Kathrin; Bennett, Sarah A.; Coleman, Max] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA.
[Van Dover, Cindy L.] Duke Univ, Marine Lab, Nicholas Sch Environm, Beaufort, NC 28516 USA.
RP Coleman, M (reprint author), NASA, Jet Prop Lab, CALTECH, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM max.coleman@jpl.nasa.gov
FU National Science Foundation [OCE-1061863, OCE-1061881]; NASA's
Astrobiology Science and Technology for Exploring Planets Program
[NNX09AB75G]; ASTEP grant [NNX09AB75G]; NSF [OCE-221061881]
FX We thank the R/V Atlantis crew (AT18-16), the ROV Jason Operations Team
and the OASES 2012 Science Party, Chief Scientist Chris German, for help
during the cruise, which was supported jointly by grants to CRG from the
National Science Foundation (OCE-1061863) and NASA's Astrobiology
Science and Technology for Exploring Planets Program (NNX09AB75G) and to
MC from the National Science Foundation (OCE-1061881). The post-cruise
contributions of KS, SAB and MC were supported through the same ASTEP
grant (NNX09AB75G) and one of the NSF grants (OCE-221061881) and were
carried out at the Jet Propulsion Laboratory (JPL), California Institute
of Technology, under contract with the National Aeronautics and Space
Administration (NASA). The authors would like to thank E. Versteegh, B.
Theiling, R. Kidd, K. Williford and R. Mielke (JPL) for their assistance
in the laboratory, A. Sessions (Caltech) for giving inputs on the
GC-IRMS technique and the JPL Planetary Surface Instruments Group led by
M. Darrach for many fruitful discussions.
NR 41
TC 1
Z9 1
U1 5
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0637
EI 1879-0119
J9 DEEP-SEA RES PT I
JI Deep-Sea Res. Part I-Oceanogr. Res. Pap.
PD JUN
PY 2015
VL 100
BP 13
EP 20
DI 10.1016/j.dsr.2015.02.003
PG 8
WC Oceanography
SC Oceanography
GA CI2PG
UT WOS:000354588900002
ER
PT J
AU Anderson, RL
AF Anderson, Rodney L.
TI Approaching Moons from Resonance via Invariant Manifolds
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT 22nd AAS/AIAA Space Flight Mechanics Meeting
CY JAN 29-FEB 02, 2012
CL Charleston, SC
SP AAS, Space Flight Mech Comm, AIAA, Astrodynam Techn Comm
ID RESTRICTED 3-BODY PROBLEM; DYNAMICAL-SYSTEMS ANALYSIS; EUROPA ORBITER
MISSION; TRAJECTORY DESIGN; HALO ORBITS; TRANSFERS; CAPTURE; COMETS;
FLYBYS; CONNECTIONS
AB In this work, the final approach typical of a trajectory traveling from the last resonance of an endgame scenario in a tour down to a moon is examined within the context of invariant manifolds. Previous analyses have usually solved this problem either by using numerical techniques or by computing a catalog of suitable trajectories. The invariant manifolds of a selected set of libration orbits and unstable resonant orbits are computed here to serve as guides for desirable approach trajectories. The analysis focuses on designing an approach phase that may be tied into the final resonance in the endgame sequence while also targeting desired conditions at the moon.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-121, Pasadena, CA 91109 USA.
NR 68
TC 3
Z9 3
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD JUN
PY 2015
VL 38
IS 6
BP 1097
EP 1109
DI 10.2514/1.G000286
PG 13
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CI2ZC
UT WOS:000354615900010
ER
PT J
AU Narayan, SR
Manohar, AK
Mukerjee, S
AF Narayan, S. R.
Manohar, Aswin K.
Mukerjee, Sanjeev
TI Bi-Functional Oxygen Electrodes - Challenges and Prospects
SO ELECTROCHEMICAL SOCIETY INTERFACE
LA English
DT Article
ID REGENERATIVE FUEL-CELLS; CARBON-BLACK ANODES; ELECTROCATALYTIC ACTIVITY;
ALKALINE ELECTROLYTE; REDUCTION REACTION; CATHODE CATALYSTS; PEROVSKITE
OXIDES; LI-O-2 BATTERIES; AIR; EVOLUTION
C1 [Narayan, S. R.] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Narayan, S. R.; Manohar, Aswin K.] Univ So Calif, Los Angeles, CA 90089 USA.
[Mukerjee, Sanjeev] Northeastern Univ, Dept Chem & Chem Biol, Boston, MA USA.
[Mukerjee, Sanjeev] Northeastern Univ, Renewable Energy Technol, New York, NY USA.
[Mukerjee, Sanjeev] LEAP, New York, NY USA.
RP Narayan, SR (reprint author), NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM sri.narayan@usc.edu; aswinkam@usc.edu; s.mukerjee@neu.edu
NR 52
TC 1
Z9 1
U1 7
U2 11
PU ELECTROCHEMICAL SOC INC
PI PENNINGTON
PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA
SN 1064-8208
EI 1944-8783
J9 ELECTROCHEM SOC INTE
JI Electrochem. Soc. Interface
PD SUM
PY 2015
VL 24
IS 2
BP 65
EP 69
DI 10.1149/2.F06152IF
PG 5
WC Electrochemistry
SC Electrochemistry
GA DM7SO
UT WOS:000376560500013
ER
PT J
AU Bowers, ML
Gao, Y
Yang, L
Gaydosh, DJ
De Graef, M
Noebe, RD
Wang, Y
Mills, MJ
AF Bowers, M. L.
Gao, Y.
Yang, L.
Gaydosh, D. J.
De Graef, M.
Noebe, R. D.
Wang, Y.
Mills, M. J.
TI Austenite grain refinement during load-biased thermal cycling of a
Ni49.9Ti50.1 shape memory alloy
SO ACTA MATERIALIA
LA English
DT Article
DE SMA; Microstructural evolution; Actuation; Orientation mapping; Defect
analysis
ID SITU NEUTRON-DIFFRACTION; SELF-ACCOMMODATION; B19' MARTENSITE; NITI;
TRANSFORMATION; STRESS; DEFORMATION; EVOLUTION; BEHAVIOR; MICROCRYSTALS
AB A near-equiatomic NiTi shape memory alloy was subjected to a variety of thermomechanical treatments including pure thermal cycling and load-biased thermal cycling to investigate microstructural evolution of the material under actuating conditions. In situ and post mortem scanning transmission electron microscopy (STEM) was used to study the effects of stress on the development of defect substructures during cycling through the martensitic transformation. High temperature observations of the austenite phase show rapid accumulation of dislocations and moderate deformation twinning upon thermomechanical cycling. Additionally, TEM-based orientation mapping suggests the emergence of fine crystallites from the original coarse austenite grain structure. A possible mechanism is proposed for the observed grain refinement based on the crystallographic theory of martensite transformation. (C) 2015 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Bowers, M. L.; Gao, Y.; Yang, L.; Wang, Y.; Mills, M. J.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA.
[De Graef, M.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA USA.
[Gaydosh, D. J.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Bowers, ML (reprint author), Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA.
RI Wang, Yunzhi/B-2557-2010
FU DOE Basic Energy Sciences award [DE-SC0001258]; NSF [DMR-1207494,
DMR-1410322]; NASA ARMD Aeronautical Sciences and Transformational Tools
& Technologies Projects
FX This work was supported in part by DOE Basic Energy Sciences award
#DE-SC0001258, NSF awards #DMR-1207494 and #DMR-1410322, and the NASA
ARMD Aeronautical Sciences and Transformational Tools & Technologies
Projects (technical discipline lead Dale Hopkins). The authors
gratefully acknowledge Noel T. Nuhfer at CMU for assisting with the
ASTAR data acquisition. We would also like to thank Dr. Othmane Benafan
for providing the as-tested 100 MPa-20cycle NiTi sample for ASTAR
analysis.
NR 36
TC 5
Z9 5
U1 3
U2 34
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 JUN 1
PY 2015
VL 91
BP 318
EP 329
DI 10.1016/j.actamat.2015.03.017
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA CH6NX
UT WOS:000354154400028
ER
PT J
AU Urschel, MR
Kubo, MD
Hoehler, TM
Peters, JW
Boyd, ES
AF Urschel, Matthew R.
Kubo, Michael D.
Hoehler, Tori M.
Peters, John W.
Boyd, Eric S.
TI Carbon Source Preference in Chemosynthetic Hot Spring Communities
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID YELLOWSTONE-NATIONAL-PARK; STREAMER BIOFILM COMMUNITIES; GEOTHERMAL
SPRINGS; SP-NOV.; HYDROTHERMAL ECOSYSTEMS; ESCHERICHIA-COLI; ENERGY;
AQUIFICALES; GROWTH; ACID
AB Rates of dissolved inorganic carbon (DIC), formate, and acetate mineralization and/or assimilation were determined in 13 high-temperature (> 73 degrees C) hot springs in Yellowstone National Park (YNP), Wyoming, in order to evaluate the relative importance of these substrates in supporting microbial metabolism. While 9 of the hot spring communities exhibited rates of DIC assimilation that were greater than those of formate and acetate assimilation, 2 exhibited rates of formate and/or acetate assimilation that exceeded those of DIC assimilation. Overall rates of DIC, formate, and acetate mineralization and assimilation were positively correlated with spring pH but showed little correlation with temperature. Communities sampled from hot springs with similar geochemistries generally exhibited similar rates of substrate transformation, as well as similar community compositions, as revealed by 16S rRNA gene-tagged sequencing. Amendment of microcosms with small (micromolar) amounts of formate suppressed DIC assimilation in short-term (< 45min) incubations, despite the presence of native DIC concentrations that exceeded those of added formate by 2 to 3 orders of magnitude. The concentration of added formate required to suppress DIC assimilation was similar to the affinity constant (Km) for formate transformation, as determined by community kinetic assays. These results suggest that dominant chemoautotrophs in high-temperature communities are facultatively autotrophic or mixotrophic, are adapted to fluctuating nutrient availabilities, and are capable of taking advantage of energy-rich organic substrates when they become available.
C1 [Urschel, Matthew R.; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
[Urschel, Matthew R.; Peters, John W.; Boyd, Eric S.] Montana State Univ, Thermal Biol Inst, Bozeman, MT 59717 USA.
[Kubo, Michael D.; Hoehler, Tori M.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Peters, John W.] Montana State Univ, Dept Chem & Biochem, Bozeman, MT 59717 USA.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
EM eboyd@montana.edu
OI Peters, John/0000-0001-9117-9568
FU NASA Exobiology and Evolutionary Biology award [NNX10AT31G]; NSF
Partnerships in International Research and Education award
[PIRE-0968421]
FX This work was supported by NASA Exobiology and Evolutionary Biology
award NNX10AT31G (to T.M.H. and E.S.B.) and NSF Partnerships in
International Research and Education award PIRE-0968421 (to J.W.P.).
NR 54
TC 4
Z9 4
U1 1
U2 13
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
EI 1098-5336
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD JUN
PY 2015
VL 81
IS 11
BP 3834
EP 3847
DI 10.1128/AEM.00511-15
PG 14
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA CH3FA
UT WOS:000353912000029
PM 25819970
ER
PT J
AU Hultquist, G
Graham, MJ
Kodra, O
Moisa, S
Liu, R
Bexell, U
Smialek, JL
AF Hultquist, G.
Graham, M. J.
Kodra, O.
Moisa, S.
Liu, R.
Bexell, U.
Smialek, J. L.
TI Corrosion of copper in distilled water without O-2 and the detection of
produced hydrogen
SO CORROSION SCIENCE
LA English
DT Article
DE Copper; AES; XPS; SIMS; Oxidation; Hydrogen absorption
ID PURE WATER; FUNDAMENTAL-ASPECTS; SOLID-SURFACES; SPECTROSCOPY; OXIDATION
AB This paper reports on hydrogen pressures measured during similar to 19,000 h immersion of copper in oxygen-free liquid distilled water. Copper corrosion products have been examined ex-situ by SEM and characterized by XPS and SIMS. XPS strongly indicates a corrosion product containing both oxygen and hydrogen. SIMS shows that oxygen is mainly present in the outer 0.3 mu m surface region and that hydrogen penetrates to depths well below the corrosion product. Thermal desorption spectroscopy shows that the reaction product formed near room-temperature is less stable than that formed in air at 350 degrees C. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Hultquist, G.] Royal Inst Technol, Surface & Corros Sci, SE-10044 Stockholm, Sweden.
[Graham, M. J.] Natl Res Council Canada, Aerosp, Ottawa, ON K1A 0R6, Canada.
[Kodra, O.; Moisa, S.] Natl Res Council Canada, Elect & Photon Mat, Ottawa, ON K1A 0R6, Canada.
[Liu, R.] Natl Univ Singapore, Fac Sci, Singapore 117551, Singapore.
[Bexell, U.] Dalarna Univ, SE-79188 Falun, Sweden.
[Smialek, J. L.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Hultquist, G (reprint author), Royal Inst Technol, Surface & Corros Sci, SE-10044 Stockholm, Sweden.
EM gunnarh@kth.se
FU Swedish Radiation Safety Authority (SSM)
FX The Swedish Radiation Safety Authority (SSM) is gratefully acknowledged
for financial support.
NR 17
TC 9
Z9 9
U1 3
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0010-938X
EI 1879-0496
J9 CORROS SCI
JI Corrosion Sci.
PD JUN
PY 2015
VL 95
BP 162
EP 167
DI 10.1016/j.corsci.2015.03.009
PG 6
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA CH4KC
UT WOS:000354001400017
ER
PT J
AU Khazendar, A
Borstad, CP
Scheuchl, B
Rignot, E
Seroussi, H
AF Khazendar, Ala
Borstad, Christopher P.
Scheuchl, Bernd
Rignot, Eric
Seroussi, Helene
TI The evolving instability of the remnant Larsen B Ice Shelf and its
tributary glaciers
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Antarctica; Larsen Ice Shelf; ice-shelf instability; laser altimetry;
InSAR ice flow speeds; numerical ice modeling
ID PINE ISLAND GLACIER; ANTARCTIC PENINSULA; RADAR INTERFEROMETRY;
ELEVATION CHANGES; LASER ALTIMETRY; COLLAPSE; SHEET; THICKNESS; FLOW;
DISINTEGRATION
AB Following the 2002 disintegration of the northern and central parts of the Larsen B Ice Shelf, the tributary glaciers of the southern surviving part initially appeared relatively unchanged and hence assumed to be buttressed sufficiently by the remnant ice shelf. Here, we modify this perception with observations from IceBridge altimetry and InSAR-inferred ice flow speeds. Our analyses show that the surfaces of Leppard and Flask glaciers directly upstream from their grounding lines lowered by 15 to 20 m in the period 2002-2011. The thinning appears to be dynamic as the flow of both glaciers and the remnant ice shelf accelerated in the same period. Flask Glacier started accelerating even before the 2002 disintegration, increasing its flow speed by similar to 55% between 1997 and 2012. Starbuck Glacier meanwhile did not change much. We hypothesize that the different evolutions of the three glaciers are related to their dissimilar bed topographies and degrees of grounding. We apply numerical modeling and data assimilation that show these changes to be accompanied by a reduction in the buttressing afforded by the remnant ice shelf, a weakening of the shear zones between its flow units and an increase in its fracture. The fast flowing northwestern part of the remnant ice shelf exhibits increasing fragmentation, while the stagnant southeastern part seems to be prone to the formation of large rifts, some of which we show have delimited successive calving events. A large rift only 12 km downstream from the grounding line is currently traversing the stagnant part of the ice shelf, defining the likely front of the next large calving event. We propose that the flow acceleration, ice front retreat and enhanced fracture of the remnant Larsen B Ice Shelf presage its approaching demise. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Khazendar, Ala; Borstad, Christopher P.; Rignot, Eric; Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Scheuchl, Bernd; Rignot, Eric] Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA.
RP Khazendar, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ala@jpl.nasa.gov
RI Rignot, Eric/A-4560-2014;
OI Rignot, Eric/0000-0002-3366-0481; Borstad,
Christopher/0000-0001-6992-1770
FU NASA's Cryospheric Sciences Program; NASA's MEaSuREs Program; NASA's
Modeling, Analysis and Prediction Program; National Aeronautics and
Space Administration
FX This work was supported by NASA's Cryospheric Sciences Program (A.K.,
C.B. and H.S.), NASA's MEaSuREs Program (B.S. and E.R.) and NASA's
Modeling, Analysis and Prediction Program (C.B.). Spaceborne SAR data
collection post 2005 was coordinated by the Space Task Group and its
successor, the Polar Space Task Group. The authors are grateful to L.
Padman for providing the ocean tide model. The authors much appreciate
the highly constructive and helpful comments made by three anonymous
reviewers.; This work was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 62
TC 8
Z9 8
U1 6
U2 39
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 JUN 1
PY 2015
VL 419
BP 199
EP 210
DI 10.1016/j.eps1.2015.03.014
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CH2JW
UT WOS:000353852500019
ER
PT J
AU Rhodes, KL
Warren-Rhodes, KA
Sweet, S
Helgenberger, M
Joseph, E
Boyle, LN
Hopkins, KD
AF Rhodes, Kevin L.
Warren-Rhodes, Kimberley A.
Sweet, Scott
Helgenberger, Mike
Joseph, Eugene
Boyle, Linda Ng
Hopkins, Kevin D.
TI Marine ecological footprint indicates unsustainability of the Pohnpei
(Micronesia) coral reef fishery
SO ENVIRONMENTAL CONSERVATION
LA English
DT Article
DE biocapacity; consumption; ecological overshoot; marine ecological
footprint; Micronesia; overfishing
ID ECOSYSTEM APPROPRIATION; PACIFIC; ISLAND; CATCH; COMMUNITIES;
MANAGEMENT; DIVERSITY; DYNAMICS; SERVICES; BIOMASS
AB Throughout the tropics, developing countries and territories are highly dependent on nearshore marine resources for food and income, however information on the sustainability and proper management of these fisheries is lacking. In Pohnpei, Micronesia, the sustainability of a coral reef finfishery was assessed by comparing coral reef fish demand to coral reef biocapacity using a marine ecological footprint (MEF) analysis. Based on geo-referenced satellite and aerial imagery, Pohnpei and surrounding atolls have 184.2 km(2) of coral reef habitat with a sustainable finfish yield of 573-1118 t yr(-1), however total harvest was estimated at 4068 t yr(-1), exceeding biocapacity by 360-710%. The MEF was supported by observed impacts to coral reef resources, including (1) long-term declines in fish spawning aggregation density, (2) reductions in mean size, age and fecundity of key commercial species, (3) reliance on undersized fish, and (4) decadal declines in mean size and abundance of fishes of iconic value and critical to ecosystem maintenance. The commercial fishery was responsible for 68% of finfish catch volume, while reef fish consumption, at 93 kg person(-1) yr(-1), was among the highest in the region. To sustainably meet current demand, up to 833 km(2) of additional reef area would be required. The study illustrates the MEF, at least rudimentarily, reflects biological reality on local reefs and represents a valuable analytical tool in a marine policymaker's toolbox.
C1 [Rhodes, Kevin L.; Hopkins, Kevin D.] Univ Hawaii, Coll Forestry Agr & Nat Resource Management, Hilo, HI 96720 USA.
[Warren-Rhodes, Kimberley A.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Sweet, Scott] TerraUnda, Dumaguete 6200, Negros Oriental, Philippines.
[Helgenberger, Mike] Off Fisheries & Aquaculture, FM-96941 Kolonia, Pohnpei, Micronesia.
[Joseph, Eugene] Conservat Soc Pohnpei, Kolonia 96941, Pohnpei, Micronesia.
[Boyle, Linda Ng] Univ Washington, Dept Ind & Syst Engn, Seattle, WA 98195 USA.
RP Rhodes, KL (reprint author), Univ Hawaii, Coll Forestry Agr & Nat Resource Management, 200 W Kawili St, Hilo, HI 96720 USA.
EM klrhodes_grouper@yahoo.com
FU US Department of Interior; NOAA Coral Reef Conservation [NA08NMF4630458,
NA05NMF4631049]; Micronesia Conservation Trust through the Margaret A.
Cargill Foundation; Nature Conservancy
FX We thank survey participants, the Pohnpei State Department of Lands and
Natural Resources, and the College of Micronesia. Surveys were conducted
and compiled by J. Amor, J. Hadley, M. Ioanis, E. John, C. Wichilmel and
M. Obispo. Administrative assistance was provided by M. Albert, L.
Yamada and P. Shed of the Conservation Society of Pohnpei, with
logistical support from D. David and the Pohnpei Office of Fisheries and
Aquaculture. Multi-year funding for fish monitoring at Kehpara was
provided to the Conservation Society of Pohnpei through the US
Department of Interior. Additional funding was made available through
NOAA Coral Reef Conservation grants to Kevin Hopkins (NA08NMF4630458),
M. Tupper (University of Guam) (NA05NMF4631049) and the Micronesia
Conservation Trust through the Margaret A. Cargill Foundation.
Additional funding was supplied by The Nature Conservancy to Scott
Sweet.
NR 70
TC 1
Z9 1
U1 7
U2 39
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0376-8929
EI 1469-4387
J9 ENVIRON CONSERV
JI Environ. Conserv.
PD JUN
PY 2015
VL 42
IS 2
BP 182
EP 190
DI 10.1017/S037689291400023X
PG 9
WC Biodiversity Conservation; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CH5AW
UT WOS:000354047300011
ER
PT J
AU Rittweger, J
Bareille, MP
Clement, G
Linnarsson, D
Paloski, WH
Wuyts, F
Zange, J
Angerer, O
AF Rittweger, Joern
Bareille, Marie-Pierre
Clement, Gilles
Linnarsson, Dag
Paloski, William H.
Wuyts, Floris
Zange, Jochen
Angerer, Oliver
TI Short-arm centrifugation as a partially effective musculoskeletal
countermeasure during 5-day head-down tilt bed rest-results from the
BRAG1 study
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Bed rest; Human physiology; Artificial gravity; Space flight;
De-conditioning; Countermeasures
ID FLYWHEEL RESISTIVE EXERCISE; LONG-DURATION SPACEFLIGHT; ARTIFICIAL
GRAVITY; BONE LOSS; RESISTANCE EXERCISE; VERTICAL JUMP; PERFORMANCE;
POWER; MICROGRAVITY; ASTRONAUTS
AB Human centrifugation, also called artificial gravity (AG), is proposed as a combined strategy against detrimental effects of microgravity in long-term space missions. This study scrutinized human short-arm centrifugation as countermeasure against musculoskeletal de-conditioning.
Eleven healthy male subjects [mean age of 34 (SD 7) years] completed the cross-over trial, including three campaigns of -6A degrees head-down tilt bed rest (HDT) for 5 days, with preceding baseline data collection and recovery phases. Bed rest without AG was used as control condition (Ctrl), and AG with 1 g at the center of mass applied once per day for 30 min in one bout (AG(1x30)) and in 6 bouts of 5 min (AG(6x5), 3-min rest between bouts) as experimental conditions. End-points were muscle strength, vertical jump performance, and biomarkers of bone and protein metabolism.
AG(6x5) was better tolerated than AG(1x30). Bone resorption markers CTX, NTX, and DPD all increased by approximately 25 % toward the end of bed rest (P < 0.001), and nitrogen balance decreased by approximately 3 g/day (P < 0.001), without any protection by AG (P > 0.4). Decreases in vertical jump height by 2.1 (SE 0.6) cm after Ctrl bed rest was prevented by either of the AG protocols (P = 0.039).
The present study yielded succinct catabolic effects upon muscle and bone metabolism that were un-prevented by AG. The preservation of vertical jump performance by AG in this study is likely caused by central nervous rather than by peripheral musculoskeletal effects.
C1 [Rittweger, Joern; Zange, Jochen] German Aerosapce Ctr DLR, Inst Aerosp Med, D-51147 Cologne, Germany.
[Bareille, Marie-Pierre] MEDES IMPS, F-31405 Toulouse 4, France.
[Clement, Gilles] CNRS, Lyon Neurosci Res Ctr, UMR5292, F-69500 Lyon, France.
[Linnarsson, Dag] Royal Inst Technol, Stockholm, Sweden.
[Paloski, William H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Wuyts, Floris] Univ Antwerp, Dept Biomed Phys, B-2020 Antwerp, Belgium.
[Angerer, Oliver] German Aerosp Ctr DLR, Space Adm, D-53227 Bonn, Germany.
RP Rittweger, J (reprint author), German Aerosapce Ctr DLR, Inst Aerosp Med, Linder Hohe 1, D-51147 Cologne, Germany.
EM joern.rittweger@dlr.de
RI Rittweger, Jorn/A-4308-2009
FU ESA [22 127/08]; CNES [70686]; German Aerospace Center (DLR) within the
project 'Artificial Gravity'
FX This study was funded by ESA contract no. 22 127/08 and by a CNES
framework agreement no. 70686. J Rittweger and J Zange were supported by
internal funding from the German Aerospace Center (DLR) within the
project 'Artificial Gravity'. In addition, J. Rittweger used private
funds to participate in the study in its planning phase (2006-2009). We
are grateful to the staff of MEDES for their excellent work and support
of this study. Special thanks go to Dr. Petra Frings-Meuthen and Gaby
Kraus from the DLR Institute of Aerospace Medicine for the assessment of
serum and urine markers of bone metabolism. Last but not least, we are
deeply indebted to the study participants-without their selfless
contribution, this work would not have been possible.
NR 38
TC 1
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U1 1
U2 7
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 JUN
PY 2015
VL 115
IS 6
BP 1233
EP 1244
DI 10.1007/s00421-015-3120-1
PG 12
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA CH9ZS
UT WOS:000354395900006
PM 25667067
ER
PT J
AU Holgate, TC
Bennett, R
Hammel, T
Caillat, T
Keyser, S
Sievers, B
AF Holgate, Tim C.
Bennett, Russell
Hammel, Tom
Caillat, Thierry
Keyser, Steve
Sievers, Bob
TI Increasing the Efficiency of the Multi-mission Radioisotope
Thermoelectric Generator
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT International Conference on Thermoelectrics (ICT)
CY JUL 06-10, 2014
CL Nashville, TN
DE Thermoelectrics; RTG; radioisotope; generator; skutterudite
ID MECHANICAL-PROPERTIES; SKUTTERUDITES
AB The National Aeronautics and Space Administration's Mars Science Laboratory terrestrial rover, Curiosity, has recently completed its first Martian year (687 Earth days) during which it has provided a wealth of information and insight into the red planet's atmosphere and geology. The success of this mission was made possible in part by the reliable electrical power provided by its onboard thermoelectric power source-the multi-mission radioisotope thermoelectric generator (MMRTG). In an effort to increase the output power and efficiency of these generators, a newly designed enhanced MMRTG (eMMRTG) that will utilize the more efficient skutterudite-based thermoelectric materials has been conceptualized and modeled, and is now being developed. A discussion of the motivations, modeling results and key design factors are presented and discussed.
C1 [Holgate, Tim C.; Bennett, Russell; Hammel, Tom; Keyser, Steve; Sievers, Bob] TESI, Hunt Valley, MD 21031 USA.
[Caillat, Thierry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Holgate, TC (reprint author), TESI, Hunt Valley, MD 21031 USA.
EM Tim.holgate@teledyne.com
NR 15
TC 2
Z9 2
U1 3
U2 38
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD JUN
PY 2015
VL 44
IS 6
BP 1814
EP 1821
DI 10.1007/s11664-014-3564-9
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA CH1WT
UT WOS:000353813700065
ER
PT J
AU Hendricks, TJ
AF Hendricks, Terry J.
TI Perturbation Methods for Real-Time In Situ Evaluation of Hot-Side
Thermal Resistances in Thermoelectric Energy Recovery Systems
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT International Conference on Thermoelectrics (ICT)
CY JUL 06-10, 2014
CL Nashville, TN
DE Thermal resistance monitoring; perturbation; thermoelectric energy
recovery
AB Thermoelectric (TE) power systems in high-temperature industrial, transportation, and military energy systems require high-performance hot-side and cold-side heat transfer to provide the critical temperature differential and transfer the required thermal energy to create the power output. Hot- and cold-side heat transfer performance is typically characterized by the hot-side and cold-side thermal resistance, R (h,th) and R (c,th), respectively. This heat transfer performance determines the hot-side temperature, T (h), and cold-side temperature, T (c), conditions when operating in energy recovery environments with available temperature differentials characterized by an external driving temperature, T (src), and ambient temperature, T (amb). It is crucial to monitor and track the hot-side thermal performance at all times during TE energy recovery system operation, thereby allowing one to track the system "health," predict future expected system performance, and anticipate/prevent system failures. This paper describes the use of a perturbation methodology and a direct coupling between the TE current, voltage, and hot-side energy flow to extract a real-time in situ evaluation of hot-side thermal resistances. External measurable TE parameters, either system current or T (src), can be perturbed during system operation, and the resulting TE system response can then be coupled mathematically to the hot-side thermal transfer performance (i.e., thermal resistance). This paper discusses the mathematical formalism of this technique, and TE module experimental data showing successful application of real-time current perturbation. This technique provides a pathway for developing faster, real-time system monitoring and diagnostics to alleviate system performance degradation, or prevent system damage from dramatic changes in hot-side thermal transfer conditions in industrial, transportation, and spacecraft TE power systems.
C1 CALTECH, NASA Jet Prop Lab, Thermal Energy Convers Grp, Power & Sensors Sect, Pasadena, CA 91125 USA.
RP Hendricks, TJ (reprint author), CALTECH, NASA Jet Prop Lab, Thermal Energy Convers Grp, Power & Sensors Sect, Pasadena, CA 91125 USA.
EM terry.j.hendricks@jpl.nasa.gov
FU NASA [43-17508]; US Department of Energy, at the Jet Propulsion
Laboratory, California Institute of Technology
FX This work was carried out under NASA Space Act Agreement No. 43-17508, a
contract between NASA and General Motors with funding from the US
Department of Energy, at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract to the National Aeronautics
and Space Administration.
NR 17
TC 0
Z9 0
U1 2
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD JUN
PY 2015
VL 44
IS 6
BP 1909
EP 1918
DI 10.1007/s11664-014-3591-6
PG 10
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA CH1WT
UT WOS:000353813700078
ER
PT J
AU Goldstein, ML
Escoubet, P
Hwang, KJ
Wendel, DE
Vinas, AF
Fung, SF
Perri, S
Servidio, S
Pickett, JS
Parks, GK
Sahraoui, F
Gurgiolo, C
Matthaeus, W
Weygand, JM
AF Goldstein, M. L.
Escoubet, P.
Hwang, K. -Joo
Wendel, D. E.
Vinas, A. -F.
Fung, S. F.
Perri, S.
Servidio, S.
Pickett, J. S.
Parks, G. K.
Sahraoui, F.
Gurgiolo, C.
Matthaeus, W.
Weygand, J. M.
TI Multipoint observations of plasma phenomena made in space by Cluster
SO JOURNAL OF PLASMA PHYSICS
LA English
DT Article
ID AURORAL KILOMETRIC RADIATION; SOLAR-WIND TURBULENCE; KELVIN-HELMHOLTZ
INSTABILITY; ELECTRON-DISTRIBUTION FUNCTIONS; PERPENDICULAR BOW SHOCK;
WHISTLER-MODE CHORUS; 3-DIMENSIONAL MAGNETIC RECONNECTION; SPECTROMETRY
CIS EXPERIMENT; WAVE-PARTICLE INTERACTIONS; STORM-TIME CHORUS
AB Plasmas are ubiquitous in nature, surround our local geospace environment, and permeate the universe. Plasma phenomena in space give rise to energetic particles, the aurora, solar flares and coronal mass ejections, as well as many energetic phenomena in interstellar space. Although plasmas can be studied in laboratory settings, it is often difficult, if not impossible, to replicate the conditions (density, temperature, magnetic and electric fields, etc.) of space. Single-point space missions too numerous to list have described many properties of near-Earth and heliospheric plasmas as measured both in situ and remotely (see http://www.nasa.gov/missions/#. U1mcVmeweRY for a list of NASA-related missions). However, a full description of our plasma environment requires three-dimensional spatial measurements. Cluster is the first, and until data begin flowing from the Magnetospheric Multiscale Mission (MMS), the only mission designed to describe the three-dimensional spatial structure of plasma phenomena in geospace. In this paper, we concentrate on some of the many plasma phenomena that have been studied using data from Cluster. To date, there have been more than 2000 refereed papers published using Cluster data but in this paper we will, of necessity, refer to only a small fraction of the published work. We have focused on a few basic plasma phenomena, but, for example, have not dealt with most of the vast body of work describing dynamical phenomena in Earth's magnetosphere, including the dynamics of current sheets in Earth's magnetotail and the morphology of the dayside high latitude cusp. Several review articles and special publications are available that describe aspects of that research in detail and interested readers are referred to them (see for example, Escoubet et al. 2005 Multiscale Coupling of Sun-Earth Processes, p. 459, Keith et al. 2005 Sur. Geophys. 26, 307-339, Paschmann et al. 2005 Outer Magnetospheric Boundaries: Cluster Results, Space Sciences Series of ISSI. Berlin: Springer, Goldstein et al. 2006 Adv. Space Res. 38, 21-36, Taylor et al. 2010 The Cluster Mission: Space Plasma in Three Dimensions, Springer, pp. 309-330 and Escoubet et al. 2013 Ann. Geophys. 31, 1045-1059).
C1 [Goldstein, M. L.; Hwang, K. -Joo; Wendel, D. E.; Vinas, A. -F.; Fung, S. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Escoubet, P.] Estec, ESA, Noordwijk, Netherlands.
[Hwang, K. -Joo] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Perri, S.; Servidio, S.] Univ Calabria, Dipartimento Fis, I-87036 Arcavacata Di Rende, Italy.
[Pickett, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Parks, G. K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Sahraoui, F.] UPMC, Observ St Maur, Ecole Polytech, CNRS,Lab Phys Plasmas, F-94107 St Maur Des Fosses, France.
[Gurgiolo, C.] Bitterroot Basic Res, Hamilton, MT 59840 USA.
[Matthaeus, W.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Weygand, J. M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM melvyn.l.goldstein@nasa.gov
RI Wendel, Deirdre/D-4429-2012; NASA MMS, Science Team/J-5393-2013
OI Wendel, Deirdre/0000-0002-1925-9413; NASA MMS, Science
Team/0000-0002-9504-5214
FU NASA headquarters; MMS Interdisciplinary Science Team at the Goddard
Space Flight Center; NSF [AGS-1155841]; project POR Calabria FSE; Marie
Curie Project 'Turboplasmas' [FP7 PIRSES-2010-269297]
FX The authors would like to thank the Cluster experiment teams for making
available their data. J. S. Pickett, S. Fung, G. K. Parks, and M. L.
Goldstein would like to acknowledge the support of NASA headquarters to
the Cluster mission. A. F. Vinas, D. E. Wendell, K.-J. Hwang, and MLG
also acknowledge support from the MMS Interdisciplinary Science Team at
the Goddard Space Flight Center for its support. J. M. Weygand was
supported, in part, by NSF grant AGS-1155841, and S. Servidio
acknowledges support by the project POR Calabria FSE 2007/2013 and the
Marie Curie Project FP7 PIRSES-2010-269297 'Turboplasmas'.
NR 377
TC 6
Z9 6
U1 4
U2 16
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-3778
EI 1469-7807
J9 J PLASMA PHYS
JI J. Plasma Phys.
PD JUN
PY 2015
VL 81
AR UNSP 325810301
DI 10.1017/S0022377815000185
PN 3
PG 74
WC Physics, Fluids & Plasmas
SC Physics
GA CH8MS
UT WOS:000354291100021
ER
PT J
AU Schneider, VI
Healy, AF
Barshi, I
Bourne, LE
AF Schneider, Vivian I.
Healy, Alice F.
Barshi, Immanuel
Bourne, Lyle E., Jr.
TI Effects of difficulty, specificity, and variability on training to
follow navigation instructions
SO PSYCHONOMIC BULLETIN & REVIEW
LA English
DT Article
DE Transfer and retention; Cognitive training; Human memory and learning
ID RETENTION
AB To study the relative merits of three training principles - difficulty of training, specificity of training, and variability of training - subjects were trained to follow navigation instructions to move in a grid on a computer screen. Subjects repeated and then followed the instructions by mouse clicking on the grid. They were trained, given a short distractor task, and then tested. There were three groups, each receiving different message lengths during training: easy (short lengths), hard (long lengths), and mixed (all lengths), with all subjects given all lengths at test. At test, the mixed group was best on most lengths, the easy group was better than the hard group on short lengths, and the hard group was better than the easy group on long lengths. The results support the advantages of both specificity and variability of training but do not support the hypothesis that difficult training of the form used here would lead to overall best performance at test.
C1 [Schneider, Vivian I.; Healy, Alice F.; Bourne, Lyle E., Jr.] Univ Colorado, Dept Psychol & Neurosci, Boulder, CO 80309 USA.
[Barshi, Immanuel] NASA, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA USA.
RP Schneider, VI (reprint author), Univ Colorado, Dept Psychol & Neurosci, Muenzinger Bldg,345 UCB, Boulder, CO 80309 USA.
EM vivian.schneider@colorado.edu
FU National Aeronautics and Space Administration [NNA07CN59A, NNX10AC87A,
NNX14AB75A]; Army Research Institute [DASW01-03-K-0002]; Army Research
Office [W911NF-05-1-0153]
FX This research was supported in part by National Aeronautics and Space
Administration Grants NNA07CN59A, NNX10AC87A, and NNX14AB75A; Army
Research Institute Contract DASW01-03-K-0002; and Army Research Office
Grant W911NF-05-1-0153 to the University of Colorado. A preliminary
version of this experiment was reported at the 2007 meeting of the
Psychonomic Society, Long Beach, California, USA. Special thanks are due
to James A. Kole for insightful comments leading to the design of this
experiment and to Henry L. Roediger III and Mark Steyvers for thoughtful
suggestions concerning an earlier version of this manuscript.
NR 25
TC 0
Z9 0
U1 1
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1069-9384
EI 1531-5320
J9 PSYCHON B REV
JI Psychon. Bull. Rev.
PD JUN
PY 2015
VL 22
IS 3
BP 856
EP 862
DI 10.3758/s13423-014-0715-1
PG 7
WC Psychology, Mathematical; Psychology, Experimental
SC Psychology
GA CH7FA
UT WOS:000354199800029
PM 25128209
ER
PT J
AU Pernice, MF
De Carvalho, NV
Ratcliffe, JG
Hallett, SR
AF Pernice, Maria Francesca
De Carvalho, Nelson V.
Ratcliffe, James G.
Hallett, Stephen R.
TI Experimental study on delamination migration in composite laminates
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Delamination; Transverse cracking; Mechanical testing; Finite element
analysis (FEA)
ID SUBSEQUENT MIGRATION; FRACTURE-TOUGHNESS; INTERFACE; CRACK; GROWTH;
SPECIMENS; DCB
AB The transition of delamination growth between different ply interfaces in composite tape laminates, known as migration, was investigated experimentally. The test method used promotes delamination growth initially along a 0/theta ply interface, which eventually migrates to a neighbouring theta/0 ply interface. Specimens with theta = 60 degrees and 75 degrees were tested. Migration occurs in two main stages: (1) the initial 0/theta interface delamination turns, transforming into intraply cracks that grow through the theta plies; this process occurs at multiple locations across the width of a specimen, (2) one or more of these cracks growing through the theta plies reaches and turns into the theta/0 ply interface, where it continues to grow as a delamination. A correlation was established between these experimental observations and the shear stress sign at the delamination front, obtained by finite element analyses.
Overall, the experiments provide insight into the key mechanisms that govern delamination growth and migration. (C) 2015 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/).
C1 [Pernice, Maria Francesca; Hallett, Stephen R.] Univ Bristol, ACCIS, Bristol BS8 1TR, Avon, England.
[De Carvalho, Nelson V.] NASA, Langley Res Ctr, Natl Inst Aerosp, Resident Durabil Damage Tolerance & Reliabil Bran, Hampton, VA 23681 USA.
[Ratcliffe, James G.] NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Hampton, VA 23681 USA.
RP Pernice, MF (reprint author), Univ Bristol, ACCIS, Bristol BS8 1TR, Avon, England.
EM aemfp@my.bristol.ac.uk
RI Hallett, Stephen/D-2573-2011;
OI Hallett, Stephen/0000-0003-0751-8323; Pernice, Maria
Francesca/0000-0002-1945-8834
FU National Aeronautics and Space Administration (NASA), Langley Research
Center, United States [NNL09AA00A]; Engineering and Physical Sciences
Research Council (EPSRC), United Kingdom, through the Centre for
Doctoral Training in Advanced Composites [EP/G036772/1]
FX This material is based on work supported by the National Aeronautics and
Space Administration (NASA), Langley Research Center, United States,
under Research Cooperative Agreement No. NNL09AA00A. The first author is
supported by the Engineering and Physical Sciences Research Council
(EPSRC), United Kingdom, through the Centre for Doctoral Training in
Advanced Composites [grant number EP/G036772/1]. Special thanks to Drs.
T.K. O'Brien, J. Reeder, M. Czabaj and W. Jackson of NASA and Prof P.
Weaver of ACCIS, for the invaluable technical discussions.
NR 33
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U1 0
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
EI 1878-5840
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD JUN
PY 2015
VL 73
BP 20
EP 34
DI 10.1016/j.compositesa.2015.02.018
PG 15
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA CH0SQ
UT WOS:000353733100003
ER
PT J
AU Hartwig, JW
Darr, SR
McQuillen, JB
Rame, E
Chato, DJ
AF Hartwig, J. W.
Darr, S. R.
McQuillen, J. B.
Rame, E.
Chato, D. J.
TI A steady state pressure drop model for screen channel liquid acquisition
devices (vol 64, pg 260, 2014)
SO CRYOGENICS
LA English
DT Correction
C1 [Hartwig, J. W.; Chato, D. J.] Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH USA.
[Darr, S. R.] Univ Florida, Gainesville, FL 32611 USA.
[McQuillen, J. B.] Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH USA.
[Rame, E.] Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH USA.
RP Hartwig, JW (reprint author), NASA, Glenn Res Ctr, M-S 301-3, Cleveland, OH 44135 USA.
EM Jason.W.Hartwig@nasa.gov
RI Chato, David/B-2698-2013
OI Chato, David/0000-0003-2990-0646
NR 1
TC 0
Z9 0
U1 0
U2 1
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 JUN
PY 2015
VL 68
BP 67
EP 67
DI 10.1016/j.cryogenics.2015.04.001
PG 1
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA CH0YB
UT WOS:000353747200007
ER
PT J
AU Quick, LC
Marsh, BD
AF Quick, Lynnae C.
Marsh, Bruce D.
TI Constraining the thickness of Europa's water-ice shell: Insights from
tidal dissipation and conductive cooling
SO ICARUS
LA English
DT Article
DE Europa; Geophysics; Interiors; Tides, solid body; Jupiter, satellites
ID ART. NO. 1233; GALILEAN SATELLITES; SUBSURFACE OCEAN; LIQUID-WATER;
GEOLOGICAL EVIDENCE; INTERIOR STRUCTURE; INTERNAL STRUCTURE; THERMAL
EVOLUTION; CHAOTIC TERRAIN; SOUTH-POLE
AB The time of crystallization of a 100 km thick ocean on Europa is estimated using a Stefan-style solidification solution. This solution is then extended to estimate the present thickness of the ice shell. It is assumed that the shell is initially in a steady-state conductive regime, and the ocean is taken to be an infinite liquid half space cooling from above. We find that in the absence of tidal heating and without the presence of low-eutectic impurities to serve as anti-freezes, a 100 km thick ocean solidifies in about 64 Myr. Conversely, when considering the present thickness of Europa's ice shell, if tidal heating is included at a global dissipation rate of similar to 1 TW, the shell is found to be, on average, approximately 28 km thick. However, if this dissipative heating is solely restricted to the shell, the local rate of heating may vary significantly due to crustal compositional heterogeneities and it is shown that this process may, in turn, produce thermal maxima in the crust, which could lead to local melting and structural instabilities, perhaps associated with the formation of chaos regions. Our approach is also extended to Ganymede and Callisto in order to estimate the time of solidification of their putative subsurface oceans and the current thicknesses of their ice-I shells. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Quick, Lynnae C.] Johns Hopkins Univ, Earth & Planetary Sci Dept, Baltimore, MD 21218 USA.
[Quick, Lynnae C.; Marsh, Bruce D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Quick, LC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab Code 698, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM lynnae.c.quick@nasa.gov
FU Johns Hopkins University Bromery Fellowship; Johns Hopkins University
Applied Physics Laboratory Graduate Student Fellowship
FX L.C.Q. gratefully acknowledges funding from the Johns Hopkins University
Bromery Fellowship and the Johns Hopkins University Applied Physics
Laboratory Graduate Student Fellowship. The authors wish to thank Dr.
Amy Barr and Dr. Julie Rathbun for helpful suggestions that improved the
quality of this manuscript. We also thank Dr. James Roberts for helpful
discussions.
NR 70
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U1 6
U2 25
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 JUN
PY 2015
VL 253
BP 16
EP 24
DI 10.1016/j.icarus.2015.02.016
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH1BD
UT WOS:000353755200002
ER
PT J
AU Dohm, JM
Hare, TM
Robbins, SJ
Williams, JP
Soare, RJ
El-Maarry, MR
Conway, SJ
Buczkowski, DL
Kargel, JS
Banks, ME
Fairen, AG
Schulze-Makuch, D
Komatsu, G
Miyamoto, H
Anderson, RC
Davila, AF
Mahaney, WC
Fink, W
Cleaves, KJ
Yan, J
Hynek, B
Maruyama, S
AF Dohm, J. M.
Hare, T. M.
Robbins, S. J.
Williams, J. -P.
Soare, R. J.
El-Maarry, M. R.
Conway, S. J.
Buczkowski, D. L.
Kargel, J. S.
Banks, M. E.
Fairen, A. G.
Schulze-Makuch, D.
Komatsu, G.
Miyamoto, H.
Anderson, R. C.
Davila, A. F.
Mahaney, W. C.
Fink, W.
Cleaves, K. J.
Yan, J.
Hynek, B.
Maruyama, S.
TI Geological and hydrological histories of the Argyre province, Mars
SO ICARUS
LA English
DT Article
DE Mars; Geological processes; Astrobiology; Tectonics
ID SURFACE GROUND ICE; MAGNETIC-FIELD; ANTARCTIC PALEOSOLS; VALLES
MARINERIS; NORTHERN PLAINS; CLIMATE-CHANGE; SLOPE STREAKS; IMPACT BASIN;
EVOLUTION; SYSTEM
AB The geologic history of the multi-ringed Argyre impact basin and surroundings has been reconstructed on the basis of geologic mapping and relative-age dating of rock materials and structures. The impact formed a primary basin, rim materials, and a complex basement structural fabric including faults and valleys that are radial and concentric about the primary basin, as well as structurally-controlled local basins. Since its formation, the basin has been a regional catchment for volatiles and sedimentary materials as well as a dominant influence on the flow of surface ice, debris flows, and groundwater through and over its basement structures. The basin is interpreted to have been occupied by lakes, including a possible Mediterranean-sized sea that formed in the aftermath of the Argyre impact event The hypothesized lakes froze and diminished through time, though liquid water may have remained beneath the ice cover and sedimentation may have continued for some time. At its deepest, the main Argyre lake may have taken more than a hundred thousand years to freeze to the bottom even absent any heat source besides the Sun, but with impact-induced hydrothermal heat, geothermal heat flow due to long-lived radioactivities in early martian history, and concentration of solutes in sub-ice brine, liquid water may have persisted beneath thick ice for many millions of years. Existence of an ice-covered sea perhaps was long enough for life to originate and evolve with gradually colder and more hypersaline conditions. The Argyre rock materials, diverse in origin and emplacement mechanisms, have been modified by impact, magmatic, eolian, fluvial, lacustrine, glacial, periglacial, alluvial, colluvial, and tectonic processes.
Post-impact adjustment of part of the impact-generated basement structural fabric such as concentric faults is apparent. Distinct basin-stratigraphic units are interpreted to be linked to large-scale geologic activity far from the basin, including growth of the Tharsis magmatic-tectonic complex and the growth into southern middle latitudes of south polar ice sheets. Along with the migration of surface and sub-surface volatiles towards the central part of the primaiy basin, the substantial difference in elevation with respect to the surrounding highlands and Tharsis and the Thaumasia highlands result in the trapping of atmospheric volatiles within the basin in the form of fog and regional or local precipitation, even today. In addition, the impact event caused long-term (millions of years) hydrothermal activity, as well as deep-seated basement structures that have tapped the internal heat of Mars, as conduits, for far greater time, possibly even today. This possibility is raised by the observation of putative open-system pingos and nearby gullies that occur in linear depressions with accompanying systems of faults and fractures. Long-term water and heat energy enrichment, complemented by the interaction of the nutrient-enriched primordial crustal and mantle materials favorable to life excavated to the surface and near-surface environs through the Argyre impact event, has not only resulted in distinct geomorphology, but also makes the Argyre basin a potential site of exceptional astrobiological significance. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Dohm, J. M.; Miyamoto, H.] Univ Tokyo, Univ Museum, Bunkyo Ku, Tokyo 1130033, Japan.
[Hare, T. M.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Robbins, S. J.] SW Res Inst, Boulder, CO 80302 USA.
[Williams, J. -P.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Soare, R. J.] Dawson Coll, Dept Geog, Montreal, PQ H3Z 1A4, Canada.
[El-Maarry, M. R.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Conway, S. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Kargel, J. S.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Banks, M. E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Banks, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Fairen, A. G.] Ctr Astrobiol, Dept Planetol & Habitabil, Madrid 28850, Spain.
[Fairen, A. G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Schulze-Makuch, D.] Tech Univ Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany.
[Komatsu, G.] Univ Annunzio, Int Res Sch Planetary Sci, I-65421 Pescara, Italy.
[Anderson, R. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davila, A. F.] SETI Inst, Mountain View, CA 94043 USA.
[Mahaney, W. C.] Quaternary Surveys, Thornhill, ON L4J 1J4, Canada.
[Fink, W.] Univ Arizona, Dept Elect & Comp Engn, Coll Engn, Tucson, AZ 85721 USA.
[Cleaves, K. J.; Maruyama, S.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528551, Japan.
[Cleaves, K. J.] Inst Adv Study, Princeton, NJ 08540 USA.
[Yan, J.] Natl Astron Observ Japan, RISE Project Off, Oshu 0230861, Japan.
[Hynek, B.] Univ Colorado, Lab Atmospher & Space Phys & Geol Sci, Boulder, CO 80309 USA.
RP Dohm, JM (reprint author), Univ Tokyo, Univ Museum, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan.
EM jmd@um.u-tokyo.ac.jp
RI Williams, Jean-Pierre/C-3531-2009; Komatsu, Goro/I-7822-2012; Miyamoto,
Hideaki/B-9666-2008; Maruyama, Shigenori/C-8288-2009;
OI Williams, Jean-Pierre/0000-0003-4163-2760; Komatsu,
Goro/0000-0003-4155-108X; Conway, Susan/0000-0002-0577-2312; EL-MAARRY,
MOHAMED RAMY/0000-0002-8262-0320; Hare, Trent/0000-0001-8842-389X;
Schulze-Makuch, Dirk/0000-0002-1923-9746; Cleaves,
Henderson/0000-0003-4101-0654
FU National Aeronautics and Space Administration (NASA) Planetary Geology &
Geophysics Program; Tokyo Dome Corporation; European Research Council
under the European Union's Seventh Framework Programme (FP7), ERC
[307496]
FX J.M. Dohm was supported by the National Aeronautics and Space
Administration (NASA) Planetary Geology & Geophysics Program. Professors
Dohm and Miyamoto express their gratitude to the Tokyo Dome Corporation
for their support of the TeNQ exhibit and the branch of Space
Exploration Education & Discovery, the University Museum, the University
of Tokyo. Work by A.G. Fairen was supported by the European Research
Council under the European Union's Seventh Framework Programme
(FP7/2007-2013), ERC Grant agreement No. 307496. We are grateful for the
thoughtful reviews by T. Ohman and an anonymous reviewer which
ultimately resulted in an improved manuscript.
NR 195
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2015
VL 253
BP 66
EP 98
DI 10.1016/j.icarus.2015.02.017
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH1BD
UT WOS:000353755200007
ER
PT J
AU Khayat, AS
Villanueva, GL
Mumma, MJ
Tokunaga, AT
AF Khayat, A. S.
Villanueva, G. L.
Mumma, M. J.
Tokunaga, A. T.
TI A search for SO2, H2S and SO above Tharsis and Syrtis volcanic districts
on Mars using ground-based high-resolution submillimeter spectroscopy
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Abundances, atmospheres; Atmospheres, structure;
Radiative transfer; Volcanism
ID MARTIAN ATMOSPHERE; ROTATIONAL TRANSITIONS; METHANE; DETECTABILITY;
SPECTROMETER; MILLIMETER; PLANETARY; EMISSION; DATABASE; SURFACE
AB We surveyed the Tharsis and Syrtis volcanic regions on Mars during 23 November 2011 to 13 May 2012 which correspOnded to its mid Northern Spring and early Northern Summer seasons (L-s = 34-110 degrees). Strong submillimeter rotational transitions of sulfur dioxide (SO2), sulfur monoxide (SO) and hydrogen sulfide (H2S) were targeted. No active release was detected, and we infer 2 sigma upper limits across the disk of the planet of 1.1 ppb, 0.7 ppb and 1.3 ppb for SO2, SO and H2S, respectively. Our derived upper limit for SO2 is comparable to previously reported limits, whereas for H2S we set a more stringent upper limit than previously measured, and we establish a limit for SO. Among the targeted molecules, SO2 is the strongest indicator for volcanic outgassing. Assuming a photochemical lifetime of 2 years for SO2, our upper limit of 1.1 ppb implies an outgassing rate less than 55 metric tons/day. This rate limits the daily amount of degassing magma to less than 12,000 m(3). Our sensitivity is sufficient to detect a volcanic release on Mars that is 4% the SO2 released continuously from Kilauea volcano in Hawaii or 5% that of the Masaya volcano in Nicaragua. The non-detection of the sulfur compounds in the atmosphere of Mars indicates the absence of major volcanic outgassing. Published by Elsevier Inc.
C1 [Khayat, A. S.; Tokunaga, A. T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Villanueva, G. L.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Khayat, AS (reprint author), Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
EM Khayat@ifa.hawaii.edu
FU National Science Foundation [AST-0838261]; NASA Planetary Astronomy
Program [NNX08AE38A]; NASA [NNH14CK55B]; RTOP [344-32-07]; NASA's
Astrobiology Program [RTOP 344-53-51]
FX We are grateful to the staff at the Caltech Submillimeter Observatory
(CSO), Simon Radford, Timm Riesen and Louis Scuderi for their support
during the Mars observing runs. This material is based upon work at the
CSO, which is operated by the California Institute of Technology under
cooperative agreement with the National Science Foundation, Grant No.
AST-0838261. We gratefully acknowledge the support from the NASA
Planetary Astronomy Program under Cooperative Agreement NNX08AE38A, NASA
contract NNH14CK55B, RTOP 344-32-07 and NASA's Astrobiology Program
(RTOP 344-53-51) that supported M.J.M., and G.L.V. A.J.K. would like to
thank Norbert Schorghofer who provided valuable ideas to the writing and
undertaking of the research summarized here. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Maunakea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 56
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2015
VL 253
BP 130
EP 141
DI 10.1016/j.icarus.2015.02.028
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH1BD
UT WOS:000353755200010
ER
PT J
AU Rhoden, AR
Hurford, TA
Roth, L
Retherford, K
AF Rhoden, Alyssa Rose
Hurford, Terry A.
Roth, Lorenz
Retherford, Kurt
TI Linking Europa's plume activity to tides, tectonics, and liquid water
SO ICARUS
LA English
DT Article
DE Europa; Tectonics; Jupiter, satellites; Satellites, surfaces
ID NONSYNCHRONOUS ROTATION; TIDAL STRESSES; SOUTH-POLE; ENCELADUS;
FRACTURES; OBLIQUITY; EARTH; OSCILLATIONS; SATELLITES; ATMOSPHERE
AB Much of the geologic activity preserved on Europa's icy surface has been attributed to tidal deformation, mainly due to Europa's eccentric orbit. Although the surface is geologically young (30-80 Myr), there is little information as to whether tidally-driven surface processes are ongoing. However, a recent detection of water vapor near Europa's south pole suggests that it may be geologically active. Initial observations indicated that Europa's plume eruptions are time-variable and may be linked to its tidal cycle. Saturn's moon, Enceladus, which shares many similar traits with Europa, displays tidally-modulated plume eruptions, which bolstered this interpretation. However, additional observations of Europa at the same time in its orbit failed to yield a plume detection, casting doubt on the tidal control hypothesis. The purpose of this study is to analyze the timing of plume eruptions within the context of Europa's tidal cycle to determine whether such a link exists and examine the inferred similarities and differences between plume activity on Europa and Enceladus. To do this, we determine the locations and orientations of hypothetical tidally-driven fractures that best match the temporal variability of the plumes observed at Europa. Specifically, we identify model faults that are in tension at the time in Europa's orbit when a plume was detected and in compression at times when the plume was not detected. We find that tidal stress driven solely by eccentricity is incompatible with the observations unless additional mechanisms are controlling the eruption timing or restricting the longevity of the plumes. The addition of obliquity tides, and corresponding precession of the spin pole, can generate a number of model faults that are consistent with the pattern of plume detections. The locations and orientations of these hypothetical source fractures are robust across a broad range of precession rates and spin pole directions. Analysis of the stress variations across the fractures suggests that the plumes would be best observed earlier in the orbit (true anomaly similar to 120 degrees). Our results indicate that Europa's plumes, if confirmed, differ in many respects from the Enceladean plumes and that either active fractures or volatile sources are rare. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Rhoden, Alyssa Rose; Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
[Rhoden, Alyssa Rose] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Roth, Lorenz; Retherford, Kurt] SW Res Inst, San Antonio, TX 78238 USA.
[Roth, Lorenz] Royal Inst Technol, Sch Elect Engn, Stockholm, Sweden.
RP Rhoden, AR (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM Alyssa.Rhoden@jhuapl.edu
RI Hurford, Terry/F-2625-2012
FU NASA through Space Telescope Science Institute [13619]; NASA
[NAS5-26555]
FX The authors would like to thank G. Collins and P. Geissler for
thoughtful reviews that improved this manuscript. A. Rhoden was
partially supported through an appointment to the NASA Postdoctoral
Program, administered by ORAU. L. Roth and K. Retherford were supported
through HST Program number 13619 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.
NR 48
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U1 9
U2 25
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 JUN
PY 2015
VL 253
BP 169
EP 178
DI 10.1016/j.icarus.2015.02.023
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH1BD
UT WOS:000353755200015
ER
PT J
AU Deau, E
AF Deau, Estelle
TI The opposition effect in Saturn's main rings as seen by Cassini ISS: 2.
Constraints on the ring particles and their regolith with analytical
radiative transfer models
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, rings; Photometry
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DENSE PLANETARY RINGS;
SELF-GRAVITY WAKES; THEORETICAL PHOTOMETRIC FUNCTION; HEAD-ON
COLLISIONS; COHERENT BACKSCATTERING; B-RING; STELLAR OCCULTATION;
LIGHT-SCATTERING; NUMERICAL-SIMULATION
AB The opposition effect in Saturn's main rings is characterized by a surge in ring brightness, when the phase angle approaches zero degree. This effect can be used to derive: physical properties of the ring particles and the ring layer, via the shadow hiding mechanism; and physical properties of the regolith grains that cover the ring particles, via the coherent backscattering mechanism. Since the exact origin of this effect is still a matter of debate, we try different combinations of the physical mechanisms cited above to derive constraints on the nature, the texture, and the disposition of the ring particles. In particular, we derive regolith grain sizes, particle sizes, differential power law indices, filling factors, and vertical thicknesses; and we compare them with independent works to validate or invalidate the assumptions of the opposition effect models used. Our coherent backscattering model provides grain sizes similar to the sizes estimated from water ice band depth modeling in the near infrared. Our shadow hiding model assuming a power law size distribution provides vertical thickness consistent with previous estimates from density waves measurements and N-body simulations. We show that the assumption of an homogeneous medium is a key parameter in the shadow hiding modeling. In the case of the B ring, we demonstrate that all previous photometric models assuming an homogeneous ring layer (i.e. uniform particle size distribution, random spacing of the particles and small filling factor) have led to a set of unconfirmed solutions. This result reinforces the idea that the Saturn's main rings should be modeled as an heterogeneous medium. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Deau, Estelle] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Deau, Estelle] CEA Saclay, IRFU, Serv Astrophys, Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France.
RP Deau, E (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr,M-S 230-207G, Pasadena, CA 91109 USA.
EM Estelle.Deau@jpl.nasa.gov
FU Conseil Regional de la Martinique; CNES (Centre National d'Etudes
Spatiales); CNRS (Centre National de la Recherche Scientifique);
Postdoctoral Program of NASA [09-CDAP09-0033]
FX This study was originally performed at CEA Saclay, and was initially
funded by the Conseil Regional de la Martinique, from E. Deau's funding;
the CNES (Centre National d'Etudes Spatiales), and the CNRS (Centre
National de la Recherche Scientifique), from A. Brahic's funding. A part
of this study was performed at JPL (Jet Propulsion Laboratory), under
contract with NASA (National Aeronautics and Space Administration) and
California Institute of Technology, and was funded by the Postdoctoral
Program of NASA, led by ORAU (OakRidge Associated Universities), and the
Cassini Project (09-CDAP09-0033). Government sponsorships acknowledged.
NR 190
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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 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2015
VL 253
BP 311
EP 345
DI 10.1016/j.icarus.2013.08.031
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH1BD
UT WOS:000353755200024
ER
PT J
AU Reese, DC
Brodeur, RD
AF Reese, Douglas C.
Brodeur, Richard D.
TI Species associations and redundancy in relation to biological hotspots
within the northern California Current ecosystem
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article
DE Hotspots; Community composition; Species associations; Redundancy;
Ecosystem resilience; Nekton; Jellyfish; California Current
ID OCEANOGRAPHIC CONDITIONS; COMMUNITY STRUCTURE; SPATIAL OVERLAP;
CLIMATE-CHANGE; OCEAN; PACIFIC; ZOOPLANKTON; IMPACTS; OREGON; FISH
AB The dynamic nature of biological hotspots, while well recognized, is not well understood. We hypothesize that the persistence of hotspots in the northern California Current System (CCS), despite seasonal and annual changes in the nekton community species composition, is related to associations among species and their functional redundancy. To address this hypothesis, sampling was conducted during June and August of 2000 and 2002 within two hotspots occurring between Newport, Oregon and Crescent City, California in the coastal CCS. Associations were examined to identify potentially complementary and redundant species. The strongest negative associations were between jellyfish and fish species, with strong positive associations evident among several fish species. Dominant species varied seasonally and annually, although evidence indicated replacement of dominant species by other similar species with respect to functional group and preferred habitat. This finding suggests that the persistence of these biological hotspots is related to species redundancy and is an important attribute contributing to stability within this highly variable system. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Reese, Douglas C.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA.
[Brodeur, Richard D.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Fish Ecol Div, Newport, OR 97365 USA.
RP Reese, DC (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA.
EM Doug.Reese@oregonstate.edu
FU U.S. GLOBEC Northeast Pacific Program
FX We thank the crew and scientists who assisted in the collection of
samples at sea, especially B. Emmett, J. Fisher, and T. Miller. T.
Miller was especially helpful in providing the information from diet
analyses used in the classification of species by functional group. We
also thank B. Pearcy, B. McCune, D. Ainley, and two anonymous reviewers
for providing valuable comments on the manuscript. Funding for this
study was provided by the U.S. GLOBEC Northeast Pacific Program.
NR 56
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U1 2
U2 14
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 JUN
PY 2015
VL 146
SI SI
BP 3
EP 16
DI 10.1016/j.jmarsys.2014.10.009
PG 14
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA CG8ZP
UT WOS:000353604500002
ER
PT J
AU Kaynak, Y
Karaca, HE
Noebe, RD
Jawahir, IS
AF Kaynak, Yusuf
Karaca, Haluk E.
Noebe, Ronald D.
Jawahir, I. S.
TI The Effect of Active Phase of the Work Material on Machining Performance
of a NiTi Shape Memory Alloy
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article; Proceedings Paper
CT Bulk Metallic Glasses 11 Symposium
CY FEB 16-20, 2014
CL TMS Annual Meeting & Exhibit, San Diego, CA
SP Bulk Met Glasses Symposia
HO TMS Annual Meeting & Exhibit
ID TOOL-WEAR; TI-6AL-4V; TRANSFORMATION; EVOLUTION; TITANIUM
AB Poor machinability with conventional machining processes is a major shortcoming that limits the manufacture of NiTi components. To better understand the effects of phase state on the machining performance of NiTi alloys, cutting temperature, tool-wear behavior, cutting force components, tool-chip contact length, chip thickness, and machined surface quality data were generated from a NiTi alloy using precooled cryogenic, dry, minimum quantity lubrication (MQL), and preheated machining conditions. Findings reveal that machining NiTi in the martensite phase, which was achieved through precooled cryogenic machining, profoundly improved the machining performance by reducing cutting force components, notch wear, and surface roughness. Machining in the austenite state, achieved through preheating, did not provide any benefit over dry and MQL machining, and these processes were, in general, inferior to cryogenic machining in terms of machining performance, particularly at higher cutting speeds.
C1 [Kaynak, Yusuf] Marmara Univ, Fac Technol, Dept Mech Engn, TR-34722 Istanbul, Turkey.
[Karaca, Haluk E.; Jawahir, I. S.] Univ Kentucky, Coll Engn, Dept Mech Engn, Lexington, KY 40506 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Jawahir, I. S.] Univ Kentucky, ISM, Lexington, KY 40506 USA.
EM yusuf.kaynak@marmara.edu.tr
FU NASA EPSCOR Program [NNX11AQ31A]; NASA FAP Aeronautical Sciences; TACP
Transformational Tools & Technologies Projects (Dale Hopkins, Technical
Lead)
FX Support from the NASA EPSCOR Program under Grant No. NNX11AQ31A and the
NASA FAP Aeronautical Sciences and TACP Transformational Tools &
Technologies Projects (Dale Hopkins, Technical Lead) are gratefully
acknowledged.
NR 29
TC 4
Z9 4
U1 2
U2 8
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 JUN
PY 2015
VL 46A
IS 6
BP 2625
EP 2636
DI 10.1007/s11661-015-2828-1
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA CG4EQ
UT WOS:000353236700034
ER
PT J
AU Pollak, L
Mehta, SK
Pierson, DL
Sacagiu, T
Kalmanovich, SA
Cohrs, RJ
AF Pollak, L.
Mehta, S. K.
Pierson, D. L.
Sacagiu, T.
Kalmanovich, S. Avneri
Cohrs, R. J.
TI Varicella-zoster DNA in saliva of patients with meningoencephalitis: a
preliminary study
SO ACTA NEUROLOGICA SCANDINAVICA
LA English
DT Article
DE varicella zoster; meningoencephalitis; saliva
ID HERPES-SIMPLEX-VIRUS; RELIABLE DETECTION; CLINICAL-FEATURES; ORAL FLUID;
REACTIVATION; INFECTIONS; DISEASE; PRESENTATIONS; COMPLICATIONS;
ENCEPHALITIS
AB ObjectivesSince the routine use of polymerase chain reaction testing (PCR) in diagnosing herpes infections, varicella-zoster virus is increasingly recognized as a cause of varicella-zoster meningoencephalitis (VZV ME) among immunocompetent patients. We were interested to determine whether patients with VZV ME had VZV DNA in their saliva during the acute phase of the illness.
Materials and methodsForty-five consecutive patients who underwent a lumbar puncture for diagnostic purposes were included in the study. The cerebrospinal fluid was examined for the presence of VZV DNA by PCR, and patients with positive findings were treated with acyclovir. The saliva was later analyzed in a blinded fashion for the presence of VZV DNA.
ResultsVZV DNA was found in saliva in four of five (80%) patients with PCR confirmed VZV ME (sensitivity 0.8, specificity 0.84, and likelihood ratio 5). This was significantly more than in patients with non-zoster viral ME (0%, P=0.009), parainfectious headache (12%, P=0.03) and controls (9.5%, P=0.007). In immunocompromised patients with systemic lymphoma and AIDS, VZV DNA was present at a similar rate (67%, P=0.6).
ConclusionsWe have found VZV DNA in saliva of patients with PCR confirmed VZV ME at a higher proportion than in controls and patients with non-VZV viral ME. This finding might be of clinical importance, especially in immunocompetent individuals with suspected VZV ME where the results of genetic and immunological testing are not conclusive.
C1 [Pollak, L.; Sacagiu, T.; Kalmanovich, S. Avneri] Tel Aviv Univ, Sackler Fac Med, Assaf Harofeh Med Ctr, Dept Neurol, Zerifin, Israel.
[Mehta, S. K.; Pierson, D. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Cohrs, R. J.] Univ Colorado, Sch Med, Dept Neurol, Aurora, CO USA.
[Cohrs, R. J.] Univ Colorado, Sch Med, Dept Microbiol, Aurora, CO USA.
RP Pollak, L (reprint author), Kibutz Galuyot 4, IL-74012 Ness Ziona, Israel.
EM lea.pollak@gmail.com
NR 23
TC 0
Z9 0
U1 1
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0001-6314
EI 1600-0404
J9 ACTA NEUROL SCAND
JI Acta Neurol. Scand.
PD JUN
PY 2015
VL 131
IS 6
BP 417
EP 421
DI 10.1111/ane.12335
PG 5
WC Clinical Neurology
SC Neurosciences & Neurology
GA CF4NH
UT WOS:000352525500011
PM 25314141
ER
PT J
AU Sen Gupta, A
Tarboton, DG
Hummel, P
Brown, ME
Habib, S
AF Sen Gupta, A.
Tarboton, D. G.
Hummel, P.
Brown, M. E.
Habib, S.
TI Integration of an energy balance snowmelt model into an open source
modeling framework
SO ENVIRONMENTAL MODELLING & SOFTWARE
LA English
DT Article
DE Model integration; Data model; Energy balance; Snow melt; Glacier melt
ID SURFACE-TEMPERATURE; INTERFACE; SYSTEM; COVER; PRECIPITATION;
SIMULATIONS; PREDICTION; DESIGN; NETCDF; MODIS
AB This paper presents a data model for organizing the inputs and outputs of an energy balance snowmelt model (the Utah Energy Balance Model, UEB) that provides a foundation for its integration into the EPA BASINS modeling framework and enables its coupling with other hydrologic models in this system. Having UEB as a BASINS component has facilitated its coupling with the Geospatial Streamflow Forecast Model (GeoSFM) to compute the melting of glaciers and subsequent streamflow in the Himalayas. The data model uses a combination of structured text and network Common Data Form (netCDF) files to represent parameters, geographical, time series, and gridded space-time data. We describe the design and structure of this data model, integration methodology of UEB and GeoSFM and illustrate the effectiveness of the resulting coupled models for the computation of surface water input and streamflow for a glaciated watershed in Nepal Himalayas. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Sen Gupta, A.; Tarboton, D. G.] Utah State Univ, Dept Civil & Environm Engn, Logan, UT 84322 USA.
[Hummel, P.] AQUA TERRA Consultants, Decatur, GA USA.
[Brown, M. E.; Habib, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sen Gupta, A (reprint author), Utah State Univ, Utah Water Res Lab, Civil & Environm Engn, 4110 Old Main Hill, Logan, UT 84322 USA.
EM avirup.sengupta@aggiemail.usu.edu
RI Sen Gupta, Avirup/L-8938-2014; Brown, Molly/E-2724-2010;
OI Sen Gupta, Avirup/0000-0001-5972-5186; Brown, Molly/0000-0001-7384-3314;
Tarboton, David/0000-0002-1998-3479
FU NASA [NNX11AK036]
FX This research was supported by NASA award NNX11AK036. The authors are
thankful to Dr. Adina Racoviteanu from Laboratoire de Glaciologie et
Geophysique de l'Environnement for providing glacier mapping and
substrate albedo data for the Langtang Khola Watershed. We would also
like to thank HKH Cryosphere Monitoring Project implemented by ICIMOD
and ICIMOD's glacier hydrologist Dr. Joseph Michael Shea for providing
monthly temperature lapse rate data for Langtang Khola watershed.
NR 75
TC 1
Z9 1
U1 2
U2 21
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 JUN
PY 2015
VL 68
BP 205
EP 218
DI 10.1016/j.envsoft.2015.02.017
PG 14
WC Computer Science, Interdisciplinary Applications; Engineering,
Environmental; Environmental Sciences
SC Computer Science; Engineering; Environmental Sciences & Ecology
GA CG1ZC
UT WOS:000353073700017
ER
PT J
AU Walsh, WA
Brodziak, J
AF Walsh, William A.
Brodziak, Jon
TI Billfish CPUE standardization in the Hawaii longline fishery: Model
selection and multimodel inference
SO FISHERIES RESEARCH
LA English
DT Article; Proceedings Paper
CT 5th International Billfish Symposium
CY NOV 04-08, 2013
CL Taipei, TAIWAN
DE Istiophoridae; Incidental catches; CPUE standardization; Model
selection; Zero-inflation; Negative binomial
ID MARLIN MAKAIRA-NIGRICANS; PACIFIC-OCEAN; BLUE MARLIN; ABUNDANCE; CATCH
AB This paper presents catch per unit effort (CPUE) standardizations and model selection procedures for four billfish species (Family Istiophoridae) caught primarily as bycatch in the Hawaii-based pelagic longline fishery during 1995-2011: Blue marlin Makaira nigricans; Striped marlin Kajikia audax;,Shortbill spearfish Tetrapturus angustirostris; and Sailfish Istiophorus platypterus. The first three species were analyzed on a fishery-wide basis. For sailfish, the fishery data came exclusively from tuna-targeted longline sets in the deep-set sector of the Hawaii-based fishery. We used fishery observer data from the NOAA Fisheries Pacific Islands Regional Observer Program to fit the CPUE standardization models. In this context, our objective was to investigate the quality of model fit for five types of generalized linear models (GLMs: Poisson; negative binomial; zero-inflated Poisson; zero-inflated negative binomial; delta-Gamma). Each of these models represented a different hypothesis about the capture process for a bycatch species for which the catch data primarily consisted of zero catch observations. The five GLMs were fitted by forward entry variable selection, and the best fitting GLM for each species was selected on the basis of Akaike Information Criterion values and calculated Akaike weights. The best-fitting model selected for each species was a zero-inflated negative binomial GLM (ZINB). The ZINB model was comprised of a negative binomial counts model for expected zero catch sets and a positive catch per set distribution along with a binomial inflation model to account for excess zeros. For each species, the important explanatory variables for standardizing CPUE were fishing year, fishing (i.e., calendar) quarter, and fishing region. The best-fitting models indicated that standardized CPUE for striped and blue marlins decreased significantly during the study period. Because the ZINB model was selected as the best fitting model for all species, we suggest that longline CPUE for incidentally caught billfishes is best represented as a process characterized by zero inflation and overdispersion in the positive catches and expected zero catches. We therefore recommend that ZINB models be considered as an a priori model for CPUE standardizations of billfishes and other bycatch species in longline fisheries. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Walsh, William A.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
[Brodziak, Jon] Natl Marine Fisheries Serv, NOAA Fisheries, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
RP Walsh, WA (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, 1845 Wasp Blvd, Honolulu, HI 96818 USA.
EM William.Walsh@noaa.gov
NR 29
TC 2
Z9 2
U1 4
U2 26
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 JUN
PY 2015
VL 166
SI SI
BP 151
EP 162
DI 10.1016/j.fishres.2014.07.015
PG 12
WC Fisheries
SC Fisheries
GA CG2AN
UT WOS:000353077400017
ER
PT J
AU Sankararaman, S
Mahadevanb, S
AF Sankararaman, Shankar
Mahadevanb, Sankaran
TI Integration of model verification, validation, and calibration for
uncertainty quantification in engineering systems
SO RELIABILITY ENGINEERING & SYSTEM SAFETY
LA English
DT Article
DE Multi-level system; Uncertainty quantification; Bayesian network;
Calibration; Validation; Verification
ID COMPUTATIONAL MODELS; ERROR ESTIMATION; EPISTEMIC UNCERTAINTY;
FINITE-ELEMENTS; CODE; SIMULATION; NETWORKS; DYNAMICS; BAYES
AB This paper proposes a Bayesian methodology to integrate model verification, validation, and calibration activities for the purpose of overall uncertainty quantification in different types of engineering systems. The methodology is first developed for single-level models, and then extended to systems that are studied using multi-level models that interact with each other. Two types of interactions amongst multilevel models are considered: (1) Type-I, where the output of a lower-level model (component and/or subsystem) becomes an input to a higher level system model, and (2) Type-II, where parameters of the system model are inferred using lower-level models and tests (that describe simplified components and/ or isolated physics). The various models, their inputs, parameters, and outputs, experimental data, and various sources of model error are connected through a Bayesian network. The results of calibration, verification, and validation with respect to each individual model are integrated using the principles of conditional probability and total probability, and propagated through the Bayesian network in order to quantify the overall system-level prediction uncertainty. The proposed methodology is illustrated with numerical examples that deal with heat conduction and structural dynamics. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Sankararaman, Shankar] SGT Inc, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Mahadevanb, Sankaran] Vanderbilt Univ, Dept Civil & Environm Engn, Nashville, TN 37235 USA.
RP Sankararaman, S (reprint author), SGT Inc, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM shankar.sankararaman@nasa.gov
FU Sandia National Laboratories [BG-7732]
FX The study in this paper was supported by funds from Sandia National
Laboratories through Contract no. BG-7732 (Technical Monitor: Dr. Angel
Urbina). The support is gratefully acknowledged.
NR 80
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U1 8
U2 28
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0951-8320
EI 1879-0836
J9 RELIAB ENG SYST SAFE
JI Reliab. Eng. Syst. Saf.
PD JUN
PY 2015
VL 138
BP 194
EP 209
DI 10.1016/j.ress.2015.01.023
PG 16
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA CF6IR
UT WOS:000352660900018
ER
PT J
AU Beck, BS
Schiller, NH
Jones, MG
AF Beck, Benjamin S.
Schiller, Noah H.
Jones, Michael G.
TI Impedance assessment of a dual-resonance acoustic liner
SO APPLIED ACOUSTICS
LA English
DT Article
DE Acoustic liners; Absorption; Noise control
ID MICRO-PERFORATED PANEL; SOUND-ABSORPTION; DETAILED ANALYSIS; ABSORBERS;
SYSTEMS; CAVITY; GAPS
AB Acoustic liners are commonly used to reduce noise from commercial aircraft engines. Engine liners are placed in the nacelle inlet and aft bypass duct to attenuate the noise radiated from the engine. Traditional engine liners are constructed of a perforated facesheet over a honeycomb structure to create a quarter-wave absorber. With this design, the low frequency performance of the liner is limited by the depth of the honeycomb. However, with advances in engine design, lower frequency sound absorption is becoming more critical while liner depth must be minimized. Acoustic metamaterials can exhibit unique acoustic behavior using periodically arranged sub-wavelength resonators. Researchers have shown that acoustic metamaterials can effectively block the propagation of low-frequency acoustic waves. Therefore, acoustic metamaterial-inspired concepts are being investigated to improve the low frequency performance of engine liners. A proposed dual-resonance liner is presented here that combines the idea of a Helmholtz resonator metamaterial with a traditional quarter-wave acoustic liner. The low frequency acoustic absorption of a traditional liner can be significantly increased by adding a second, low frequency resonance to the system. The normal incidence absorption coefficient of the proposed liner is more than 10 times larger than a conventional honeycomb liner at the designed Helmholtz resonance frequency while retaining similar performance at higher frequencies. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Beck, Benjamin S.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Schiller, Noah H.; Jones, Michael G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Beck, BS (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM ben.beck@nasa.gov
NR 27
TC 0
Z9 0
U1 6
U2 51
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0003-682X
EI 1872-910X
J9 APPL ACOUST
JI Appl. Acoust.
PD JUN
PY 2015
VL 93
BP 15
EP 22
DI 10.1016/j.apacoust.2015.01.011
PG 8
WC Acoustics
SC Acoustics
GA CF0QL
UT WOS:000352249200003
ER
PT J
AU Moreno-Madrinan, MJ
Rickman, DL
Ogashawara, I
Irwin, DE
Ye, J
Al-Hamdan, MZ
AF Moreno-Madrinan, Max J.
Rickman, Douglas L.
Ogashawara, Igor
Irwin, Daniel E.
Ye, Jun
Al-Hamdan, Mohammad Z.
TI Using remote sensing to monitor the influence of river discharge on
watershed outlets and adjacent coral Reefs: Magdalena River and Rosario
Islands, Colombia
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Remote sensing; MODIS; TRMM; Water quality; Suspended sediments
ID TOTAL SUSPENDED MATTER; TAMPA-BAY; MONTASTRAEA-ANNULARIS; CARIBBEAN SEA;
250-M IMAGERY; TURBIDITY; IMPACT; USA
AB Worldwide, coral reef ecosystems are being increasingly threatened by sediments loads from river discharges, which in turn are influenced by changing rainfall patterns due to climate change and by growing human activity in their watersheds. In this case study, we explored the applicability of using remote sensing (RS) technology to estimate and monitor the relationship between water quality at the coral reefs around the Rosario Islands, in the Caribbean Sea, and the rainfall patterns in the Magdalena River watershed. From the Moderate Resolution Imaging Spectroradiometer (MODIS), this study used the water surface reflectance product (MOD09GQ) to estimate water surface reflectance as a proxy for sediment concentration and the land cover product (MCD12Q1 V51) to characterize land cover of the watershed. Rainfall was estimated by using the 3B43 V7 product from the Tropical Rainforest Measuring Mission (TRMM). For the first trimester of each year, we investigated the inter-annual temporal variation in water surface reflectance at the Rosario Islands and at the three main mouths of the Magdalena River watershed. No increasing or decreasing trends of water surface reflectance were detected for any of the sites for the study period 2001-2014 (p > 0.05) but significant correlations were detected among the trends of each site at the watershed mouths (r = 0.57-0.90, p < 0.05) and between them and the inter-annual variation in rainfall on the watershed (r = 0.63-0.67,p < 0.05). Those trimesters with above-normal water surface reflectance at the mouths and above-normal rainfall at the watershed coincided with La Nina conditions while the opposite was the case during El Nino conditions. Although, a preliminary analysis of inter-annual land cover trends found only cropland cover in the watershed to be significantly correlated with water surface reflectance at two of the watershed mouths (r = 0.58 and 0.63, p < 0.05), the validation analysis draw only a 40.7% of accuracy in this land cover classification. This requires further analysis to confirm the impact of the cropland on the water quality at the watershed outlets. Spatial analysis with MOD09GQ imagery detected the overpass of river plumes from Barbacoas Bay over the Rosario Islands waters. (C) 2015 The Authors. Published by Elsevier B.V.
C1 [Moreno-Madrinan, Max J.] Indiana Univ, Fairbanks Sch Publ Hlth, Dept Environm Hlth, IUPUI, Indianapolis, IN 46202 USA.
[Rickman, Douglas L.] NASA, Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
[Ogashawara, Igor] Indiana Univ Purdue Univ, Sch Sci, Dept Earth Sci, IUPUI, Indianapolis, IN 46202 USA.
[Irwin, Daniel E.] NASA, Earth Sci Off, SERVIR, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Ye, Jun] Univ Akron, Dept Stat, Akron, OH 44325 USA.
[Al-Hamdan, Mohammad Z.] Univ Space Res Assoc, NASA, Inst Sci & Technol, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Moreno-Madrinan, MJ (reprint author), Indiana Univ, Fairbanks Sch Publ Hlth, Dept Environm Hlth, IUPUI, Indianapolis, IN 46202 USA.
EM mmorenom@iu.edu
OI Rickman, Doug/0000-0003-3409-2882
FU NASA Postdoctoral Program (NPP); SERVIR/MSFC through the NPP under
contract with Oak Ridge Associated Universities
FX This research was conceived and initiated while the main author was
working with SERVIR at the Marshall Space Flight Center (MSFC) during
his fellowship with the NASA Postdoctoral Program (NPP). Partial funds
were provided by SERVIR/MSFC through the NPP under contract with Oak
Ridge Associated Universities. We thank Africa Flores-Cordova from
University of Alabama in Huntsville (UAH) for her help with SRTM data
and delineating the watershed and Dr. Ashutosh Limaye from NASA/MSFC for
his advice with the use of TRMM data. We also thank Damien Jules
Sulla-Menashe from Boston University for his advice regarding use and
limitations of the land cover product, MCD12Q1.
NR 39
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U1 3
U2 41
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD JUN
PY 2015
VL 38
BP 204
EP 215
DI 10.1016/j.jag.2015.01.008
PG 12
WC Remote Sensing
SC Remote Sensing
GA CE6TC
UT WOS:000351970100021
ER
PT J
AU Abrams, M
Tsu, H
Hulley, G
Iwao, K
Pieri, D
Cudahy, T
Kargel, J
AF Abrams, Michael
Tsu, Hiroji
Hulley, Glynn
Iwao, Koki
Pieri, David
Cudahy, Tom
Kargel, Jeffrey
TI The Advanced Spaceborne Thermal Emission and Reflection Radiometer
(ASTER) after fifteen years: Review of global products
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Review
DE ASTER; Terra; Earth Observing System; Global data
ID MULTISPECTRAL SATELLITE DATA; LAND-SURFACE TEMPERATURE; DEM; METHODOLOGY
AB The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) is a 15-channel imaging instrument operating on NASA's Terra satellite. A joint project between the U.S. National Aeronautics and Space Administration and Japan's Ministry of Economy, Trade, and Industry, ASTER has been acquiring data for 15 years, since March 2000. The archive now contains over 2.8 million scenes; for the majority of them, a stereo pair was collected using nadir and backward telescopes imaging in the NIR wavelength. The majority of users require only a few to a few dozen scenes for their work. Studies have ranged over numerous scientific disciplines, and many practical applications have benefited from ASTER's unique data. A few researchers have been able to mine the entire ASTER archive, that is now global in extent due to the long duration of the mission. Six examples of global products are described in this contribution: the ASTER Global Digital Elevation Model (GDEM), the most complete, highest resolution DEM available to all users; the ASTER Emissivity Database (ASTER GED), a global 5-band emissivity map of the land surface; the ASTER Global Urban Area Map (AGURAM), a 15-m resolution database of over 3500 cities; the ASTER Volcano Archive (AVA), an archive of over 1500 active volcanoes; ASTER Geoscience products of the continent of Australia; and the Global Ice Monitoring from Space (GUMS) project. (C) 2015. Elsevier B.V. All rights reserved.
C1 [Abrams, Michael; Hulley, Glynn; Pieri, David] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Tsu, Hiroji] Japan Space Syst, Tokyo, Japan.
[Iwao, Koki] Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki, Japan.
[Cudahy, Tom] CSIRO, Perth, WA, Australia.
[Kargel, Jeffrey] Univ Arizona, Tucson, AZ USA.
RP Abrams, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 40
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U1 4
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD JUN
PY 2015
VL 38
BP 292
EP 301
DI 10.1016/j.jag.2015.01.013
PG 10
WC Remote Sensing
SC Remote Sensing
GA CE6TC
UT WOS:000351970100029
ER
PT J
AU Parsani, M
Carpenter, MH
Nielsen, EJ
AF Parsani, Matteo
Carpenter, Mark H.
Nielsen, Eric J.
TI Entropy stable discontinuous interfaces coupling for the
three-dimensional compressible Navier-Stokes equations
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Entropy stability; Discontinuous interface coupling; Summation-by-parts
(SBP) operators; Compressible Navier-Stokes equations; High order
discontinuous methods
ID CONSERVATION-LAWS; SCHEMES; SYSTEMS; EULER; FORM
C1 [Parsani, Matteo; Carpenter, Mark H.; Nielsen, Eric J.] NASA Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA.
RP Parsani, M (reprint author), NASA Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA.
EM matteo.parsani@nasa.gov; mark.h.carpenter@nasa.gov;
eric.j.nielsen@nasa.gov
OI Parsani, Matteo/0000-0001-7300-1280
FU NASA Postdoctoral Program at the Langley Research Center; NASA
FX Special thanks are extended to Dr. Mujeeb Malik for funding this work as
part of the "Revolutionary Computational Aerosciences" project. This
research was also supported by an appointment to the NASA Postdoctoral
Program at the Langley Research Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The authors are
also grateful to Professor Magnus Svard for the fruitful discussions on
entropy stability.
NR 16
TC 5
Z9 5
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 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD JUN 1
PY 2015
VL 290
BP 132
EP 138
DI 10.1016/j.jcp.2015.02.042
PG 7
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA CE4XK
UT WOS:000351833400007
ER
PT J
AU Beyer, AD
Shaw, MD
Marsili, F
Allman, MS
Lita, AE
Verma, VB
Resta, GV
Stern, JA
Mirin, RP
Nam, SW
Farr, WH
AF Beyer, Andrew D.
Shaw, Matthew D.
Marsili, Francesco
Allman, M. Shane
Lita, Adriana E.
Verma, Varun B.
Resta, Giovanni V.
Stern, Jeffrey A.
Mirin, Richard P.
Nam, Sae Woo
Farr, William H.
TI Tungsten Silicide Superconducting Nanowire Single-Photon Test Structures
Fabricated Using Optical Lithography
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article
DE Nanolithography; optical detectors; superconducting detectors;
superconducting materials
ID DETECTOR
AB Single-pixel fiber-coupled superconducting nanowire single-photon detectors (SNSPDs) operating at 1550 nm and utilizing amorphous superconducting tungsten silicide (WSi) films have proven ability to detect photons with: high system-detection efficiency (SDE) of up to 93%, low-jitter on the order of similar to 150 ps, dark count rates of similar to 1 kcps, and fast reset times on the order of tens of nanoseconds. Additionally, WSi SNSPD devices with 12-pixels have recently demonstrated downlink data rates of 79 Mbps between a terminal in orbit around the moon and a terminal on earth, as part of the Lunar Laser Communication Demonstration (LLCD) at the Lunar Lasercomm OCTL Terminal (LLOT). To further extend the performance of SNSPD devices for optical and quantum communication for terrestrial and space-based applications, the next generation of devices will need to incorporate hundreds to thousands of SNSPD pixels and to be free-space coupled. The wire widths necessary for optimal performance of WSi (similar to 120-220 nm) devices have to date been achieved using electron-beam lithography (EBL) to pattern photoresists for etch-back fabrication methods. The high cost and time to fabricate kilo-pixel arrays of SNSPDs using EBL will become prohibitive in producing such devices. Here, we report fabrication of a WSi SNSPD test structure with 64 pixels using optical lithography instead of EBL. Specifically, we used Canon EX3 and EX6 deep-UV (DUV) steppers with KrF excimer lasers (lambda = 248 nm) in the Micro Devices Laboratory at the Jet Propulsion Laboratory to fabricate the array. Dies with 8 x 8 pixels with 166-nm-wide wires were produced, with pixels having a 100 mu m pitch in the vertical and horizontal directions. Two improvements were observed: 1) the time to pattern the 8 x 8 SNSPD pixels on 3.5 mm x 3.5 mm dies filling a 4-in Si wafer required similar to 24 hours using EBL while optical lithography wrote the same dies in approximately 15 minutes; and 2) the cost to write one 4-in wafer using EBL was comparable to the cost for one optical mask for use in the stepper to write many 4-in wafers. While fabrication times and costs will vary from facility to facility, the improvements in speed and cost for optical lithography versus EBL are apparent, and this technological advance should scale and enable fast and rapid production of kilo-pixel arrays in the future.
C1 [Beyer, Andrew D.; Shaw, Matthew D.; Marsili, Francesco; Resta, Giovanni V.; Stern, Jeffrey A.; Farr, William H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Allman, M. Shane; Lita, Adriana E.; Verma, Varun B.; Mirin, Richard P.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA.
RP Beyer, AD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Andrew.d.beyer@jpl.nasa.gov; gvresta@gmail.com
OI Mirin, Richard/0000-0002-4472-4655
FU National Aeronautics and Space Administration; DARPA
FX This work was supported in part by a contract with the National
Aeronautics and Space Administration and by DARPA.
NR 12
TC 1
Z9 1
U1 6
U2 50
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1051-8223
EI 1558-2515
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2015
VL 25
IS 3
AR 2200805
DI 10.1109/TASC.2014.2378232
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA CE0AZ
UT WOS:000351465400010
ER
PT J
AU Fore, AG
Chapman, BD
Hawkins, BP
Hensley, S
Jones, CE
Michel, TR
Muellerschoen, RJ
AF Fore, Alexander G.
Chapman, Bruce D.
Hawkins, Brian P.
Hensley, Scott
Jones, Cathleen E.
Michel, Thierry R.
Muellerschoen, Ronald J.
TI UAVSAR Polarimetric Calibration
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne radar; radar cross-sections; radar imaging; radar measurements;
radar polarimetry; radar remote sensing; synthetic aperture radar (SAR);
polarimetric SAR
ID SAR CALIBRATION; ALGORITHM
AB Uninhabited aerial vehicle synthetic aperture radar (UAVSAR) is a reconfigurable polarimetric L-band SAR that operates in quad-polarization mode and is specifically designed to acquire airborne repeat-track SAR data for interferometric measurements. In this paper, we present details of the UAVSAR radar performance, the radiometric calibration, and the polarimetric calibration. For the radiometric calibration, we employ an array of trihedral corner reflectors, as well as distributed targets. We show that UAVSAR is a well-calibrated SAR system for polarimetric applications, with absolute radiometric calibration bias better than 1 dB, residual root-mean-square (RMS) errors of similar to 0.7 dB, and RMS phase errors similar to 5.3 degrees. For the polarimetric calibration, we have evaluated the methods of Quegan and Ainsworth et al. for crosstalk calibration and find that the method of Quegan gives crosstalk estimates that depend on target type, whereas the method of Ainsworth et al. gives more stable crosstalk estimates. We find that both methods estimate leakage of the copolarizations into the cross-polarizations to be on the order of -30 dB.
C1 [Fore, Alexander G.; Chapman, Bruce D.; Hawkins, Brian P.; Hensley, Scott; Jones, Cathleen E.; Michel, Thierry R.; Muellerschoen, Ronald J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fore, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Fore@jpl.nasa.gov
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX This work was supported under contract with the National Aeronautics and
Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology.
NR 13
TC 6
Z9 9
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 JUN
PY 2015
VL 53
IS 6
BP 3481
EP 3491
DI 10.1109/TGRS.2014.2377637
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 CD4OV
UT WOS:000351063800037
ER
PT J
AU Narvekar, PS
Entekhabi, D
Kim, SB
Njoku, EG
AF Narvekar, Parag S.
Entekhabi, Dara
Kim, Seung-Bum
Njoku, Eni G.
TI Soil Moisture Retrieval Using L-Band Radar Observations
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Radar roughness (RR); radar soil moisture; radar vegetation
ID INTEGRAL-EQUATION MODEL; POWER-LAW SPECTRUM; SURFACE-ROUGHNESS;
BACKSCATTERING MODEL; ERS SCATTEROMETER; SAR DATA; C-BAND; VEGETATION;
SCATTERING; SENSITIVITY
AB An algorithm for surface soil moisture estimation using L-band radar observations is introduced. The formulation envelops a wide range of land surface conditions based on three limiting cases defined in terms of end-members: smooth bare soil, rough bare soil, and a maximum vegetation covered soil. Parameterizations for these end-members are obtained using forward electromagnetic scattering models. Modulation due to soil surface roughness and overlying vegetation scattering effects between end-members are accounted using the radar vegetation index and the newly introduced radar roughness index. Hence, the retrieval algorithm developed here does not depend on ancillary vegetation or roughness information. The algorithm is tested with ground-based truck-mounted bare soil observations and observations from several airborne field campaigns that represent a wide range of surface conditions.
C1 [Narvekar, Parag S.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA.
[Kim, Seung-Bum; Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Narvekar, PS (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
NR 50
TC 8
Z9 8
U1 1
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 JUN
PY 2015
VL 53
IS 6
BP 3492
EP 3506
DI 10.1109/TGRS.2014.2377714
PG 15
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CD4OV
UT WOS:000351063800038
ER
PT J
AU Wolak, MA
Acharya, N
Tan, T
Cunnane, D
Karasik, BS
Xi, XX
AF Wolak, Matthaeus A.
Acharya, Narendra
Tan, Teng
Cunnane, Daniel
Karasik, Boris S.
Xi, Xiaoxing
TI Fabrication and Characterization of Ultrathin MgB2 Films for
Hot-Electron Bolometer Applications
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article
DE Hot electron bolometers; HPCVD; magnesium diboride; superconducting thin
films
ID CHEMICAL VAPOR-DEPOSITION; THIN-FILMS; SINGLE-CRYSTALS; RESISTIVITY;
BANDWIDTH; RESISTANCE; MIXERS
AB Hot-electron bolometer mixers employing thin films of conventional superconducting materials have already been successfully fabricated in the past. Magnesium diboride (MgB2) is a promising alternative to conventional superconductors, and we report the fabrication and study of ultrathin MgB, films of down to 10 nm deposited by hybrid physical-chemical vapor deposition technique. The MgB2 films showed T-c of above 36 K, while residual resistivities of up to 26 mu Omega . cm were achieved. Critical currents of more than 6 x 10(6) A . cm(-2) at 20 K have been measured for the films with thicknesses ranging from 10 to 100 nm. Fishtail structures have been observed in the magnetic field dependence of the critical current density for the thinnest of these films, indicating the presence of defects, which act as vortex pinning centers. From the magnetic field dependence, an average distance between adjacent pinning centers of 35 nm has been obtained for the thinnest films.
C1 [Wolak, Matthaeus A.; Acharya, Narendra; Tan, Teng; Xi, Xiaoxing] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA.
[Cunnane, Daniel; Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wolak, MA (reprint author), Temple Univ, Dept Phys, Philadelphia, PA 19122 USA.
EM matthaeus.wolak@temple.edu
FU DoD DURIP Award from the Office of Naval Research [N0014-12-1-0777]
FX This work made use of the CoE-NIC facility at Temple University
supported by the DoD DURIP Award N0014-12-1-0777 from the Office of
Naval Research.
NR 36
TC 0
Z9 0
U1 5
U2 37
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1051-8223
EI 1558-2515
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2015
VL 25
IS 3
AR 7500005
DI 10.1109/TASC.2015.2390415
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA CD5PE
UT WOS:000351139500006
ER
PT J
AU Szypryt, P
Mazin, BA
Bumble, B
Leduc, HG
Baker, L
AF Szypryt, P.
Mazin, B. A.
Bumble, B.
Leduc, H. G.
Baker, L.
TI Ultraviolet, Optical, and Near-IR Microwave Kinetic Inductance Detector
Materials Developments
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article
DE Infrared imaging; optical imaging; superconducting device fabrication;
superconducting microwave devices; superconducting resonators
ID ARCONS
AB We have fabricated 2024 pixel microwave kinetic inductance detector (MKID) arrays in the ultraviolet/optical/ near-IR (UVOIR) regime that are currently in use in astronomical instruments. In order to make MKIDs desirable for novel instruments, larger arrays with nearly perfect yield need to be fabricated. As array size increases, however, the percent yield often decreases due to frequency collisions in the readout. The per-pixel performance must also be improved, namely, the energy resolution. We are investigating ways to reduce frequency collisions and to improve the per-pixel performance of our devices through new superconducting material systems and fabrication techniques. There are two main routes that we are currently exploring. First, we are attempting to create more uniform titanium nitride films through the use of atomic layer deposition rather than the more traditional sputtering method. In addition, we are experimenting with completely new material systems for MKIDs, such as platinum silicide.
C1 [Szypryt, P.; Mazin, B. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bumble, B.; Leduc, H. G.; Baker, L.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Szypryt, P (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM pszypryt@physics.ucsb.edu; bmazin@physics.ucsb.edu
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
FU NASA Space Technology Research Fellowship
FX This work was supported by a NASA Space Technology Research Fellowship.
NR 15
TC 3
Z9 3
U1 2
U2 29
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1051-8223
EI 1558-2515
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2015
VL 25
IS 3
AR 2400604
DI 10.1109/TASC.2014.2377598
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA CB4UV
UT WOS:000349624700002
ER
PT J
AU O'Neill, S
Ortega, S
AF O'Neill, Sean
Ortega, Sam
TI 3D print a home on Mars
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Ortega, Sam] NASA, Centennial Challenges, Washington, DC USA.
[Ortega, Sam] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 0
TC 1
Z9 1
U1 1
U2 10
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD MAY 30
PY 2015
VL 226
IS 2023
BP 27
EP 27
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CJ6BU
UT WOS:000355578800016
ER
PT J
AU Polk, JE
Capece, AM
AF Polk, James E.
Capece, Angela M.
TI Materials characterization of impregnated W and W-Ir cathodes after
oxygen poisoning
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE Cathodes; Oxygen poisoning; Barium tungstate
AB Electric thrusters use hollow cathodes as the electron source for generating the plasma discharge and for beam neutralization. These cathodes contain porous tungsten emitters impregnated with BaO material to achieve a lower surface work function and are operated with xenon propellant. Oxygen contaminants in the xenon plasma can poison the emitter surface, resulting in a higher work function and increased operating temperature. This could lead directly to cathode failure by preventing discharge ignition or could accelerate evaporation of the BaO material. Exposures over hundreds of hours to very high levels of oxygen can result in increased temperatures, oxidation of the tungsten substrate, and the formation of surface layers of barium tungstates. In this work, we present results of a cathode test in which impregnated tungsten and tungsten-iridium emitters were operated with 100 ppm of oxygen in the xenon plasma for several hundred hours. The chemical and morphological changes were studied using scanning electron microscopy, energy dispersive spectroscopy, and laser profilometry. The results provide strong evidence that high concentrations of oxygen accelerate the formation of tungstate layers in both types of emitters, a phenomenon not inherent to normal cathode operation. Deposits of pure tungsten were observed on the W-Ir emitter, indicating that tungsten is preferentially removed from the surface and transported in the insert plasma. A W-Ir cathode surface will therefore evolve to a pure W composition, eliminating the work function benefit of W-Ir. However, the W-Ir emitter exhibited less erosion and redeposition at the upstream end than the pure W emitter. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Polk, James E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Capece, Angela M.] CALTECH, Pasadena, CA 91125 USA.
RP Polk, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.e.polk@jpl.nasa.gov
OI Capece, Angela/0000-0003-4147-7174
FU National Aeronautics and Space Administration
FX The authors would like to thank Al Owens, Ray Swindlehurst, and Ron
Watkins for their assistance in preparing the test facility and Ron Ruiz
and Jim Kulleck for their contributions in electron microscopy. The
research described in this paper was carried out by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 17
TC 2
Z9 2
U1 0
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
EI 1873-5584
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD MAY 30
PY 2015
VL 338
BP 27
EP 34
DI 10.1016/j.apsusc.2015.02.116
PG 8
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA CE2EL
UT WOS:000351626700004
ER
PT J
AU Meyer, ET
Georganopoulos, M
Sparks, WB
Perlman, E
van der Marel, RP
Anderson, J
Sohn, ST
Biretta, J
Norman, C
Chiaberge, M
AF Meyer, Eileen T.
Georganopoulos, Markos
Sparks, William B.
Perlman, Eric
van der Marel, Roeland P.
Anderson, Jay
Sohn, Sangmo Tony
Biretta, John
Norman, Colin
Chiaberge, Marco
TI A kiloparsec-scale internal shock collision in the jet of a nearby radio
galaxy
SO NATURE
LA English
DT Article
ID GAMMA-RAY BURSTS; HUBBLE-SPACE-TELESCOPE; M87 JET; 3C 264; EMISSION;
MOTION; MODEL
AB Jets of highly energized plasma with relativistic velocities are associated with black holes ranging in mass from a few times that of the Sun to the billion-solar-mass black holes at the centres of galaxies(1). A popular but unconfirmed hypothesis to explain how the plasma is energized is the 'internal shock model', in which the relativistic flow is unsteady(2). Faster components in the jet catch up to and collide with slower ones, leading to internal shocks that accelerate particles and generate magnetic fields(3). This mechanism can explain the variable, high-energy emission from a diverse set of objects(4-7), with the best indirect evidence being the unseen fast relativistic flow inferred to energize slower components in X-ray binary jets(8,9). Mapping of the kinematic profiles in resolved jets has revealed precessing and helical patterns in X-ray binaries(10,11), apparent superluminal motions(12,13), and the ejection of knots (bright components) from standing shocks in the jets of active galaxies(14,15). Observations revealing the structure and evolution of an internal shock in action have, however, remained elusive, hindering measurement of the physical parameters and ultimate efficiency of the mechanism. Here we report observations of a collision between two knots in the jet of nearby radio galaxy 3C 264. Abright knot with an apparent speed of (7.0 +/- 0.8)c, where c is the speed of light in a vacuum, is in the incipient stages of a collision with a slower-moving knot of speed (1.8 +/- 0.5)c just downstream, resulting in brightening of both knots-as seen in the most recent epoch of imaging.
C1 [Meyer, Eileen T.; Sparks, William B.; van der Marel, Roeland P.; Anderson, Jay; Biretta, John; Norman, Colin; Chiaberge, Marco] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Meyer, Eileen T.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perlman, Eric] Florida Inst Technol, Melbourne, FL 32901 USA.
[Sohn, Sangmo Tony; Norman, Colin; Chiaberge, Marco] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Chiaberge, Marco] Ist Radio Astron, Ist Nazl Astrofis, I-40129 Bologna, Italy.
RP Meyer, ET (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM eileen.meyer@gmail.com
FU HST [GO-13327]
FX E.T.M. acknowledges HST grant GO-13327.
NR 28
TC 2
Z9 2
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 28
PY 2015
VL 521
IS 7553
BP 495
EP +
DI 10.1038/nature14481
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF8BN
UT WOS:000371582000002
PM 26017450
ER
PT J
AU Case, NA
MacDonald, EA
Heavner, M
Tapia, AH
Lalone, N
AF Case, N. A.
MacDonald, E. A.
Heavner, M.
Tapia, A. H.
Lalone, N.
TI Mapping auroral activity with Twitter
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE aurora; mapping; Twitter; citizen science
ID GEOMAGNETIC STORMS; EARTHQUAKE
AB Twitter is a popular, publicly accessible, social media service that has proven useful in mapping large-scale events in real time. In this study, for the first time, the use of Twitter as a measure of auroral activity is investigated. Peaks in the number of aurora-related tweets are found to frequently coincide with geomagnetic disturbances (detection rate of 91%). Additionally, the number of daily aurora-related tweets is found to strongly correlate with several auroral strength proxies (r(avg)approximate to 0.7). An examination is made of the bias for location and time of day within Twitter data, and a first-order correction of these effects is presented. Overall, the results suggest that Twitter can provide both specific details about an individual aurora and accurate real-time indication of when, and even from where, an aurora is visible.
C1 [Case, N. A.; MacDonald, E. A.; Heavner, M.] New Mexico Consortium, Los Alamos, NM 87544 USA.
[Case, N. A.; MacDonald, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Heavner, M.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Tapia, A. H.; Lalone, N.] Penn State Univ, Coll Informat Sci & Technol, University Pk, PA 16802 USA.
RP Case, NA (reprint author), New Mexico Consortium, Los Alamos, NM 87544 USA.
EM nathan.a.case@nasa.gov
OI Case, Nathan/0000-0003-0692-1778
FU National Science Foundation (NSF) [1344296]
FX This material is based upon work supported, in part, by the National
Science Foundation (NSF) under grant 1344296. Any opinions, findings,
and conclusions or recommendations expressed in this material are those
of the author(s) and do not necessarily reflect the views of NSF. The
OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov. The Hemispheric Power data were provided
by the National Oceanic and Atmosphere Administration (NOAA) POES
satellites and were obtained through the Space Weather Prediction Center
(http://www.swpc.noaa.gov/).
NR 25
TC 5
Z9 5
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3668
EP 3676
DI 10.1002/2015GL063709
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300006
ER
PT J
AU Mlynczak, MG
Hunt, LA
Marshall, BT
Russell, JM
Mertens, CJ
Thompson, RE
Gordley, LL
AF Mlynczak, Martin G.
Hunt, Linda A.
Marshall, B. Thomas
Russell, James M., III
Mertens, Christopher J.
Thompson, R. Earl
Gordley, Larry L.
TI A combined solar and geomagnetic index for thermospheric climate
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Sun-Earth connection; space climate; thermosphere; nitric oxide
AB Infrared radiation from nitric oxide (NO) at 5.3 mu m is a primary mechanism by which the thermosphere cools to space. The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASA Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics satellite has been measuring thermospheric cooling by NO for over 13years. In this letter we show that the SABER time series of globally integrated infrared power (watts) radiated by NO can be replicated accurately by a multiple linear regression fit using the F-10.7, Ap, and Dst indices. This allows reconstruction of the NO power time series back nearly 70years with extant databases of these indices. The relative roles of solar ultraviolet and geomagnetic processes in determining the NO cooling are derived and shown to vary significantly over the solar cycle. The NO power is a fundamental integral constraint on the thermospheric climate, and the time series presented here can be used to test upper atmosphere models over seven different solar cycles.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA Langley Res Ctr, Hampton, VA USA.
[Hunt, Linda A.] SSAI, Hampton, VA USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] GATS, Newport News, VA USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
RP Mlynczak, MG (reprint author), NASA Langley Res Ctr, Hampton, VA USA.
EM m.g.mlynczak@nasa.gov
OI Hunt, Linda/0000-0002-5330-541X
FU NASA Heliophysics Division Thermosphere-Ionosphere-Mesosphere Energetics
and Dynamics mission
FX The authors acknowledge support from the NASA Heliophysics Division
Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics mission. The
Ap and F10.7 solar flux are obtained from the daily
geomagnetic and daily solar data sets prepared by the NOAA Space Weather
Prediction Center. The Dst data are obtained from the Data Analysis
Center for geomagnetism and Space Magnetism at the World Data Center for
Geomagnetism in Kyoto, Japan. The daily sunspot data are downloaded from
the WDC-SILSO (World Data Center for Sunspot Index and Long-term Solar
Observations) at the Royal Observatory of Belgium, Brussels. The NO
power data are available by contacting the first author of this article.
NR 6
TC 3
Z9 3
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3677
EP 3682
DI 10.1002/2015GL064038
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300007
ER
PT J
AU Sun, WJ
Slavin, JA
Fu, SY
Raines, JM
Zong, QG
Imber, SM
Shi, QQ
Yao, ZH
Poh, G
Gershman, DJ
Pu, ZY
Sundberg, T
Anderson, BJ
Korth, H
Baker, DN
AF Sun, Wei-Jie
Slavin, James A.
Fu, Suiyan
Raines, Jim M.
Zong, Qiu-Gang
Imber, Suzanne M.
Shi, Quanqi
Yao, Zhonghua
Poh, Gangkai
Gershman, Daniel J.
Pu, Zuyin
Sundberg, Torbjoern
Anderson, Brian J.
Korth, Haje
Baker, Daniel N.
TI MESSENGER observations of magnetospheric substorm activity in Mercury's
near magnetotail
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetospheric substorm; Mercury; dipolarization; field-aligned current
ID SOLAR-WIND CONDITIONS; MAGNETIC-FIELD; MAGNETOPAUSE; RECONNECTION;
MODEL; ACCELERATION; INSTRUMENT; PARTICLES; FLYBY; TAIL
AB MErcury Surface, Space ENviroment, GEochemistry, and Ranging (MESSENGER) magnetic field and plasma measurements taken during crossings of Mercury's magnetotail from 2011 to 2014 have been examined for evidence of substorms. A total of 26 events were found during which an Earth-like growth phase was followed by clear near-tail expansion phase signatures. During the growth phase, just as at Earth, the thinning of the plasma sheet and the increase of the magnetic field intensity in the lobe are observed, but the fractional increase in field intensity could be approximate to 3 to 5 times that at Earth. The average timescale of the growth phase is approximate to 1min. The dipolarization that marks the initiation of the substorm expansion phase is only a few seconds in duration. During the expansion phase, lasting approximate to 1min, the plasma sheet is observed to thicken and engulf the spacecraft. The duration of the substorm observed in this paper is consistent with previous observations of Mercury's Dungey cycle. The reconfiguration of the magnetotail during Mercury's substorm is very similar to that at Earth despite its very compressed timescale.
C1 [Sun, Wei-Jie; Fu, Suiyan; Zong, Qiu-Gang; Pu, Zuyin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
[Sun, Wei-Jie; Slavin, James A.; Raines, Jim M.; Poh, Gangkai] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Shi, Quanqi] Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China.
[Yao, Zhonghua] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Sundberg, Torbjoern] Queen Mary Univ London, Sch Phys & Astron, London, England.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Sun, WJ (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
EM weijiesun@pku.edu.cn
RI Poh, Gangkai/O-5378-2016; Slavin, James/H-3170-2012;
OI Poh, Gangkai/0000-0002-5775-2006; Slavin, James/0000-0002-9206-724X;
Sun, Weijie/0000-0001-5260-658X; Yao, Zhonghua/0000-0001-6826-2486
FU NASA [NASW-00002, NAS5-97271, NNX15AJ68G]; Chinese Scholarship Council;
National Nature Science Foundation of China [41474139, 41322031,
41421003]; Major Project of Chinese National Programs for Fundamental
Research and Development [2012CB825603]
FX The data used in this study were available from the Planetary Data
System (PDS): http://pds.jpl.nasa.gov. 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. Wei-Jie Sun is supported
by the State Scholarship Fund of Chinese Scholarship Council. This work
is supported by the National Nature Science Foundation of China (grants
41474139, 41322031, and 41421003) and Major Project of Chinese National
Programs for Fundamental Research and Development (2012CB825603). This
work is also supported by the NASA Heliophysics Supporting Research
Program under grant NNX15AJ68G.
NR 38
TC 8
Z9 8
U1 2
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3692
EP 3699
DI 10.1002/2015GL064052
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300009
ER
PT J
AU Benna, M
Mahaffy, PR
Halekas, JS
Elphic, RC
Delory, GT
AF Benna, M.
Mahaffy, P. R.
Halekas, J. S.
Elphic, R. C.
Delory, G. T.
TI Variability of helium, neon, and argon in the lunar exosphere as
observed by the LADEE NMS instrument
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Moon; exosphere; helium; neon; argon; variability
ID GAMMA-RAY SPECTROMETER; SOLAR-WIND; ATMOSPHERE; SIMULATION; SURFACE;
MOON
AB The Neutral Mass Spectrometer (NMS) onboard the Lunar Atmosphere and Dust Environment Explorer (LADEE) provided the first global characterization of He and Ar along with the discovery of Ne in the lunar exosphere. The mapping of the equatorial distribution of these noble gases revealed new selenographic and temporal variations. Helium was found to be controlled by the supply of solar wind alpha particles and by the presence of an endogenous source that supplies the exosphere at a rate of 1.9x10(23)atomss(-1). Neon was detected over the nightside at levels comparable to He and was found to exhibit the spatial distribution of a surface accommodated noncondensable gas. The global measurements of NMS revealed the presence of a localized Ar enhancement that has never been identified before at the western maria. The variability resulting from this local enhancement is coupled to a more global but transient source.
C1 [Benna, M.; Mahaffy, P. R.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Benna, M.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21228 USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Elphic, R. C.; Delory, G. T.] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Benna, M (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mehdi.benna@nasa.gov
RI Benna, Mehdi/F-3489-2012;
OI Halekas, Jasper/0000-0001-5258-6128
FU NASA; NASA [NAS5-02099]
FX The LADEE/NMS investigation was supported by NASA. Tests and
calibrations were done at the Planetary Environment Laboratory of NASA's
Goddard Space Flight Center. We are grateful for engineering/technical
support especially from T. King (Instrument Manager), E. Weidner, E.
Lyness, K. Patel, M. Nagaraja (Instrument Operations), and E. Raaen
(Calibration). We acknowledge NASA contract NAS5-02099 and V.
Angelopoulos for use of data from the ARTEMIS Mission, and specifically
C. W. Carlson and J.P. McFadden for use of ESA data. The NMS data
supporting this article are publicly available at the Planetary Data
System
(http://pds-atmospheres.nmsu.edu/data_and_services/atmospheres_data/LADE
E/nms.html).
NR 29
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Z9 10
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 MAY 28
PY 2015
VL 42
IS 10
BP 3723
EP 3729
DI 10.1002/2015GL064120
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300013
ER
PT J
AU Heavens, NG
Cantor, BA
Hayne, PO
Kass, DM
Kleinbohl, A
McCleese, DJ
Piqueux, S
Schofield, JT
Shirley, JH
AF Heavens, N. G.
Cantor, B. A.
Hayne, P. O.
Kass, D. M.
Kleinboehl, A.
McCleese, D. J.
Piqueux, S.
Schofield, J. T.
Shirley, J. H.
TI Extreme detached dust layers near Martian volcanoes: Evidence for dust
transport by mesoscale circulations forced by high topography
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE topographic circulation; dust; Mars; volcanoes; mesoscale
ID ORBITER CAMERA OBSERVATIONS; MARS CLIMATE SOUNDER; WATER-VAPOR;
VERTICAL-DISTRIBUTION; SOLAR OCCULTATIONS; ATMOSPHERE; CLOUDS; STORMS;
SPECTROMETER; THARSIS
AB Modeling suggests that thermal circulations over Mars's highest volcanoes transport water vapor and dust from the surface into the middle atmosphere, forming detached layers in these constituents. Intense vertical mixing also takes place in regional and global dust storms, which can generate detached layers that are extreme in both altitude and magnitude. Here we employ observations by the Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter, taking advantage of improved vertical coverage in MCS's aerosol retrievals, to discover a new class of extreme detached dust layers (EDDLs). Observed during minimal dust storm activity and furthermore distinguished by their potentially large and measurable horizontal extent (>1000km), these EDDLs cluster near Olympus Mons and the Tharsis Montes, from which they likely originate. The existence of these EDDLs suggests that vertical mixing by topographic circulations can be much stronger than previously modeled and more frequent than previously observed.
C1 [Heavens, N. G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
[Cantor, B. A.] Malin Space Sci Syst, San Diego, CA USA.
[Hayne, P. O.; Kass, D. M.; Kleinboehl, A.; McCleese, D. J.; Piqueux, S.; Schofield, J. T.; Shirley, J. H.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
RP Heavens, NG (reprint author), Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
EM Nicholas.Heavens@hamptonu.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU NASA Jet Propulsion Laboratory; Caltech [1471216]; NASA [NNX14AM32G]
FX N.G. Heavens acknowledges support from the NASA Jet Propulsion
Laboratory, Caltech (subcontract 1471216) and NASA's Mars Data Analysis
Program (NNX14AM32G). We thank an anonymous reviewer and Jim Murphy for
their helpful comments. All MRO-MCS data used here are freely available
from NASA's Planetary Data System (PDS). Any analytical code is
available from the first author by request.
NR 37
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U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3730
EP 3738
DI 10.1002/2015GL064004
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300014
ER
PT J
AU Neish, CD
Barnes, JW
Sotin, C
MacKenzie, S
Soderblom, JM
Le Mouelic, S
Kirk, RL
Stiles, BW
Malaska, MJ
Le Gall, A
Brown, RH
Baines, KH
Buratti, B
Clark, RN
Nicholson, PD
AF Neish, C. D.
Barnes, J. W.
Sotin, C.
MacKenzie, S.
Soderblom, J. M.
Le Mouelic, S.
Kirk, R. L.
Stiles, B. W.
Malaska, M. J.
Le Gall, A.
Brown, R. H.
Baines, K. H.
Buratti, B.
Clark, R. N.
Nicholson, P. D.
TI Spectral properties of Titan's impact craters imply chemical weathering
of its surface
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE erosion and weathering; impact cratering; Titan
ID CASSINI VIMS; HUYGENS PROBE; LANDING SITE; RADAR; ATMOSPHERE;
TRANSMISSION; CONSTRAINTS; TOPOGRAPHY; EVAPORITE; IMAGES
AB We examined the spectral properties of a selection of Titan's impact craters that represent a range of degradation states. The most degraded craters have rims and ejecta blankets with spectral characteristics that suggest that they are more enriched in water ice than the rims and ejecta blankets of the freshest craters on Titan. The progression is consistent with the chemical weathering of Titan's surface. We propose an evolutionary sequence such that Titan's craters expose an intimate mixture of water ice and organic materials, and chemical weathering by methane rainfall removes the soluble organic materials, leaving the insoluble organics and water ice behind. These observations support the idea that fluvial processes are active in Titan's equatorial regions.
C1 [Neish, C. D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Barnes, J. W.; MacKenzie, S.] Univ Idaho, Dept Phys, Moscow, ID USA.
[Sotin, C.; Stiles, B. W.; Malaska, M. J.; Baines, K. H.; Buratti, B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Soderblom, J. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Le Mouelic, S.] Univ Nantes, Lab Planetol & Geodynam, LPGNantes, CNRS UMR 6112, Nantes, France.
[Kirk, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Le Gall, A.] Univ Versailles St Quentin, Lab Atmospheres, Milieux, Observat Spatiales LATMOS, Paris, France.
[Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Clark, R. N.] US Geol Survey, Denver, CO 80225 USA.
[Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Neish, CD (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
EM cneish@fit.edu
RI Barnes, Jason/B-1284-2009;
OI Barnes, Jason/0000-0002-7755-3530; Malaska, Michael/0000-0003-0064-5258
FU NASA [NNH11ZDA001N-OPR, NNH13ZDA001N-OPR]; NASA
FX We wish to acknowledge the Cassini VIMS and RADAR teams for acquiring
and processing the data presented here. Data from the Cassini mission
are made publicly available through the Planetary Data System
(pds.nasa.gov). We also wish to thank E. Turtle and an anonymous
individual for their careful reviews and J. Lunine for input that helped
to improve the manuscript. C.N. and C.S. acknowledge support from the
NASA Outer Planets Research Program (NNH11ZDA001N-OPR and
NNH13ZDA001N-OPR). Part of this work was performed at the Jet Propulsion
Laboratory, California Institute of Technology under contract with NASA.
NR 52
TC 6
Z9 6
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3746
EP 3754
DI 10.1002/2015GL063824
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300016
ER
PT J
AU Han, SC
Sauber, J
Pollitz, F
AF Han, Shin-Chan
Sauber, Jeanne
Pollitz, Fred
TI Coseismic compression/dilatation and viscoelastic uplift/subsidence
following the 2012 Indian Ocean earthquakes quantified from satellite
gravity observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE gravity change; strike-slip earthquake; GPS; viscoelastic relaxation;
elastic deformation
ID DEFORMATION; SEISMICITY; RELAXATION; AFTERSLIP; EARTH
AB The 2012 Indian Ocean earthquake sequence (M-w 8.6, 8.2) is a rare example of great strike-slip earthquakes in an intraoceanic setting. With over a decade of Gravity Recovery and Climate Experiment (GRACE) data, we were able to measure and model the unanticipated large coseismic and postseismic gravity changes of these events. Using the approach of normal mode decomposition and spatial localization, we computed the gravity changes corresponding to five moment tensor components. Our analysis revealed that the gravity changes are produced predominantly by coseismic compression and dilatation within the oceanic crust and upper mantle and by postseismic vertical motion. Our results suggest that the postseismic positive gravity and the postseismic uplift measured with GPS within the coseismic compressional quadrant are best fit by ongoing uplift associated with viscoelastic mantle relaxation. Our study demonstrates that the GRACE data are suitable for analyzing strike-slip earthquakes as small as M-w 8.2 with the noise characteristics of this region.
C1 [Han, Shin-Chan] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
[Sauber, Jeanne] NASA Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA.
[Pollitz, Fred] US Geol Survey, Menlo Pk, CA 94025 USA.
RP Han, SC (reprint author), Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
EM shin-chan.han@newcastle.edu.au
NR 23
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U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 3764
EP 3772
DI 10.1002/2015GL063819
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300018
ER
PT J
AU Wu, WY
Lan, CW
Lo, MH
Reager, JT
Famiglietti, JS
AF Wu, Wen-Ying
Lan, Chia-Wei
Lo, Min-Hui
Reager, John T.
Famiglietti, James S.
TI Increases in the annual range of soil water storage at northern middle
and high latitudes under global warming
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE annual range; CMIP5; global warming
ID CLIMATE-CHANGE; CMIP5; PRECIPITATION; AVAILABILITY; GRACE; SIMULATIONS;
IMPACTS; DROUGHT; RUNOFF; MODELS
AB Soil water storage is a fundamental signal in the land hydrological cycle and changes in soil moisture can affect regional climate. In this study, we used simulations from Coupled Model Intercomparison Project Phase 5 archives to investigate changes in the annual range of soil water storage under global warming at northern middle and high latitudes. Results show that future warming could lead to significant declines in snowfall, and a corresponding lack of snowmelt water recharge to the soil, which makes soil water less available during spring and summer. Conversely, more precipitation as rainfall results in higher recharge to soil water during its accumulating season. Thus, the wettest month of soil water gets wetter, and the driest month gets drier, resulting in an increase of the annual range and suggesting that stronger heterogeneity in global water distribution (changing extremes) could occur under global warming; this has implications for water management and water security under a changing climate.
C1 [Wu, Wen-Ying; Lan, Chia-Wei; Lo, Min-Hui] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan.
[Reager, John T.; Famiglietti, James S.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA.
RP Lo, MH (reprint author), Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan.
EM minhuilo@ntu.edu.tw
OI LO, MIN-HUI/0000-0002-8653-143X
FU MOST [103-2111-M-002-006, 104-2923-M-002-002-MY4]; NASA
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
output. 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. GRACE land data
were processed by Sean Swenson, supported by the NASA MEaSUREs Program,
and are available at http://grace.jpl.nasa.gov. This study was supported
by the MOST 103-2111-M-002-006 and MOST 104-2923-M-002-002-MY4 to
National Taiwan University. A portion of this research was conducted at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA.
NR 32
TC 2
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U1 5
U2 14
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 MAY 28
PY 2015
VL 42
IS 10
BP 3903
EP 3910
DI 10.1002/2015GL064110
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300035
ER
PT J
AU Thompson, DR
Seidel, FC
Gao, BC
Gierach, MM
Green, RO
Kudela, RM
Mouroulis, P
AF Thompson, David R.
Seidel, Felix C.
Gao, Bo Cai
Gierach, Michelle M.
Green, Robert O.
Kudela, Raphael M.
Mouroulis, Pantazis
TI Optimizing irradiance estimates for coastal and inland water imaging
spectroscopy
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE imaging spectroscopy; phytoplankton; atmospheric correction; solar
irradiance
ID HYPERSPECTRAL IMAGER; SPECTROMETER; CALIBRATION; AIRBORNE; DESIGN; ATLAS
AB Next generation orbital imaging spectrometers, with advanced global remote sensing capabilities, propose to address outstanding ocean science questions related to coastal and inland water environments. These missions require highly accurate characterization of solar irradiance in the critical 380-600nm spectral range. However, the irradiance in this spectral region is temporally variable and difficult to measure directly, leading to considerable variance between different models. Here we optimize an irradiance estimate using data from the NASA airborne Portable Remote Imaging Spectrometer (PRISM), leveraging spectrally smooth in-scene targets. We demonstrate improved retrievals for both PRISM and the Next Generation Airborne Visible Infrared Imaging Spectrometer.
C1 [Thompson, David R.; Seidel, Felix C.; Gierach, Michelle M.; Green, Robert O.; Mouroulis, Pantazis] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Gao, Bo Cai] US Naval Res Lab, Washington, DC USA.
[Kudela, Raphael M.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.r.thompson@jpl.nasa.gov
OI Seidel, Felix/0000-0002-4282-2198; Thompson, David/0000-0003-1100-7550
FU JPL Earth System Science Formulation office
FX The optimized irradiance spectrum and all PRISM and AVIRIS-NG radiance
spectra are available at http://prism.jpl.nasa.gov and
http://aviris-ng.jpl.nasa.gov. Data for Figures 3-6 are provided as
supporting information. This research was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. We
thank the JPL PRISM team: D. Cohen, K. Balasubramanian, S. Leland, F.
Loya, D. Moore, D. Randall, J. Rodriguez, C. Sarture, E. Urquiza, V.
White, and K. Yee. We thank D. A. Roberts, E. Pennington, and B. Bue for
assistance with AVIRIS-NG ground truth data. K. Hayashi Negrey of the
University of California, Santa Cruz provided invaluable support with
the collection of in situ reflectance data. We thank J. M. Fontenla for
his counsel and assistance. We also thank B. Mateer, I. McCubbin, and C.
V. White, and acknowledge the financial support of the JPL Earth System
Science Formulation office. Copyright 2015 California Institute of
Technology. All Rights Reserved.
NR 18
TC 3
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 MAY 28
PY 2015
VL 42
IS 10
BP 4116
EP 4123
DI 10.1002/2015GL063287
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300061
ER
PT J
AU Tian, BJ
AF Tian, Baijun
TI Spread of model climate sensitivity linked to double-Intertropical
Convergence Zone bias
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE global climate models (GCMs); double-ITCZ bias; equilibrium climate
sensitivity (ECS); Coupled Model Intercomparison Project (CMIP5);
emergent constraint
ID GENERAL-CIRCULATION MODELS; DOUBLE-ITCZ PROBLEM; FUTURE; CMIP5;
TEMPERATURE; PACIFIC; OCEAN
AB Despite decades of climate research and model development, two outstanding problems still plague the latest global climate models (GCMs): the double-Intertropical Convergence Zone (ITCZ) bias and the 2-5 degrees C spread of equilibrium climate sensitivity (ECS). Here we show that the double-ITCZ bias and ECS in 44 GCMs from Coupled Model Intercomparison Project Phases 3/5 are negatively correlated. The models with weak (strong) double-ITCZ biases have high (low)-ECS values of similar to 4.1(2.2)degrees C. This indicates that the double-ITCZ bias is a new emergent constraint for ECS based on which ECS might be in the higher end of its range (similar to 4.0 degrees C) and most models might have underestimated ECS. In addition, we argue that the double-ITCZ bias can physically affect both cloud and water vapor feedbacks (thus ECS) and is a more easily measured emergent constraint for ECS than previous ones. It can be used as a performance metric for evaluating and comparing different GCMs.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tian, BJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM baijun.tian@jpl.nasa.gov
RI Tian, Baijun/A-1141-2007
OI Tian, Baijun/0000-0001-9369-2373
FU AIRS project at JPL
FX I thank Jonathan Jiang for providing the HadGEM2-ES model precipitation
data, Eric Fetzer, Brian Kahn, Graeme Stephens, Hui Su, Duane Waliser,
Steven Sherwood, Sandrine Bony, Brian Soden, and two anonymous reviewers
for comments. This research was performed at Jet Propulsion Laboratory
(JPL) under a contract with National Aeronautics and Space
Administration (NASA). It was supported by the AIRS project at JPL. I
acknowledge the World Climate Research Program's (WCRP) Working Group on
Coupled Modeling (WGCM), which is responsible for CMIP, and the U.S.
Department of Energy's (DOE) Program for Climate Model Diagnosis and
Intercomparison (PCMDI), which provides coordinating support and leads
development of software infrastructure in partnership with the Global
Organization for Earth System Science Portals. I thank the climate
modeling groups around the world for producing and making available
their model output. The observational data used in this work were
provided by the Obs4MIPs project, initiated by NASA and DOE, with
governance provided by the WCRP's Data Advisory Council (WDAC).
Copyright 2015. All rights reserved.
NR 32
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Z9 9
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 MAY 28
PY 2015
VL 42
IS 10
BP 4133
EP 4141
DI 10.1002/2015GL064119
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300063
ER
PT J
AU Strahan, SE
Oman, LD
Douglass, AR
Coy, L
AF Strahan, S. E.
Oman, L. D.
Douglass, A. R.
Coy, L.
TI Modulation of Antarctic vortex composition by the quasi-biennial
oscillation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE stratospheric chlorine; stratospheric transport; quasi-biennial
oscillation; Antarctic ozone
ID STRATOSPHERIC POLAR VORTEX; INTERANNUAL VARIABILITY; OZONESONDE
MEASUREMENTS; TROPICAL STRATOSPHERE; TRACE GASES; SOUTH-POLE;
CIRCULATION; QBO; TRANSPORT; DESCENT
AB Using a decade of Aura Microwave Limb Sounder observations, we show distinctly different N2O distributions in Southern Hemisphere winter that depend on the phase of the quasi-biennial oscillation (QBO). Composites of the nitrous oxide (N2O) anomalies calculated for westerly and easterly phases show that QBO-generated variability originating in the subtropical middle stratosphere fills the midlatitude surf zone by late winter. After the spring vortex breakup, the anomaly is transported to the Antarctic where it remains until the next vortex forms in fall. Trapped in the newly formed vortex, the anomaly descends in isolation through fall and winter, arriving in the Antarctic lower stratosphere in Septemberabout 1year after it formed. This transport pathway explains previously reported variability of N2O and inorganic chlorine (Cl-y) inside the Antarctic vortex and demonstrates that the middle stratosphere QBO affects ozone depletion by modulating Antarctic Cl-y.
C1 [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Strahan, S. E.; Oman, L. D.; Douglass, A. R.; Coy, L.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Coy, L.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Strahan, SE (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.
EM susan.e.strahan@nasa.gov
RI Douglass, Anne/D-4655-2012; Oman, Luke/C-2778-2009
OI Oman, Luke/0000-0002-5487-2598
FU NASA Atmospheric Composition Modeling and Analysis Program
FX This work was supported by the NASA Atmospheric Composition
Modeling and Analysis Program. MLS data are available at
http://mls.jpl.nasa.gov. The MERRA reanalysis can be obtained from the
Goddard Earth Science Data and Information Services Center,
http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl. We thank Darryn
Waugh and Paul Newman for their helpful discussions.
NR 41
TC 2
Z9 2
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 4216
EP 4223
DI 10.1002/2015GL063759
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300073
ER
PT J
AU Orbe, C
Waugh, DW
Newman, PA
AF Orbe, Clara
Waugh, Darryn W.
Newman, Paul A.
TI Air-mass origin in the tropical lower stratosphere: The influence of
Asian boundary layer air
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE boundary layer origin; troposphere-stratosphere transport; asian monsoon
ID WATER-VAPOR; CIRCULATION MODELS; MONSOON TRANSPORT; AEROSOL LAYER;
TRANSIT-TIME; PIPE MODEL; AGE; CLIMATE; OZONE; DISTRIBUTIONS
AB A climatology of air-mass origin in the tropical lower stratosphere is presented for the Goddard Earth Observing System Chemistry Climate Model. During late boreal summer and fall, air-mass fractions reveal that as much as 20% of the air in the tropical lower stratosphere last contacted the planetary boundary layer (PBL) over Asia; by comparison, the air-mass fractions corresponding to last PBL contact over North America and over Europe are negligible. Asian air reaches the extratropical tropopause within a few days of leaving the boundary layer and is quasi-horizontally transported into the tropical lower stratosphere, where it persists until January. The rapid injection of Asian air into the lower stratosphereand its persistence in the deep tropics through late (boreal) winteris important as industrial emissions over East Asia continue to increase. Hence, the Asian monsoon may play an increasingly important role in shaping stratospheric composition.
C1 [Orbe, Clara; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
EM clara.orbe@nasa.gov
RI Waugh, Darryn/K-3688-2016
OI Waugh, Darryn/0000-0001-7692-2798
FU Goddard Space Flight Center; NSF [AGS-1403676]; NASA [NNX14AP58G]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The authors also
acknowledge support from NSF grant AGS-1403676 (D.W.W.) and NASA grant
NNX14AP58G (D.W.W.). The authors are thankful for the discussions with
Bill Randel, Laura Pan, and Mijeong Park. All data presented in this
paper are available from the corresponding author upon direct request.
NR 51
TC 7
Z9 7
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 28
PY 2015
VL 42
IS 10
BP 4240
EP 4248
DI 10.1002/2015GL063937
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CL0KJ
UT WOS:000356631300076
ER
PT J
AU Vega-Rodriguez, M
Muller-Karger, FE
Hallock, P
Quiles-Perez, GA
Eakin, CM
Colella, M
Jones, DL
Li, J
Soto, I
Guild, L
Lynds, S
Ruzicka, R
AF Vega-Rodriguez, M.
Mueller-Karger, F. E.
Hallock, P.
Quiles-Perez, G. A.
Eakin, C. M.
Colella, M.
Jones, D. L.
Li, J.
Soto, I.
Guild, L.
Lynds, S.
Ruzicka, R.
TI Influence of water-temperature variability on stony coral diversity in
Florida Keys patch reefs
SO MARINE ECOLOGY PROGRESS SERIES
LA English
DT Article
DE Coral reef; Florida Keys; Sea surface temperature; Degree Heating Weeks;
Species richness; Shannon diversity
ID CLIMATE-CHANGE; THERMAL TOLERANCE; ACROPORA-PALMATA; LONG-TERM; STRESS;
PATTERNS; DISEASE; FUTURE; HETEROGENEITY; ZOOXANTHELLAE
AB Annual surveys conducted by the Coral Reef Evaluation and Monitoring Project (CREMP) reported that average benthic cover of stony corals in the Florida Keys National Marine Sanctuary, USA declined from similar to 13% in 1996 to 8% in 2009. Keys-wide, mean species richness (SR) declined by similar to 2.3 species per station. Stress due to temperature extremes is suspected to be a major driver of this trend. We tested the potential for sea surface temperature (SST) variability and acute warm-temperature events (assessed with Degree Heating Weeks) to affect stony coral diversity in the Florida Keys. Benthic cover of 43 stony coral species was examined with respect to SST variability and habitat type (patch, offshore shallow, and offshore deep reefs). For each CREMP site, SST annual variance was classified as low (<7.0 degrees C-2), intermediate (7.0 to 10.9 degrees C-2), or high (>= 11.0 degrees C-2). Nonparametric MANOVA analyses showed that in the Upper, Middle, and Lower Keys regions, massive-type stony coral species (e.g. Siderastrea siderea, Pseudodiploria strigosa, Orbicella annularis complex, Montastraea cavernosa, and Colpophyllia natans) were prevalent in the patch reef habitats exposed to intermediate to high SST variability. Intermediate SST variability was also correlated with higher Shannon diversity means in patch reefs in the Upper Keys and higher SR means in the Middle Keys, indicating either that the stony coral species in these habitats are adapted to an intermediate temperature range or that individual colonies have acclimatized to that range. No significant relationships were found between stony coral diversity and SST variability in the Dry Tortugas region.
C1 [Vega-Rodriguez, M.; Mueller-Karger, F. E.; Hallock, P.; Quiles-Perez, G. A.; Jones, D. L.; Soto, I.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Eakin, C. M.; Li, J.] NOAA, Coral Reef Watch, Ctr Satellite Applicat & Res, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA.
[Colella, M.; Ruzicka, R.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA.
[Guild, L.] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA.
[Lynds, S.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP Vega-Rodriguez, M (reprint author), Univ S Florida, Coll Marine Sci, 140 Seventh Ave South, St Petersburg, FL 33701 USA.
EM mariavegarod@mail.usf.edu
RI Eakin, C. Mark/F-5585-2010
FU NOAA Coral Reef Conservation Program; NASA Ames Research Center;
University of South Florida's Institute for Marine Remote Sensing by
NASA Grant [NNX09AV24G]; NASA [NNX12AN94H]; NSF FG-LSAMP Bridge to the
Doctorate (HRD) [0929435]; USF-CMS Bridge to the Doctorate Endowed;
Alfred P. Sloan Fellowship; ARCS; USEPA Water Quality Protection Program
[X7-97468002]; State of Florida Marine Resource Conservation Trust Fund;
NOAA; US Army Corps of Engineers [MOA-2001-683]; National Science
Foundation [NSF-1015342]
FX This work was possible thanks to a collaboration among the NOAA Coral
Reef Watch program funded by the NOAA Coral Reef Conservation Program,
the NASA Ames Research Center, and the University of South Florida's
Institute for Marine Remote Sensing funded by NASA Grant NNX09AV24G to
F.E.M.K., C.M.E., L.G., C. Hu, and S.L. We thank W. Turner for the NASA
support. Additional funding was provided to M.V.R. by NASA headquarters
under the NASA Earth and Science Fellowship Program (NNX12AN94H), the
NSF FG-LSAMP Bridge to the Doctorate (HRD # 0929435), USF-CMS Bridge to
the Doctorate Endowed and Alfred P. Sloan Fellowship, and ARCS (Tampa
Bay Chapter). Funding to support the CREMP program is achieved through
the USEPA Water Quality Protection Program (X7-97468002), the State of
Florida Marine Resource Conservation Trust Fund, NOAA, the US Army Corps
of Engineers (MOA-2001-683), and the National Science Foundation
(NSF-1015342). The authors thank S. Donahue (FKNMS) for providing the
thermograph data, N. Melo for support with the Surfer software, and the
Editor and anonymous reviewers for providing helpful comments which led
to the improvement of the manuscript. The manuscript contents are solely
the opinions of the authors and do not constitute a statement of policy,
decision, or position on behalf of NOAA or the US government. IMaRS
contribution 167.
NR 60
TC 2
Z9 2
U1 10
U2 38
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0171-8630
EI 1616-1599
J9 MAR ECOL PROG SER
JI Mar. Ecol.-Prog. Ser.
PD MAY 28
PY 2015
VL 528
BP 173
EP 186
DI 10.3354/meps11268
PG 14
WC Ecology; Marine & Freshwater Biology; Oceanography
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Oceanography
GA CK2WR
UT WOS:000356075600013
ER
PT J
AU Klimchuk, JA
AF Klimchuk, James A.
TI Key aspects of coronal heating
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE corona; coronal heating; magnetic fields
ID SOLAR ACTIVE-REGION; HI-C; MAGNETIC-FIELDS; LOOP MODELS; FLUX-TUBE;
DYNAMICS; NANOFLARES; EMISSION; RECONNECTION; RESOLUTION
AB We highlight 10 key aspects of coronal heating that must be understood before we can consider the problem to be solved. (1) All coronal heating is impulsive. (2) The details of coronal heating matter. (3) The corona is filled with elemental magnetic stands. (4) The corona is densely populated with current sheets. (5) The strands must reconnect to prevent an infinite build-up of stress. (6) Nanoflares repeat with different frequencies. (7) What is the characteristic magnitude of energy release? (8) What causes the collective behaviour responsible for loops? (9) What are the onset conditions for energy release? (10) Chromospheric nanoflares are not a primary source of coronal plasma. Significant progress in solving the coronal heating problem will require coordination of approaches: observational studies, field-aligned hydrodynamic simulations, large-scale and localized three-dimensional magnetohydrodynamic simulations, and possibly also kinetic simulations. There is a unique value to each of these approaches, and the community must strive to coordinate better.
C1 NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Code 661, Greenbelt, MD 20771 USA.
EM james.a.klimchuk@nasa.gov
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU NASA
FX This work was supported by the NASA Heliophysics Guest Investigator and
Supporting Research and Technology Programs.
NR 65
TC 11
Z9 11
U1 1
U2 3
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 MAY 28
PY 2015
VL 373
IS 2042
AR UNSP 20140256
DI 10.1098/rsta.2014.0256
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CG5BL
UT WOS:000353304600001
ER
PT J
AU Schmelz, JT
Winebarger, AR
AF Schmelz, J. T.
Winebarger, A. R.
TI What can observations tell us about coronal heating?
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE solar corona; coronal loops; hot plasma
ID X-RAY TELESCOPE; EUV IMAGING SPECTROMETER; ACTIVE-REGION LOOPS; EMISSION
MEASURE DISTRIBUTIONS; TRANSITION-REGION; TEMPERATURE-MEASUREMENTS;
SOLAR CORONA; DIAGNOSTIC SPECTROMETER; MULTITHERMAL ANALYSIS;
DENSITY-MEASUREMENTS
AB The actual source of coronal heating is one of the longest standing unsolved mysteries in all of astrophysics, but it is only in recent years that observations have begun making significant contributions. Coronal loops, their structure and sub-structure, their temperature and density details, and their evolution with time, may hold the key to solving this mystery. Because spatial resolution of current observatories cannot resolve fundamental scale lengths, information about the heating of the corona must be inferred from indirect observations. Loops with unexpectedly high densities and multi-thermal cross-field temperatures were not consistent with results expected from steady uniform heating models. The hot (T > 5 MK) plasma component of loops may also be a key observation; a new sounding rocket instrument called the Marshall Grazing Incidence X-ray Spectrometer will specifically target this observable. Finally, a loop is likely to be a tangle of magnetic strands. The High Resolution Coronal Imager observed magnetic braids untwisting and reconnecting, dispersing enough energy to heat the surrounding plasma. The existence of multi-thermal, cooling loops and hot plasma provides observational constraints that all viable coronal heating models will need to explain.
C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Winebarger, A. R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
NR 75
TC 2
Z9 2
U1 0
U2 1
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 MAY 28
PY 2015
VL 373
IS 2042
AR UNSP 20140257
DI 10.1098/rsta.2014.0257
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CG5BL
UT WOS:000353304600002
ER
PT J
AU Wang, HL
Su, WY
AF Wang, Hailan
Su, Wenying
TI The ENSO effects on tropical clouds and top-of-atmosphere cloud
radiative effects in CMIP5 models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE global climate models; cloud; cloud radiative effect; El Nino-Southern
Oscillation
ID GENERAL-CIRCULATION MODELS; 1997/98 EL-NINO; DIURNAL CYCLE;
INTERCOMPARISON PROJECT; CLIMATE MODEL; OCEAN; PACIFIC; ISCCP;
SIMULATION; CONVECTION
AB The El Nino-Southern Oscillation (ENSO) effects on tropical clouds and top-of-atmosphere (TOA) cloud radiative effects (CREs) in Coupled Model Intercomparison Project Phase 5 (CMIP5) models are evaluated using satellite-based observations and International Satellite Cloud Climatology Project satellite simulator output. Climatologically, most CMIP5 models produce considerably less total cloud amount with higher cloud top and notably larger reflectivity than observations in tropical Indo-Pacific (60 degrees E-200 degrees E; 10 degrees S-10 degrees N). During ENSO, most CMIP5 models strongly underestimate TOA CRE and cloud changes over western tropical Pacific. Over central tropical Pacific, while the multi-model mean resembles observations in TOA CRE and cloud amount anomalies, it notably overestimates cloud top pressure (CTP) decreases; there are also substantial inter-model variations. The relative effects of changes in cloud properties, temperature, and humidity on TOA CRE anomalies during ENSO in the CMIP5 models are assessed using cloud radiative kernels. The CMIP5 models agree with observations in that their TOA shortwave CRE anomalies are primarily contributed by total cloud amount changes, and their TOA longwave CRE anomalies are mostly contributed by changes in both total cloud amount and CTP. The model biases in TOA CRE anomalies particularly the strong underestimations over western tropical Pacific are, however, mainly explained by model biases in CTP and cloud optical thickness () changes. Despite the distinct model climatological cloud biases particularly in regime, the TOA CRE anomalies from total cloud amount changes are comparable between the CMIP5 models and observations, because of the strong compensations between model underestimation of TOA CRE anomalies from thin clouds and overestimation from medium and thick clouds.
C1 [Wang, Hailan; Su, Wenying] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Wang, Hailan] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Wang, HL (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
EM Hailan.Wang@nasa.gov
FU NASA CLOUDSAT and CALIPSO Science Team Recompete program
[NNH09ZDA001N-CCST]
FX This study is supported by the NASA CLOUDSAT and CALIPSO Science Team
Recompete program (NNH09ZDA001N-CCST). We acknowledge the World Climate
Research Programme's Working Group on Coupled Modeling, which is
responsible for CMIP, and we thank the climate modeling groups (listed
in Table 1 of this paper) for producing and making available their model
output. For CMIP, the U.S. Department of Energy's Program for Climate
Model Diagnosis and Intercomparison provides coordinating support and
led development of software infrastructure in partnership with the
Global Organization for Earth System Science Portals. The CERES EBAF
Edition 2.7 data were obtained from the NASA Langley Research Center
CERES ordering tool at http://ceres.larc.nasa.gov/cmip5_data.php/. The
ISCCP data were obtained from the website
http://climserv.ipsl.polytechnique.fr/cfmip-obs/. We thank Mark Zelinka
and two anonymous reviewers for their constructive comments and
suggestions which have significantly improved this paper.
NR 60
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Z9 1
U1 0
U2 5
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 MAY 27
PY 2015
VL 120
IS 10
BP 4443
EP 4465
DI 10.1002/2014JD022337
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800002
ER
PT J
AU Klingaman, NP
Jiang, XA
Xavier, PK
Petch, J
Waliser, D
Woolnough, SJ
AF Klingaman, Nicholas P.
Jiang, Xianan
Xavier, Prince K.
Petch, Jon
Waliser, Duane
Woolnough, Steven J.
TI Vertical structure and physical processes of the Madden-Julian
oscillation: Synthesis and summary
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Madden-Julian oscillation; diabatic processes; tropical convection;
general circulation models
ID MOIST STATIC ENERGY; COMMUNITY ATMOSPHERE MODEL; INTRASEASONAL
VARIABILITY; EASTWARD PROPAGATION; MJO SIMULATION; CLIMATE MODELS;
CONVECTION; BUDGET; PARAMETERIZATION; ORGANIZATION
AB The Vertical structure and physical processes of the Madden-Julian oscillation (MJO) project comprises three experiments, designed to evaluate comprehensively the heating, moistening, and momentum associated with tropical convection in general circulation models (GCMs). We consider here only those GCMs that performed all experiments. Some models display relatively higher or lower MJO fidelity in both initialized hindcasts and climate simulations, while others show considerable variations in fidelity between experiments. Fidelity in hindcasts and climate simulations are not meaningfully correlated. The analysis of each experiment led to the development of process-oriented diagnostics, some of which distinguished between GCMs with higher or lower fidelity in that experiment. We select the most discriminating diagnostics and apply them to data from all experiments, where possible, to determine if correlations with MJO fidelity hold across scales and GCM states. While normalized gross moist stability had a small but statistically significant correlation with MJO fidelity in climate simulations, we find no link with fidelity in medium-range hindcasts. Similarly, there is no association between time step to time step rainfall variability, identified from short hindcasts and fidelity in medium-range hindcasts or climate simulations. Two metrics that relate precipitation to free-tropospheric moisturethe relative humidity for extreme daily precipitation and variations in the height and amplitude of moistening with rain ratesuccessfully distinguish between higher-fidelity and lower fidelity GCMs in hindcasts and climate simulations. To improve the MJO, developers should focus on relationships between convection and both total moisture and its rate of change. We conclude by offering recommendations for further experiments.
C1 [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Jiang, Xianan; Waliser, Duane] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Jiang, Xianan; Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Xavier, Prince K.; Petch, Jon] Met Off, Exeter, Devon, England.
RP Klingaman, NP (reprint author), Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
EM n.p.klingaman@reading.ac.uk
RI Klingaman, Nicholas/H-4610-2012
OI Klingaman, Nicholas/0000-0002-2927-9303
FU National Centre for Atmospheric Science, a collaborative center of the
Natural Environment Research Council [R8/H12/83/001]; NSF Climate and
Large-Scale Dynamics Program [AGS-1228302]; NOAA MAPP program
[NA12OAR4310075]; Office of Naval Research [ONRBAA12-001]; NSF
[AGS-1221013]; Jet Propulsion Laboratory, California Institute of
Technology under National Aeronautics and Space Administration
FX All data from all experiments in this project are freely available
through http://earthsystemcog.org/projects/gass-yotc-mip. The authors
express their gratitude to the nine modeling centers that contributed
GCM data to all three experiments in this project, each of which was
demanding enough on its own. Comments from Chidong Zhang and an
anonymous reviewer helped us to improve the manuscript. Nicholas
Klingaman and Steven Woolnough were funded by the National Centre for
Atmospheric Science, a collaborative center of the Natural Environment
Research Council, under contract R8/H12/83/001. Xianan Jiang
acknowledges support by NSF Climate and Large-Scale Dynamics Program
under award AGS-1228302 and NOAA MAPP program under award
NA12OAR4310075. Duane Waliser acknowledges support from the Office of
Naval Research under Project ONRBAA12-001 and NSF AGS-1221013, and the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 55
TC 14
Z9 14
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 4671
EP 4689
DI 10.1002/2015JD023196
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800015
ER
PT J
AU Klingaman, NP
Woolnough, SJ
Jiang, XN
Waliser, D
Xavier, PK
Petch, J
Caian, M
Hannay, C
Kim, D
Ma, HY
Merryfield, WJ
Miyakawa, T
Pritchard, M
Ridout, JA
Roehrig, R
Shindo, E
Vitart, F
Wang, HL
Cavanaugh, NR
Mapes, BE
Shelly, A
Zhang, GJ
AF Klingaman, Nicholas P.
Woolnough, Steven J.
Jiang, Xianan
Waliser, Duane
Xavier, Prince K.
Petch, Jon
Caian, Mihaela
Hannay, Cecile
Kim, Daehyun
Ma, Hsi-Yen
Merryfield, William J.
Miyakawa, Tomoki
Pritchard, Mike
Ridout, James A.
Roehrig, Romain
Shindo, Eiki
Vitart, Frederic
Wang, Hailan
Cavanaugh, Nicholas R.
Mapes, Brian E.
Shelly, Ann
Zhang, Guang J.
TI Vertical structure and physical processes of the Madden-Julian
oscillation: Linking hindcast fidelity to simulated diabatic heating and
moistening
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Madden-Julian oscillation; tropical convection; diabatic heating; model
evaluation; hindcasts; diabatic moistening
ID TEMPERATURE-GRADIENT APPROXIMATION; TROPICAL INTRASEASONAL OSCILLATION;
COMMUNITY ATMOSPHERE MODEL; MULTIVARIATE MJO INDEX; 30-50 DAY
VARIABILITY; GLOBAL CLIMATE MODEL; PART I; SYSTEMATIC-ERRORS; FORECAST
SYSTEM; SUMMER MONSOON
AB Many theories for the Madden-Julian oscillation (MJO) focus on diabatic processes, particularly the evolution of vertical heating and moistening. Poor MJO performance in weather and climate models is often blamed on biases in these processes and their interactions with the large-scale circulation. We introduce one of the three components of a model evaluation project, which aims to connect MJO fidelity in models to their representations of several physical processes, focusing on diabatic heating and moistening. This component consists of 20day hindcasts, initialized daily during two MJO events in winter 2009-2010. The 13 models exhibit a range of skill: several have accurate forecasts to 20days lead, while others perform similarly to statistical models (8-11days). Models that maintain the observed MJO amplitude accurately predict propagation, but not vice versa. We find no link between hindcast fidelity and the precipitation-moisture relationship, in contrast to other recent studies. There is also no relationship between models' performance and the evolution of their diabatic heating profiles with rain rate. A more robust association emerges between models' fidelity and net moistening: the highest-skill models show a clear transition from low-level moistening for light rainfall to midlevel moistening at moderate rainfall and upper level moistening for heavy rainfall. The midlevel moistening, arising from both dynamics and physics, may be most important. Accurately representing many processes may be necessary but not sufficient for capturing the MJO, which suggests that models fail to predict the MJO for a broad range of reasons and limits the possibility of finding a panacea.
C1 [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Jiang, Xianan; Waliser, Duane] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Jiang, Xianan; Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Xavier, Prince K.; Petch, Jon; Shelly, Ann] UK Met Off, Exeter, Devon, England.
[Caian, Mihaela] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden.
[Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Ma, Hsi-Yen] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA.
[Merryfield, William J.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Dept Coupled Ocean Atmosphere Land Proc Res, Yokosuka, Kanagawa 2370061, Japan.
[Miyakawa, Tomoki] Univ Tokyo, Atmosphere & Ocean Res Inst, Tokyo, Japan.
[Pritchard, Mike] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Ridout, James A.] Naval Res Lab, Monterey, CA USA.
[Roehrig, Romain] Meteo France, CNRM GAME, Toulouse, France.
[Roehrig, Romain] CNRS, Toulouse, France.
[Shindo, Eiki] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan.
[Vitart, Frederic] European Ctr Medium Range Weather Forecasts, Reading, Berks, England.
[Wang, Hailan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cavanaugh, Nicholas R.; Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Mapes, Brian E.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Coral Gables, FL 33124 USA.
RP Klingaman, NP (reprint author), Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England.
EM n.p.klingaman@reading.ac.uk
RI Klingaman, Nicholas/H-4610-2012; Ma, Hsi-Yen/K-1019-2013
OI Klingaman, Nicholas/0000-0002-2927-9303;
FU National Centre for Atmospheric Science, a collaborative center of the
Natural Environment Research Council [R8/H12/83/001]; NSF Climate and
Large-Scale Dynamics program [AGS-1228302]; NOAA MAPP program
[NA12OAR4310075]; Office of Naval Research [ONRBAA12-001, 0601153N]; NSF
[AGS-1221013, OCI-1053575, AGS-1015964]; Jet Propulsion Laboratory,
California Institute of Technology under National Aeronautics and Space
Administration; National Science Foundation; NASA [NNX13AM18G]; Korea
Meteorological Administration Research and Development Program [CATER
2013-3142]; U.S. DOE as part of the CAPT; U.S. DOE by LLNL
[DE-AC52-07NA27344]; NOAA CGC postdoctoral fellowship; NOAA
[NA11OAR4310098]; DOE [DE-SC0008880]; [ATM-0425247]
FX The complete archive of data produced by this project and analyzed in
this manuscript is freely available for download from
https://earthsystemcog.org/projects/gass-yotc-mip/. The authors are
grateful to Chindong Zhang and three anonymous reviewers for their
comments and suggestions on this manuscript. Nicholas Klingaman and
Steven Woolnough were funded by the National Centre for Atmospheric
Science, a collaborative center of the Natural Environment Research
Council, under contract R8/H12/83/001. Xianan Jiang acknowledges support
by NSF Climate and Large-Scale Dynamics program under award AGS-1228302
and NOAA MAPP program under award NA12OAR4310075. Duane Waliser
acknowledges support from the Office of Naval Research under project
ONRBAA12-001, and NSF AGS-1221013, and the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The National Center for
Atmospheric Research is sponsored by the National Science Foundation.
Daehyun Kim appreciates the NASA/GISS modeling group, especially Maxwell
Kelley, Mao-Sung Yao, and Anthony Del Genio, for their invaluable and
unlimited support. Daehyun Kim was supported by the NASA grant
NNX13AM18G and the Korea Meteorological Administration Research and
Development Program under grant CATER 2013-3142. The effort of Hsi-Yen
Ma was funded by the RGCM and ASR programs of the U.S. DOE as part of
the CAPT. This work was performed under the auspices of the U.S. DOE by
LLNL under contract DE-AC52-07NA27344. William Merryfield acknowledges
Jason Cole and Mike Lazare for their roles in producing CanCM4 data and
Woo-Sung Lee for performing the CanCM4 simulations. Tomoki Miyakawa
acknowledges the NICAM and MIROC teams for developing the models; M.
Watanabe, H. Miura, and T. Nasuno for supervising the simulations; N.
Hirota and T. Hashino for assistance in data processing; and a grant of
supercomputing resources from the Earth Simulator Center. Mike Pritchard
was supported by a NOAA CGC postdoctoral fellowship; he thanks Marat
Khairoutdinov for developing and making SPCAM3 available through the
Center for Multiscale Modeling of Atmospheric Processes, a National
Science Foundation (NSF) Science and Technology Center managed by
Colorado State University under cooperative agreement ATM-0425247.
Computing resources for SPCAM3 simulations were provided courtesy of the
Extreme Science and Engineering Discovery Environment, supported by NSF
grant OCI-1053575 under allocation TG-ATM120034. James Ridout gratefully
acknowledges support from the Office of Naval Research program element
0601153N, a grant of computing time from the United States Department of
Defense High Performance Computing Modernization Program, and assistance
from Maria Flatau in preparing the NavGEM1 hindcasts. Frederic Vitart
acknowledges Peter Bechtold for assisting in producing tendency output
from the ECMWF IFS hindcasts. Guang Zhang was supported by NSF
AGS-1015964, NOAA NA11OAR4310098, and DOE DE-SC0008880.
NR 103
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U1 2
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 4690
EP 4717
DI 10.1002/2014JD022374
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800016
ER
PT J
AU Jiang, X
Waliser, DE
Xavier, PK
Petch, J
Klingaman, NP
Woolnough, SJ
Guan, B
Bellon, G
Crueger, T
DeMott, C
Hannay, C
Lin, H
Hu, WT
Kim, D
Lappen, CL
Lu, MM
Ma, HY
Miyakawa, T
Ridout, JA
Schubert, SD
Scinocca, J
Seo, KH
Shindo, E
Song, XL
Stan, C
Tseng, WL
Wang, WQ
Wu, TW
Wu, XQ
Wyser, K
Zhang, GJ
Zhu, HY
AF Jiang, Xianan
Waliser, Duane E.
Xavier, Prince K.
Petch, Jon
Klingaman, Nicholas P.
Woolnough, Steven J.
Guan, Bin
Bellon, Gilles
Crueger, Traute
DeMott, Charlotte
Hannay, Cecile
Lin, Hai
Hu, Wenting
Kim, Daehyun
Lappen, Cara-Lyn
Lu, Mong-Ming
Ma, Hsi-Yen
Miyakawa, Tomoki
Ridout, James A.
Schubert, Siegfried D.
Scinocca, John
Seo, Kyong-Hwan
Shindo, Eiki
Song, Xiaoliang
Stan, Cristiana
Tseng, Wan-Ling
Wang, Wanqiu
Wu, Tongwen
Wu, Xiaoqing
Wyser, Klaus
Zhang, Guang J.
Zhu, Hongyan
TI Vertical structure and physical processes of the Madden-Julian
oscillation: Exploring key model physics in climate simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Madden-Julian oscillation; general circulation model; moist convection;
multiscale interaction
ID TROPICAL INTRASEASONAL OSCILLATION; CONVECTIVE MOMENTUM TRANSPORT;
GENERAL-CIRCULATION MODEL; MOIST STATIC ENERGY; COUPLED EQUATORIAL
WAVES; TEMPERATURE-GRADIENT APPROXIMATION; SEA-SURFACE TEMPERATURES;
ASIAN SUMMER MONSOON; 1997-98 EL-NINO; TOGA COARE IOP
AB Aimed at reducing deficiencies in representing the Madden-Julian oscillation (MJO) in general circulation models (GCMs), a global model evaluation project on vertical structure and physical processes of the MJO was coordinated. In this paper, results from the climate simulation component of this project are reported. It is shown that the MJO remains a great challenge in these latest generation GCMs. The systematic eastward propagation of the MJO is only well simulated in about one fourth of the total participating models. The observed vertical westward tilt with altitude of the MJO is well simulated in good MJO models but not in the poor ones. Damped Kelvin wave responses to the east of convection in the lower troposphere could be responsible for the missing MJO preconditioning process in these poor MJO models. Several process-oriented diagnostics were conducted to discriminate key processes for realistic MJO simulations. While large-scale rainfall partition and low-level mean zonal winds over the Indo-Pacific in a model are not found to be closely associated with its MJO skill, two metrics, including the low-level relative humidity difference between high- and low-rain events and seasonal mean gross moist stability, exhibit statistically significant correlations with the MJO performance. It is further indicated that increased cloud-radiative feedback tends to be associated with reduced amplitude of intraseasonal variability, which is incompatible with the radiative instability theory previously proposed for the MJO. Results in this study confirm that inclusion of air-sea interaction can lead to significant improvement in simulating the MJO.
C1 [Jiang, Xianan; Waliser, Duane E.; Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90089 USA.
[Jiang, Xianan; Waliser, Duane E.; Guan, Bin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Xavier, Prince K.; Petch, Jon] UK Met Off, Exeter, Devon, England.
[Klingaman, Nicholas P.; Woolnough, Steven J.] Natl Ctr Atmospher Sci, Reading, Berks, England.
[Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Bellon, Gilles] CNRS, Meteo France, CNRM GAME, Toulouse, France.
[Crueger, Traute] Max Planck Inst Meteorol, Hamburg, Germany.
[DeMott, Charlotte] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Lin, Hai] Environm Canada, Dorval, PQ, Canada.
[Hu, Wenting] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Numer Modeling Atmospher Sci & Geop, Beijing, Peoples R China.
[Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA.
[Lappen, Cara-Lyn] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Lu, Mong-Ming] Cent Weather Bur, Taipei, Taiwan.
[Ma, Hsi-Yen] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Dept Coupled Ocean Atmosphere Land Proc Res, Yokosuka, Kanagawa 2370061, Japan.
[Ridout, James A.] Naval Res Lab, Monterey, CA USA.
[Schubert, Siegfried D.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Scinocca, John] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Seo, Kyong-Hwan] Pusan Natl Univ, Dept Atmospher Sci, Pusan 609735, South Korea.
[Shindo, Eiki] Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 305, Japan.
[Song, Xiaoliang; Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Stan, Cristiana] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA.
[Tseng, Wan-Ling] Acad Sinica, Univ Res Ctr Environm Changes, Taipei 115, Taiwan.
[Wang, Wanqiu] NOAA, Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD USA.
[Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China.
[Wu, Xiaoqing] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA USA.
[Wyser, Klaus] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden.
[Zhu, Hongyan] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
RP Jiang, XA (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90089 USA.
EM xianan@ucla.edu
RI Stan, Cristiana/B-4376-2009; Klingaman, Nicholas/H-4610-2012; DeMott,
Charlotte/L-7414-2015; Ma, Hsi-Yen/K-1019-2013; Guan, Bin/F-6735-2010;
OI Stan, Cristiana/0000-0002-0076-0574; Klingaman,
Nicholas/0000-0002-2927-9303; DeMott, Charlotte/0000-0002-3975-1288;
Bellon, Gilles/0000-0003-3981-1225
FU National Science Foundation (NSF) Climate and Large-Scale Dynamics
Program [AGS-1228302]; NOAA MAPP program [NA12OAR4310075]; Office of
Naval Research [ONRBAA12-001, 0601153N]; NSF [AGS-1221013, AGS-1211848,
ATM-0935263]; Jet Propulsion Laboratory, California Institute of
Technology under NASA; National Centre for Atmospheric Science, a
National Environment Research Council collaborative center
[R8/H12/83/001]; Joint DECC/Defra Met Office Hadley Centre Climate
Programme [GA01101]; NASA [NNX13AM18G]; Korea Meteorological
Administration Research and Development Program [CATER 2013-3142];
National Science Foundation; European Union [244067]; U.S. DOE as part
of the CAPT; U.S. DOE by LLNL [DE-AC52-07NA27344]; National Research
Foundation of Korea - Ministry of Education, Science and Technology
[2011-0015486]
FX The multimodel output collected by this project and analyzed in this
study is available for free download from
https://earthsystemcog.org/projects/gassyotc-mip/. We acknowledge the
insightful comments from the Editor, C. Zhang, and J. Lin and other two
reviewers, which greatly helped improve this manuscript. We would like
to thank E. Maloney and J. Benedict for their help with the calculation
of gross moist stability. We are indebted to E. Maloney, A. Del Genio,
B. Wang, B. Mapes, M. Moncrieff, A. Majda, C. Zhang, T. Li, and WGNE MJO
Task Force members for stimulating discussions during the course of this
study. X. Jiang acknowledges support by National Science Foundation
(NSF) Climate and Large-Scale Dynamics Program under awards AGS-1228302,
and NOAA MAPP program under award NA12OAR4310075. D. Waliser
acknowledges the Office of Naval Research under Project ONRBAA12-001,
NSF AGS-1221013, and the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the NASA. N. Klingaman and S.
Woolnough were supported by the National Centre for Atmospheric Science,
a National Environment Research Council collaborative center, under
contract R8/H12/83/001. P. Xavier and J. Petch are supported by the
Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101).
D. Kim was supported by the NASA grant NNX13AM18G and the Korea
Meteorological Administration Research and Development Program under
grant CATER 2013-3142, and he appreciates the NASA/GISS modeling group,
especially M. Kelley, M.-S. Yao, and A. Del Genio for their invaluable
and unlimited supports. J. Ridout gratefully acknowledges support from
the Office of Naval Research Program Element 0601153N, a grant of
computing time from the United States Department of Defense High
Performance Computing Modernization Program. The SMHI simulations were
performed on resources provided by the Swedish National Infrastructure
for Computing (SNIC) at the Parallel Computing Centre (PDC). The
National Center for Atmospheric Research is sponsored by the National
Science Foundation. Some of this research by T. Crueger has received
funding from the European Union, Seventh Framework Programme
(FP7/2007-2013) under grant agreement 244067. The effort of H.-Y. Ma was
funded by the RGCM and ASR programs of the U.S. DOE as part of the CAPT.
This work was performed under the auspices of the U.S. DOE by LLNL under
contract DE-AC52-07NA27344. C. Stan was supported by NSF grant
AGS-1211848. K.-H. Seo is supported by the National Research Foundation
of Korea grant (2011-0015486) funded by the Ministry of Education,
Science and Technology. X. Wu is supported by the NSF under grant
ATM-0935263. T. Miyakawa acknowledges M. Watanabe and N. Hirota for
their support in providing MIROC data set, and the Earth Simulator
(JIMSTEC) for the computation. W-L Tseng was supported by the German
BMBF NORDATLANTIK project, and the Norddeutscher Verbund fur Hoch- und
Hochstleistungsrechnen for the computation.
NR 204
TC 39
Z9 39
U1 7
U2 40
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 4718
EP 4748
DI 10.1002/2014JD022375
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800017
ER
PT J
AU Xavier, PK
Petch, JC
Klingaman, NP
Woolnough, SJ
Jiang, XA
Waliser, DE
Caian, M
Cole, J
Hagos, SM
Hannay, C
Kim, D
Miyakawa, T
Pritchard, MS
Roehrig, R
Shindo, E
Vitart, F
Wang, HL
AF Xavier, Prince K.
Petch, Jon C.
Klingaman, Nicholas P.
Woolnough, Steve J.
Jiang, Xianan
Waliser, Duane E.
Caian, Mihaela
Cole, Jason
Hagos, Samson M.
Hannay, Cecile
Kim, Daehyun
Miyakawa, Tomoki
Pritchard, Michael S.
Roehrig, Romain
Shindo, Eiki
Vitart, Frederic
Wang, Hailan
TI Vertical structure and physical processes of the Madden-Julian
Oscillation: Biases and uncertainties at short range
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE diabatic processes; Madden-Julian Oscillation; modeling; convection;
Year of Tropical convection; uncertainties
ID CONVECTIVE MOMENTUM TRANSPORT; GLOBAL CLIMATE MODEL; TOGA COARE;
INTRASEASONAL OSCILLATION; POTENTIAL PREDICTABILITY; TROPICAL
CONVECTION; WEATHER PREDICTION; SYSTEMATIC-ERRORS; ACTIVE CONVECTION;
PART II
AB An analysis of diabatic heating and moistening processes from 12 to 36h lead time forecasts from 12 Global Circulation Models are presented as part of the Vertical structure and physical processes of the Madden-Julian Oscillation (MJO) project. A lead time of 12-36h is chosen to constrain the large-scale dynamics and thermodynamics to be close to observations while avoiding being too close to the initial spin-up of the models as they adjust to being driven from the Years of Tropical Convection (YOTC) analysis. A comparison of the vertical velocity and rainfall with the observations and YOTC analysis suggests that the phases of convection associated with the MJO are constrained in most models at this lead time although the rainfall in the suppressed phase is typically overestimated. Although the large-scale dynamics is reasonably constrained, moistening and heating profiles have large intermodel spread. In particular, there are large spreads in convective heating and moistening at midlevels during the transition to active convection. Radiative heating and cloud parameters have the largest relative spread across models at upper levels during the active phase. A detailed analysis of time step behavior shows that some models show strong intermittency in rainfall and differences in the precipitation and dynamics relationship between models. The wealth of model outputs archived during this project is a very valuable resource for model developers beyond the study of the MJO. In addition, the findings of this study can inform the design of process model experiments, and inform the priorities for field experiments and future observing systems.
C1 [Xavier, Prince K.; Petch, Jon C.] Met Off, Exeter, Devon, England.
[Klingaman, Nicholas P.; Woolnough, Steve J.] Univ Reading, Natl Ctr Atmospher Sci Climate, Reading, Berks, England.
[Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Caian, Mihaela] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden.
[Cole, Jason] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Hagos, Samson M.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Yokosuka, Kanagawa, Japan.
[Pritchard, Michael S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Roehrig, Romain] Meteo France, CNRM, GAME, Toulouse, France.
[Roehrig, Romain] CNRS, Toulouse, France.
[Shindo, Eiki] Meteorol Res Inst, Climate Res Dept, Ibaraki, Japan.
[Vitart, Frederic] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Wang, Hailan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Xavier, PK (reprint author), Met Off, Exeter, Devon, England.
EM prince.xavier@metoffice.gov.uk
RI Klingaman, Nicholas/H-4610-2012;
OI Klingaman, Nicholas/0000-0002-2927-9303; Cole, Jason/0000-0003-0450-2748
FU Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101];
U.S. National Science Foundation (NSF); NASA Modeling, Analysis and
Prediction (MAP) program; National Aeronautics and Space Administration;
NSF Climate and Large-Scale Dynamics Program [AGS-1228302]; NOAA MAPP
program [NA12OAR4310075]; National Centre for Atmospheric Science, a
Natural Environment Research Council collaborative center; Office of
Biological and Environmental Research of the U. S. Department of Energy
as part of the Atmospheric Systems Research Program; NASA [NNX13AM18G];
Korea Meteorological Administration Research and Development Program
[CATER 2013-3142]; U.S. National Science Foundation; NOAA CGC
postdoctoral fellowship; NSF [OCI-1053575]; [ATM-0425247]
FX The GASS-YoTC Vertical Structure and Physical Processes Multi-model
Experiment was supported by the World Climate Research Program and World
Weather Research Program and organized by the GEWEX Global Atmospheric
System Studies (GASS) subproject and the YoTC/WGNE MJO Task Force. IT
support and data services hosted by the NASA Jet Propulsion Laboratory.
P. Xavier and J. Petch are supported by the Joint DECC/Defra Met Office
Hadley Centre Climate Programme (GA01101). Support for D. Waliser was
provided by the U.S. National Science Foundation (NSF) and the NASA
Modeling, Analysis and Prediction (MAP) program with his research
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. X. Jiang acknowledges support by NSF Climate and
Large-Scale Dynamics Program under award AGS-1228302 and NOAA MAPP
program under award NA12OAR4310075. Support for N. Klingaman and S.
Woolnough was provided by the National Centre for Atmospheric Science, a
Natural Environment Research Council collaborative center. T. Miyakawa
acknowledges the MIROC team (for developing the model), M. Watanabe (for
supervising the simulations), N. Hirota and T. Hashino (for their
support in data processing), and the Earth simulator (for computation).
S. Hagos acknowledges support from the Office of Biological and
Environmental Research of the U. S. Department of Energy as part of the
Atmospheric Systems Research Program. D. Kim appreciates the NASA/GISS
modeling group, especially M. Kelley, M.-S. Yao, and A. Del Genio for
their invaluable and unlimited support. D. Kim was supported by the NASA
grant NNX13AM18G and the Korea Meteorological Administration Research
and Development Program under grant CATER 2013-3142. NCAR is sponsored
by the U.S. National Science Foundation. M. Pritchard was supported by a
NOAA CGC postdoctoral fellowship; he thanks M. Khairoutdinov for
developing and making SPCAM3 available through the Center for Multiscale
Modeling of Atmospheric Processes, a NSF Science and Technology Center
managed by Colorado State University under Cooperative agreement
ATM-0425247. Computing resources for SPCAM3 simulations were provided
courtesy of the Extreme Science and Engineering Discovery Environment,
supported by NSF grant OCI-1053575 under allocation TG-ATM120034. We
acknowledge the insightful comments from C. Zhang and three anonymous
reviewers which helped improve the manuscript. M. Webb and A.
Bodas-Salcedo are acknowledged for providing information on cloud
radiative heating. Quality-controlled model data from all three
experiments are archived at Earth System Grid
(https://earthsystemcog.org/projects/gass-yotc-mip/) and are available
for download.
NR 75
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U1 2
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 4749
EP 4763
DI 10.1002/2014JD022718
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800018
ER
PT J
AU Painemal, D
Minnis, P
Nordeen, M
AF Painemal, David
Minnis, Patrick
Nordeen, Michele
TI Aerosol variability, synoptic-scale processes, and their link to the
cloud microphysics over the northeast Pacific during MAGIC
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol indirect effect; boundary layer clouds; northeast Pacific;
satellite clouds microphysics; MAGIC campaign
ID DATA ASSIMILATION SYSTEM; MARINE STRATOCUMULUS; CALIFORNIA COAST;
BOUNDARY-LAYER; OPTICAL DEPTH; VOCALS-REX; SATELLITE; REANALYSIS;
CLIMATE
AB Shipborne aerosol measurements collected from October 2012 to September 2013 along 36 transects between the port of Los Angeles, California (33.7 degrees N, 118.2 degrees), and Honolulu, Hawaii (21.3 degrees N, 157.8 degrees W), during the Marine ARM GPCI (Global Energy and Water Cycle Experiment (GEWEX)-Cloud System Study (GCSS)-Pacific Cross-section Intercomparison) Investigation of Clouds campaign are analyzed to determine the circulation patterns that modulate the synoptic and monthly variability of cloud condensation nuclei (CCN) in the boundary layer. Seasonal changes in CCN are evident, with low magnitudes during autumn/winter, and high CCN during spring/summer accompanied with a characteristic westward decrease. CCN monthly evolution is consistent with satellite-derived cloud droplet number concentration N-d from the Moderate Resolution Imaging Spectroradiometer. One-point correlation (r) analysis between the 1000hPa zonal wind time series over a region between 125 degrees W and 135 degrees W, 35 degrees N and 45 degrees N, and the N-d field yields a negative r (up to -0.55) over a domain that covers a zonal extent of at least 20 degrees from the California shoreline, indicating that N-d decreases when the zonal wind intensifies. The negative r expands southwestward as the zonal wind precedes N-d by up to 3days, suggesting a transport mechanism from the coast of North America mediated by the California low-coastal jet, which intensifies in summer when the aerosol concentration and N-d reach a maximum. A first assessment of aerosol-cloud interaction (ACI) is performed by combining CCN and satellite N-d values from the Fifteenth Geostationary Operational Environmental Satellite. The CCN-N-d correlation is 0.66-0.69, and the ACI metric defined as ACI=ln(N-d)/ln(CCN) is high at 0.9, similar to other aircraft-based studies and substantially greater than those inferred from satellites and climate models.
C1 [Painemal, David; Nordeen, Michele] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Painemal, David; Minnis, Patrick; Nordeen, Michele] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Painemal, D (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM david.painemal@nasa.gov
FU U.S. Department of Energy, Office of Biological and Environmental
Research, Atmospheric System Research Program [DE-FOA-0000885]
FX This research was supported by the U.S. Department of Energy, Office of
Biological and Environmental Research, Atmospheric System Research
Program grant DE-FOA-0000885. The MAGIC data set was downloaded from the
ARM archive available at http://www.archive.arm.gov/. MODIS retrievals
are available at http://ceres.larc.nasa.gov/order_data.php and GOES 15
at http://www-pm.larc.nasa.gov or upon request. The authors thank the
NOAA Air Resources Laboratory for making available the HYSPLIT online
application used to perform the back trajectory analysis
(http://www.ready.noaa.gov). We acknowledge Horizon Lines and the
Captain and crew of the Horizon Spirit, as well as the leadership of
MAGIC PI Ernie Lewis and the work of scientists and technicians involved
in the data collection and postprocessing.
NR 45
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U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 5122
EP 5139
DI 10.1002/2015JD023175
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800038
ER
PT J
AU Sun, K
Cady-Pereira, K
Miller, DJ
Tao, L
Zondlo, MA
Nowak, JB
Neuman, JA
Mikoviny, T
Muller, M
Wisthaler, A
Scarino, AJ
Hostetler, CA
AF Sun, Kang
Cady-Pereira, Karen
Miller, David J.
Tao, Lei
Zondlo, Mark A.
Nowak, John B.
Neuman, J. A.
Mikoviny, Tomas
Mueller, Markus
Wisthaler, Armin
Scarino, Amy J.
Hostetler, Chris A.
TI Validation of TES ammonia observations at the single pixel scale in the
San Joaquin Valley during DISCOVER-AQ
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE TES; ammonia; validation; NH3
ID IASI SATELLITE-OBSERVATIONS; QUANTUM CASCADE-LASER; ATMOSPHERIC AMMONIA;
OPEN-PATH; PARTICULATE MATTER; EMISSIONS; NH3; RESOLUTION; MODEL;
CALIBRATION
AB Ammonia measurements from a vehicle-based, mobile open-path sensor and those from aircraft were compared with Tropospheric Emission Spectrometer (TES) NH3 columns at the pixel scale during the NASA Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality field experiment. Spatial and temporal mismatches were reduced by having the mobile laboratory sample in the same areas as the TES footprints. To examine how large heterogeneities in the NH3 surface mixing ratios may affect validation, a detailed spatial survey was performed within a single TES footprint around the overpass time. The TES total NH3 column above a single footprint showed excellent agreement with the in situ total column constructed from surface measurements with a difference of 2% (within the combined measurement uncertainties). The comparison was then extended to a TES transect of nine footprints where aircraft data (5-80ppbv) were available in a narrow spatiotemporal window (<10km, <1h). The TES total NH3 columns above the nine footprints agreed to within 6% of the in situ total columns derived from the aircraft-based measurements. Finally, to examine how TES captures surface spatial gradients at the interpixel scale, ground-based, mobile measurements were performed directly underneath a TES transect, covering nine footprints within 1.5h of the overpass. The TES total columns were strongly correlated (R-2=0.82) with the median NH3 mixing ratios measured at the surface. These results provide the first in situ validation of the TES total NH3 column product, and the methodology is applicable to other satellite observations of short-lived species at the pixel scale.
C1 [Sun, Kang; Miller, David J.; Tao, Lei; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Sun, Kang; Miller, David J.; Tao, Lei; Zondlo, Mark A.] ERC, NSF, Infrared Technol Hlth & Environm, Ctr Mid, Princeton, NJ USA.
[Cady-Pereira, Karen] Atmospher & Environm Res, Lexington, MA USA.
[Nowak, John B.] Aerodyne Res Inc, Billerica, MA USA.
[Neuman, J. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Neuman, J. A.] NOAA Earth Syst Res Lab, Boulder, CO 80309 USA.
[Mikoviny, Tomas; Wisthaler, Armin] Inst Ionenphys & Angew Phys, Innsbruck, Austria.
[Mikoviny, Tomas; Wisthaler, Armin] Univ Oslo, Dept Chem, Oslo, Norway.
[Mueller, Markus] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Scarino, Amy J.] Sci Syst & Applications Inc, Hampton, VA USA.
[Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Zondlo, MA (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
EM mzondlo@princeton.edu
RI Nowak, John/B-1085-2008; Muller, Markus/L-1699-2014; Neuman,
Andy/A-1393-2009; Zondlo, Mark/R-6173-2016; Manager, CSD
Publications/B-2789-2015
OI Nowak, John/0000-0002-5697-9807; Muller, Markus/0000-0003-4110-8950;
Neuman, Andy/0000-0002-3986-1727; Zondlo, Mark/0000-0003-2302-9554;
FU Center for Mid-Infrared Technologies for Health and the Environment
under National Science Foundation [EEC-0540832]; NASA Earth and Space
Science Fellowship [NN12AN64H]; NASA Jet Propulsion Laboratory; Austrian
Federal Ministry for Transport, Innovation and Technology (bmvit)
through Austrian Space Applications Programme of the Austrian Research
Promotion Agency (FFG) [9, 840086]; National Institute of Aerospace;
NASA
FX We acknowledge the support of the NASA DISCOVER-AQ California 2013
science team, as well as Trent Proctor of the U.S. Forest Service for
providing work and storage space in Porterville, California. We thank
Michael Shook, Jennifer Olson, and Gao Chen for providing the merged
airborne NH3 data set and PBL heights derived from P-3B data
and Robert Herman for providing the TES footprint coordinates before the
overpass. The sensor development was supported by the Center for
Mid-Infrared Technologies for Health and the Environment under National
Science Foundation grant EEC-0540832. Kang Sun acknowledges support by
NASA Earth and Space Science Fellowship (NN12AN64H). Work at AER was
funded through a contract with the NASA Jet Propulsion Laboratory. The
CRDS NH3 measurements were made possible by the generous
support from the DISCOVER-AQ program. NH3 measurements by the
PTR-ToF-MS aboard the NASA P-3B were supported by the Austrian Federal
Ministry for Transport, Innovation and Technology (bmvit) through the
Austrian Space Applications Programme 9 of the Austrian Research
Promotion Agency (FFG) (840086). The measurement instrument was
developed in joint work with Ionicon Analytik GmbH (Innsbruck, Austria).
Armin Wisthaler received support from the Visiting Scientist Program at
the National Institute of Aerospace. Tomas Mikoviny was supported by an
appointment to the NASA Postdoctoral Program at the Langley Research
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. The aircraft measurement teams acknowledge NASA
B-200 King Air and P-3B flight crew for their outstanding work
supporting these flights. All data used in this study are available at
DISCOVER-AQ data archive
(http://www-air.larc.nasa.gov/cgi-bin/ArcView/discover-aq.ca-2013).
NR 42
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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 MAY 27
PY 2015
VL 120
IS 10
BP 5140
EP 5154
DI 10.1002/2014JD022846
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800039
ER
PT J
AU Liu, JJ
Bowman, KW
Henze, DK
AF Liu, Junjie
Bowman, Kevin W.
Henze, Daven K.
TI Source-receptor relationships of column-average CO2 and implications for
the impact of observations on flux inversions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE adjoint sensitivity; local versus nonlocal flux contributions;
observation impact; GOSAT column CO2
ID VARIATIONAL DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; ATMOSPHERIC CO2;
FIRE EMISSIONS; MODEL; OCEAN; ADJOINT; COMMUNITIES; INFORMATION;
TRANSPORT
AB Source-receptor relationships are the fundamental quantities used in atmosphere CO2 flux inversions. In this study, we systematically investigate the global source-receptor relationships of column CO2 (X-CO2) in 12 continental-scale receptors in terms of transport and local versus nonlocal flux contributions using the GEOS-Chem adjoint model. Using simulated Greenhouse gases Observing Satellite (GOSAT) X-CO2, we quantify the impact of inclusion (add-on) or exclusion of observations (data-denial) within a receptor region on flux inversion. We discuss the connections between the observation impact and the underlying source-receptor relationships. The strong sensitivity of X-CO2 to nonlocal fluxes makes the X-CO2 observations have strong impact on nonlocal flux estimation. On an annual mean, the impact of GOSAT X-CO2 over Europe on North America flux estimation is 10%-39% of the full observation impact. Because the Southern Hemisphere midlatitude X-CO2 are most sensitive to local and tropical fluxes, the mean impact of GOSAT X-CO2 over Southern South America on Northern South America (N-S-America) flux estimation is 30%-59% of the full observation impact. Because of the strong sensitivity of the X-CO2 over N-S-America to Central Africa (C-Africa) fluxes, the mean impact on C-Africa flux estimation is between 14% and 31% of the full observation impact in spite of the sparse observation coverage. The results also show that X-CO2 have similar sensitivity to local and nonlocal fluxes occurring 3 months before, which indicates that X-CO2 observations cannot differentiate any fluxes occurring beyond 3 months.
C1 [Liu, Junjie; Bowman, Kevin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
RP Liu, JJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM junjie.liu@jpl.nasa.gov
RI Chem, GEOS/C-5595-2014;
OI LIu, Junjie/0000-0002-7184-6594
FU OCO-2 science team grant [11-OCO211-24]; NASA Carbon Monitoring System
program
FX Data to support this article can be obtained by contacting the
corresponding author by email (junjie.liu@jpl.nasa.gov). We appreciate
the constructive comments from the three anonymous reviewers. We
acknowledge the funding support from OCO-2 science team grant
(11-OCO211-24) and NASA Carbon Monitoring System program. The GOSAT-ACOS
XCO2 data were produced by the ACOS/OCO-2 project at the Jet
Propulsion Laboratory, California Institute of Technology, and obtained
from the ACOS/OCO-2 data archive maintained at the NASA Goddard Earth
Science Data and Information Services Center. The GOSAT spectra were
provided to the ACOS Team through a GOSAT Research Announcement (RA)
agreement between the California Institute of Technology and the three
parties, JAXA, NIES, and the MOE. A portion 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. All the computations were performed in NASA AMES
supercomputers.
NR 47
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Z9 7
U1 3
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 MAY 27
PY 2015
VL 120
IS 10
BP 5214
EP 5236
DI 10.1002/2014JD022914
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800042
ER
PT J
AU Houweling, S
Baker, D
Basu, S
Boesch, H
Butz, A
Chevallier, F
Deng, F
Dlugokencky, EJ
Feng, L
Ganshin, A
Hasekamp, O
Jones, D
Maksyutov, S
Marshall, J
Oda, T
O'Dell, CW
Oshchepkov, S
Palmer, PI
Peylin, P
Poussi, Z
Reum, F
Takagi, H
Yoshida, Y
Zhuravlev, R
AF Houweling, S.
Baker, D.
Basu, S.
Boesch, H.
Butz, A.
Chevallier, F.
Deng, F.
Dlugokencky, E. J.
Feng, L.
Ganshin, A.
Hasekamp, O.
Jones, D.
Maksyutov, S.
Marshall, J.
Oda, T.
O'Dell, C. W.
Oshchepkov, S.
Palmer, P. I.
Peylin, P.
Poussi, Z.
Reum, F.
Takagi, H.
Yoshida, Y.
Zhuravlev, R.
TI An intercomparison of inverse models for estimating sources and sinks of
CO2 using GOSAT measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE carbon cycle; carbon dioxide; inverse modeling; model intercomparison;
satellite remote sensing
ID ATMOSPHERIC CO2; TRANSPORT SIMULATIONS; RETRIEVAL ALGORITHM; REGIONAL
CO2; GLOBAL CO2; ENSEMBLE; FLUXES; XCO2; VALIDATION; CHEMISTRY
AB This study presents the outcome of an inverse modeling intercomparison experiment on the use of total column CO2 retrievals from Greenhouse Gas Observing Satellite (GOSAT) for quantifying global sources and sinks of CO2. Eight research groups submitted inverse modeling results for the first year of GOSAT measurements. Inversions were carried out using only GOSAT data, a combination of GOSAT and surface measurements, and using only surface measurements. As expected, the most robust flux estimates are obtained at large scales (e.g., within 20% of the annual flux at the global scale), and they quickly diverge toward the scale of the subcontinental TRANSCOM regions and beyond (to >100% of the annual flux). We focus our analysis on a shift in the CO2 uptake over land from the Tropics toward the Northern Hemisphere Extra tropics of approximate to 1 PgC/yr when GOSAT data are used in the inversions. This shift is largely driven by TRANSCOM regions Europe and Northern Africa, showing, respectively, an increased uptake and release of 0.7 and 0.9 PgC/yr. Inversions using GOSAT data show a reduced gradient between midlatitudes of the Northern Hemisphere and the Tropics, consistent with the latitudinal shift in carbon uptake. However, the reduced gradients degrade the agreement with background aircraft and surface measurements. To narrow the range of inversion-derived flux, estimates will require further efforts to understand the differences not only between the retrieval schemes but also between inverse models, as their contributions to the overall uncertainty are estimated to be of similar magnitude.
C1 [Houweling, S.; Hasekamp, O.] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Houweling, S.] Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands.
[Baker, D.] Colorado State Univ, CIRA, Boulder, CO USA.
[Basu, S.; Dlugokencky, E. J.; Oda, T.] NOAA ESRL, Boulder, CO USA.
[Boesch, H.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Butz, A.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany.
[Chevallier, F.; Peylin, P.] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Deng, F.; Jones, D.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Feng, L.; Palmer, P. I.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland.
[Ganshin, A.; Zhuravlev, R.] Cent Aerol Observ, Dolgoprudnyi, Russia.
[Maksyutov, S.; Oshchepkov, S.; Takagi, H.; Yoshida, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Marshall, J.; Reum, F.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Oda, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oda, T.] GESTAR, Columbia, MD USA.
[O'Dell, C. W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Poussi, Z.] Climmod, Orsay, France.
RP Houweling, S (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands.
EM s.houweling@sron.nl
RI Maksyutov, Shamil/G-6494-2011; Butz, Andre/A-7024-2013; Boesch,
Hartmut/G-6021-2012; Ganshin, Alexander/C-1626-2014; Vuichard,
Nicolas/A-6629-2011; Chevallier, Frederic/E-9608-2016; Jones,
Dylan/O-2475-2014;
OI Maksyutov, Shamil/0000-0002-1200-9577; Butz, Andre/0000-0003-0593-1608;
Ganshin, Alexander/0000-0002-2835-3145; Chevallier,
Frederic/0000-0002-4327-3813; Jones, Dylan/0000-0002-1935-3725; Deng,
Feng/0000-0002-1381-0243
FU ESA via the GHG-CCI project
FX This study made use of several measurement data sets that were kindly
made available to us and are essential for our research, including:
HIPPO (http://hippo.ucar.edu), CONTRAIL
(http://www.cger.nies.go.jp/contrail/contrail.html), NOAA aircraft
profiles (http://www.esrl.noaa.gov/gmd/ccgg/aircraft/), TCCON
(http://www.tccon.caltech.edu), and various surface measurement networks
(CSIRO, EC, Niwa, JMA, and LSCE) who make their data available through
the World Data Centre for Greenhouse Gases
(http://ds.data.jma.go.jp/gmd/wdcgg/). We would like to thank the GOSAT
project for making the GOSAT-observed spectral radiances freely
available. In addition, we thank the organizers of GOSAT RA to stimulate
international collaboration by organizing meetings, which initiated this
intercomparison initiative. University of Leicester, SRON and KIT
received funding from ESA via the GHG-CCI project.
NR 42
TC 11
Z9 12
U1 3
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 5253
EP 5266
DI 10.1002/2014JD022962
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800044
ER
PT J
AU Fleming, EL
George, C
Heard, DE
Jackman, CH
Kurylo, MJ
Mellouki, W
Orkin, VL
Swartz, WH
Wallington, TJ
Wine, PH
Burkholder, JB
AF Fleming, Eric L.
George, Christian
Heard, Dwayne E.
Jackman, Charles H.
Kurylo, Michael J.
Mellouki, Wahid
Orkin, Vladimir L.
Swartz, William H.
Wallington, Timothy J.
Wine, Paul H.
Burkholder, James B.
TI The impact of current CH4 and N2O atmospheric loss process uncertainties
on calculated ozone abundances and trends
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE stratospheric ozone; chemical uncertainties; laboratory measurements
ID LASER-INDUCED FLUORESCENCE; OH RADICAL REACTIONS; GAS-PHASE REACTIONS;
RATE CONSTANTS; TEMPERATURE-DEPENDENCE; FLASH-PHOTOLYSIS; BRANCHING
RATIOS; ULTRAVIOLET-ABSORPTION; DEPLETING SUBSTANCES; SUBSTITUTED
METHANES
AB The atmospheric loss processes of N2O and CH4, their estimated uncertainties, lifetimes, and impacts on ozone abundance and long-term trends are examined using atmospheric model calculations and updated kinetic and photochemical parameters and uncertainty factors from Stratospheric Processes and their Role in Climate (SPARC) (2013). The uncertainty ranges in calculated N2O and CH4 global lifetimes computed using the SPARC estimated uncertainties are reduced by nearly a factor of 2 compared with uncertainties from Sander et al. (2011). Uncertainties in CH4 loss due to reaction with OH and O(D-1) have relatively small impacts on present-day global total ozone (0.2-0.5%). Uncertainty in the Cl+CH4 reaction affects the amount of chlorine in radical versus reservoir forms and has a modest impact on present-day southern hemisphere (SH) polar ozone (similar to 6%) and on the rate of past ozone decline and future recovery. Uncertainty in the total rate coefficient for the O(D-1)+N2O reaction results in a substantial range in present-day stratospheric odd nitrogen (20-25%) and global total ozone (1.5-2.5%). Uncertainty in the O(D-1)+N2O reaction branching ratio for the O-2+N-2 and 2NO product channels results in moderate impacts on odd nitrogen (+/- 10%) and global ozone (+/- 1%), with uncertainty in N2O photolysis resulting in relatively small impacts (+/- 5% in odd nitrogen, +/- 0.5% in global ozone). Uncertainties in the O(D-1)+N2O reaction and its branching ratio also affect the rate of past global total ozone decline and future recovery, with a range in future ozone projections of +/- 1-1.5% by 2100, relative to present day.
C1 [Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA.
[George, Christian] Univ Lyon 1, CNRS, IRCELYON, CRNS, F-69365 Lyon, France.
[Heard, Dwayne E.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Kurylo, Michael J.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Program, Greenbelt, MD USA.
[Mellouki, Wahid] CNRS, Inst Combust Aerotherm Reactivite & Environm, Orleans 02, France.
[Orkin, Vladimir L.] NIST, Gaithersburg, MD 20899 USA.
[Swartz, William H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Wallington, Timothy J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA.
[Wine, Paul H.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[Wine, Paul H.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA.
RP Fleming, EL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM eric.l.fleming@nasa.gov; James.B.Burkholder@noaa.gov
RI Jackman, Charles/D-4699-2012; Wine, Paul/J-4820-2015; Swartz,
William/A-1965-2010; Mellouki, Abdelwahid/H-5219-2011; Manager, CSD
Publications/B-2789-2015
OI Wine, Paul/0000-0002-5537-4304; Swartz, William/0000-0002-9172-7189;
Mellouki, Abdelwahid/0000-0002-6594-5262;
FU NOAAs Climate Goal and NASAs Atmospheric Composition Program
FX We thank Susan Strahan and Steve Steenrod of the Global Modeling
Initiative project for running the GMI CTM simulations used in this
work. We also thank four anonymous reviewers for their helpful comments
and suggestions. This work was supported in part by NOAAs Climate Goal
and NASAs Atmospheric Composition Program. GSFC 2-D model output used in
this manuscript will be provided to interested individuals upon request
to E. Fleming (eric.l.fleming@nasa.gov).
NR 78
TC 1
Z9 1
U1 1
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2015
VL 120
IS 10
BP 5267
EP 5293
DI 10.1002/2014JD022067
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL1IT
UT WOS:000356696800045
ER
PT J
AU Thebault, E
Finlay, CC
Beggan, CD
Alken, P
Aubert, J
Barrois, O
Bertrand, F
Bondar, T
Boness, A
Brocco, L
Canet, E
Chambodut, A
Chulliat, A
Coisson, P
Civet, F
Du, A
Fournier, A
Fratter, I
Gillet, N
Hamilton, B
Hamoudi, M
Hulot, G
Jager, T
Korte, M
Kuang, W
Lalanne, X
Langlais, B
Leger, JM
Lesur, V
Lowes, FJ
Macmillan, S
Mandea, M
Manoj, C
Maus, S
Olsen, N
Petrov, V
Ridley, V
Rother, M
Sabaka, TJ
Saturnino, D
Schachtschneider, R
Sirol, O
Tangborn, A
Thomson, A
Toffner-Clausen, L
Vigneron, P
Wardinski, I
Zvereva, T
AF Thebault, Erwan
Finlay, Christopher C.
Beggan, Ciaran D.
Alken, Patrick
Aubert, Julien
Barrois, Olivier
Bertrand, Francois
Bondar, Tatiana
Boness, Axel
Brocco, Laura
Canet, Elisabeth
Chambodut, Aude
Chulliat, Arnaud
Coisson, Pierdavide
Civet, Francois
Du, Aimin
Fournier, Alexandre
Fratter, Isabelle
Gillet, Nicolas
Hamilton, Brian
Hamoudi, Mohamed
Hulot, Gauthier
Jager, Thomas
Korte, Monika
Kuang, Weijia
Lalanne, Xavier
Langlais, Benoit
Leger, Jean-Michel
Lesur, Vincent
Lowes, Frank J.
Macmillan, Susan
Mandea, Mioara
Manoj, Chandrasekharan
Maus, Stefan
Olsen, Nils
Petrov, Valeriy
Ridley, Victoria
Rother, Martin
Sabaka, Terence J.
Saturnino, Diana
Schachtschneider, Reyko
Sirol, Olivier
Tangborn, Andrew
Thomson, Alan
Toffner-Clausen, Lars
Vigneron, Pierre
Wardinski, Ingo
Zvereva, Tatiana
TI International Geomagnetic Reference Field: the 12th generation
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE Geomagnetism; Field modeling; IGRF
ID MODELS; IGRF
AB The 12th generation of the International Geomagnetic Reference Field (IGRF) was adopted in December 2014 by the Working Group V-MOD appointed by the International Association of Geomagnetism and Aeronomy (IAGA). It updates the previous IGRF generation with a definitive main field model for epoch 2010.0, a main field model for epoch 2015.0, and a linear annual predictive secular variation model for 2015.0-2020.0. Here, we present the equations defining the IGRF model, provide the spherical harmonic coefficients, and provide maps of the magnetic declination, inclination, and total intensity for epoch 2015.0 and their predicted rates of change for 2015.0-2020.0. We also update the magnetic pole positions and discuss briefly the latest changes and possible future trends of the Earth's magnetic field.
C1 [Thebault, Erwan; Civet, Francois; Langlais, Benoit; Saturnino, Diana] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, F-44322 Nantes, France.
[Finlay, Christopher C.; Olsen, Nils; Toffner-Clausen, Lars] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Beggan, Ciaran D.; Hamilton, Brian; Macmillan, Susan; Ridley, Victoria; Thomson, Alan] British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland.
[Alken, Patrick; Chulliat, Arnaud; Manoj, Chandrasekharan; Maus, Stefan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Alken, Patrick; Chulliat, Arnaud; Manoj, Chandrasekharan] NOAA, NCEI, Boulder, CO 80305 USA.
[Aubert, Julien; Brocco, Laura; Coisson, Pierdavide; Fournier, Alexandre; Hulot, Gauthier; Lalanne, Xavier; Sirol, Olivier; Vigneron, Pierre] Univ Paris Diderot, CNRS, Inst Phys Globe Paris, Sorbonne Paris Cite, F-75005 Paris, France.
[Barrois, Olivier; Gillet, Nicolas] Univ Grenoble Alpes, CNRS, ISTerre, F-38041 Grenoble, France.
[Bertrand, Francois; Boness, Axel; Jager, Thomas; Leger, Jean-Michel] Univ Grenoble Alpes, F-38000 Grenoble, France.
[Bertrand, Francois; Boness, Axel; Jager, Thomas; Leger, Jean-Michel] CEA, LETI, F-38054 Grenoble, France.
[Bondar, Tatiana; Petrov, Valeriy; Zvereva, Tatiana] IZMIRAN, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Moscow, Russia.
[Canet, Elisabeth] ETH, Inst Geophys, Earth & Planetary Magnetism Grp, CH-8093 Zurich, Switzerland.
[Chambodut, Aude] Univ Strasbourg, CNRS, EOST, Inst Phys Globe Strasbourg,UMR 7516, Strasbourg, France.
[Du, Aimin] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earth & Planetary Phys, Beijing 100029, Peoples R China.
[Fratter, Isabelle] Ctr Natl Etudes Spati, F-31400 Toulouse, France.
[Hamoudi, Mohamed; Korte, Monika; Lesur, Vincent; Rother, Martin; Schachtschneider, Reyko; Wardinski, Ingo] GFZ German Res Ctr Geosci Telegrafenberg, D-14473 Potsdam, Germany.
[Sabaka, Terence J.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Lowes, Frank J.] Newcastle Univ, Sch Chem, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Mandea, Mioara] CNES, F-75001 Paris, France.
[Hamoudi, Mohamed] Univ Algiers, USTHB, Dept Geophys, Algiers, Algeria.
[Tangborn, Andrew] UMBC, Joint Ctr Earth Syst Technol, Baltimore, MD USA.
RP Thebault, E (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, 1 Chem Houssiniere, F-44322 Nantes, France.
EM erwan.thebault@univ-nantes.fr
RI MANDEA, Mioara/E-4892-2012; CHAMBODUT, Aude/E-9615-2017; Thebault,
Erwan/A-5670-2011; Aubert, Julien/A-5616-2011; Hulot,
Gauthier/A-5627-2011; Korte, Monika/A-6086-2009; Chulliat,
Arnaud/A-5747-2011; Coisson, Pierdavide/C-5942-2012; Lesur,
Vincent/H-1031-2012; Olsen, Nils/H-1822-2011; Finlay,
Christopher/B-5062-2014; Langlais, Benoit/K-5366-2012; Fournier,
Alexandre/A-5774-2011; Kuang, Weijia/K-5141-2012
OI CHAMBODUT, Aude/0000-0001-8793-1315; Toffner-Clausen,
Lars/0000-0003-4314-3776; Aubert, Julien/0000-0002-2756-0724; Korte,
Monika/0000-0003-2970-9075; Chulliat, Arnaud/0000-0001-7414-9631;
Coisson, Pierdavide/0000-0003-4155-2111; Lesur,
Vincent/0000-0003-2568-320X; Olsen, Nils/0000-0003-1132-6113; Finlay,
Christopher/0000-0002-4592-2290; Langlais, Benoit/0000-0001-5207-304X;
Fournier, Alexandre/0000-0003-3276-0496; Kuang,
Weijia/0000-0001-7786-6425
FU CHAMP mission by the German Aerospace Center (DLR); Federal Ministry of
Education and Research; Danish Government; NASA; ESA; CNES; DARA; Thomas
B. Thriges Foundation; Centre National des Etudes Spatiales (CNES)
within the context of the project of the 'Travaux preparatoires et
exploitation de la mission Swarm'; NSF; French 'Agence Nationale de la
Recherche' [ANR-11-BS56-011]; Region Pays de Loire, France; DFG [SPP
1488]
FX The institutes that support magnetic observatories together with
INTERMAGNET are thanked for promoting high standards of observatory
practice and prompt reporting. The support of the CHAMP mission by the
German Aerospace Center (DLR) and the Federal Ministry of Education and
Research is gratefully acknowledged. The Orsted Project was made
possible by extensive support from the Danish Government, NASA, ESA,
CNES, DARA, and the Thomas B. Thriges Foundation. The authors also
acknowledge ESA for providing access to the Swarm L1b data. E. Canet
acknowledges the support of ESA through the Support to Science Element
(STSE) program. This work was partly funded by the Centre National des
Etudes Spatiales (CNES) within the context of the project of the
'Travaux preparatoires et exploitation de la mission Swarm.' W. Kuang
and A. Tangborn were funded by NASA and the NSF. This work was partly
supported by the French 'Agence Nationale de la Recherche' under the
grant ANR-11-BS56-011 and by the Region Pays de Loire, France. I.
Wardinski was supported by the DFG through SPP 1488. The IGRF-12 task
force finally wishes to express their gratitude to C. Manoj and A. Woods
for maintaining the IGRF web pages at NGDC. This is IPGP contribution
no. 3625.
NR 32
TC 48
Z9 49
U1 8
U2 39
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
EI 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD MAY 27
PY 2015
VL 67
AR 79
DI 10.1186/s40623-015-0228-9
PG 19
WC Geosciences, Multidisciplinary
SC Geology
GA CK2IR
UT WOS:000356034500001
ER
PT J
AU Zhang, RY
Wang, GH
Guo, S
Zarnora, ML
Ying, Q
Lin, Y
Wang, WG
Hu, M
Wang, Y
AF Zhang, Renyi
Wang, Gehui
Guo, Song
Zarnora, Misti L.
Ying, Qi
Lin, Yun
Wang, Weigang
Hu, Min
Wang, Yuan
TI Formation of Urban Fine Particulate Matter
SO CHEMICAL REVIEWS
LA English
DT Review
ID SECONDARY ORGANIC AEROSOL; IONIZATION MASS-SPECTROMETRY; MASTER CHEMICAL
MECHANISM; PROTON-TRANSFER-REACTION; MILAGRO 2006 CAMPAIGN; CATALYZED
HETEROGENEOUS REACTIONS; OH-INITIATED REACTIONS; AIR-POLLUTION SOURCES;
ATMOSPHERIC NANOPARTICLE GROWTH; THERMODYNAMIC-EQUILIBRIUM MODEL
C1 [Zhang, Renyi; Wang, Gehui; Guo, Song; Zarnora, Misti L.; Lin, Yun; Wang, Weigang] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Zhang, Renyi; Wang, Gehui; Guo, Song; Zarnora, Misti L.; Lin, Yun; Wang, Weigang] Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.
[Zhang, Renyi; Guo, Song; Hu, Min] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
[Wang, Gehui] Chinese Acad Sci, Inst Earth Environm, State Key Lab Loess & Quaternary Geol, Key Lab Aerosol Phys & Chem, Beijing 100864, Peoples R China.
[Wang, Weigang] Chinese Acad Sci, Inst Chem, State Key Lab Struct Chem Unstable & Stable Spec, BNLMS, Beijing 100864, Peoples R China.
[Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM Renyi-zhang@tamu.edu
RI Wang, Weigang/L-1786-2013; Guo, Song/D-9218-2012; Zhang,
Renyi/A-2942-2011;
OI Guo, Song/0000-0002-9661-2313; Lin, Yun/0000-0001-8222-0346
FU Robert A. Welch Foundation [A-1417]; Ministry of Science and Technology
of China [2013CB955800]; collaborative research program by Texas AM
University; National Natural Science Foundation of China [41227805,
21190052]; Texas A&M University-Weizmann Collaborative Program;
Strategic Priority Research Program of the Chinese Academy of Sciences
[41325014, XDA05100103, XDB05020401]; Visiting Scholar Program by the
Chinese Academy of Science; National Basic Research Program, China
Ministry of Science and Technology [2013CB228503]; NASA ROSES10-COUND
program
FX This work was supported by the Robert A. Welch Foundation (Grant
A-1417), the Ministry of Science and Technology of China (Grant
2013CB955800), a collaborative research program by Texas A&M University
and the National Natural Science Foundation of China, and a Texas A&M
University-Weizmann Collaborative Program. G.W. acknowledged the
National Natural Science Foundation of China and the Strategic Priority
Research Program of the Chinese Academy of Sciences for financial
support (Grants 41325014, XDA05100103, and XDB05020401). W.W.
acknowledged financial support for the Visiting Scholar Program by the
Chinese Academy of Science and the National Natural Science Foundation
of China (Grant 41227805). M.H. was supported by the National Basic
Research Program, China Ministry of Science and Technology (Grant
2013CB228503), and National Natural Science Foundation of China
(21190052). Y.W. was supported by the NASA ROSES10-COUND program. We
were grateful to Professor A. R. Ravishankara of Colorado State
University, Professor of Robert D. Kuchta of University of Colorado at
Boulder, and Dr. Sasha Madronich of NCAR for helpful suggestions and
discussions.
NR 485
TC 76
Z9 79
U1 72
U2 289
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0009-2665
EI 1520-6890
J9 CHEM REV
JI Chem. Rev.
PD MAY 27
PY 2015
VL 115
IS 10
BP 3803
EP 3855
DI 10.1021/acs.chemrev.5b00067
PG 53
WC Chemistry, Multidisciplinary
SC Chemistry
GA CJ3KZ
UT WOS:000355383900005
PM 25942499
ER
PT J
AU Fujishima, K
Venter, C
Wang, K
Ferreira, R
Rothschild, LJ
AF Fujishima, Kosuke
Venter, Chris
Wang, Kendrick
Ferreira, Raphael
Rothschild, Lynn J.
TI An overhang-based DNA block shuffling method for creating a customized
random library
SO SCIENTIFIC REPORTS
LA English
DT Article
ID IN-VITRO SELECTION; PROTEINS; EVOLUTION; DISPLAY; REPEATS; DESIGN;
GALAXY
AB We present an overhang-based DNA block shuffling method to create a customized random DNA library with flexible sequence design and length. Our method enables the efficient and seamless assembly of short DNA blocks with dinucleotide overhangs through a simple ligation process. Next generation sequencing analysis of the assembled DNA library revealed that ligation was accurate, directional and unbiased. This straightforward DNA assembly method should fulfill the versatile needs of both in vivo and in vitro functional screening of random peptides and RNA created with a desired amino acid and nucleotide composition, as well as making highly repetitive gene constructs that are difficult to synthesize de novo.
C1 [Fujishima, Kosuke] Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Venter, Chris; Wang, Kendrick] NASA, Ames Res Ctr, NASA Educ Associates Program EAP, Moffett Field, CA 94035 USA.
[Wang, Kendrick] Stanford Univ, Dept Bioengn, Stanford, CA 94305 USA.
[Ferreira, Raphael] Univ Paris 07, Diderot, France.
[Rothschild, Lynn J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fujishima, K (reprint author), Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM kosuke.fujishima@nasa.gov; lynn.j.rothschild@nasa.gov
OI Fujishima, Kosuke/0000-0002-8844-812X
FU NASA Ames Directors Discretionary Fund; NASA Ames Science Innovation
Fund
FX We thank Russell Durrett for helping the DNA sequence analysis and Ryan
Kent for reviewing the final manuscript. We are grateful to the NASA
Ames Directors Discretionary Fund and the NASA Ames Science Innovation
Fund for support.
NR 17
TC 0
Z9 0
U1 1
U2 12
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 MAY 26
PY 2015
VL 5
AR 9740
DI 10.1038/srep09740
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CJ5KT
UT WOS:000355527000001
PM 26010273
ER
PT J
AU Bahr, CJ
Zawodny, NS
Bertolucci, B
Li, J
Sheplak, M
Cattafesta, LN
AF Bahr, Christopher J.
Zawodny, Nikolas S.
Bertolucci, Brandon
Li, Jian
Sheplak, Mark
Cattafesta, Louis N.
TI A plasma-based non-intrusive point source for acoustic beamforming
applications
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID SHEAR-LAYER; SPACE; SOUND
AB A laser-generated plasma acoustic point source is used to directly measure the point spread function (PSF) of a microphone phased array. In beamforming analysis of microphone phased array data, the true acoustic field is convolved with the array's PSF. By directly measuring the PSF, corrections to the array analysis can be computed and applied. The acoustic source is measured in an open-jet aeroacoustic facility to evaluate the effects of sampling rate, microphone installation, source shift, reflections, shear layer refraction and model presence. Results show that measurements exhibit behavior consistent with theory with regard to source shift and shear layer refraction. Application of a measured PSF in beamforming analysis shows that the process provides an effective in situ method for array calibration both with and without flow and allows for corrections to incorporate reflections and scattering. The technique improves the agreement of beamforming results with the true spectrum of a known source, especially in the presence of reflections. Published by Elsevier Ltd.
C1 [Bahr, Christopher J.; Zawodny, Nikolas S.] NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA.
[Bertolucci, Brandon] Boeing Aircraft Co, Boeing ANP Labs, Seattle, WA USA.
[Li, Jian] Univ Florida, Dept Elect & Comp Engn, Gainesville, FL USA.
[Sheplak, Mark] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL USA.
[Cattafesta, Louis N.] Florida State Univ, Dept Mech Engn, Tallahassee, FL 32306 USA.
RP Bahr, CJ (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA.
EM christophor.j.bahr@nasa.gov
OI Bahr, Christopher/0000-0002-3095-4265
FU Florida Center for Advanced Aero-Propulsion
FX The authors acknowledge the financial support provided by the Florida
Center for Advanced Aero-Propulsion. They thank Dr. Fei Liu, Kyle
Woolwine, and Derek Dussault for their efforts in this research, along
with James Underbrink for extensive discussion of array measurement
techniques and his input on this body of work.
NR 33
TC 4
Z9 4
U1 1
U2 11
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD MAY 26
PY 2015
VL 344
BP 59
EP 80
DI 10.1016/j.jsv.2015.01.023
PG 22
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA CD3RJ
UT WOS:000350997600005
ER
PT J
AU Johnson, CL
Phillips, RJ
Purucker, ME
Anderson, BJ
Byrne, PK
Denevi, BW
Feinberg, JM
Hauck, SA
Head, JW
Korth, H
James, PB
Mazarico, E
Neumann, GA
Philpott, LC
Siegler, MA
Tsyganenko, NA
Solomon, SC
AF Johnson, Catherine L.
Phillips, Roger J.
Purucker, Michael E.
Anderson, Brian J.
Byrne, Paul K.
Denevi, Brett W.
Feinberg, Joshua M.
Hauck, Steven A., II
Head, James W., III
Korth, Haje
James, Peter B.
Mazarico, Erwan
Neumann, Gregory A.
Philpott, Lydia C.
Siegler, Matthew A.
Tsyganenko, Nikolai A.
Solomon, Sean C.
TI Low-altitude magnetic field measurements by MESSENGER reveal Mercury's
ancient crustal field
SO SCIENCE
LA English
DT Article
ID THERMOCHEMICAL EVOLUTION; GLOBAL CONTRACTION; ORIGIN; SURFACE; PLAINS;
ORBIT
AB Magnetized rocks can record the history of the magnetic field of a planet, a key constraint for understanding its evolution. From orbital vector magnetic field measurements of Mercury taken by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft at altitudes below 150 kilometers, we have detected remanent magnetization in Mercury's crust. We infer a lower bound on the average age of magnetization of 3.7 to 3.9 billion years. Our findings indicate that a global magnetic field driven by dynamo processes in the fluid outer core operated early in Mercury's history. Ancient field strengths that range from those similar to Mercury's present dipole field to Earth-like values are consistent with the magnetic field observations and with the low iron content of Mercury's crust inferred from MESSENGER elemental composition data.
C1 [Johnson, Catherine L.; Philpott, Lydia C.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada.
[Johnson, Catherine L.; Siegler, Matthew A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
[Purucker, Michael E.; Mazarico, Erwan; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Denevi, Brett W.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Byrne, Paul K.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Feinberg, Joshua M.] Univ Minnesota, Inst Rock Magnetism, Dept Earth Sci, Minneapolis, MN 55455 USA.
[Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA.
[Head, James W., III] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[James, Peter B.; Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Siegler, Matthew A.] So Methodist Univ, Dept Earth Sci, Dallas, TX 75205 USA.
[Tsyganenko, Nikolai A.] St Petersburg State Univ, Inst & Fac Phys, St Petersburg 199034, Russia.
[Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Johnson, CL (reprint author), Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada.
EM cjohnson@eos.ubc.ca
RI Denevi, Brett/I-6502-2012; Mazarico, Erwan/N-6034-2014; Neumann,
Gregory/I-5591-2013; Hauck, Steven/A-7865-2008; Tsyganenko,
Nikolai/J-7377-2012;
OI Denevi, Brett/0000-0001-7837-6663; Mazarico, Erwan/0000-0003-3456-427X;
Neumann, Gregory/0000-0003-0644-9944; Hauck, Steven/0000-0001-8245-146X;
Tsyganenko, Nikolai/0000-0002-5938-1579; Philpott,
Lydia/0000-0002-5286-8528
FU NASA Discovery Program; MESSENGER Participating Scientist Program;
Natural Sciences and Engineering Research Council of Canada
FX We thank the MESSENGER operations and engineering teams for enabling the
low-altitude observations reported here. We are also grateful for the
contributions of our friend and colleague M. H. Acuna whose expertise
was critical to the Magnetometer development. The MESSENGER mission is
supported by the NASA Discovery Program and the MESSENGER Participating
Scientist Program. C.L.J. and L.C.P. also acknowledge support from the
Natural Sciences and Engineering Research Council of Canada. Data from
the MESSENGER mission are archived with the NASA Planetary Data System.
We thank three reviewers for thoughtful comments that improved the
manuscript.
NR 29
TC 15
Z9 15
U1 4
U2 20
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAY 22
PY 2015
VL 348
IS 6237
BP 892
EP 895
DI 10.1126/science.aaa8720
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CI6NW
UT WOS:000354877900039
PM 25953822
ER
PT J
AU Kuin, NPM
Landsman, W
Breeveld, AA
Page, MJ
Lamoureux, H
James, C
Mehdipour, M
Still, M
Yershov, V
Brown, PJ
Carter, M
Mason, KO
Kennedy, T
Marshall, F
Roming, PWA
Siegel, M
Oates, S
Smith, PJ
De Pasquale, M
AF Kuin, N. P. M.
Landsman, W.
Breeveld, A. A.
Page, M. J.
Lamoureux, H.
James, C.
Mehdipour, M.
Still, M.
Yershov, V.
Brown, P. J.
Carter, M.
Mason, K. O.
Kennedy, T.
Marshall, F.
Roming, P. W. A.
Siegel, M.
Oates, S.
Smith, P. J.
De Pasquale, M.
TI Calibration of the Swift-UVOT ultraviolet and visible grisms
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: spectrographs; space vehicles: instruments; techniques:
imaging spectroscopy
ID WOLF-RAYET STARS; DYNAMIC-RANGE; TELESCOPE; SPECTROPHOTOMETRY;
SPECTROSCOPY; PERFORMANCE; MISSION; CATALOG; ATLAS
AB We present the calibration of the Swift Ultraviolet and Optical Telescope (UVOT) grisms, of which there are two, providing low-resolution field spectroscopy in the ultraviolet and optical bands, respectively. The UV grism covers the range lambda 1700-5000 angstrom with a spectral resolution (lambda/Delta lambda) of 75 at lambda 2600 angstrom for source magnitudes of u= 10-16 mag, while the visible grism covers the range lambda 2850-6600 angstrom with a spectral resolution of 100 at lambda 4000 angstrom for source magnitudes of b=12-17 mag. This calibration extends over all detector positions, for all modes used during operations. The wavelength accuracy (1 sigma) is 9 angstrom in the UV grism clocked mode, 17 angstrom in the UV grism nominal mode and 22 angstrom in the visible grism. The range below lambda 2740 angstrom in the UV grism and lambda 5200 angstrom in the visible grism never suffers from overlapping by higher spectral orders. The flux calibration of the grisms includes a correction we developed for coincidence loss in the detector. The error in the coincidence loss correction is less than 20 per cent. The position of the spectrum on the detector only affects the effective area (sensitivity) by a fewper cent in the nominal modes, but varies substantially in the clocked modes. The error in the effective area is from 9 per cent in the UV grism clocked mode to 15 per cent in the visible grism clocked mode
C1 [Kuin, N. P. M.; Breeveld, A. A.; Page, M. J.; Lamoureux, H.; James, C.; Mehdipour, M.; Yershov, V.; Carter, M.; Kennedy, T.; Oates, S.; De Pasquale, M.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England.
[Landsman, W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Still, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, P. J.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Mason, K. O.] Harwell Oxford, Satellite Applicat Catapult, Harwell OX11 0QR, Berks, England.
[Marshall, F.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Roming, P. W. A.; Siegel, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Roming, P. W. A.] Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA.
[Roming, P. W. A.] Univ Texas San Antonio, Phys & Astron Dept, San Antonio, TX 78249 USA.
[Oates, S.] Inst Astrofs Andalucia IAA CSIC, E-18008 Granada, Spain.
[De Pasquale, M.] IASF Palermo, I-90146 Palermo, Italy.
RP Kuin, NPM (reprint author), Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England.
EM npkuin@gmail.com
FU UK Space Agency; PSU by NASA [NAS5-00136]
FX Throughout the calibration many people provided feedback and helped
refine the understanding of what was possible and what could be improved
through their use of the grisms for observational studies. We wish to
thank all of them for their efforts, help and patience. A special thanks
goes to all the Swift planners who through their effort ensured the
success of this calibration. The optical design of the grisms was by the
late Richard Bingham. We are grateful to Fred Walter, Ed Sion, and Greg
Schwartz for sharing their HST and optical spectra, some of which were
taken during several Swift-HST observing campaigns, which helped the
calibration effort. This work was supported by the UK Space Agency
through a grant for Swift Post Launch Support at UCL-MSSL. This work is
sponsored at PSU by NASA contract NAS5-00136. We acknowledge the use of
data from the SIMBAD and Vizier data bases at the CDS in Strassbourg,
the online WR spectra from Hamann, the STScI MAST and HLA archive, the
ESA INES IUE archive, the HEASARC archives, and the NIST atomic data
base on the WWW. We used 'Astropy', a community-developed core PYTHON
package for Astronomy (Astropy Collaboration, 2013).
NR 32
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 MAY 21
PY 2015
VL 449
IS 3
BP 2514
EP 2538
DI 10.1093/mnras/stv408
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TP
UT WOS:000355337800025
ER
PT J
AU Gullberg, B
De Breuck, C
Vieira, JD
Weiss, A
Aguirre, JE
Aravena, M
Bethermin, M
Bradford, CM
Bothwell, MS
Carlstrom, JE
Chapman, SC
Fassnacht, CD
Gonzalez, AH
Greve, TR
Hezaveh, Y
Holzapfel, WL
Husband, K
Ma, J
Malkan, M
Marrone, DP
Menten, K
Murphy, EJ
Reichardt, CL
Spilker, JS
Stark, AA
Strandet, M
Welikala, N
AF Gullberg, B.
De Breuck, C.
Vieira, J. D.
Weiss, A.
Aguirre, J. E.
Aravena, M.
Bethermin, M.
Bradford, C. M.
Bothwell, M. S.
Carlstrom, J. E.
Chapman, S. C.
Fassnacht, C. D.
Gonzalez, A. H.
Greve, T. R.
Hezaveh, Y.
Holzapfel, W. L.
Husband, K.
Ma, J.
Malkan, M.
Marrone, D. P.
Menten, K.
Murphy, E. J.
Reichardt, C. L.
Spilker, J. S.
Stark, A. A.
Strandet, M.
Welikala, N.
TI The nature of the [C II] emission in dusty star-forming galaxies from
the SPT survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared:
galaxies; submillimetre: galaxies
ID 158 MU-M; ULTRALUMINOUS INFRARED GALAXIES; SOUTH-POLE TELESCOPE;
LUMINOUS SUBMILLIMETER GALAXIES; SPACE-OBSERVATORY MEASUREMENTS; ACTIVE
GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; MICRON LINE DEFICIT; HUBBLE
DEEP FIELD; SIMILAR-TO 1-2
AB We present [C II] observations of 20 strongly lensed dusty star-forming galaxies at 2.1 < z < 5.7 using Atacama Pathfinder EXperiment and Herschel. The sources were selected on their 1.4 mm flux (S-1.4mm > 20 mJy) from the South Pole Telescope (SPT) survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. 11 out of 20 sources observed in [C II] also have low-J CO detections from Australia Telescope Compact Array. A comparison with mid-and high-J CO lines from Atacama Large Millimeter/submillimeter Array reveals consistent [C II] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [C II], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [C II] to CO(1-0) luminosity ratios in the SPT sample of 5200 +/- 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [C II] and CO emitting gas with a higher [C II] than CO excitation temperature, high CO optical depth tau(CO)(1-0) >> 1, and low to moderate [CII] optical depth tau[C II] less than or similar to 1. The geometric structure of photodissociation regions allows for such conditions.
C1 [Gullberg, B.; De Breuck, C.; Bethermin, M.] European So Observ, D-85748 Garching, Germany.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Weiss, A.; Menten, K.; Strandet, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA.
[Aravena, M.] European So Observ, Santiago 19, Chile.
[Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
[Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England.
[Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Chapman, S. C.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Hezaveh, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Murphy, E. J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Welikala, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
RP Gullberg, B (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM bgullber@eso.org
RI Holzapfel, William/I-4836-2015;
OI Marrone, Daniel/0000-0002-2367-1080; De Breuck,
Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996
FU National Aeronautics and Space Administration; Commonwealth of
Australia; US National Science Foundation [AST-1312950]; National
Science Foundation [PLR-1248097]; NSF Physics Frontier Center
[PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF
947]
FX This publication is based on data acquired with the APEX. APEX is a
collaboration between the Max-Planck-Institut fur Radioastronomie, the
European Southern Observatory, and the Onsala Space Observatory. This
paper makes use of the following ALMA data: ADS/JAO.
ALMA#2011.0.00957.S, ADS/JAO.ALMA#2011.0.00958.S and ADS/JAO.
ALMA#2012.1.00844.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 Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The ATCA
is part of the Australia Telescope National Facility which is funded by
the Commonwealth of Australia for operation as a National Facility
managed by CSIRO. This research has made use of the NED which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. This research has made use of NASA's Astrophysics Data
System Bibliographic Services; This material is based on work supported
by the US National Science Foundation under grant no. AST-1312950. The
SPT is supported by the National Science Foundation through grant
PLR-1248097. Partial support is also provided by the NSF Physics
Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological
Physics at the University of Chicago, the Kavli Foundation, and the
Gordon and Betty Moore Foundation grant GBMF 947.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2015
VL 449
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DI 10.1093/mnras/stv372
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TP
UT WOS:000355337800055
ER
PT J
AU Littlejohns, OM
Butler, NR
Cucchiara, A
Watson, AM
Fox, OD
Lee, WH
Kutyrev, AS
Richer, MG
Klein, CR
Prochaska, JX
Bloom, JS
Troja, E
Ramirez-Ruiz, E
de Diego, JA
Georgiev, L
Gonzalez, J
Roman-Zuniga, CG
Gehrels, N
Moseley, H
AF Littlejohns, O. M.
Butler, N. R.
Cucchiara, A.
Watson, A. M.
Fox, O. D.
Lee, W. H.
Kutyrev, A. S.
Richer, M. G.
Klein, C. R.
Prochaska, J. X.
Bloom, J. S.
Troja, E.
Ramirez-Ruiz, E.
de Diego, J. A.
Georgiev, L.
Gonzalez, J.
Roman-Zuniga, C. G.
Gehrels, N.
Moseley, H.
TI A detailed study of the optical attenuation of gamma-ray bursts in the
Swift era
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray bursts: general; galaxies: distances and redshifts; galaxies:
ISM
ID DIGITAL SKY SURVEY; WIDE-FIELD CAMERA; X-RAY; COLUMN DENSITIES; COMPLETE
SAMPLE; LIGHT CURVES; PHOTOMETRIC REDSHIFT; INTERSTELLAR-MEDIUM;
AFTERGLOW EMISSION; GLOBULAR-CLUSTERS
AB We present optical and near-infrared (NIR) photometry of 28 gamma-ray bursts (GRBs) detected by the Swift satellite and rapidly observed by the Reionization and Transients Infrared/Optical (RATIR) camera. We compare the optical flux at fiducial times of 5.5 and 11 h after the high-energy trigger to that in the X-ray regime to quantify optical darkness. 46 +/- 9 per cent (13/28) of all bursts in our sample and 55 +/- 10 per cent (13/26) of long GRBs are optically dark, which is statistically consistently with previous studies. Fitting RATIR optical and NIR spectral energy distributions of 19 GRBs, most (6/7) optically dark GRBs either occur at high redshift (z > 4.5) or have a high dust content in their host galaxies (A(V) > 0.3). Performing Kolmogorov-Smirnov tests, we compare the RATIR sample to those previously presented in the literature, finding our distributions of redshift, optical darkness, host dust extinction and X-ray-derived column density to be consistent. The one reported discrepancy is with host galaxy dust content in the BAT6 sample, which appears inconsistent with our sample and other previous literature. Comparing X-ray-derived host galaxy hydrogen column densities to host galaxy dust extinction, we find that GRBs tend to occur in host galaxies with a higher metal-to-dust ratio than our own Galaxy, more akin to the Large and Small Magellanic Clouds. Finally, to mitigate time evolution of optical darkness, we measure beta(OX, rest) at a fixed rest-frame time, t(rest) = 1.5 h and fixed rest-frame energies in the X-ray and optical regimes. Choosing to evaluate optical flux at lambda(rest) = 0.25 mu m, we remove high redshift as a source of optical darkness, demonstrating that optical darkness must result from either high redshift, dust content in the host galaxy along the GRB sight line, or a combination of the two.
C1 [Littlejohns, O. M.; Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Cucchiara, A.; Kutyrev, A. S.; Troja, E.; Gehrels, N.; Moseley, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Watson, A. M.; Lee, W. H.; de Diego, J. A.; Georgiev, L.; Gonzalez, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Fox, O. D.; Klein, C. R.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Richer, M. G.; Roman-Zuniga, C. G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Prochaska, J. X.; Ramirez-Ruiz, E.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Littlejohns, OM (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM owenlittlejohns@gmail.com; natbutler@asu.edu
RI Roman-Zuniga, Carlos/F-6602-2016; Gonzalez, Jose/L-6687-2014
OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Gonzalez,
Jose/0000-0002-3724-1583
FU NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT
[INFR-2009-01-122785, CB-2008-101958]; UNAM PAPIIT [IN113810]; UC
MEXUS-CONACyT [CN 09-283]; NASA Postdoctoral Programme at the Goddard
Space Flight Center; NASA
FX We thank Pall Jakobsson for useful comments and suggestions on the
manuscript. We also thank Jochen Greiner for supplying us with detailed
data related to Greiner et al. (2011). We thank the RATIR project team
and the staff of the Observatorio Astronomico Nacional on Sierra San
Pedro Martir. RATIR is a collaboration between the University of
California, the Universidad Nacional Autonoma de Mexico, NASA Goddard
Space Flight Center and Arizona State University, benefiting from the
loan of an H2RG detector and hardware and software support from Teledyne
Scientific and Imaging. RATIR, the automation of the Harold L. Johnson
Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro
Martir, and the operation of both are funded through NASA grants
NNX09AH71G, NNX09AT02G, NNX10AI27G and NNX12AE66G, CONACyT grants
INFR-2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IN113810 and
UC MEXUS-CONACyT grant CN 09-283. AC is supported by the NASA
Postdoctoral Programme at the Goddard Space Flight Center, administered
by Oak Ridge Associated Universities through a contract with NASA. This
work made use of data supplied by the UKSSDC at the University of
Leicester.
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JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2015
VL 449
IS 3
BP 2919
EP 2936
DI 10.1093/mnras/stv479
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TP
UT WOS:000355337800058
ER
PT J
AU Littlefield, C
Mukai, K
Mumme, R
Cain, R
Magno, KC
Corpuz, T
Sandefur, D
Boyd, D
Cook, M
Ulowetz, J
Martinez, L
AF Littlefield, Colin
Mukai, Koji
Mumme, Raymond
Cain, Ryan
Magno, Katrina C.
Corpuz, Taylor
Sandefur, Davis
Boyd, David
Cook, Michael
Ulowetz, Joseph
Martinez, Luis
TI Periodic eclipse variations in asynchronous polar V1432 Aql: evidence of
a shifting threading region
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: V1432 Aql; stars:
individual: RX J1940.1-1025; stars: magnetic field; novae, cataclysmic
variables; white dwarfs
ID NEAR-SYNCHRONOUS POLAR; ACCRETION GEOMETRY; RX J1940.1-1025; HU AQUARII;
OLD NOVA; SYNCHRONIZATION; AM; AQUILAE; DWARF; CYGNI
AB We report the results of a 28-month photometric campaign studying V1432 Aql, the only known eclipsing, asynchronous polar. Our data show that both the residual eclipse flux and eclipse O-C timings vary strongly as a function of the spin-orbit beat period. Relying upon a new model of the system, we show that cyclical changes in the location of the threading region along the ballistic trajectory of the accretion stream could produce both effects. This model predicts that the threading radius is variable, in contrast to previous studies which have assumed a constant threading radius. Additionally, we identify a very strong photometric maximum which is only visible for half of the beat cycle. The exact cause of this maximum is unclear, but we consider the possibility that it is the optical counterpart of the third accreting polecap proposed by Rana et al. Finally, the rate of change of the white dwarf's spin period is consistent with it being proportional to the difference between the spin and orbital periods, implying that the spin period is approaching the orbital period asymptotically.
C1 [Littlefield, Colin; Mumme, Raymond; Cain, Ryan; Magno, Katrina C.; Corpuz, Taylor; Sandefur, Davis] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Littlefield, Colin] Wesleyan Univ, Dept Astron, Middletown, CT 06459 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.
[Mukai, Koji] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Boyd, David] CBA Oxford, W Challow OX12 9TX, Wantage, England.
[Cook, Michael] Newcastle Observ, CBA Ontario, Newcastle, ON L1B 1M5, Canada.
[Ulowetz, Joseph] CBA Illinois, Northbrook, IL 60062 USA.
[Martinez, Luis] Lenomiya Observ, Casa Grande, AZ 85122 USA.
RP Littlefield, C (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
EM clittlef@alumni.nd.edu; koji.mukai@nasa.gov
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JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
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DI 10.1093/mnras/stv462
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TP
UT WOS:000355337800070
ER
PT J
AU Kennedy, GM
Matra, L
Marmier, M
Greaves, JS
Wyatt, MC
Bryden, G
Holland, W
Lovis, C
Matthews, BC
Pepe, F
Sibthorpe, B
Udry, S
AF Kennedy, Grant M.
Matra, Luca
Marmier, Maxime
Greaves, Jane S.
Wyatt, Mark C.
Bryden, Geoffrey
Holland, Wayne
Lovis, Christophe
Matthews, Brenda C.
Pepe, Francesco
Sibthorpe, Bruce
Udry, Stephane
TI Kuiper belt structure around nearby super-Earth host stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE planet-disc interactions; circumstellar matter; stars: individual: 61
Vir; stars: individual: HD 20794; stars: individual: HD 38858; stars:
individual: HD 69830
ID INFRARED INTERFEROMETRIC SURVEY; GENEVA-COPENHAGEN SURVEY; STEADY-STATE
EVOLUTION; NEPTUNE-MASS PLANETS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS;
SUN-LIKE STARS; DEBRIS DISKS; CIRCUMSTELLAR DISK; BETA-PICTORIS
AB We present new observations of the Kuiper belt analogues around HD 38858 and HD 20794, hosts of super-Earth mass planets within 1 au. As two of the four nearby G-type stars (with HD 69830 and 61 Vir) that form the basis of a possible correlation between low-mass planets and debris disc brightness, these systems are of particular interest. The disc around HD 38858 is well resolved with Herschel and we constrain the disc geometry and radial structure. We also present a probable James Clerk Maxwell Telescope sub-mm continuum detection of the disc and a CO J = 2-1 upper limit. The disc around HD 20794 is much fainter and appears marginally resolved with Herschel, and is constrained to be less extended than the discs around 61 Vir and HD 38858. We also set limits on the radial location of hot dust recently detected around HD 20794 with near-IR interferometry. We present High Accuracy Radial velocity Planet Searcher upper limits on unseen planets in these four systems, ruling out additional super-Earths within a few au, and Saturn-mass planets within 10 au. We consider the disc structure in the three systems with Kuiper belt analogues (HD 69830 has only a warm dust detection), concluding that 61 Vir and HD 38858 have greater radial disc extent than HD 20794. We speculate that the greater width is related to the greater minimum planet masses (10-20 M-circle plus versus 3-5 M-circle plus), arising from an eccentric planetesimal population analogous to the Solar system's scattered disc. We discuss alternative scenarios and possible means to distinguish among them.
C1 [Kennedy, Grant M.; Matra, Luca; Wyatt, Mark C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Matra, Luca] ESO Vitacura, Santiago 19001, Chile.
[Marmier, Maxime; Lovis, Christophe; Pepe, Francesco; Udry, Stephane] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland.
[Greaves, Jane S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Holland, Wayne] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Holland, Wayne] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Matthews, Brenda C.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada.
[Matthews, Brenda C.] Univ Victoria, Victoria, BC V8W 3P6, Canada.
[Sibthorpe, Bruce] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
RP Kennedy, GM (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM gkennedy@ast.cam.ac.uk
OI Kennedy, Grant/0000-0001-6831-7547
FU European Union through ERC [279973]; STFC; ESO; Swiss National Science
Foundation (SNSF)
FX We thank the referee for a thoughtful review. This work was supported by
the European Union through ERC grant number 279973 (GMK, LM, and MCW).
LM also acknowledges support by both STFC and ESO through graduate
studentships. MM, CL, FP, and SU acknowledge the Swiss National Science
Foundation (SNSF) for the continuous support of the RV research
programmes.
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JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2015
VL 449
IS 3
BP 3121
EP 3136
DI 10.1093/mnras/stv511
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TP
UT WOS:000355337800071
ER
PT J
AU Cao, Y
Kulkarni, SR
Howell, DA
Gal-Yam, A
Kasliwal, MM
Valenti, S
Johansson, J
Amanullah, R
Goobar, A
Sollerman, J
Taddia, F
Horesh, A
Sagiv, I
Cenko, SB
Nugent, PE
Arcavi, I
Surace, J
Wozniak, PR
Moody, DI
Rebbapragada, UD
Bue, BD
Gehrels, N
AF Cao, Yi
Kulkarni, S. R.
Howell, D. Andrew
Gal-Yam, Avishay
Kasliwal, Mansi M.
Valenti, Stefano
Johansson, J.
Amanullah, R.
Goobar, A.
Sollerman, J.
Taddia, F.
Horesh, Assaf
Sagiv, Ilan
Cenko, S. Bradley
Nugent, Peter E.
Arcavi, Iair
Surace, Jason
Wozniak, P. R.
Moody, Daniela I.
Rebbapragada, Umaa D.
Bue, Brian D.
Gehrels, Neil
TI A strong ultraviolet pulse from a newborn type Ia supernova
SO NATURE
LA English
DT Article
ID TIME OPTICAL-SPECTRA; SN 2011FE; COMPANION STAR; LOW-RESOLUTION; DATA
RELEASE; SWIFT; PROGENITOR; TELESCOPE; SPECTROGRAPH; CONSTRAINTS
AB Type Ia supernovae(1) are destructive explosions of carbon-oxygen white dwarfs(2,3). Although they are used empirically to measure cosmological distances(4-6), the nature of their progenitors remains mysterious(3). One of the leading progenitor models, called the single degenerate channel, hypothesizes that a white dwarf accretes matter from a companion star and the resulting increase in its central pressure and temperature ignites thermonuclear explosion(3,7,8). Here we report observations with the Swift Space Telescope of strong but declining ultraviolet emission from a type Ia supernova within four days of its explosion. This emission is consistent with theoretical expectations of collision between material ejected by the supernova and a companion star(9), and therefore provides evidence that some type Ia supernovae arise from the single degenerate channel.
C1 [Cao, Yi; Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Kulkarni, S. R.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Howell, D. Andrew; Valenti, Stefano; Arcavi, Iair] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Howell, D. Andrew; Valenti, Stefano] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Gal-Yam, Avishay; Horesh, Assaf; Sagiv, Ilan] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Johansson, J.; Amanullah, R.; Goobar, A.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Sollerman, J.; Taddia, F.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Cenko, S. Bradley; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Wozniak, P. R.; Moody, Daniela I.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Rebbapragada, Umaa D.; Bue, Brian D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cao, Y (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA.
EM ycao@astro.caltech.edu
RI Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Sollerman,
Jesper/0000-0003-1546-6615; Wozniak, Przemyslaw/0000-0002-9919-3310
FU W. M. Keck Foundation; National Science Foundation; EU/FP7 via an ERC
grant; "Quantum Universe" I-Core programme; ISF; Minerva and Weizmann-UK
grants; Kimmel Award; Carnegie-Princeton fellowship; Swedish Research
Council; Knut and Alice Wallenberg Foundation; Office of Science of the
US Department of Energy [DE-AC02-05CH11231]; US Department of Energy as
part of the Laboratory Directed Research and Development programme;
National Aeronautics and Space Administration
FX We thank A. L. Piro, M. Kromer and J. Cohen for discussions. We also
thank A. Waszczak, A. Rubin, O. Yaron, A. De Cia, D. A. Perley, G. E.
Duggan, O. Smirnova, S. Papadogiannakis, A. Nyholm, Y. F. Martinez and
the staff at the Nordic Optical Telescope and Gemini for observation and
data reduction. Some of the data presented here were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California and
NASA. The observatory was made possible by the generous financial
support of the W. M. Keck Foundation. Some data were obtained with the
Nordic Optical Telescope, which is operated by the Nordic Optical
Telescope Scientific Association at the Observatorio del Roque de los
Muchachos, La Palma, Spain. This work also makes use of observations
from the Las Cumbres Observatory Global Telescope (LCOGT) network.
Research at California Institute of Technology is supported by the
National Science Foundation. D.A.H. acknowledges support from the
National Science Foundation. A.G.-Y. acknowledges support from the
EU/FP7 via an ERC grant, the "Quantum Universe" I-Core programme, the
ISF, Minerva and Weizmann-UK grants, and the Kimmel Award. M.M.K.
acknowledges generous support from the Carnegie-Princeton fellowship.
Supernova research at the Oskar Klein Centre is supported by the Swedish
Research Council and by the Knut and Alice Wallenberg Foundation. The
National Energy Research Scientific Computing Center, which is supported
by the Office of Science of the US Department of Energy under contract
number DE-AC02-05CH11231, provided staff, computational resources, and
data storage for this project. The participation of the Los Alamos
National Laboratory (LANL) in iPTF is supported by the US Department of
Energy as part of the Laboratory Directed Research and Development
programme. A portion of this work was carried out at the Jet Propulsion
Laboratory under a Research and Technology Development Grant, under
contract with the National Aeronautics and Space Administration.
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PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 21
PY 2015
VL 521
IS 7552
BP 328
EP +
DI 10.1038/nature14440
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CI5RM
UT WOS:000354816500050
PM 25993962
ER
PT J
AU Brightman, M
Balokovic, M
Stern, D
Arevalo, P
Ballantyne, DR
Bauer, FE
Boggs, SE
Craig, WW
Christensen, FE
Comastri, A
Fuerst, F
Gandhi, P
Hailey, CJ
Harrison, FA
Hickox, RC
Koss, M
LaMassa, S
Puccetti, S
Rivers, E
Vasudevan, R
Walton, DJ
Zhang, WW
AF Brightman, M.
Balokovic, M.
Stern, D.
Arevalo, P.
Ballantyne, D. R.
Bauer, F. E.
Boggs, S. E.
Craig, W. W.
Christensen, F. E.
Comastri, A.
Fuerst, F.
Gandhi, P.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
Koss, M.
LaMassa, S.
Puccetti, S.
Rivers, E.
Vasudevan, R.
Walton, D. J.
Zhang, W. W.
TI DETERMINING THE COVERING FACTOR OF COMPTON-THICK ACTIVE GALACTIC NUCLEI
WITH NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 424, NGC 1068, NGC 4945,
Circinus); X-rays: galaxies
ID X-RAY-SPECTRA; SEYFERT 2 GALAXIES; H2O MASER EMISSION; SWIFT-BAT SURVEY;
XMM-NEWTON; NGC 4945; CIRCINUS GALAXY; LUMINOSITY DEPENDENCE; OBSCURED
FRACTION; TORUS MODELS
AB The covering factor of Compton-thick (CT) obscuring material associated with the torus in active galactic nuclei (AGNs) is at present best understood through the fraction of sources exhibiting CT absorption along the line of sight (N-H > 1.5 x 10(24) cm(-2)) in the X-ray band, which reveals the average covering factor. Determining this CT fraction is difficult, however, due to the extreme obscuration. With its spectral coverage at hard X-rays (>10 keV), Nuclear Spectroscopic Telescope Array (NuSTAR). is sensitive to the AGNs covering factor since Compton scattering of X-rays off optically thick material dominates at these energies. We present a spectral analysis of 10 AGNs observed with NuSTAR. where the obscuring medium is optically thick to Compton scattering, so-called CT AGNs. We use the torus models of Brightman & Nandra that predict the X-ray spectrum from reprocessing in a torus and include the torus opening angle as a free parameter and aim to determine the covering factor of the CT gas in these sources individually. Across the sample we find mild to heavy CT columns, with N-H measured from 10(24) to 10(26) cm(-2), and a wide range of covering factors, where individual measurements range from 0.2 to 0.9. We find that the covering factor, f(c), is a strongly decreasing function of the intrinsic 2-10 keV luminosity, L-X, where f(c) = (-0.41 +/- 0.13) log(10)(L-X/erg s(-1))+18.31 +/- 5.33, across more than two orders of magnitude in L-X (10(41.5) - 10(44) erg s-1). The covering factors measured here agree well with the obscured fraction as a function of L-X as determined by studies of local AGNs with L-X > 10(42.5) erg s(-1)
C1 [Brightman, M.; Balokovic, M.; Harrison, F. A.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[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.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago, 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.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy.
[Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, 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, SNSF Ambiz Fellow, CH-8093 Zurich, Switzerland.
[LaMassa, S.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
[Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Vasudevan, R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Brightman, M (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA.
RI Koss, Michael/B-1585-2015; Comastri, Andrea/O-9543-2015; Boggs,
Steven/E-4170-2015;
OI Koss, Michael/0000-0002-7998-9581; Comastri, Andrea/0000-0003-3451-9970;
Boggs, Steven/0000-0001-9567-4224; Puccetti,
Simonetta/0000-0002-2734-7835
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NASA
Headquarters under the NASA Earth and Space Science Fellowship Program
[NNX14AQ07H]; NSF [AST 1008067]; STFC [ST/J003697/1]; Swiss National
Science Foundation (SNSF) through the Ambizione fellowship grant [PZ00P2
154799/1]; Iniciativa Cientifica Milenio del Ministerio de Economia,
Fomento y Turismo [IC120009]; CONICYT-Chile grants Basal-CATA
[PFB-06/2007]; FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101];
"Millennium Institute of Astrophysics (MAS)" of the Iniciativa
Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
[IC120009]
FX This work was supported under NASA Contract No. NNG08FD60C and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software, and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA). The work presented here was also based on
observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA Member States and
NASA. This research has also made use of data and software provided by
the High Energy Astrophysics Science Archive Research Center (HEASARC),
which is a service of the Astrophysics Science Division at NASA/GSFC and
the High Energy Astrophysics Division of the Smithsonian Astrophysical
Observatory. Furthermore, this research has made use of the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. M. Balokovic acknowledges
support from NASA Headquarters under the NASA Earth and Space Science
Fellowship Program, grant NNX14AQ07H. D.R.B. acknowledges support from
NSF award AST 1008067; P.G. acknowledges support from STFC (grant
reference ST/J003697/1), M.K. acknowledges support from the Swiss
National Science Foundation (SNSF) through the Ambizione fellowship
grant PZ00P2 154799/1. We also acknowledge support from CONICYT-Chile
grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), "EMBIGGEN"
Anillo ACT1101 (FEB), Project IC120009 "Millennium Institute of
Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio
de Economia, Fomento y Turismo (FEB).
NR 73
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 41
DI 10.1088/0004-637X/805/1/41
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300041
ER
PT J
AU Ciardi, DR
Beichman, CA
Horch, EP
Howell, SB
AF Ciardi, David R.
Beichman, Charles A.
Horch, Elliott P.
Howell, Steve B.
TI UNDERSTANDING THE EFFECTS OF STELLAR MULTIPLICITY ON THE DERIVED PLANET
RADII FROM TRANSIT SURVEYS: IMPLICATIONS FOR KEPLER, K2, AND TESS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; planetary systems
ID SOLAR-TYPE STARS; CANDIDATES; MISSION; OBJECTS; SAMPLE; AU; COMPANIONS;
VALIDATION; SYSTEMS
AB We present a study on the effect of undetected stellar companions on the derived planetary radii for Kepler Objects of Interest (KOIs). The current production of the KOI list assumes that each KOI is a single star. Not accounting for stellar multiplicity statistically biases the planets toward smaller radii. The bias toward smaller radii depends on the properties of the companion stars and whether the planets orbit the primary or the companion stars. Defining a planetary radius correction factor, X-R, we find that if the KOIs are assumed to be single, then, on average, the planetary radii may be underestimated by a factor of < X-R > approximate to 1.5. If typical radial velocity and high-resolution imaging observations are performed and no companions are detected, then this factor reduces to < X-R > approximate to 1.2. The correction factor < X-R > is dependent on the primary star properties and ranges from < X-R > approximate to 1.6 for A and F stars to < X-R > approximate to 1.2 for K and M stars. For missions like K2 and TESS where the stars may be closer than the stars in the Kepler target sample, observational vetting (primary imaging) reduces the radius correction factor to < X-R > approximate to 1.1. Finally, we show that if the stellar multiplicity rates are not accounted for correctly, then occurrence rate calculations for Earth-sized planets may overestimate the frequency of small planets by as much as 15%-20%.
C1 [Ciardi, David R.; Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Mountain View, CA USA.
RP Ciardi, DR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
EM ciardi@ipac.caltech.edu
OI Ciardi, David/0000-0002-5741-3047
NR 37
TC 13
Z9 13
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 MAY 20
PY 2015
VL 805
IS 1
AR 16
DI 10.1088/0004-637X/805/1/16
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300016
ER
PT J
AU Dangi, BB
Kim, YS
Krasnokutski, SA
Kaiser, RI
Bauschlicher, CW
AF Dangi, Beni B.
Kim, Yong S.
Krasnokutski, Serge A.
Kaiser, Ralf I.
Bauschlicher, Charles W., Jr.
TI TOWARD THE FORMATION OF CARBONACEOUS REFRACTORY MATTER IN HIGH
TEMPERATURE HYDROCARBON-RICH ATMOSPHERES OF EXOPLANETS UPON
MICROMETEOROID IMPACT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; planets and satellites: atmospheres; solid state:
refractory; techniques: imaging spectroscopy
ID GJ 1214B; RAMAN-SPECTRA; TRANSMISSION SPECTRUM; HD 189733B; METHANE;
SPECTROSCOPY; DISEQUILIBRIUM; APPROXIMATION; CHEMISTRY; GRAPHITE
AB We report on laboratory simulation experiments mimicking the chemical processing of model atmospheres of exoplanets containing C3 and C4 hydrocarbons at moderate temperatures of 400 K upon interaction of catalytic surfaces of micrometeoroids. By utilizing an ultrasonic levitator device and heating singly levitated particles under simulated microgravity conditions, Raman spectroscopy is utilized as a non-invasive tool to probe on line and in situ the conversion of C3 and C4 hydrocarbons to refractory carbonaceous matter on the surfaces of levitated particles. Secondary Ion Mass Spectrometry and electron microscopic imaging were also conducted to gain further insight into the elementary composition and structures of the refractories formed. Our results provide compelling evidence that in the presence of a catalytic surface, which can be supplied in the form of micrometeoroids and atmospheric dust particles, hydrocarbon gases present in the atmospheres of exoplanets can be converted to refractory, carbon-rich carbonaceous matter of mainly graphitic structure with a carbon content of at least 90% at elevated temperatures. This finding might explain the low methane to carbon monoxide (CH4-CO) ratio in the hot Neptune GJ 436b, where the abundant methane photochemically converts to higher order hydrocarbons and ultimately to refractory graphite-like carbon in the presence of a silicon surface.
C1 [Dangi, Beni B.; Kim, Yong S.; Krasnokutski, Serge A.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Bauschlicher, Charles W., Jr.] NASA Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
FU National Science Foundation [CHE-1360658]
FX The authors thank Tina Carvalho of the University of Hawaii Biological
Electron Microscope Facility for help with the SEM and TEM image
acquisition. Funding for the research from the National Science
Foundation (CHE-1360658) is greatly acknowledged. They would also would
like to thank Dr. Anupam Mishra and Tayro Acosta of the Hawaiian
Institute of Geophysics and Planetology (HIGP) for the use of
micro-Raman systems and Professor Yuk L. Yung (California Institute of
Technology) for helpful discussions.
NR 40
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 76
DI 10.1088/0004-637X/805/1/76
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300076
ER
PT J
AU Fukumura, K
Tombesi, F
Kazanas, D
Shrader, C
Behar, E
Contopoulos, I
AF Fukumura, Keigo
Tombesi, Francesco
Kazanas, Demosthenes
Shrader, Chris
Behar, Ehud
Contopoulos, Ioannis
TI MAGNETICALLY DRIVEN ACCRETION DISK WINDS AND ULTRA-FAST OUTFLOWS IN PG
1211+143
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: individual (PG1211+143); galaxies:
Seyfert; methods: numerical; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; HIGH-VELOCITY OUTFLOW; X-RAY ABSORBERS;
RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS; HUBBLE-SPACE-TELESCOPE; BROAD
ABSORPTION-LINES; K-SHELL ABSORPTION; SEYFERT 1 GALAXIES; PDS 456;
PHYSICAL CONDITIONS
AB We present a study of X-ray ionization of MHD accretion-disk winds in an effort to constrain the physics underlying the highly ionized ultra-fast outflows (UFOs) inferred by X-ray absorbers often detected in various sub. classes of Seyfert active galactic nuclei (AGNs). Our primary focus is to show that magnetically driven outflows are indeed physically plausible candidates for the observed outflows accounting for the AGN absorption properties of the present X-ray spectroscopic observations. Employing a stratified MHD wind launched across the entire AGN accretion disk, we calculate its X-ray ionization and the ensuing X-ray absorption-line spectra. Assuming an appropriate ionizing AGN spectrum, we apply our MHD winds to model the absorption features in an XMM-Newton/EPIC spectrum of the narrow-line Seyfert, PG 1211+143. We find, through identifying the detected features with Fe K alpha transitions, that the absorber has a characteristic ionization parameter of log (xi(c)[erg cm s(-1)]) similar or equal to 5-6 and a column density on the order of N-H similar or equal to 10(23) cm(-2) outflowing at a characteristic velocity of v(c)/c similar or equal to 0.1-0.2 (where c is the speed of light). The best-fit model favors its radial location at r(c) similar or equal to 200 R-o (R-o is the black hole's innermost stable circular orbit), with an inner wind truncation radius at R-t similar or equal to 30 R-o. The overall K-shell feature in the data is suggested to be dominated by Fe XXV with very little contribution from Fe XXVI and weakly ionized iron, which is in good agreement with a series of earlier analyses of the UFOs in various AGNs, including PG 1211+143.
C1 [Fukumura, Keigo] James Madison Univ, Harrisonburg, VA 22807 USA.
[Tombesi, Francesco; Kazanas, Demosthenes; Shrader, Chris] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tombesi, Francesco] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Shrader, Chris] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, Athens 11527, Greece.
RP Fukumura, K (reprint author), James Madison Univ, Harrisonburg, VA 22807 USA.
EM fukumukx@jmu.edu
NR 90
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Z9 12
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 MAY 20
PY 2015
VL 805
IS 1
AR 17
DI 10.1088/0004-637X/805/1/17
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300017
ER
PT J
AU Ly, C
Rigby, JR
Cooper, M
Yan, RB
AF Ly, Chun
Rigby, Jane R.
Cooper, Michael
Yan, Renbin
TI METAL-POOR, STRONGLY STAR-FORMING GALAXIES IN THE DEEP2 SURVEY: THE
RELATIONSHIP BETWEEN STELLAR MASS, TEMPERATURE-BASED METALLICITY, AND
STAR FORMATION RATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: distances and redshifts; galaxies:
evolution; galaxies: ISM; galaxies: photometry; galaxies: starburst
ID EMISSION-LINE GALAXIES; DIGITAL SKY SURVEY; SIMILAR-TO 2; SPECTROSCOPIC
PARALLEL SURVEY; HIGH-REDSHIFT GALAXIES; NEWH-ALPHA SURVEY; PHYSICAL
CONDITIONS; FUNDAMENTAL PLANE; LENSED GALAXIES; DWARF GALAXIES
AB We report on the discovery of 28 z approximate to 0.8 metal-poor galaxies in DEEP2. These galaxies were selected for their detection of the weak [O III] lambda 4363 emission line, which provides a "direct" measure of the gas-phase metallicity. A primary goal for identifying these rare galaxies is to examine whether the fundamental metallicity relation (FMR) between stellar mass, gas metallicity, and star formation rate (SFR) holds for low stellar mass and high SFR galaxies. The FMR suggests that higher SFR galaxies have lower metallicity (at fixed stellar mass). To test this trend, we combine spectroscopic measurements of metallicity and dust-corrected SFR with stellar mass estimates from modeling the optical photometry. We find that these galaxies are 1.05 +/- 0.61 dex above the z similar to 1 stellar mass-SFR relation and 0.23 +/- 0.23 dex below the local mass-metallicity relation. Relative to the FMR, the latter offset is reduced to 0.01 dex, but significant dispersion remains (0.29 dex with 0.16 dex due to measurement uncertainties). This dispersion suggests that gas accretion, star formation, and chemical enrichment have not reached equilibrium in these galaxies. This is evident by their short stellar mass doubling timescale of approximate to 100(-75)(+310) Myr, which suggests stochastic star formation. Combining our sample with other z similar to 1 metal-poor galaxies, we find a weak positive SFR-metallicity dependence (at fixed stellar mass) that is significant at 94.4% confidence. We interpret this positive correlation as recent star formation that has enriched the gas but has not had time to drive the metal-enriched gas out with feedback mechanisms.
C1 [Ly, Chun; Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Cooper, Michael] UCI, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA USA.
[Yan, Renbin] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
RP Ly, C (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM chun.ly@nasa.gov
OI Ly, Chun/0000-0002-4245-2318; Yan, Renbin/0000-0003-1025-1711
FU NSF [AST-9509298, AST-0071048, AST-0507428, AST-0507483]; NASA LTSA
grant [NNG04GC89G]; NASA Postdoctoral Program
FX Based on observations taken at the W. M. Keck Observatory, which is
operated jointly by the National Aeronautics and Space Administration
(NASA), the University of California, and the California Institute of
Technology. Funding for the DEEP2 Galaxy Redshift Survey has been
provided by NSF grants AST-9509298, AST-0071048, AST-0507428, and
AST-0507483, as well as NASA LTSA grant NNG04GC89G. C.L. is funded
through the NASA Postdoctoral Program. We thank Jeffrey Newman, Alaina
Henry, Massimo Ricotti, and Kate Whitaker for insightful discussions,
and the anonymous referee for insightful comments that improved the
paper.
NR 72
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 45
DI 10.1088/0004-637X/805/1/45
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300045
ER
PT J
AU Pasham, DR
Cenko, SB
Levan, AJ
Bower, GC
Horesh, A
Brown, GC
Dolan, S
Wiersema, K
Filippenko, AV
Fruchter, AS
Greiner, J
O'Brien, PT
Page, KL
Rau, A
Tanvir, NR
AF Pasham, Dheeraj R.
Cenko, S. Bradley
Levan, Andrew J.
Bower, Geoffrey C.
Horesh, Assaf
Brown, Gregory C.
Dolan, Stephen
Wiersema, Klaas
Filippenko, Alexei V.
Fruchter, Andrew S.
Greiner, Jochen
O'Brien, Paul T.
Page, Kim L.
Rau, Arne
Tanvir, Nial R.
TI A MULTIWAVELENGTH STUDY OF THE RELATIVISTIC TIDAL DISRUPTION CANDIDATE
SWIFT J2058.4+0516 AT LATE TIMES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; astrometry; black hole physics; relativistic
processes
ID MASSIVE BLACK-HOLES; GAMMA-RAY BURST; PHOTON IMAGING CAMERA; FUNDAMENTAL
PLANE; ACCRETION FLOWS; RADIO-EMISSION; SOLAR MASSES; XMM-NEWTON;
GALAXY; EVENT
AB We report a multiwavelength (X-ray, ultraviolet/optical/infrared (UVOIR), radio) analysis of the relativistic tidal disruption event (TDE) candidate Sw J2058+05 from 3 months to 3 yr post-discovery in order to study its properties and compare its behavior with that of Sw J1644+57. Our main results are as follows: (1) The long-term X-ray light curve of Sw J2058+05 shows a remarkably similar trend to that of Sw J1644+57. After a prolonged power-law decay, the X-ray flux drops off rapidly by a factor of greater than or similar to 160 within a span of Delta t/t <= 0.95. Associating this sudden decline with the transition from super-Eddington to sub-Eddington accretion, we estimate the black hole mass to be in the range of 10(4-6) M-circle dot. (2) We detect rapid (less than or similar to 500 s) X-ray variability before the drop-off, suggesting that, even at late times, the X-rays originate from close to the black hole (ruling out a forward-shock origin). (3) We confirm using Hubble Space Telescope and Very Long Baseline Array astrometry that the location of the source coincides with the galaxy's center to within less than or similar to 400 pc (in projection). (4) We modeled Sw J2058+05's UVOIR spectral energy distribution with a single-temperature blackbody and find that while the radius remains more or less constant at a value of 63.4 +/- 4.5 AU (similar to 10(15) cm) at all times during the outburst, the blackbody temperature drops significantly from similar to 30,000 K at early times to a value of similar to 15,000 K at late times (before the Xray drop-off). Our results strengthen Sw J2058+05's interpretation as a TDE similar to Sw J1644+57.
C1 [Pasham, Dheeraj R.; Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
[Pasham, Dheeraj R.; Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Levan, Andrew J.; Brown, Gregory C.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA.
[Horesh, Assaf] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Dolan, Stephen] Oxford Astrophys, Oxford OX1 3RH, England.
[Wiersema, Klaas; O'Brien, Paul T.; Page, Kim L.; Tanvir, Nial R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fruchter, Andrew S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Greiner, Jochen; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Pasham, DR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
EM dheerajrangareddy.pasham@nasa.gov
RI Horesh, Assaf/O-9873-2016
OI Horesh, Assaf/0000-0002-5936-1156
FU NSF Grant [1066293]; UK Space Agency; National Aeronautics and Space
Administration (NASA) through Chandra Award [GO3-14107X]; NASA
[NAS8-03060, NAS 5-26555]; HST [GO-13611-006 A]; NSF [AST-1211916]; ESA
Member States; NASA; W. M. Keck Foundation
FX We thank the XMM-Newton and HST teams, in particular Project Scientist
N. Schartel and STScI director M. Mountain, for the approval and prompt
scheduling of our DD requests. We are also grateful to James Guillochon
and Ryan Chornock for valuable discussions. D.R.P. is grateful for
valuable discussions with Sjoert van Velzen and Nick Stone. S.B.C.
thanks the Aspen Center for Physics and NSF Grant #1066293 for
hospitality during the preparation of this manuscript. K.L.P.
acknowledges support from the UK Space Agency. Support for this work was
provided by the National Aeronautics and Space Administration (NASA)
through Chandra Award Number GO3-14107X 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. D.R.P.
and S.B.C. also acknowledge support from HST grant GO-13611-006 A. The
work of A.V.F. was made possible by NSF grant AST-1211916, the TABASGO
Foundation, and the Christopher R. Redlich Fund. A.V.F. and S.B.C. also
acknowledge the support of Gary and Cynthia Bengier. Finally, we would
like to thank the referee for his/her careful comments and suggestions.
The scientific results reported in this article are based in part on
observations made by the Chandra X-ray Observatory, NASA/ESA Hubble
Space Telescope, obtained from the 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, and
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. 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. Also, observations were obtained at the Gemini Observatory,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under a cooperative agreement with the NSF on behalf of
the Gemini partnership: the National Science Foundation (United States),
the National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia, Tecnologia e
Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). Also, based on observations made with ESO
Telescopes at the La Silla or Paranal Observatories. We acknowledge the
use of public data from the Swift data archive.
NR 76
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 68
DI 10.1088/0004-637X/805/1/68
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300068
ER
PT J
AU Pontin, DI
Wyper, PF
AF Pontin, D. I.
Wyper, P. F.
TI THE EFFECT OF RECONNECTION ON THE STRUCTURE OF THE SUN'S OPEN-CLOSED
FLUX BOUNDARY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; solar wind; Sun: corona; Sun: magnetic fields
ID SLOW SOLAR-WIND; OPEN MAGNETIC-FIELD; CORONAL NULL-POINT; FLARE RIBBONS;
MODEL; PSEUDOSTREAMERS; TOPOLOGY; CONNECTIVITY; TRANSPORT; DYNAMICS
AB Global magnetic field extrapolations are now revealing the huge complexity of the Sun's corona, and in particular the structure of the boundary between open and closed magnetic flux. Moreover, recent developments indicate that magnetic reconnection in the corona likely occurs in highly fragmented current layers, and that this typically leads to a dramatic increase in the topological complexity beyond that of the equilibrium field. In this paper we use static models to investigate the consequences of reconnection at the open-closed flux boundary ("interchange reconnection") in a fragmented current layer. We demonstrate that it leads to efficient mixing of magnetic flux (and therefore plasma) from open and closed field regions. This corresponds to an increase in the length and complexity of the open-closed boundary. Thus, whenever reconnection occurs at a null point or separator of this open-closed boundary, the associated separatrix arc of the so-called S-web in the high corona becomes not a single line but a band of finite thickness within which the open-closed boundary is highly structured. This has significant implications for the acceleration of the slow solar wind, for which the interaction of open and closed field is thought to be important, and may also explain the coronal origins of certain solar energetic particles. The topological structures examined contain magnetic null points, separatrices and separators, and include a model for a pseudo-streamer. The potential for understanding both the large scale morphology and fine structure observed in flare ribbons associated with coronal nulls is also discussed.
C1 [Pontin, D. I.] Univ Dundee, Div Math, Dundee, Scotland.
[Wyper, P. F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Pontin, DI (reprint author), Univ Dundee, Div Math, Dundee, Scotland.
EM dpontin@maths.dundee.ac.uk; peter.f.wyper@nasa.gov
RI Wyper, Peter/H-9166-2013; Pontin, David/E-2313-2011
OI Pontin, David/0000-0002-1089-9270
FU UK's STFC [ST/K000993]; Leverhulme Trust; appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center; NASA
FX D.P. acknowledges financial support from the UK's STFC (grant number
ST/K000993) and the Leverhulme Trust. P.W. acknowledges support from an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 63
TC 3
Z9 3
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 39
DI 10.1088/0004-637X/805/1/39
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300039
ER
PT J
AU Shariff, K
Cuzzi, JN
AF Shariff, Karim
Cuzzi, Jeffrey N.
TI THE SPHERICALLY SYMMETRIC GRAVITATIONAL COLLAPSE OF A CLUMP OF SOLIDS IN
A GAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; protoplanetary disks
ID PROTOPLANETARY DISKS; SOLAR NEBULA; PLANETESIMAL FORMATION; PREFERENTIAL
CONCENTRATION; STREAMING INSTABILITIES; ISOTROPIC TURBULENCE; PAIR
DISPERSION; PARTICLES; DUST; DYNAMICS
AB In the subject of planetesimal formation, several mechanisms have been identified that create dense particle clumps in the solar nebula. The present work is concerned with the gravitational collapse of such clumps, idealized as being spherically symmetric. Fully nonlinear simulations using the two-fluid model are carried out (almost) up to the time when a central density singularity forms. We refer to this as the collapse time. The end result of the study is a parametrization of the collapse time, in order that it may be compared with timescales for various disruptive effects to which clumps may be subject in a particular situation. An important effect that determines the collapse time is that as the clump compresses, it also compresses the gas due to drag. This increases gas pressure, which retards particle collapse and can lead to oscillation in the size and density of the clump. In the limit of particles perfectly coupled to the gas, the characteristic ratio of gravitational force to gas pressure becomes relevant and defines a two-phase Jeans parameter, Jt, which is the classical Jeans parameter with the speed of sound replaced by an effective wave speed in the coupled two-fluid medium. The parameter J(t) remains useful even away from the perfect coupling limit because it makes the simulation results insensitive to the initial density ratio of particles to gas (Phi(0)) as a separate parameter. A simple ordinary differential equation model is developed. It takes the form of two coupled non-linear oscillators and reproduces key features of the simulations. Finally, a parametric study of the time to collapse is performed and a formula (fit to the simulations) is developed. In the incompressible limit J(t) -> 0, collapse time equals the self-sedimentation time, which is inversely proportional to the Stokes number. As J(t) increases, the collapse time decreases with J(t) and eventually becomes approximately equal to the dynamical time. Values of collapse time versus clump size are given for a minimum-mass solar nebula. Finally, the timescale of clump erosion due to turbulent strain is estimated.
C1 [Shariff, Karim; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Shariff, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
OI Shariff, Karim/0000-0002-7256-2497
NR 47
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 MAY 20
PY 2015
VL 805
IS 1
AR 42
DI 10.1088/0004-637X/805/1/42
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300042
ER
PT J
AU Zhang, K
Crockett, N
Salyk, C
Pontoppidan, K
Turner, NJ
Carpenter, JM
Blake, GA
AF Zhang, Ke
Crockett, Nathan
Salyk, Colette
Pontoppidan, Klaus
Turner, Neal J.
Carpenter, John M.
Blake, Geoffrey A.
TI DIMMING AND CO ABSORPTION TOWARD THE AA TAU PROTOPLANETARY DISK: AN
INFALLING FLOW CAUSED BY DISK INSTABILITY?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE protoplanetary disks; stars: individual (AA Tau); stars: pre-main
sequence; stars: variables: T Tauri, Herbig Ae/Be
ID X-RAY-ABSORPTION; MAGNETOSPHERIC ACCRETION; PROTOSTELLAR DISKS;
CHEMICAL-PROCESSES; INNER DISK; EMISSION; SPECTROSCOPY; CONSTRAINTS;
VARIABILITY; STARS
AB AA Tau, a classical T Tauri star in the Taurus cloud, has been the subject of intensive photometric monitoring for more than two decades due to its quasi-cyclic variation in optical brightness. Beginning in 2011, AA Tau showed another peculiar variation-its median optical though near-IR flux dimmed significantly, a drop consistent with a 4-mag increase in visual extinction. It has stayed in the faint state since. Here we present 4.7 mu m CO rovibrational spectra of AA Tau over eight epochs, covering an 11 yr time span, that reveal enhanced (CO)-C-12 and (CO)-C-13 absorption features in the J(low) <= 13 transitions after the dimming. These newly appeared absorptions require molecular gas along the line of sight with T similar to 500 K and a column density of log (N (CO)-C-12) similar to 18.5 cm(-2), with line centers that show a constant 6 km s(-1) redshift. The properties of the molecular gas confirm an origin in the circumstellar material. We suggest that the dimming and absorption are caused by gas and dust lifted to large heights by a magnetic buoyancy instability. This material is now propagating inward, and on reaching the star within a few years will be observed as an accretion outburst.
C1 [Zhang, Ke; Carpenter, John M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Crockett, Nathan; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Salyk, Colette] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Pontoppidan, Klaus] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zhang, K (reprint author), CALTECH, Div Phys Math & Astron, MC 249-17, Pasadena, CA 91125 USA.
EM kzhang@astro.caltech.edu
OI Salyk, Colette/0000-0003-3682-6632
FU NSF AAG program; NOAO Leo Goldberg Fellowship program; Origins of Solar
Systems Program [13-OSS13-0114]; NSF award [AST-1140063]; W. M. Keck
Foundation; NASA Origins of Solar Systems program; [179.C-0151]
FX We thank Jerome Bouvier and Konstantin Grankin for sharing their AA Tau
photometric data, and the anonymous referee for helpful comments. K.Z.,
N.C. and G.A.B. gratefully acknowledge support from the NSF AAG and NASA
Origins of Solar Systems programs. C.S. acknowledges the financial
support of the NOAO Leo Goldberg Fellowship program. N.J.T.'s
contributions were made at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA and with support from
Origins of Solar Systems Program grant 13-OSS13-0114. J.M.C.
acknowledges support from NSF award AST-1140063. The spectra presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California and NASA. The Observatory was made possible
by the generous financial support of the W. M. Keck Foundation. The VLT
data presented were acquired under program ID 179.C-0151. Finally, the
authors wish to acknowledge the significant cultural role of the summit
of Mauna Kea.
NR 47
TC 3
Z9 3
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2015
VL 805
IS 1
AR 55
DI 10.1088/0004-637X/805/1/55
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300055
ER
PT J
AU Zhao, L
DeVore, CR
Antiochos, SK
Zurbuchen, TH
AF Zhao, L.
DeVore, C. R.
Antiochos, S. K.
Zurbuchen, T. H.
TI NUMERICAL SIMULATIONS OF HELICITY CONDENSATION IN THE SOLAR CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: corona; Sun: magnetic fields
ID MAGNETIC-FLUX TUBES; RECONNECTION; FIELDS; RELAXATION; FILAMENTS;
SUPERGRANULATION; DISSIPATION; COALESCENCE; CHIRALITY; PATTERNS
AB The helicity condensation model has been proposed by Antiochos to explain the observed smoothness of coronal loops and the observed buildup of magnetic shear at filament channels. The basic hypothesis of the model is that magnetic reconnection in the corona causes the magnetic stress injected by photospheric motions to collect only at those special locations where prominences are observed to form. In this work we present the first detailed quantitative MHD simulations of the reconnection evolution proposed by the helicity condensation model. We use the well-known ansatz of modeling the closed corona as an initially uniform field between two horizontal photospheric plates. The system is driven by applying photospheric rotational flows that inject magnetic helicity into the corona. The flows are confined to a finite region on the photosphere so as to mimic the finite flux system of a bipolar active region, for example. The calculations demonstrate that, contrary to common belief, opposite helicity twists do not lead to significant reconnection in such a coronal system, whereas twists with the same sense of helicity do produce substantial reconnection. Furthermore, we find that for a given amount of helicity injected into the corona, the evolution of the magnetic shear is insensitive to whether the pattern of driving photospheric motions is fixed or quasi-random. In all cases, the shear propagates via reconnection to the boundary of the flow region while the total magnetic helicity is conserved, as predicted by the model. We discuss the implications of our results for solar observations and for future, more realistic simulations of the helicity condensation process.
C1 [Zhao, L.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA.
[DeVore, C. R.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Zhao, L (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA.
RI DeVore, C/A-6067-2015;
OI DeVore, C/0000-0002-4668-591X; Zhao, Liang/0000-0002-5975-7476
FU NASA Earth and Space Science Fellowship Program-Grant [NNX09AV13H]; TRT
Program; SRT Program; LWS [NNX10AQ61G, NNX13AH66G]; NSF [AGS-1432100]
FX We gratefully acknowledge financial support for our research from NASA
Earth and Space Science Fellowship Program-Grant NNX09AV13H (L.Z.), TR&T
and SR&T Programs (C.R.D. and S.K.A.), LWS NNX10AQ61G and NNX13AH66G
(T.H.Z.), and NSF AGS-1432100 (L.Z.). Also, we thank the DoD High
Performance Computing and Modernization Program for providing computer
resources for our large-scale numerical simulations during the time that
C.R.D. held a staff position at the Naval Research Laboratory.
NR 40
TC 4
Z9 4
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 MAY 20
PY 2015
VL 805
IS 1
AR 61
DI 10.1088/0004-637X/805/1/61
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300061
ER
PT J
AU Zhu, W
Udalski, A
Gould, A
Dominik, M
Bozza, V
Han, C
Yee, JC
Novati, SC
Beichman, CA
Carey, S
Poleski, R
Skowron, J
Kozlowski, S
Mroz, P
Pietrukowicz, P
Pietrzynski, G
Szymanski, MK
Soszynski, I
Ulaczyk, K
Wyrzykowski, L
Gaudi, BS
Pogge, RW
DePoy, DL
Jung, YK
Choi, JY
Hwang, KH
Shin, IG
Park, H
Jeong, J
AF Zhu, Wei
Udalski, A.
Gould, A.
Dominik, M.
Bozza, V.
Han, C.
Yee, J. C.
Novati, S. Calchi
Beichman, C. A.
Carey, S.
Poleski, R.
Skowron, J.
Kozlowski, S.
Mroz, P.
Pietrukowicz, P.
Pietrzynski, G.
Szymanski, M. K.
Soszynski, I.
Ulaczyk, K.
Wyrzykowski, L.
Gaudi, B. S.
Pogge, R. W.
DePoy, D. L.
Jung, Y. K.
Choi, J. -Y.
Hwang, K. -H.
Shin, I. -G.
Park, H.
Jeong, J.
CA OGLE Collaboration
FUN Collaboration
TI SPITZER AS A MICROLENS PARALLAX SATELLITE: MASS AND DISTANCE
MEASUREMENTS OF BINARY LENS SYSTEM OGLE-2014-BLG-1050L
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID GALACTIC BULGE; ISOLATED STAR; HOST STAR; OGLE-III; EVENTS;
MAGNIFICATION; DWARF; PREDICTIONS; DISCOVERY; MOTIONS
AB We report the first mass and distance measurements of a caustic-crossing binary system OGLE-2014-BLG-1050 L using the space-based microlens parallax method. Spitzer captured the second caustic. crossing of the event, which occurred similar to 10 days before that seen from Earth. Due to the coincidence that the source-lens relative motion was almost parallel to the direction of the binary-lens axis, the fourfold degeneracy, which was known before only to occur in single-lens events, persists in this case, leading to either a lower-mass (0.2 and 0.07 M-circle dot) binary at similar to 1.1 kpc or a higher-mass (0.9 and 0.35 M-circle dot) binary at similar to 3.5 kpc. However, the latter solution is strongly preferred for reasons including blending and lensing probability. OGLE-2014-BLG-1050 L demonstrates the power of microlens parallax in probing stellar and substellar binaries.
C1 [Zhu, Wei; Gould, A.; Poleski, R.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Udalski, A.; Poleski, R.; Skowron, J.; Kozlowski, S.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Dominik, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Bozza, V.; Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Han, C.; Jung, Y. K.; Choi, J. -Y.; Hwang, K. -H.; Shin, I. -G.; Park, H.; Jeong, J.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Novati, S. Calchi; Beichman, C. A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, S. Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
RP Zhu, W (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013;
OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X;
ZHU, WEI/0000-0003-4027-4711
FU NSF [AST 1103471]; JPL [1500811]; NASA [NNX12AB99G]; Creative Research
Initiative Program of the National Research Foundation of Korea
[2009-0081561]; NASA through the Sagan Fellowship Program; European
Research Council under the European Community's Seventh Framework
Programme (FP7)/ERC [246678]
FX Work by W.Z., A.G., and B.S.G. was supported by NSF grant AST 1103471.
Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. A.G.,
B.S.G., and R.W.P. were supported by NASA grant NNX12AB99G. Work by C.H.
was supported by the Creative Research Initiative Program (2009-0081561)
of the National Research Foundation of Korea. Work by J.C.Y. was
performed under contract with the California Institute of Technology
(Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the
Sagan Fellowship Program executed by the NASA Exoplanet Science
Institute. Work by C.A.B. was carried out in part at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with the National Aeronautics and Space Administration. The OGLE project
has received funding from the European Research Council under the
European Community's Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement no. 246678 to AU. This work is based in part on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA.
NR 56
TC 17
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 MAY 20
PY 2015
VL 805
IS 1
AR 8
DI 10.1088/0004-637X/805/1/8
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8BA
UT WOS:000354991300008
ER
PT J
AU Lin, Y
Han, XG
Campbell, CJ
Kim, JW
Zhao, B
Luo, W
Dai, JQ
Hu, LB
Connell, JW
AF Lin, Yi
Han, Xiaogang
Campbell, Caroline J.
Kim, Jae-Woo
Zhao, Bin
Luo, Wei
Dai, Jiaqi
Hu, Liangbing
Connell, John W.
TI Holey Graphene Nanomanufacturing: Structure, Composition, and
Electrochemical Properties
SO ADVANCED FUNCTIONAL MATERIALS
LA English
DT Article
ID ENERGY-STORAGE; NANOMESH; CARBON; LITHOGRAPHY; OXIDE
AB Topology is critical for properties and function of 2D nanomaterials. Membranes and films from 2D nanomaterials usually suffer from large tortuosity as a result from dense restacking of the nanosheets and thus have limited utility in applications such as electrodes for supercapacitor and batteries, which require ion transport through the nanosheet thickness. In comparison with conventional porous 2D nanomaterials, introducing holes through the nanosheets to create holey 2D nanomaterials with retention of the 2D-related properties is a more viable approach to improve molecular transport. Here, graphene is used as a model to study the fundamental structure-property relationship as a result from defect-enabled hole creation. Specifically, the correlation of electrochemical capacitive properties with structure and composition for holey graphene materials is prepared using a highly scalable controlled air oxidation process. The presence of holes on graphene sheets is not sufficient to account for the observed capacitance improvement. Rather, the improvement is achieved through the combination of an enhanced mesopore fraction with simultaneous oxygen doping while retaining the graphitic carbon network with minimal damage. The detailed understanding might be further applied to other 2D materials toward a broader range of both energy-related and other applications.
C1 [Lin, Yi; Campbell, Caroline J.; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
[Han, Xiaogang; Zhao, Bin; Luo, Wei; Dai, Jiaqi; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
[Connell, John W.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Exploration Way, Hampton, VA 23666 USA.
EM yi.lin-1@nasa.gov; binghu@umd.edu
RI Kim, Jae-Woo/A-8314-2008; Luo, Wei/E-1582-2011
OI Luo, Wei/0000-0002-4019-4634
FU Leading Edge Aeronautics Research for NASA (LEARN) program [NNX13AB88A];
NSF-CBET [1335944, 1335979]; LEARN
FX The authors would like to thank M. Funk, L. Garcia, P. Tiemsin, and C.
Chamberlain for experimental assistance. Y.L. acknowledges the financial
support from the Leading Edge Aeronautics Research for NASA (LEARN)
program (Grant No. NNX13AB88A). L.H. gratefully acknowledge the support
from NSF-CBET (Grant Nos. 1335944 and 1335979), respectively. C.J.C. was
a Langley Aerospace Research Summer Scholars (LARSS) Program scholar
supported by LEARN.
NR 21
TC 22
Z9 22
U1 28
U2 205
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1616-301X
EI 1616-3028
J9 ADV FUNCT MATER
JI Adv. Funct. Mater.
PD MAY 20
PY 2015
VL 25
IS 19
BP 2920
EP 2927
DI 10.1002/adfm.201500321
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 CI3DC
UT WOS:000354626800015
ER
PT J
AU Laslandes, M
Patterson, K
Pellegrino, S
AF Laslandes, Marie
Patterson, Keith
Pellegrino, Sergio
TI Optimized actuators for ultrathin deformable primary mirrors
SO APPLIED OPTICS
LA English
DT Article
ID OPTICS
AB A novel design and selection scheme for surface-parallel actuators for ultrathin, lightweight mirrors is presented. The actuation system consists of electrodes printed on a continuous layer of piezoelectric material bonded to an optical-quality substrate. The electrodes provide almost full coverage of the piezoelectric layer, in order to maximize the amount of active material that is available for actuation, and their shape is optimized to maximize the correctability and stroke of the mirror for a chosen number of independent actuators and for a dominant imperfection mode. The starting point for the design of the electrodes is the observation that the correction of a figure error that has at least two planes of mirror symmetry is optimally done with twin actuators that have the same optimized shape but are rotated through a suitable angle. Additional sets of optimized twin actuators are defined by considering the intersection between the twin actuators, and hence an arbitrarily fine actuation pattern can be generated. It is shown that this approach leads to actuator systems with better performance than simple, geometrically based actuators. Several actuator patterns to correct third-order astigmatism aberrations are presented, and an experimental demonstration of a 41-actuator mirror is also presented. (C) 2015 Optical Society of America
C1 [Laslandes, Marie; Pellegrino, Sergio] CALTECH, Pasadena, CA 91125 USA.
[Patterson, Keith] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pellegrino, S (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM sergiop@caltech.edu
FU Defense Advanced Research Projects Agency (DARPA) [W31P4Q-14-1-0008];
French Defence procurement agency (DGA) through Aix-Marseille
University, France; Keck Institute of Space Studies; Dow Resnick Bridge
program at Caltech; National Aeronautics and Space Administration (NASA)
FX Defense Advanced Research Projects Agency (DARPA) (W31P4Q-14-1-0008);
National Aeronautics and Space Administration (NASA).; We thank Xin Ning
(Caltech) for help with the optimization algorithm and John Steeves
(Caltech) for advice on mirror fabrication. We thank Dr. Harish Manohara
(JPL) for providing access to the Microdevices Lab (MDL) cleanroom
facilities for sample fabrication. We thank Dr. Risaku Toda (JPL) and
Mr. Victor White (JPL) for processing equipment training and usage
advice at the MDL. ML acknowledges the support of a postdoctoral grant
from the French Defence procurement agency (DGA) held through
Aix-Marseille University, France. Financial support from the Keck
Institute of Space Studies and the Dow Resnick Bridge program at Caltech
is gratefully acknowledged. A part of this research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with National Aeronautics and Space Administration (NASA).
NR 30
TC 0
Z9 0
U1 1
U2 13
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD MAY 20
PY 2015
VL 54
IS 15
BP 4937
EP 4952
DI 10.1364/AO.54.004937
PG 16
WC Optics
SC Optics
GA CI6UL
UT WOS:000354898100042
PM 26192533
ER
PT J
AU Aartsen, MG
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bos, F
Bose, D
Boser, S
Botner, O
Brayeur, L
Bretz, HP
Brown, AM
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Christy, B
Clark, K
Classen, L
Clevermann, F
Coenders, S
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
De Ridder, S
Desiati, P
de Vries, KD
de With, M
DeYoung, T
Diaz-Velez, JC
Dunkman, M
Eagan, R
Eberhardt, B
Ehrhardt, T
Eichmann, B
Eisch, J
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Frantzen, K
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Gier, D
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Goodman, JA
Gora, D
Grant, D
Gretskov, P
Groh, JC
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallen, P
Hallgren, A
Halzen, F
Hanson, K
Hebecker, D
Heereman, D
Heinen, D
Helbing, K
Hellauer, R
Hellwig, D
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huang, F
Huelsnitz, W
Hulth, PO
Hultqvist, K
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Jero, K
Jlelati, O
Jurkovic, M
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kauer, M
Keivani, A
Kelley, JL
Kheirandish, A
Kiryluk, J
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Koob, A
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Kriesten, A
Krings, K
Kroll, G
Kroll, M
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larsen, DT
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Lunemann, J
Madsen, J
Maggi, G
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meli, A
Meures, T
Miarecki, S
Middell, E
Middlemas, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Paul, L
Penke, O
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Putz, J
Quinnan, M
Radel, L
Rameez, M
Rawlins, K
Redl, P
Rees, I
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Riedel, B
Robertson, S
Rodrigues, JP
Rongen, M
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Sander, HG
Sandroos, J
Santander, M
Sarkar, S
Schatto, K
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Sestayo, Y
Seunarine, S
Shanidze, R
Smith, MWE
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stanisha, NA
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Strotjohann, NL
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Tosi, D
Tselengidou, M
Unger, E
Usner, M
Vallecorsa, S
van Eijndhoven, N
Vandenbroucke, J
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallraff, M
Weaver, C
Wellons, M
Wendt, C
Westerhoff, S
Whelan, BJ
Whitehorn, N
Wichary, C
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zoll, M
AF Aartsen, M. G.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Classen, L.
Clevermann, F.
Coenders, S.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de With, M.
DeYoung, T.
Diaz-Valez, J. C.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Eisch, J.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Gier, D.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Goodman, J. A.
Gora, D.
Grant, D.
Gretskov, P.
Groh, J. C.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallen, P.
Hallgren, A.
Halzen, F.
Hanson, K.
Hebecker, D.
Heereman, D.
Heinen, D.
Helbing, K.
Hellauer, R.
Hellwig, D.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huang, F.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Jurkovic, M.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kheirandish, A.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koob, A.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kriesten, A.
Krings, K.
Kroll, G.
Kroll, M.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larsen, D. T.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Luenemann, J.
Madsen, J.
Maggi, G.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meli, A.
Meures, T.
Miarecki, S.
Middell, E.
Middlemas, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Paul, L.
Penke, O.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Puetz, J.
Quinnan, M.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Rees, I.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Riedel, B.
Robertson, S.
Rodrigues, J. P.
Rongen, M.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Sander, H. -G.
Sandroos, J.
Santander, M.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Sestayo, Y.
Seunarine, S.
Shanidze, R.
Smith, M. W. E.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stanisha, N. A.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Stroem, R.
Strotjohann, N. L.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Tosi, D.
Tselengidou, M.
Unger, E.
Usner, M.
Vallecorsa, S.
van Eijndhoven, N.
Vandenbroucke, J.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallraff, M.
Weaver, Ch.
Wellons, M.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Whitehorn, N.
Wichary, C.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zoll, M.
TI SEARCH FOR PROMPT NEUTRINO EMISSION FROM GAMMA-RAY BURSTS WITH ICECUBE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; neutrinos
ID HIGH-ENERGY NEUTRINOS; 1ST 2 YEARS; COSMIC-RAYS; SPECTRAL CATALOG; MUON
NEUTRINOS; ACCELERATION; TELESCOPE; MISSION; SIMULATIONS; FIREBALLS
AB We present constraints derived from a search of four years of IceCube data for a prompt neutrino flux from gammaray bursts (GRBs). A single low-significance neutrino, compatible with the atmospheric neutrino background, was found in coincidence with one of the 506 observed bursts. Although GRBs have been proposed as candidate sources for ultra-high-energy cosmic rays, our limits on the neutrino flux disfavor much of the parameter space for the latest models. We also find that no more than similar to 1% of the recently observed astrophysical neutrino flux consists of prompt emission from GRBs that are potentially observable by existing satellites.
C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. J.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bernhard, A.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.; Brown, A. M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Aguilar, J. A.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
[Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Valez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Valez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Ahrens, M.; Bohm, C.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Gretskov, P.; Haack, C.; Hallen, P.; Heinen, D.; Hellwig, D.; Koob, A.; Kriesten, A.; Leuermann, M.; Paul, L.; Penke, O.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys, D-52056 Aachen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Baum, V.; Boeser, S.; Eberhardt, B.; Ehrhardt, T.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Fedynitch, A.; Kroll, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Berley, D.; Blaufuss, E.; Cheung, E.; Christy, B.; Felde, J.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Bernhard, A.; Coenders, S.; Gross, A.; Jurkovic, M.; Krings, K.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
[Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Odrowski, S.; Riedel, B.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[de Andre, J. P. A. M.; DeYoung, T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[De Ridder, S.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Meli, A.; Ryckbosch, D.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Kurahashi, N.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aartsen, MG (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
RI Koskinen, David/G-3236-2014; Maruyama, Reina/A-1064-2013; Tjus,
Julia/G-8145-2012; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011;
Wiebusch, Christopher/G-6490-2012;
OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Koskinen,
David/0000-0002-0514-5917; Maruyama, Reina/0000-0003-2794-512X; Sarkar,
Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch,
Christopher/0000-0002-6418-3008; Schukraft, Anne/0000-0002-9112-5479;
Groh, John/0000-0001-9880-3634; Larsen, Dag Toppe/0000-0002-9898-2174;
Maunu, Ryan/0000-0002-5755-3437; Perez de los Heros,
Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730;
Arguelles Delgado, Carlos/0000-0003-4186-4182
FU U.S. National Science Foundation-office of Polar Programs; U.S. National
Science Foundation-physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada; WestGrid and Compute/Calcul
Canada; Swedish Research Council; Swedish Polar Research Secretariat;
Swedish National Infrastructure for Computing (SNIC); Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz
Alliance for Astroparticle Physics (HAP); Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland; National Research Foundation of Korea
(NRF); Danish National Research Foundation, Denmark (DNRF)
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-office of Polar Programs, U.S. National Science
Foundation-physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; Natural Sciences and Engineering
Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish
Research Council, Swedish Polar Research Secretariat, Swedish National
Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg
Foundation, Sweden; German Ministry for Education and Research (BMBF),
Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for
Astroparticle Physics (HAP), Research Department of Plasmas with Complex
Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO),
FWO Odysseus programme, Flanders Institute to encourage scientific and
technological research in industry (IWT), Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Australian Research Council; Japan Society for Promotion of
Science (JSPS); the Swiss National Science Foundation (SNSF),
Switzerland; National Research Foundation of Korea (NRF); Danish
National Research Foundation, Denmark (DNRF).
NR 44
TC 27
Z9 28
U1 0
U2 15
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 MAY 20
PY 2015
VL 805
IS 1
AR L5
DI 10.1088/2041-8205/805/1/L5
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI4VS
UT WOS:000354752600005
ER
PT J
AU Schopf, JW
Kudryavtsev, AB
Walter, MR
Van Kranendonk, MJ
Williford, KH
Kozdon, R
Valley, JW
Gallardo, VA
Espinoza, C
Flannery, DT
AF Schopf, J. William
Kudryavtsev, Anatoliy B.
Walter, Malcolm R.
Van Kranendonk, Martin J.
Williford, Kenneth H.
Kozdon, Reinhard
Valley, John W.
Gallardo, Victor A.
Espinoza, Carola
Flannery, David T.
TI Reply to Dvorak et al.: Apparent evolutionary stasis of ancient
subseafloor sulfur cycling biocoenoses
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
C1 [Schopf, J. William] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.] Univ Calif Los Angeles, Ctr Study Evolut & Origin Life, Los Angeles, CA 90095 USA.
[Schopf, J. William] Univ Calif Los Angeles, Inst Mol Biol, Los Angeles, CA 90095 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.; Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Astrobiol Res Consortium, Madison, WI 53706 USA.
[Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Walter, Malcolm R.; Van Kranendonk, Martin J.; Flannery, David T.] Univ New S Wales, Australian Ctr Astrobiol, Randwick, NSW 2052, Australia.
[Walter, Malcolm R.; Van Kranendonk, Martin J.; Flannery, David T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Randwick, NSW 2052, Australia.
[Van Kranendonk, Martin J.] Univ New S Wales, Australian Res Council Ctr Excellence, Core Crust Fluid Syst, Randwick, NSW 2052, Australia.
[Williford, Kenneth H.; Flannery, David T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gallardo, Victor A.; Espinoza, Carola] Univ Concepcion, Fac Ciencias Nat & Oceanog, Dept Oceanog, Concepcion, Chile.
RP Schopf, JW (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
EM schopf@ess.ucla.edu
NR 5
TC 0
Z9 0
U1 1
U2 7
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 MAY 19
PY 2015
VL 112
IS 20
BP E2560
EP E2560
DI 10.1073/pnas.1503754112
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CI4OD
UT WOS:000354729500004
PM 25902537
ER
PT J
AU Beebe, M
Wang, L
Madaras, SE
Klopf, JM
Li, Z
Brantley, D
Heimburger, M
Wincheski, RA
Kittiwatanakul, S
Lu, J
Wolf, SA
Lukaszew, RA
AF Beebe, M.
Wang, L.
Madaras, S. E.
Klopf, J. M.
Li, Z.
Brantley, D.
Heimburger, M.
Wincheski, R. A.
Kittiwatanakul, S.
Lu, J.
Wolf, S. A.
Lukaszew, R. A.
TI Surface plasmon resonance modulation in nanopatterned Au gratings by the
insulator-metal transition in vanadium dioxide films
SO OPTICS EXPRESS
LA English
DT Article
ID THIN-FILMS; VO2; METAMATERIALS
AB Correlated experimental and simulation studies on the modulation of Surface Plasmon Polaritons (SPP) in Au/VO2 bilayers are presented. The modification of the SPP wave vector by the thermallyinduced insulator-to-metal phase transition (IMT) in VO2 was investigated by measuring the optical reflectivity of the sample. Reflectivity changes are observed for VO2 when transitioning between the insulating and metallic states, enabling modulation of the SPP in the Au layer by the thermally induced IMT in the VO2 layer. Since the IMT can also be optically induced using ultrafast laser pulses, we postulate the viability of SPP ultrafast modulation for sensing or control. (C)2015 Optical Society of America
C1 [Beebe, M.; Wang, L.; Madaras, S. E.; Klopf, J. M.; Li, Z.; Brantley, D.; Heimburger, M.; Lukaszew, R. A.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Wincheski, R. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Kittiwatanakul, S.; Lu, J.; Wolf, S. A.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA.
[Wolf, S. A.] Univ Virginia, Dept Phys, Charlottesville, VA 22904 USA.
RP Beebe, M (reprint author), Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
EM mrbeebe@email.wm.edu
FU National Science Foundation [NSF-DMR-1006013]; Virginia Microelectronics
Consortium (VMEC)
FX Aspects of this work were supported by a grant from the National Science
Foundation (NSF-DMR-1006013) and by the Virginia Microelectronics
Consortium (VMEC).
NR 19
TC 1
Z9 1
U1 10
U2 66
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD MAY 18
PY 2015
VL 23
IS 10
BP 13222
EP 13229
DI 10.1364/OE.23.013222
PG 8
WC Optics
SC Optics
GA CI4GQ
UT WOS:000354706800072
PM 26074574
ER
PT J
AU Goldstein, R
Burch, JL
Mokashi, P
Broiles, T
Mandt, K
Hanley, J
Cravens, T
Rahmati, A
Samara, M
Clark, G
Hassig, M
Webster, JM
AF Goldstein, R.
Burch, J. L.
Mokashi, P.
Broiles, T.
Mandt, K.
Hanley, J.
Cravens, T.
Rahmati, A.
Samara, M.
Clark, G.
Haessig, M.
Webster, J. M.
TI The Rosetta Ion and Electron Sensor (IES) measurement of the development
of pickup ions from comet 67P/Churyumov-Gerasimenko
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE comets; plasma; pickup
ID SOLAR-WIND; PLASMA CONSORTIUM; CHARGE-EXCHANGE; HALLEY; RPC
AB The Rosetta Ion and Electron Sensor (IES) has been measuring solar wind ions intermittently since exiting from hibernation in May 2014. On 19 August, when Rosetta was similar to 80km from the comet 67P/Churyumov-Gerasimenko, which was similar to 3.5AU from the Sun, IES began to see ions at its lowest energy range, similar to 4-10eV. We identify these as ions created from neutral species emitted by the comet nucleus, photoionized by solar UV radiation in the neighborhood of the Rosetta spacecraft (S/C), and attracted by the small negative potential of the S/C resulting from the population of thermal electrons. Later, IES began to see higher-energy ions that we identify as having been picked up and accelerated by the solar wind. IES continues to measure changes in the solar wind and the development of the pickup ion structure.
C1 [Goldstein, R.; Burch, J. L.; Mokashi, P.; Broiles, T.; Mandt, K.; Hanley, J.; Haessig, M.; Webster, J. M.] Southwest Res Inst, San Antonio, TX 78227 USA.
[Cravens, T.; Rahmati, A.] Univ Kansas, Phys & Astron, Lawrence, KS 66045 USA.
[Samara, M.; Clark, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Haessig, M.] Univ Bern, Inst Phys, Bern, Switzerland.
RP Goldstein, R (reprint author), Southwest Res Inst, San Antonio, TX 78227 USA.
EM rgoldstein@swri.edu
RI Clark, George/L-6433-2015;
OI Broiles, Thomas/0000-0001-6910-2724; Mandt, Kathleen/0000-0001-8397-3315
FU U.S. National Aeronautics and Space Administration [1345493]; Jet
Propulsion Laboratory, California Institute of Technology
FX The data for this work are available from ESA's PSA archive or NASA's
PDS Small Bodies Archive. The work on IES was supported, in part, by the
U.S. National Aeronautics and Space Administration through contract
1345493 with the Jet Propulsion Laboratory, California Institute of
Technology. We thank the teams at Imperial College London and ESA who
have been responsible for the operation of IES.
NR 14
TC 18
Z9 18
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2015
VL 42
IS 9
BP 3093
EP 3099
DI 10.1002/2015GL063939
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300004
ER
PT J
AU Farrell, WM
Hurley, DM
Zimmerman, MI
AF Farrell, W. M.
Hurley, D. M.
Zimmerman, M. I.
TI Spillage of lunar polar crater volatiles onto adjacent terrains: The
case for dynamic processes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Moon; volatiles; craters; water
ID WATER; MOON; ICE
AB We present an investigation of the release and transport of lunar polar crater volatiles onto topside regions surrounding the cold traps. The volatiles are liberated via surface energization processes associated with the harsh space environment, including solar wind plasma sputtering and impact vaporization. We find that some fraction of these volatiles can migrate from crater floors onto topside regions (those regions directly adjacent to and above the polar crater floors), and that these surrounding terrains should contain a sampling of the material originating within the crater itself. It is concluded that the nature of the volatile content on crater floors can be obtained by sampling the surface volatiles that have migrated or spilled out onto the adjacent terrain. This spillage effect could make human or robotic prospecting for crater resources significantly easier, since an assessment may not require direct entry into the very harsh polar crater environment. We also suggest that there are dynamic processes actively operating on the crater floors, and we estimate their source rates assuming dynamic equilibrium of the observed water frost and our modeled loss rates.
C1 [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Farrell, W. M.; Hurley, D. M.; Zimmerman, M. I.] NASA, Solar Syst Explorat Res Virtual Inst, Ames Res Ctr, Moffett Field, CA USA.
[Hurley, D. M.; Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM william.m.farrell@nasa.gov
RI Hurley, Dana/F-4488-2015; Farrell, William/I-4865-2013
OI Hurley, Dana/0000-0003-1052-1494;
FU Solar System Exploration Research Virtual Institute (SSERVI)
FX The data presented is from a set of Interactive Data Language (IDL)
custom-coded models that are maintained by the authors and available
upon request. We gratefully acknowledge funding for this work from the
Solar System Exploration Research Virtual Institute (SSERVI) and
encouragement from its director Yvonne Pendleton. We also thank David
Goldstein and Raul Baragiola who generously provided thoughtful
discussion following our presentation to "SSERVI's Friends of Lunar
Volatiles" focus group.
NR 18
TC 1
Z9 1
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2015
VL 42
IS 9
BP 3160
EP 3165
DI 10.1002/2015GL063200
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300012
ER
PT J
AU Mazarico, E
Genova, A
Neumann, GA
Smith, DE
Zuber, MT
AF Mazarico, Erwan
Genova, Antonio
Neumann, Gregory A.
Smith, David E.
Zuber, Maria T.
TI Simulated recovery of Europa's global shape and tidal Love numbers from
altimetry and radio tracking during a dedicated flyby tour
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Europa; tide; altimetry; flyby; gravity
ID GRAVITY-FIELD; LASER ALTIMETRY; ICE SHELL; TOPOGRAPHY; TITAN; MARS;
MERCURY
AB The fundamental scientific objectives for future spacecraft exploration of Jupiter's moon Europa include confirmation of the existence of subsurface ocean beneath the surface ice shell and constraints on the physical properties of the ocean. Here we conduct a comprehensive simulation of a multiple-flyby mission. We demonstrate that radio tracking data can provide an estimate of the gravitational tidal Love number k(2) with sufficient precision to confirm the presence of a liquid layer. We further show that a capable long-range laser altimeter can improve determination of the spacecraft position, improve the k(2) determination (<1% error), and enable the estimation of the planetary shape and Love number h(2) (3-4% error), which is directly related to the amplitude of the surface tidal deformation. These measurements, in addition to the global shape accurately constrained by the long altimetric profiles, can yield further constraints on the interior structure of Europa.
C1 [Mazarico, Erwan; Genova, Antonio; Neumann, Gregory A.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Genova, Antonio; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Mazarico, E (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM erwan.m.mazarico@nasa.gov
RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014; Genova,
Antonio/M-1400-2016
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X; Genova, Antonio/0000-0001-5584-492X
FU NASA
FX We acknowledge the NASA support of the simulation effort by the Europa
Pre-Project, through a grant to MIT. We thank F. Nimmo (UCSC) for
providing the topographic models. The simulation was performed using the
trajectory made available for the ICEE proposal
(http://solarsystem.nasa.gov/europa/iceedocs.cfm).
NR 41
TC 1
Z9 1
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2015
VL 42
IS 9
BP 3166
EP 3173
DI 10.1002/2015GL063224
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300013
ER
PT J
AU Hand, KP
Carlson, RW
AF Hand, K. P.
Carlson, R. W.
TI Europa's surface color suggests an ocean rich with sodium chloride
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE planetary science; Europa; Jupiter; astrobiology
ID GALILEAN SATELLITES; SUBSURFACE OCEAN; EXCESS ELECTRONS;
RADIATION-DAMAGE; HALIDE CLUSTERS; MU-M; NACL; CONSTRAINTS; ABSORPTION;
FLUXES
AB The composition of Europa's surface may be representative of the subsurface ocean; however, considerable debate persists regarding the endogenous or exogenous nature of a hydrated sulfate feature on Europa. Direct evidence of oceanic salts on Europa's surface has been largely inconclusive. We show that the observed color within geologically young features on Europa's surface can be explained by sodium chloride delivered from the ocean below. We find that sodium chloride, when exposed to Europa surface conditions, accumulates electrons in F and M centers, yielding a yellow-brown discoloration comparable to Europa's surface. Irradiation of sodium chloride from Europa's ocean thus provides a simple and elegant solution to the color of the non-ice material observed on Europa. This evidence for endogenous salts suggests that Europa's ocean is interacting with a silicate seafloor, a critical consideration for assessing habitability.
C1 [Hand, K. P.; Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM khand@jpl.nasa.gov
FU National Aeronautics and Space Administration; internal Research and
Technology Development program; Instrument Concepts for Europa
Exploration program within the National Aeronautics and Space
Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and funded in part through the
internal Research and Technology Development program. R.W.C. and K.P.H.
acknowledge support from the Instrument Concepts for Europa Exploration
program within the National Aeronautics and Space Administration. Data
presented in this manuscript, including spectra and images from our
laboratory experiments, are freely available by contacting K.P. Hand at
khand@jpl.nasa.gov.
NR 29
TC 14
Z9 14
U1 3
U2 27
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 MAY 16
PY 2015
VL 42
IS 9
BP 3174
EP 3178
DI 10.1002/2015GL063559
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300014
ER
PT J
AU Schnepf, NR
Kuvshinov, A
Sabaka, T
AF Schnepf, N. R.
Kuvshinov, A.
Sabaka, T.
TI Can we probe the conductivity of the lithosphere and upper mantle using
satellite tidal magnetic signals?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE geomagnetic induction; electrical properties; satellite magnetics;
marine electromagnetics; ocean tides; composition of the crust and
mantle
ID ELECTRICAL-CONDUCTIVITY; WATER-CONTENT; ELECTROMAGNETIC INDUCTION;
GLOBAL INDUCTION; OBSERVATORY DATA; DOMAIN APPROACH; EARTHS MANTLE;
INVERSION; PACIFIC; FIELDS
AB A few studies convincingly demonstrated that the magnetic fields induced by the lunar semidiurnal (M2) ocean flow can be identified in satellite observations. This result encourages using M2 satellite magnetic data to constrain subsurface electrical conductivity in oceanic regions. Traditional satellite-based induction studies using signals of magnetospheric origin are mostly sensitive to conducting structures because of the inductive coupling between primary and induced sources. In contrast, galvanic coupling from the oceanic tidal signal allows for studying less conductive, shallower structures. We perform global 3-D electromagnetic numerical simulations to investigate the sensitivity of M2 signals to conductivity distributions at different depths. The results of our sensitivity analysis suggest it will be promising to use M2 oceanic signals detected at satellite altitude for probing lithospheric and upper mantle conductivity. Our simulations also suggest that M2 seafloor electric and magnetic field data may provide complementary details to better constrain lithospheric conductivity.
C1 [Schnepf, N. R.] MIT, Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Kuvshinov, A.] ETH, Inst Geophys, CH-8093 Zurich, Switzerland.
[Sabaka, T.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Schnepf, NR (reprint author), MIT, Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM nschnepf@mit.edu
FU NSF
FX N.R.S. would like to thank the NSF Graduate Research Fellowship Program
for support. The CM5 data used here may be obtained by contacting T. J.
Sabaka (terence.j.sabaka@nasa.gov) and the model output may be obtained
by contacting N. R. Schnepf (nschnepf@mit.edu).
NR 36
TC 4
Z9 4
U1 1
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2015
VL 42
IS 9
BP 3233
EP 3239
DI 10.1002/2015GL063540
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300022
ER
PT J
AU Hall, T
Hereid, K
AF Hall, Timothy
Hereid, Kelly
TI The frequency and duration of US hurricane droughts
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE hurricanes; statistical modeling; risk analysis
ID TROPICAL CYCLONE TRACKS; RISK
AB As of the end of the 2014 hurricane season, the U.S. has experienced no major hurricane landfall since Hurricane Wilma in 2005, a drought that currently stands at 9years. Here we use a stochastic tropical cyclone model to calculate the mean waiting time for multiyear landfall droughts. We estimate that the mean time to wait for a 9year drought is 177years. We also find that the average probability of ending the drought with a major landfall in the next year is 0.39 and is independent of the drought duration, as one would expect for a Bernoulli process.
C1 [Hall, Timothy] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hereid, Kelly] ACE Tempest Re, Stamford, CT USA.
RP Hall, T (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM timothy.m.hall@nasa.gov
OI Hereid, Kelly/0000-0003-0322-2664
FU NASA National Climate Assessment Award
FX This work was supported in part by a NASA National Climate Assessment
Award. Data used for the analysis are publicly available and maintained
by the Hurricane Research Division of NOAA.
NR 10
TC 4
Z9 4
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2015
VL 42
IS 9
BP 3482
EP 3485
DI 10.1002/2015GL063652
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300052
ER
PT J
AU Saide, PE
Peterson, DA
da Silva, A
Anderson, B
Ziemba, LD
Diskin, G
Sachse, G
Hair, J
Butler, C
Fenn, M
Jimenez, JL
Campuzano-Jost, P
Perring, AE
Schwarz, JP
Markovic, MZ
Russell, P
Redemann, J
Shinozuka, Y
Streets, DG
Yan, F
Dibb, J
Yokelson, R
Toon, OB
Hyer, E
Carmichael, GR
AF Saide, Pablo E.
Peterson, David A.
da Silva, Arlindo
Anderson, Bruce
Ziemba, Luke D.
Diskin, Glenn
Sachse, Glen
Hair, Johnathan
Butler, Carolyn
Fenn, Marta
Jimenez, Jose L.
Campuzano-Jost, Pedro
Perring, Anne E.
Schwarz, Joshua P.
Markovic, Milos Z.
Russell, Phil
Redemann, Jens
Shinozuka, Yohei
Streets, David G.
Yan, Fang
Dibb, Jack
Yokelson, Robert
Toon, O. Brian
Hyer, Edward
Carmichael, Gregory R.
TI Revealing important nocturnal and day-to-day variations in fire smoke
emissions through a multiplatform inversion
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE inversion; fire emissions; biomass burning; SEAC4RS; WRF-Chem; AERONET
ID BIOMASS BURNING EMISSIONS; AEROSOL OPTICAL DEPTH; HIGH-RESOLUTION;
ORGANIC AEROSOL; UNITED-STATES; MODEL; FOREST; CARBON; WILDFIRES;
INDONESIA
AB We couple airborne, ground-based, and satellite observations; conduct regional simulations; and develop and apply an inversion technique to constrain hourly smoke emissions from the Rim Fire, the third largest observed in California, USA. Emissions constrained with multiplatform data show notable nocturnal enhancements (sometimes over a factor of 20), correlate better with daily burned area data, and are a factor of 2-4 higher than a priori estimates, highlighting the need for improved characterization of diurnal profiles and day-to-day variability when modeling extreme fires. Constraining only with satellite data results in smaller enhancements mainly due to missing retrievals near the emissions source, suggesting that top-down emission estimates for these events could be underestimated and a multiplatform approach is required to resolve them. Predictions driven by emissions constrained with multiplatform data present significant variations in downwind air quality and in aerosol feedback on meteorology, emphasizing the need for improved emissions estimates during exceptional events.
C1 [Saide, Pablo E.; Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
[Peterson, David A.] CNR, Monterey, CA USA.
[da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Bruce; Ziemba, Luke D.; Diskin, Glenn; Hair, Johnathan; Butler, Carolyn; Fenn, Marta] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Sachse, Glen] Natl Inst Aerosp, Hampton, VA USA.
[Jimenez, Jose L.; Campuzano-Jost, Pedro] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Jimenez, Jose L.; Campuzano-Jost, Pedro] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Perring, Anne E.; Schwarz, Joshua P.; Markovic, Milos Z.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Russell, Phil; Redemann, Jens] NASA Ames, Moffett Field, CA USA.
[Shinozuka, Yohei] NASA, Ames Res Ctr, Cooperat Res Earth Sci & Technol, Moffett Field, CA 94035 USA.
[Shinozuka, Yohei] Bay Area Environm Res Inst, Petaluma, CA USA.
[Streets, David G.; Yan, Fang] Argonne Natl Lab, Div Energy Syst, Argonne, IL 60439 USA.
[Dibb, Jack] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Yokelson, Robert] Univ Montana, Dept Chem, Missoula, MT 59812 USA.
[Toon, O. Brian] Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Hyer, Edward] Naval Res Lab, Marine Meteorol Div, Monterey, CA USA.
RP Saide, PE (reprint author), Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
EM pablo-saide@uiowa.edu
RI Yokelson, Robert/C-9971-2011; Hyer, Edward/E-7734-2011; Perring,
Anne/G-4597-2013; Jimenez, Jose/A-5294-2008; peterson,
david/L-2350-2016; schwarz, joshua/G-4556-2013; Manager, CSD
Publications/B-2789-2015
OI Yokelson, Robert/0000-0002-8415-6808; Hyer, Edward/0000-0001-8636-2026;
Perring, Anne/0000-0003-2231-7503; Jimenez, Jose/0000-0001-6203-1847;
schwarz, joshua/0000-0002-9123-2223;
FU NSF [1049140 NCE]; NASA [NNX11AI52G, NNH12AT27i, NNX12AC03G, NNX12AC20G,
NNX12AC64G]; EPA [83503701]; National Center for Research Resources, a
part of the National Institutes of Health [UL1RR024979]
FX We thank all SEAC4RS participants that made the field experiment
possible, especially Project Manager Hal Maring. We also thank Brent
Holben, Patrick Arnott, Min Hao, Craig Coburn, Adriana Predoi-Cross, and
their staff for establishing and maintaining the AERONET sites used in
this investigation. This work was carried out with the aid of NSF grant
1049140 NCE; NASA grants NNX11AI52G, NNH12AT27i, NNX12AC03G, NNX12AC20G,
and NNX12AC64G; EPA grant 83503701; and grant number UL1RR024979 from
the National Center for Research Resources, a part of the National
Institutes of Health. Its contents are solely the responsibility of the
authors and do not necessarily represent the official views of the
funding institutions. Contact P. E. Saide (pablo-saide@uiowa.edu) or G.
R. Carmichael (gregory-carmichael@uiowa.edu) for data requests.
NR 50
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Z9 10
U1 8
U2 44
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 MAY 16
PY 2015
VL 42
IS 9
BP 3609
EP 3618
DI 10.1002/2015GL063737
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CK0EM
UT WOS:000355878300069
ER
PT J
AU He, Y
Risi, C
Gao, J
Masson-Delmotte, V
Yao, TD
Lai, CT
Ding, YJ
Worden, J
Frankenberg, C
Chepfer, H
Cesana, G
AF He, You
Risi, Camille
Gao, Jing
Masson-Delmotte, Valerie
Yao, Tandong
Lai, Chun-Ta
Ding, Yongjian
Worden, John
Frankenberg, Christian
Chepfer, Helene
Cesana, Gregory
TI Impact of atmospheric convection on south Tibet summer precipitation
isotopologue composition using a combination of in situ measurements,
satellite data, and atmospheric general circulation modeling
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE precipitation isotopic composition; Tibetan Plateau; Indian monsoon;
Rayleigh distillation; atmospheric general circulation modeling
ID WATER-VAPOR; ICE CORES; DELTA-D; ISOTOPIC COMPOSITION; STABLE-ISOTOPES;
DEEP CONVECTION; ASIAN MONSOON; PLATEAU; CLIMATE; RESOLUTION
AB Precipitation isotopologues recorded in natural archives from the southern Tibetan Plateau may document past variations of Indian monsoon intensity. The exact processes controlling the variability of precipitation isotopologue composition must therefore first be deciphered and understood. This study investigates how atmospheric convection affects the summer variability of O-18 in precipitation (O-18(p)) and D in water vapor (D-v) at the daily scale. This is achieved using isotopic data from precipitation samples at Lhasa, isotopic measurements of water vapor retrieved from satellites (Tropospheric Emission Spectrometer (TES), GOSAT) and atmospheric general circulation modeling. We reveal that both O-18(p) and D-v at Lhasa are well correlated with upstream convective activity, especially above northern India. First, during days of strong convection, northern India surface air contains large amounts of vapor with relatively low D-v. Second, when this low-D-v moisture is uplifted toward southern Tibet, this initial depletion in HDO is further amplified by Rayleigh distillation as the vapor moves over the Himalayan. The intraseasonal variability of the isotopologue composition of vapor and precipitation over the southern Tibetan Plateau results from these processes occurring during air mass transportation.
C1 [He, You; Ding, Yongjian] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Beijing, Peoples R China.
[He, You; Gao, Jing; Yao, Tandong] Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Tibetan Environm Changes & Land Surface, Beijing, Peoples R China.
[He, You; Risi, Camille; Chepfer, Helene; Cesana, Gregory] CNRS, Inst Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France.
[Gao, Jing; Yao, Tandong] Chinese Acad Sci, CAS Ctr Excellence Tibetan Plateau Earth Sci, Beijing, Peoples R China.
[Masson-Delmotte, Valerie] CEA, CNRS, Lab Sci Climat & Environm, Inst Pierre Simon Laplace,UVSQ,UMR 8212, F-91198 Gif Sur Yvette, France.
[Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA.
[Worden, John; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Gao, J (reprint author), Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Tibetan Environm Changes & Land Surface, Beijing, Peoples R China.
EM JingGao@itpcas.ac.cn
RI Masson-Delmotte, Valerie/G-1995-2011; Frankenberg, Christian/A-2944-2013
OI Masson-Delmotte, Valerie/0000-0001-8296-381X; Frankenberg,
Christian/0000-0002-0546-5857
FU CAS [XDB03030100]; National Natural Science Foundation of China
[41471053, 41190080]; China-France Caiyuanpei Program; National
Aeronautics and Space Administration; U.S. National Science Foundation,
Division of Atmospheric and Geo-space Sciences [AGS-0956425]
FX This work is supported by CAS Strategic Priority Research
Program(B)-Interactions among Multiple Geo-spheres on Tibetan Plateau
and their Resource-Environment Effects (grant XDB03030100), by the
National Natural Science Foundation of China (grants 41471053 and
41190080), and by the China-France Caiyuanpei Program. This work was
finished in Laboratoire de Meteorologie Dynamique, Institut Pierre Simon
Laplace, CNRS, Paris, France. LMDZ simulations were performed on the
supercomputer of the IDRIS computing center. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. C.-T Lai was supported by the U.S. National Science
Foundation, Division of Atmospheric and Geo-space Sciences under Grant
AGS-0956425. We thank Laurent Li and Pang Hongxi for their constructive
comments. We also thank the staffs from Tibet observation stations for
collecting the samples and staffs for measuring the samples, and all
those who contributed to the field work. Part of in situ
delta18Op data are from Third Pole Environment
Database (http://en.tpedatabase.cn/). The back trajectories and the OLR
(Outgoing Longwave Radiation) are computed using National Centers for
Environmental Prediction (NCEP) reanalysis data. LMDZiso data can be
acquired by contacting Camille Risi (Camille.Risi@lmd.jussieu.fr). TES
and GOSAT satellite data can also be acquired by contacting John Worden
(john.r.worden@jpl.nasa.gov). CALIPSO data can also be acquired by
contacting Gregory Cesana (gregory.cesana@lmd.polytechnique.fr). In situ
delta18Op data can also be acquired by contacting
Gao Jing (gaojing@itpcas.ac.cn).
NR 80
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U1 3
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 16
PY 2015
VL 120
IS 9
BP 3852
EP 3871
DI 10.1002/2014JD022180
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800016
ER
PT J
AU Battaglia, A
Tanelli, S
Mroz, K
Tridon, F
AF Battaglia, A.
Tanelli, S.
Mroz, K.
Tridon, F.
TI Multiple scattering in observations of the GPM dual-frequency
precipitation radar: Evidence and impact on retrievals
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE radar; GPM-DPR; multiple scattering; graupel
ID SURFACE REFERENCE TECHNIQUE; RAIN-PROFILING ALGORITHM; PART II;
APPROXIMATION; ATTENUATION; CONVECTION; RANGE; OCEAN
AB This paper illustrates how multiple scattering signatures affect Global Precipitation Measuring (GPM) Mission Dual-Frequency Precipitation Radar (DPR) Ku and Ka band reflectivity measurements and how they are consistent with prelaunch assessments based on theoretical considerations and confirmed by airborne observations. In particular, in the presence of deep convection, certain characteristics of the dual-wavelength reflectivity profiles cannot be explained with single scattering, whereas they are readily explained by multiple-scattering theory. Examples of such signatures are the absence of surface reflectivity peaks and anomalously small reflectivity slopes in the lower troposphere. These findings are relevant for DPR-based rainfall retrievals and stratiform/convective classification algorithms when dealing with deep convective regions. A path to refining the rainfall inversion problem is proposed by adopting a methodology based on a forward operator which accounts for multiple scattering. A retrieval algorithm based on this methodology is applied to a case study over Africa, and it is compared to the standard DPR products obtained with the at-launch version of the standard algorithms.
C1 [Battaglia, A.] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.
[Battaglia, A.; Mroz, K.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester LE1 7RH, Leics, England.
[Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Battaglia, A (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.
EM a.battaglia@leicester.ac.uk
RI Measurement, Global/C-4698-2015; Tridon, Frederic/M-4127-2013;
OI Tridon, Frederic/0000-0002-0436-283X; Battaglia,
Alessandro/0000-0001-9243-3484
FU project "Calibration and validation studies over the North Atlantic and
UK for the Global Precipitation Mission," by the UK NERC [NE/L007169/1];
National Aeronautics and Space Administration
FX The work done by A. Battaglia and F. Tridon was funded by the project
"Calibration and validation studies over the North Atlantic and UK for
the Global Precipitation Mission," which was funded by the UK NERC
(NE/L007169/1). The work done by S. Tanelli was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work was carried out for the GPM mission under the Precipitation
Measurement Missions program, and support by Ramesh Kakar is gratefully
acknowledged. V03B-GPM and MSG data were downloaded from the
Precipitation Processing System (DOI 10.5067/GPM/DPR/DPR/2A,
10.5067/GPM/DPR/Ku/2A, and 10.5067/GPM/DPR/Ka/2A for the 2A-DPR, 2A-Ku,
and 2A-Ka, respectively) and the EumetSat Earth Observation Portal,
respectively. The forward radar model code was courteously provided by
R. Hogan (http://www.met.rdg.ac.uk/clouds/multiscatter/).
NR 35
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Z9 7
U1 4
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 16
PY 2015
VL 120
IS 9
BP 4090
EP 4101
DI 10.1002/2014JD022866
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800030
ER
PT J
AU Cho, HM
Zhang, ZB
Meyer, K
Lebsock, M
Platnick, S
Ackerman, AS
Di Girolamo, L
C-Labonnote, L
Cornet, C
Riedi, J
Holz, RE
AF Cho, Hyoun-Myoung
Zhang, Zhibo
Meyer, Kerry
Lebsock, Matthew
Platnick, Steven
Ackerman, Andrew S.
Di Girolamo, Larry
C-Labonnote, Laurent
Cornet, Celine
Riedi, Jerome
Holz, Robert E.
TI Frequency and causes of failed MODIS cloud property retrievals for
liquid phase clouds over global oceans
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE MODIS; cloud; failure; inhomogeneity; drizzle; A-Train
ID CALIPSO LIDAR MEASUREMENTS; VIEW-ANGLE DEPENDENCE; SOLAR ZENITH ANGLE;
SATELLITE-OBSERVATIONS; OPTICAL-THICKNESS; ATTENUATED BACKSCATTER;
INSTRUMENT SIMULATORS; WATER CLOUDS; AEROSOLS; DEPOLARIZATION
AB Moderate Resolution Imaging Spectroradiometer (MODIS) retrieves cloud droplet effective radius (r(e)) and optical thickness () by projecting observed cloud reflectances onto a precomputed look-up table (LUT). When observations fall outside of the LUT, the retrieval is considered failed because no combination of and r(e) within the LUT can explain the observed cloud reflectances. In this study, the frequency and potential causes of failed MODIS retrievals for marine liquid phase (MLP) clouds are analyzed based on 1year of Aqua MODIS Collection 6 products and collocated CALIOP and CloudSat observations. The retrieval based on the 0.86 mu m and 2.1 mu m MODIS channel combination has an overall failure rate of about 16% (10% for the 0.86 mu m and 3.7 mu m combination). The failure rates are lower over stratocumulus regimes and higher over the broken trade wind cumulus regimes. The leading type of failure is the r(e) too large failure accounting for 60%-85% of all failed retrievals. The rest is mostly due to the r(e) too small or retrieval failures. Enhanced retrieval failure rates are found when MLP cloud pixels are partially cloudy or have high subpixel inhomogeneity, are located at special Sun-satellite viewing geometries such as sunglint, large viewing or solar zenith angles, or cloudbow and glory angles, or are subject to cloud masking, cloud overlapping, and/or cloud phase retrieval issues. The majority (more than 84%) of failed retrievals along the CALIPSO track can be attributed to at least one or more of these potential reasons. The collocated CloudSat radar reflectivity observations reveal that the remaining failed retrievals are often precipitating. It remains an open question whether the extremely large r(e) values observed in these clouds are the consequence of true cloud microphysics or still due to artifacts not included in this study.
C1 [Cho, Hyoun-Myoung; Zhang, Zhibo] Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
[Meyer, Kerry; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meyer, Kerry] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Di Girolamo, Larry] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA.
[C-Labonnote, Laurent; Cornet, Celine; Riedi, Jerome] Univ Sci & Technol Lille, Lab Opt Atmospher, CNRS, Villeneuve Dascq, France.
[Holz, Robert E.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
RP Zhang, ZB (reprint author), Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
EM zhibo.zhang@umbc.edu
RI Zhang, Zhibo/D-1710-2010; Meyer, Kerry/E-8095-2016; Platnick,
Steven/J-9982-2014
OI Zhang, Zhibo/0000-0001-9491-1654; Meyer, Kerry/0000-0001-5361-9200;
Platnick, Steven/0000-0003-3964-3567
FU NASA [NNX11AI98G, NNX14AJ25G]; U.S. National Science Foundation through
the MRI program [CNS-0821258, CNS-1228778]; SCREMS program
[DMS-0821311]; UMBC
FX This research is supported by NASA grants NNX11AI98G and NNX14AJ25G
managed by Richard Eckman. Zhibo Zhang would like to thank Gala Wind,
Thomas Arnold, and Nandana Amarasinghe for their help on MODIS C6 data.
The computations in this study were performed on UMBC High Performance
Computing Facility (HPCF). The facility is supported by the U.S.
National Science Foundation through the MRI program (grants CNS-0821258
and CNS-1228778) and the SCREMS program (grant DMS-0821311), with
additional substantial support from UMBC. The MODIS data are obtained
from NASA's Level 1 and Atmosphere Archive and Distribution System
(LAADS http://ladsweb.nascom.nasa.gov/). The CALIOP data are obtained
from NASA' Atmospheric Science Data Center (ASDC,
https://eosweb.larc.nasa.gov/). The CloudSat data are obtained from
CloudSat data processing center
(http://www.cloudsat.cira.colostate.edu/dataHome.php).
NR 65
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Z9 12
U1 3
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 MAY 16
PY 2015
VL 120
IS 9
BP 4132
EP 4154
DI 10.1002/2015JD023161
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800033
ER
PT J
AU Huang, L
Jiang, JH
Wang, Z
Su, H
Deng, M
Massie, S
AF Huang, Lei
Jiang, Jonathan H.
Wang, Zhien
Su, Hui
Deng, Min
Massie, Steven
TI Climatology of cloud water content associated with different cloud types
observed by A-Train satellites
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE cloud climatology; cloud water content; cloud type; cloud fraction;
cloud profile
ID TRANSPORT PATHWAYS; UPPER TROPOSPHERE; PRECIPITATION; DISTRIBUTIONS;
VALIDATION; PRODUCTS; CAMPAIGN; RADAR; CO
AB This study investigates the climatology of vertical distributions of cloud liquid water content, ice water content, and cloud fraction (CFR) associated with eight different cloud types, by utilizing the combined CloudSat radar and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations lidar measurements. The geographical and seasonal variations of these cloud properties for each cloud type are also analyzed. The cloud water content (CWC) of each cloud type is sorted by three parameters obtained from colocated satellite observations to investigate the relationships between large-scale conditions and the vertical structure of clouds. Results show that different cloud types have different altitudes of CWC and CFR peaks, and the altitude of CFR peak does not always overlap with that of CWC peak. Each type of cloud shows a clear asymmetric pattern of spatial distribution between Northern Hemisphere (NH) and Southern Hemisphere (SH). Stratocumulus and stratus clouds make the greatest contribution to the liquid water path, while the ice water path is mostly contributed by deep convective cloud over the tropics and nimbostratus over the middle and high latitudes. Over both middle and high latitudes, clouds have larger seasonal variation in the NH than in the SH. Over ocean, large CWCs of deep convective cloud, cirrus, and altostratus are above 7 km, and are associated with high convective available potential energy (>2000J/kg), warm sea surface temperature (>303 K), and relatively high precipitation (>1mm/h). Over land, most of the middle and high clouds have similar CWC distributions compared to those over ocean, but altocumulus and low clouds are quite different from those over ocean.
C1 [Huang, Lei; Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Zhien; Deng, Min] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Massie, Steven] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
RP Huang, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Lei.Huang@jpl.nasa.gov
RI Wang, Zhien/F-4857-2011
FU NASA AST program; NASA MAP program; NASA CloudSat/CALIPSO program
FX This research is supported by the NASA AST, MAP, and CloudSat/CALIPSO
programs. The study was performed at NASA Jet Propulsion Laboratory
(JPL) at the California Institute of Technology, under contract with
NASA. We thank Gerald G. Mace for useful discussions. We also appreciate
the comments from three anonymous reviewers that led to significant
improvements of this paper. The CloudSat Level 2 data sets are obtained
from the CloudSat Data Processing Center, located at the Cooperative
Institute for Research in the Atmosphere at Colorado State University.
The SST data are obtained from the Remote Sensing Systems
(http://www.remss.com). AIRS Level 3 products are obtained from AIRS
Data Server
(http://disc.sci.gsfc.nasa.gov/AIRS/data-holdings/by-data-product-v5/air
sL3_STD_AIRS_AMSU.shtml). TRMM precipitation data are obtained from GES
DISC
(http://mirador.gsfc.nasa.gov/cgi-bin/mirador/homepageAlt.pl?keyword=3B4
2).
NR 49
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 16
PY 2015
VL 120
IS 9
BP 4196
EP 4212
DI 10.1002/2014JD022779
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800036
ER
PT J
AU Kahn, RA
Gaitley, BJ
AF Kahn, Ralph A.
Gaitley, Barbara J.
TI An analysis of global aerosol type as retrieved by MISR
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol remote sensing; aerosol type; multiangle imaging; MISR; particle
pollution; desert dust
ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; SIZE DISTRIBUTIONS;
IN-SITU; DUST; SENSITIVITY; AERONET; COMPONENT; NETWORK; MODELS
AB In addition to aerosol optical depth (AOD), aerosol type is required globally for climate forcing calculations, constraining aerosol transport models and other applications. However, validating satellite aerosol-type retrievals is more challenging than testing AOD results, because aerosol type is a more complex quantity, and ground truth data are far less numerous and generally not as robust. We evaluate the Multiangle Imaging Spectroradiometer (MISR) Version 22 aerosol-type retrievals by assessing product self-consistency on a regional basis and by making comparisons with general expectation and with the Aerosol Robotic Network aerosol-type climatology, as available. The results confirm and add detail to the observation that aerosol-type discrimination improves dramatically where midvisible AOD exceeds about 0.15 or 0.2. When the aerosol-type information content of the observations is relatively low, increased scattering-angle range improves particle-type sensitivity. The MISR standard, operational product discriminates among small, medium, and large particles and exhibits qualitative sensitivity to single-scattering albedo (SSA) under good aerosol-type retrieval conditions, providing a categorical aerosol-type classification. MISR angstrom ngstrom exponent deviates systematically from ground truth where particle types missing from the algorithm climatology are present, or where cloud contamination is likely to occur, and SSA tends to be overestimated where absorbing particles are found. We determined that the number of mixtures passing the algorithm acceptance criteria (#SuccMix) represents aerosol-type retrieval quality effectively, providing a useful aerosol-type quality flag.
C1 [Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Gaitley, Barbara J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kahn, RA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM Ralph.Kahn@nasa.gov
FU NASA; EOS-MISR
FX We thank our colleagues on the Jet Propulsion Laboratory's MISR
instrument team and at the NASA Langley Research Center's Atmospheric
Sciences Data Center for their roles in producing the MISR data sets
(available from http://eosweb.larc.nasa.gov), and Brent Holben, Tom Eck,
and the AERONET scientists for the validation data sets used in this
study (available from http://aeronet.gsfc.nasa.gov). We also thank Tom
Eck, James Limbacher, Lauren Zamora, David Diner, Michael Garay, and two
anonymous reviewers for their comments on early versions of the
manuscript. The work of R. Kahn is supported in part by NASA's Climate
and Radiation Research and Analysis Program, under H. Maring, NASA's
Atmospheric Composition Program under R. Eckman, and the EOS-MISR
project.
NR 70
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 16
PY 2015
VL 120
IS 9
BP 4248
EP 4281
DI 10.1002/2015JD023322
PG 34
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800039
ER
PT J
AU de Gouw, JA
McKeen, SA
Aikin, KC
Brock, CA
Brown, SS
Gilman, JB
Graus, M
Hanisco, T
Holloway, JS
Kaiser, J
Keutsch, FN
Lerner, BM
Liao, J
Markovic, MZ
Middlebrook, AM
Min, KE
Neuman, JA
Nowak, JB
Peischl, J
Pollack, IB
Roberts, JM
Ryerson, TB
Trainer, M
Veres, PR
Warneke, C
Welti, A
Wolfe, GM
AF de Gouw, J. A.
McKeen, S. A.
Aikin, K. C.
Brock, C. A.
Brown, S. S.
Gilman, J. B.
Graus, M.
Hanisco, T.
Holloway, J. S.
Kaiser, J.
Keutsch, F. N.
Lerner, B. M.
Liao, J.
Markovic, M. Z.
Middlebrook, A. M.
Min, K. -E.
Neuman, J. A.
Nowak, J. B.
Peischl, J.
Pollack, I. B.
Roberts, J. M.
Ryerson, T. B.
Trainer, M.
Veres, P. R.
Warneke, C.
Welti, A.
Wolfe, G. M.
TI Airborne measurements of the atmospheric emissions from a fuel ethanol
refinery
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE fuel ethanol
ID ORGANIC-COMPOUND EMISSIONS; LAND-USE CHANGE; CELLULOSIC ETHANOL;
GASOLINE VEHICLES; OZONE FORMATION; BIOFUEL CROPS; AIR-QUALITY; IMPACTS;
CULTIVATION; REDUCTION
AB Ethanol made from corn now constitutes approximately 10% of the fuel used in gasoline vehicles in the U.S. The ethanol is produced in over 200 fuel ethanol refineries across the nation. We report airborne measurements downwind from Decatur, Illinois, where the third largest fuel ethanol refinery in the U.S. is located. Estimated emissions are compared with the total point source emissions in Decatur according to the 2011 National Emissions Inventory (NEI-2011), in which the fuel ethanol refinery represents 68.0% of sulfur dioxide (SO2), 50.5% of nitrogen oxides (NOx=NO+NO2), 67.2% of volatile organic compounds (VOCs), and 95.9% of ethanol emissions. Emissions of SO2 and NOx from Decatur agreed with NEI-2011, but emissions of several VOCs were underestimated by factors of 5 (total VOCs) to 30 (ethanol). By combining the NEI-2011 with fuel ethanol production numbers from the Renewable Fuels Association, we calculate emission intensities, defined as the emissions per ethanol mass produced. Emission intensities of SO2 and NOx are higher for plants that use coal as an energy source, including the refinery in Decatur. By comparing with fuel-based emission factors, we find that fuel ethanol refineries have lower NOx, similar VOC, and higher SO2 emissions than from the use of this fuel in vehicles. The VOC emissions from refining could be higher than from vehicles, if the underestimated emissions in NEI-2011 downwind from Decatur extend to other fuel ethanol refineries. Finally, chemical transformations of the emissions from Decatur were observed, including formation of new particles, nitric acid, peroxyacyl nitrates, aldehydes, ozone, and sulfate aerosol.
C1 [de Gouw, J. A.; McKeen, S. A.; Aikin, K. C.; Brock, C. A.; Brown, S. S.; Gilman, J. B.; Graus, M.; Holloway, J. S.; Lerner, B. M.; Liao, J.; Markovic, M. Z.; Middlebrook, A. M.; Min, K. -E.; Neuman, J. A.; Nowak, J. B.; Peischl, J.; Pollack, I. B.; Roberts, J. M.; Ryerson, T. B.; Trainer, M.; Veres, P. R.; Warneke, C.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[de Gouw, J. A.; McKeen, S. A.; Aikin, K. C.; Gilman, J. B.; Graus, M.; Holloway, J. S.; Lerner, B. M.; Liao, J.; Markovic, M. Z.; Min, K. -E.; Neuman, J. A.; Nowak, J. B.; Peischl, J.; Pollack, I. B.; Veres, P. R.; Warneke, C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[de Gouw, J. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Graus, M.] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria.
[Hanisco, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kaiser, J.] Univ Wisconsin, Madison, WI USA.
[Keutsch, F. N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Markovic, M. Z.] Environm Canada, Air Qual Proc Res Div, Toronto, ON, Canada.
[Min, K. -E.] Gwangju Inst Sci & Technol, Gwangju, South Korea.
[Nowak, J. B.] Aerodyne Res Inc, Billerica, MA USA.
[Welti, A.] ETH, Zurich, Switzerland.
[Wolfe, G. M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP de Gouw, JA (reprint author), NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
EM Joost.deGouw@noaa.gov
RI Kaiser, Jennifer/N-7732-2014; Lerner, Brian/H-6556-2013; Brown,
Steven/I-1762-2013; Trainer, Michael/H-5168-2013; Gilman,
Jessica/E-7751-2010; Manager, CSD Publications/B-2789-2015; Pollack,
Ilana/F-9875-2012; Roberts, James/A-1082-2009; Warneke,
Carsten/E-7174-2010; Aikin, Kenneth/I-1973-2013; Middlebrook,
Ann/E-4831-2011; Veres, Patrick/E-7441-2010; Neuman, Andy/A-1393-2009;
Nowak, John/B-1085-2008; Ryerson, Tom/C-9611-2009; Peischl,
Jeff/E-7454-2010; Graus, Martin/E-7546-2010; Wolfe, Glenn/D-5289-2011;
de Gouw, Joost/A-9675-2008
OI Lerner, Brian/0000-0001-8721-8165; Gilman, Jessica/0000-0002-7899-9948;
Roberts, James/0000-0002-8485-8172; Middlebrook,
Ann/0000-0002-2984-6304; Veres, Patrick/0000-0001-7539-353X; Neuman,
Andy/0000-0002-3986-1727; Nowak, John/0000-0002-5697-9807; Peischl,
Jeff/0000-0002-9320-7101; Graus, Martin/0000-0002-2025-9242; de Gouw,
Joost/0000-0002-0385-1826
FU STAR grant program of the U.S. Environmental Protection Agency; U.S.
Weather Research Program within NOAA/OAR Office of Weather and Air
Quality
FX Data used in this work are archived at
http://www.esrl.noaa.gov/csd/groups/csd7/measurements/2013senex/P3/DataD
ownload/. The formaldehyde measurements were made possible with
financial support from the STAR grant program of the U.S. Environmental
Protection Agency. Some of this material (S.A. McKeen) is based upon
work supported by the U.S. Weather Research Program within NOAA/OAR
Office of Weather and Air Quality. We are thankful for the staff at the
NOAA Aircraft Operations Center and the WP-3D flight crew for the help
in instrumenting the aircraft and for conducting the flights.
NR 50
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 16
PY 2015
VL 120
IS 9
BP 4385
EP 4397
DI 10.1002/2015JD023138
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CJ8IY
UT WOS:000355744800046
ER
PT J
AU Norris, KJ
Garrett, MP
Zhang, J
Coleman, E
Tompa, GS
Kobayashi, NP
AF Norris, Kate J.
Garrett, Matthew P.
Zhang, Junce
Coleman, Elane
Tompa, Gary S.
Kobayashi, Nobuhiko P.
TI Silicon nanowire networks for multi-stage thermoelectric modules
SO ENERGY CONVERSION AND MANAGEMENT
LA English
DT Article
DE Nanowire network; Plasma Enhanced Chemical Vapor Deposition (PECVD);
Silicon; TiN nucleation layer; Copper substrate
ID THERMAL-CONDUCTIVITY; POWER; GENERATOR; HEAT; DEVICES
AB We present the fabrication and characterization of single, double, and quadruple stacked flexible silicon nanowire network based thermoelectric modules. From double to quadruple stacked modules, power production increased 27%, demonstrating that stacking multiple nanowire thermoelectric devices in series is a scalable method to generate power by supplying larger temperature gradient. We present a vertically scalable multi-stage thermoelectric module design using semiconducting nanowires, eliminating the need for both n-type and p-type semiconductors for modules. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Norris, Kate J.; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Norris, Kate J.; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Coleman, Elane; Tompa, Gary S.] Struct Mat Ind Inc, Piscataway, NJ USA.
RP Norris, KJ (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
EM katejeannenorris@gmail.com
FU NASA SBIR [NNX11CE14P]; National Science Foundation Graduate Research
Fellowship [DGE-0809125]; Semiconductor Research Corporation CSR fund
FX This work was supported by NASA SBIR NNX11CE14P. The authors are
grateful to HP labs (Palo Alto, California), specifically Stanley
Williams and the HP Quantum Science Research (QSR) group. We would also
like to thank the MACS facility (Moffett Field, California) at Advanced
Studies Laboratories, University of California Santa Cruz, and NASA Ames
Research Center for continuous support on analytical equipment. This
material is based upon work supported by the National Science Foundation
Graduate Research Fellowship under Grant No. DGE-0809125. Support by
Semiconductor Research Corporation CSR fund (Dr. Victor Zhirnov) is also
highly appreciated.
NR 31
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0196-8904
EI 1879-2227
J9 ENERG CONVERS MANAGE
JI Energy Conv. Manag.
PD MAY 15
PY 2015
VL 96
BP 100
EP 104
DI 10.1016/j.enconman.2015.02.050
PG 5
WC Thermodynamics; Energy & Fuels; Mechanics
SC Thermodynamics; Energy & Fuels; Mechanics
GA CH0RD
UT WOS:000353729200011
ER
PT J
AU Alexander, C
AF Alexander, Claudia
TI We Could Not Fail The First African Americans in the Space Program
SO SCIENCE
LA English
DT Book Review
C1 [Alexander, Claudia] Jet Prop Lab, Pasadena, CA 91740 USA.
RP Alexander, C (reprint author), Jet Prop Lab, Pasadena, CA 91740 USA.
EM claudia.j.alexander@jpl.nasa.gov
NR 3
TC 0
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U1 0
U2 1
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 MAY 15
PY 2015
VL 348
IS 6236
BP 764
EP 764
DI 10.1126/science.aaa8008
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CI0LN
UT WOS:000354428700025
ER
PT J
AU Sanders, GB
AF Sanders, Gerald B.
TI Preface: Terrestrial Fieldwork to Support in situ Resource Utilization
(ISRU) and Robotic Resource Prospecting for Future Activities in Space
SO ADVANCES IN SPACE RESEARCH
LA English
DT Editorial Material
C1 NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, Houston, TX 77058 USA.
RP Sanders, GB (reprint author), NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM gerald.b.sanders@nasa.gov
NR 0
TC 0
Z9 0
U1 2
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD MAY 15
PY 2015
VL 55
IS 10
BP 2379
EP 2380
DI 10.1016/j.asr.2015.03.018
PG 2
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900001
ER
PT J
AU Sanders, GB
Larson, WE
AF Sanders, Gerald B.
Larson, William E.
TI Final review of analog field campaigns for In Situ Resource Utilization
technology and capability maturation
SO ADVANCES IN SPACE RESEARCH
LA English
DT Review
DE Analog testing; In Situ Resource Utilization; Lunar human exploration;
Field testing
AB A key aspect of enabling an affordable and sustainable program of human exploration beyond low Earth orbit is the ability to locate, extract, and harness the resources found in space to reduce what needs to be launched from Earth's deep gravity well and to minimize the risk of dependence on Earth for survival. Known as In Situ Resource Utilization or ISRU, the ability to convert space resources into useful and mission critical products has been shown in numerous studies to be mission and architecture enhancing or enabling. However at the time of the release of the US Vision for Space Exploration in 2004, only concept feasibility hardware for ISRU technologies and capabilities had been built and tested in the laboratory; no ISRU hardware had ever flown in a mission to the Moon or Mars. As a result, an ISRU development project was established with phased development of multiple generations of hardware and systems. To bridge the gap between past ISRU feasibility hardware and future hardware needed for space missions, and to increase confidence in mission and architecture planners that ISRU capabilities would meet exploration needs, the ISRU development project incorporated extensive ground and analog site testing to mature hardware, operations, and interconnectivity with other exploration systems linked to ISRU products. This report documents the series of analog test activities performed from 2008 to 2012, the stepwise progress achieved, and the end-to-end system and mission demonstrations accomplished in this test program. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Sanders, Gerald B.] NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, Houston, TX 77058 USA.
[Larson, William E.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
RP Sanders, GB (reprint author), NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM gerald.b.sanders@nasa.gov; william.e.larson@nasa.gov
NR 31
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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 MAY 15
PY 2015
VL 55
IS 10
BP 2381
EP 2404
DI 10.1016/j.asr.2014.12.024
PG 24
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900002
ER
PT J
AU Graham, L
Graff, TG
Yingst, RA
ten Kate, IL
Russell, P
AF Graham, Lee
Graff, Trevor G.
Yingst, R. Aileen
ten Kate, Inge L.
Russell, Patrick
TI 2012 Moon Mars Analog Mission Activities on Mauna Kea, Hawai'i
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Geology; Moon; Mars; Rover
ID GROUND-PENETRATING RADAR; MOSSBAUER SPECTROMETER
AB Rover-based 2012 Moon and Mars Analog Mission Activities (MMAMA) scientific investigations were completed at Mauna Kea, Hawaii. Scientific investigations, scientific input, and science operations constraints were tested in the context of an existing project and protocols for the field activities designed to help NASA achieve the Vision for Space Exploration. Four separate science investigations were integrated in a Martian analog environment with initial science operations planned based on a model similar to the operations control of the Mars Exploration Rovers (MER). However, evolution of the operations process occurred during the initial planning sessions and as the analog mission progressed. We review here the overall program of the investigation into the origin of the valley including preliminary sensor data results, an applicable methodology for developing an optimum science input based on productive engineering, and science trades and the science operations approach for an investigation into the valley on the upper slopes of Mauna Kea identified as "Apollo Valley". Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Graham, Lee] NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Houston, TX 77058 USA.
[Graff, Trevor G.] NASA, Lyndon B Johnson Space Ctr, Dept Sci, JACOBS, Houston, TX 77058 USA.
[Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ 85719 USA.
[ten Kate, Inge L.] Univ Utrecht, Dept Earth Sci, NL-3584 CD Utrecht, Netherlands.
[Russell, Patrick] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA.
RP Graham, L (reprint author), NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Mail Code X14,2101 NASA Pkwy, Houston, TX 77058 USA.
EM lee.d.graham@nasa.gov
NR 14
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U1 4
U2 9
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 MAY 15
PY 2015
VL 55
IS 10
BP 2405
EP 2413
DI 10.1016/j.asr.2015.01.024
PG 9
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900003
ER
PT J
AU Heldmann, JL
Colaprete, A
Elphic, RC
Mattes, G
Ennico, K
Fritzler, E
Marinova, MM
McMurray, R
Morse, S
Roush, TL
Stoker, CR
AF Heldmann, Jennifer L.
Colaprete, Anthony
Elphic, Richard C.
Mattes, Greg
Ennico, Kimberly
Fritzler, Erin
Marinova, Margarita M.
McMurray, Robert
Morse, Stephanie
Roush, Ted L.
Stoker, Carol R.
TI Real-time science operations to support a lunar polar volatiles rover
mission
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Moon; Volatiles; Rover; Missions
AB Future human exploration of the Moon will likely rely on in situ resource utilization (ISRU) to enable long duration lunar missions. Prior to utilizing ISRU on the Moon, the natural resources (in this case lunar volatiles) must be identified and characterized, and ISRU demonstrated on the lunar surface. To enable future uses of ISRU, NASA and the CSA are developing a lunar rover payload that can (1) locate near subsurface volatiles, (2) excavate and analyze samples of the volatile-bearing regolith, and (3) demonstrate the form, extractability and usefulness of the materials. Such investigations are important both for ISRU purposes and for understanding the scientific nature of these intriguing lunar volatile deposits.
Temperature models and orbital data suggest near surface volatile concentrations may exist at briefly lit lunar polar locations outside persistently shadowed regions. A lunar rover could be remotely operated at some of these locations for the similar to 2-14 days of expected sunlight at relatively low cost. Due to the limited operational time available, both science and rover operations decisions must be made in real time, requiring immediate situational awareness, data analysis, and decision support tools. Given these constraints, such a mission requires a new concept of operations.
In this paper we outline the results and lessons learned from an analog field campaign in July 2012 which tested operations for a lunar polar rover concept. A rover was operated in the analog environment of Hawaii by an off-site Flight Control Center, a rover navigation center in Canada, a Science Backroom at NASA Ames Research Center in California, and support teams at NASA Johnson Space Center in Texas and NASA Kennedy Space Center in Florida. We find that this type of mission requires highly efficient, real time, remotely operated rover operations to enable low cost, scientifically relevant exploration of the distribution and nature of lunar polar volatiles. The field demonstration illustrated the need for science operations personnel in constant communications with the flight mission operators and the Science Backroom to provide immediate and continual science support and validation throughout the mission. Specific data analysis tools are also required to enable immediate data monitoring, visualization, and decision making. The field campaign demonstrated that this novel methodology of real-time science operations is possible and applicable to providing important new insights regarding lunar polar volatiles for both science and exploration. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Heldmann, Jennifer L.; Colaprete, Anthony; Elphic, Richard C.; Ennico, Kimberly; Roush, Ted L.; Stoker, Carol R.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
[Mattes, Greg] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Fritzler, Erin; McMurray, Robert; Morse, Stephanie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marinova, Margarita M.] BAER Inst, Sonoma, CA 95476 USA.
RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
EM jennifer.heldmann@nasa.gov
NR 6
TC 5
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U1 2
U2 6
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 MAY 15
PY 2015
VL 55
IS 10
BP 2427
EP 2437
DI 10.1016/j.asr.2014.07.037
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900005
ER
PT J
AU Elphic, RC
Heldmann, JL
Marinova, MM
Colaprete, A
Fritzler, EL
McMurray, RE
Morse, S
Roush, TL
Stoker, CR
Deans, MC
Smith, TF
AF Elphic, Richard C.
Heldmann, Jennifer L.
Marinova, Margarita M.
Colaprete, Anthony
Fritzler, Erin L.
McMurray, Robert E.
Morse, Stephanie
Roush, Ted L.
Stoker, Carol R.
Deans, Matthew C.
Smith, Trey F.
TI Simulated real-time lunar volatiles prospecting with a rover-borne
neutron spectrometer
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Moon; Volatiles; Rover; Neutron spectroscopy
ID GAMMA-RAY; EXPLORATION; DETECTOR; WATER
AB In situ resource utilization (ISRU) may one day enable long duration lunar missions. But the efficacy of such an approach greatly depends on (1) physical and chemical makeup of the resource, and (2) the logistical cost of exploiting the resource. Establishing these key strategic factors requires prospecting: the capability of locating and characterizing potential resources. There is already considerable evidence from orbital and impact missions that the lunar poles harbor plausibly rich reservoirs of volatiles. The next step is to land on the Moon and assess the nature, "ore-grade", and extractability of water ice and other materials. In support of this next step, a mission simulation was carried out on the island of Hawai'i in July of 2012. A robotic rover, provided by the Canadian Space Agency, carried several NASA ISRU-supporting instruments in a field test to address how such a mission might be carried out. This exercise was meant to test the ability to (a) locate and characterize volatiles, (b) acquire subsurface samples in a volatile-rich location, and (c) analyze the form and composition of the volatiles to determine their utility. This paper describes the successful demonstration of neutron spectroscopy as a prospecting and decision support system to locate and evaluate potential ISRU targets in the field exercise. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Elphic, Richard C.; Heldmann, Jennifer L.; Colaprete, Anthony; Roush, Ted L.; Stoker, Carol R.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
[Marinova, Margarita M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Fritzler, Erin L.; McMurray, Robert E.; Morse, Stephanie] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA.
[Deans, Matthew C.; Smith, Trey F.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Elphic, RC (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
EM richard.c.elphic@nasa.gov
NR 19
TC 3
Z9 3
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 MAY 15
PY 2015
VL 55
IS 10
BP 2438
EP 2450
DI 10.1016/j.asr.2015.01.035
PG 13
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900006
ER
PT J
AU Roush, TL
Colaprete, A
Elphic, R
Ennico-Smith, K
Heldmann, J
Stoker, C
Marinova, M
McMurray, R
Fritzler, E
Morse, S
AF Roush, Ted L.
Colaprete, Anthony
Elphic, Richard
Ennico-Smith, Kimberly
Heldmann, Jennifer
Stoker, Carol
Marinova, Margarita
McMurray, Robert
Fritzler, Erin
Morse, Stephanie
TI In Situ Resource Utilization (ISRU) field expedition 2012: Near-Infrared
Volatile Spectrometer System (NIRVSS) science measurements compared to
site knowledge
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Lunar; Volatile; Prospecting; Rover
AB The scientific information collected and evaluated using the Near-Infrared Volatile Spectrometer System (NIRVSS) during the 2012 In Situ Resource Utilization (ISRU) field campaign, exhibits variations related to differing surface materials and presence of volatiles during both rover traverses and auger activities demonstrating the promise of using NIRVSS for volatile prospecting on the lunar surface. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Roush, Ted L.; Colaprete, Anthony; Elphic, Richard; Ennico-Smith, Kimberly; Heldmann, Jennifer; Stoker, Carol] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
[Marinova, Margarita] BAER Inst, Petaluma, CA 94952 USA.
[McMurray, Robert] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA.
[Fritzler, Erin; Morse, Stephanie] NASA, Ames Res Ctr, Strateg Management & Anal Div, Lockheed Martin Space, Moffett Field, CA 94035 USA.
RP Roush, TL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, MS 245-3, Moffett Field, CA 94035 USA.
EM ted.l.roush@nasa.gov
FU NASA's Human Exploration and Operations Mission Directorate
FX We thank NASA's Human Exploration and Operations Mission Directorate for
their support of the July 2012 Hawaii ISRU field campaign. We thank the
many individuals from NASA KSC, JSC, ARC, Glenn, the Canadian Space
Agency, and Pacific International Space Center for Exploration Systems
for their assistance in organizing and supporting the Hawaii 2012 field
test. Without their efforts this work would not have been possible. We
acknowledge the Gemini Observatory for the atmospheric transmission
spectrum for Mauna Kea shown in Fig. 3. We thank two anonymous reviewers
for their comments that helped to improve the original manuscript.
NR 11
TC 4
Z9 4
U1 1
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD MAY 15
PY 2015
VL 55
IS 10
BP 2451
EP 2456
DI 10.1016/j.asr.2014.08.033
PG 6
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900007
ER
PT J
AU Captain, JE
Weis, K
Cryderman, K
Coan, M
Lance, L
Levine, L
Loftin, KB
Santiago-Maldonado, E
Bauer, B
Quinn, J
AF Captain, Janine E.
Weis, Kyle
Cryderman, Katherine
Coan, Mary
Lance, Lucas
Levine, Lanfang
Loftin, Kathleen Brooks
Santiago-Maldonado, Edgardo
Bauer, Brint
Quinn, Jaqueline
TI Design and development of volatile analysis system for analog field test
of lunar exploration mission
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE In Situ Resource Utilization; Field test; Volatile analysis; Lunar
regolith; Lunar resources
AB The recent evidence of water in the lunar crater Cabeus from the LCROSS mission (Colaprete et al., 2010) provides confirmation of a valuable resource on the lunar surface. To understand this resource and the impact it can have on future exploration, further information is needed on the distribution and availability of the water ice. The Lunar Advanced Volatile Analysis (LAVA) subsystem is a part of the Regolith & Environment Science and Oxygen & Lunar Volatile Extraction (RESOLVE) payload, designed to provide ground truth to the volatile distribution near the permanently shadowed regions on the lunar surface. The payload is designed to drill and extract a regolith core sample, heat the regolith to drive off the volatiles, and identify and quantify the volatile resources. The LAVA subsystem is specifically responsible for processing and analyzing the volatile gas sample from the lunar regolith sample. The main objective of this paper is to provide insight into the operations and hardware for volatile analysis developed and deployed at the 2012 RESOLVE Field Test on the slopes of Mauna Kea. The vision of employing Commercial Off the Shelf (COTS) and modified COTS hardware to lower the cost for mission-enabling field tests will be highlighted. This paper will discuss how the LAVA subsystem hardware supported several high level RESOLVE mission objectives to demonstrate the challenging lunar mission concept proposed. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Captain, Janine E.; Cryderman, Katherine; Coan, Mary; Lance, Lucas; Loftin, Kathleen Brooks; Santiago-Maldonado, Edgardo; Quinn, Jaqueline] NASA, Kennedy Space Ctr, FL 32899 USA.
[Weis, Kyle; Levine, Lanfang; Bauer, Brint] QinetiQ, Kennedy Space Ctr, FL 32899 USA.
RP Captain, JE (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA.
EM Janine.E.Captain@nasa.gov
FU National Aeronautics and Space Administration
FX The authors would like to thank the Pacific International Space Center
for Exploration System (PISCES), the Canadian Space Agency (CSA) and
numerous volunteers involved in this field test. This work was funded by
the National Aeronautics and Space Administration.
NR 31
TC 1
Z9 1
U1 1
U2 2
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 MAY 15
PY 2015
VL 55
IS 10
BP 2457
EP 2471
DI 10.1016/j.asr.2014.11.006
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CH0ZC
UT WOS:000353749900008
ER
PT J
AU Chao, Y
Farrara, JD
Schumann, G
Andreadis, KM
Moller, D
AF Chao, Yi
Farrara, John D.
Schumann, Guy
Andreadis, Konstantinos M.
Moller, Delwyn
TI Sea surface salinity variability in response to the Congo river
discharge
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Sea surface salinity variability; River discharge; Hydrological forcing;
Freshwater budget
ID ATLANTIC-OCEAN; AQUARIUS; CIRCULATION; SENSOR; SPACE; PLUME; GULF; SMOS
AB Sea surface salinity (SSS) variability associated with the Congo River discharge is examined using Aquarius satellite-retrieved SSS data and vertical profiles of salinity measured by the Argo floats. The Congo River and its adjacent coastal ocean region are selected for study because of their global importance in ocean-freshwater dynamics undermined by the lack of observational data and coordinated efforts to make in situ measurements in this region. With a weekly repeat orbit, Aquarius provides a unique opportunity to routinely map the SSS in this relatively remote and understudied region. The Congo River plume can be clearly identified in the Aquarius SSS data with a northwestward extension of 500-1000 km off the coast of the Democratic Republic of Congo (DRC). The peak amplitude of the SSS variability associated with the Congo River discharge exceeds 3.0 psu, significantly greater than the designed Aquarius SSS retrieval accuracy of 0.2 psu. Using the first two years of Aquarius data from September 2011 to August 2013, a well-defined seasonal cycle is described: maximum freshwater anomalies are found in the boreal winter and spring seasons. The anomalies during the 2012-2013 winter and spring seasons are significantly fresher than the 2011-2012 winter and spring seasons, suggesting a strong year-to-year variability.
A strong correlation is found between month-to-month variations in upper ocean salinity (as revealed by Aquarius satellite and Argo observations) and month-to-month variations in the freshwater discharge from the Congo River over a region off the coast of West Africa that is large enough to be easily observed by the Aquarius satellite. Vertical profiles of salinity derived from Argo floats reveal that these freshwater anomalies can be traced to 30 m below the sea surface. Combining the spatial area characterized by strong negative correlations between Aquarius SSS data and Congo discharge with the Argo vertical profiles of salinity, the volume of the freshwater anomalies is inferred and used to estimate the Congo River discharge. Reasonably good agreement is found between the Congo River discharge as observed by a stream gauge at Brazzaville and that estimated from the combined Aquarius and Argo data, especially during the freshening portion of the seasonal cycle (during this phase the correlation is 0.84, implying similar to 70% of the variance can be explained). The precipitation minus evaporation portion of the freshwater flux is found to play a secondary role in this region. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Chao, Yi; Farrara, John D.; Moller, Delwyn] Remote Sensing Solut Inc, Pasadena, CA 91107 USA.
[Chao, Yi; Farrara, John D.; Schumann, Guy] Univ Calif Los Angeles, Los Angeles, CA USA.
[Andreadis, Konstantinos M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Farrara, JD (reprint author), Remote Sensing Solut Inc, Pasadena, CA 91107 USA.
EM jfarrara@jifresse.ucla.edu
FU JPL Aquarius project [1425025B]; Ocean Salinity Science Team (OSST)
grant from Oregon State University [NS235A-A]; National Aeronautics and
Space Administration (NASA) [NNX12AF67G]; UCLA Joint Institute for
Regional Earth System Science and Engineering (JIFRESSE); NOAA Climate
Observations and Monitoring (COM) program
FX The research of Y. Chao at Remote Sensing Solutions, Inc. is supported
by the JPL Aquarius project through a subcontract (1425025B). The
research of Y. Chao and J. Farrara at the University of California at
Los Angeles (UCLA) is supported by the Ocean Salinity Science Team
(OSST) grant through a subcontract (NS235A-A) from Oregon State
University. The research of K. Andreadis and G. Schumann was carried out
at the Jet Propulsion Laboratory (JPL), California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration (NASA) (Grant no. NNX12AF67G). Staff support from the
UCLA Joint Institute for Regional Earth System Science and Engineering
(JIFRESSE) is also acknowledged. Thanks go to Raphael Tshimanga from the
Congo Basin Network for Research and Capacity Development in Water
Resources (CB-Hydronet) for providing the Congo River discharge data at
Brazzaville station and to Fiachra O'Loughlin at the School of
Geographical Sciences at the University of Bristol (UK) for providing
the GRDC discharge data at Kinshasa station. Discussions with a number
of OSST team members (Ricardo Matano, Alberto Piola, Raul Guerrero,
Elbio Palma, Martin Saraceno, Ted Strub) on the South Atlantic ocean
circulation and variability are acknowledged. The global ocean
evaporation products were provided by the WHOI OAFlux project
(http://oaflux.whoi.edu) funded by the NOAA Climate Observations and
Monitoring (COM) program. The GPCP data provided by the NOAA/OAR/ESRL
PSD, Boulder, Colorado, USA, from their Web site at
http://www.esrl.noaa.gov/psd/. The GPCP combined precipitation data were
developed and computed by the NASA/Goddard Space Flight Center's
Laboratory for Atmospheres as a contribution to the GEWEX Global
Precipitation Climatology Project.
NR 26
TC 1
Z9 1
U1 5
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
EI 1873-6955
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD MAY 15
PY 2015
VL 99
BP 35
EP 45
DI 10.1016/j.csr.2015.03.005
PG 11
WC Oceanography
SC Oceanography
GA CH2PE
UT WOS:000353866300004
ER
PT J
AU Li, WQ
Beard, BL
Li, CX
Xu, HF
Johnson, CM
AF Li, Weiqiang
Beard, Brian L.
Li, Chengxiang
Xu, Huifang
Johnson, Clark M.
TI Experimental calibration of Mg isotope fractionation between dolomite
and aqueous solution and its geological implications
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID MAGNESIUM-ISOTOPE; HIGH-TEMPERATURE; DISORDERED DOLOMITE; SEAWATER
CHEMISTRY; SEDIMENTARY DOLOMITE; CARBONATE MINERALOGY; WESTERN
NEWFOUNDLAND; SALT-SOLUTIONS; DOLOMITIZATION; CALCITE
AB Hydrothermal experiments at 220, 160, and 130 degrees C were performed to calibrate the Mg isotope fractionation factor between dolomite and aqueous Mg. Hydrothermal experiments included synthesis of dolomite using different starting materials, as well as exchange experiments that used poorly-ordered proto-dolomite. The morphology of synthesized dolomite was dependent on starting mineralogy, suggesting that dolomite was synthesized by different pathways. Hydrothermally synthesized dolomite was initially fine-grained disordered or poorly-ordered dolomite that, with time, recrystallized to coarser-grained ordered dolomite. Isotopic exchange was monitored using Sr-87/Sr-86 ratios and Mg-25 tracers, and these indicated near-complete isotope exchange between dolomite and aqueous solutions at the end of most hydrothermal experiments. The Mg isotope fractionation factor between dolomite and aqueous solution obtained from synthesis and exchange experiments converged with time and was independent of dolomite morphology, suggesting attainment of isotopic equilibrium. Combining results from synthesis and exchange experiments, the temperature dependent Mg isotope fractionation factor for ordered dolomite is:
Delta Mg-26(dolo-aq) = -0.1554(+/- 0.0096) x 10(6)/T-2
where T is in Kelvin. In contrast, poorly-ordered dolomite has a Delta Mg-26(dolo-aq) fractionation factor that is up to 0.25 parts per thousand lower than that of ordered dolomite, and this is attributed to longer Mg-O bonds in imperfectly ordered dolomite. The experimentally calibrated Delta Mg-26(dolo-aq) fractionation factors lie between those calculated by Schauble (2011) and Rustad et al. (2010). The Delta Mg-26(dolo-aq) fractionation factor extrapolated to lower temperatures using the Delta Mg-26-T function of this study matches the Delta Mg-26(dolo-aq) fractionation factor obtained by modeling of Mg isotope compositions of ODP drill core samples. This study shows that significant Mg isotope fractionation occurs during dolomite precipitation. These results collectively demonstrate that Mg isotopes in dolomite are a useful tool for studying Mg global cycling and dolomitization. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Li, Weiqiang; Beard, Brian L.; Xu, Huifang; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Li, Weiqiang; Beard, Brian L.; Xu, Huifang; Johnson, Clark M.] NASA, Astrobiol Inst, Washington, DC USA.
[Li, Weiqiang; Li, Chengxiang] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210093, Jiangsu, Peoples R China.
RP Li, WQ (reprint author), Nanjing Univ, Sch Earth Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China.
EM liweiqiang@nju.edu.cn
RI Li, Weiqiang/D-2975-2011
OI Li, Weiqiang/0000-0003-2648-7630
FU NASA Astrobiology Institute of United States; National Science
Foundation of China [41473002]
FX This paper benefited from discussions with Or Bialik, Fangfu Zhang and
Zhizhang Shen, and constructive comments from John Higgins and Josh
Wimpenny, as well as editorial comments by Jeff Alt. This study was
supported by the NASA Astrobiology Institute of United States. W. Li is
supported by the National Science Foundation of China (41473002).
NR 70
TC 17
Z9 19
U1 5
U2 44
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAY 15
PY 2015
VL 157
BP 164
EP 181
DI 10.1016/j.gca.2015.02.024
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CG3XX
UT WOS:000353214100010
ER
PT J
AU Peters, TJ
Simon, JI
Jones, JH
Usui, T
Moriwaki, R
Economos, RC
Schmitt, AK
McKeegan, KD
AF Peters, T. J.
Simon, J. I.
Jones, J. H.
Usui, T.
Moriwaki, R.
Economos, R. C.
Schmitt, A. K.
McKeegan, K. D.
TI Tracking the source of the enriched martian meteorites in olivine-hosted
melt inclusions of two depleted shergottites, Yamato 980459 and Tissint
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE martian mantle melting; mantle depletion; olivine-phyric shergottites;
olivine-hosted melt inclusions; Rare Earth Elements; crustal recycling
ID MANTLE; MARS; YAMATO-980459; PETROGENESIS; CONSTRAINTS; ORIGIN;
CLINOPYROXENE; SYSTEMATICS; MAGMATISM; EVOLUTION
AB The apparent lack of plate tectonics on all terrestrial planets other than Earth has been used to support the notion that for most planets, once a primitive crust forms, the crust and mantle evolve geochemically-independent through time. This view has had a particularly large impact on models for the evolution of Mars and its silicate interior. Recent data indicating a greater potential that there may have been exchange between the martian crust and mantle has led to a search for additional geochemical evidence to support the alternative hypothesis, that some mechanism of crustal recycling may have operated early in the history of Mars.
In order to study the most juvenile melts available to investigate martian mantle source(s) and melting processes, the trace element compositions of olivine-hosted melt inclusions for two incompatible-element-depleted olivine-phyric shergottites, Yamato 980459 (Y98) and Tissint, and the interstitial glass of Y98, have been measured by Secondary Ionization Mass Spectrometry (SIMS). Chondrite-normalized Rare Earth Element (REE) patterns for both Y98 and Tissint melt inclusions, and the Y98 interstitial glass, are characteristically light-REE depleted and parallel those of their host rock. For Y98, a clear flattening and upward inflection of La and Ce, relative to predictions based on middle and heavier REE, provides evidence for involvement of an enriched component early in their magmatic history; either inherited from a metasomatized mantle or crustal source, early on and prior to extensive host crystallization.
Comparing these melt inclusion and interstitial glass analyses to existing melt inclusion and whole-rock data sets for the shergottite meteorite suite, defines mixing relationships between depleted and enriched end members, analogous to mixing relationships between whole rock Sr and Nd isotopic measurements. When considered in light of their petrologic context, the origin of these trace element enriched and isotopically evolved signatures represents either (1) crustal assimilation during the final few km of melt ascent towards the martian surface, or (2) assimilation soon after melt segregation, through melt-rock interaction with a portion of the martian crust recycled back into the mantle. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Peters, T. J.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Peters, T. J.; Simon, J. I.; Jones, J. H.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA.
[Peters, T. J.; Simon, J. I.] NASA, Johnson Space Ctr, Ctr Isotope Cosmochem & Geochronol, Houston, TX 77058 USA.
[Usui, T.; Moriwaki, R.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan.
[Economos, R. C.; Schmitt, A. K.; McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
RP Peters, TJ (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
EM Peterstj2313@gmail.com
RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011;
OI McKeegan, Kevin/0000-0002-1827-729X; Schmitt, Axel/0000-0002-9029-4211
FU NASA [NNX11AF57G]; Instrumentation and Facilities Program, Division of
Earth Sciences, National Science Foundation
FX We are grateful to Dr. Anne Peslier at Johnson Space Center (JSC) for
assistance with Electron Microprobe analyses (EMPA), and Dr. Kent Ross
and Dr. Eve Berger for assistance with the JSC Field Emission Scanning
Electron Microscope. Editorial handling and suggestions by Tamsin
Mather, and comments by David Baratoux and Jon Wade, significantly
improved upon the original manuscript. NASA funding comes from the Mars
Fundamental Research Program (NNX11AF57G). The ion microprobe facility
at UCLA is partly supported by a grant from the Instrumentation and
Facilities Program, Division of Earth Sciences, National Science
Foundation.
NR 59
TC 5
Z9 5
U1 1
U2 14
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 MAY 15
PY 2015
VL 418
BP 91
EP 102
DI 10.1016/j.epsl.2015.02.033
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CF6KI
UT WOS:000352665200009
ER
PT J
AU Pankine, AA
Tamppari, LK
AF Pankine, Alexey A.
Tamppari, Leslie K.
TI Constraints on water vapor vertical distribution at the Phoenix landing
site during summer from MGS TES day and night observations
SO ICARUS
LA English
DT Article
DE Mars; Mars, atmosphere; Infrared observations; Atmospheres, structure
ID THERMAL EMISSION SPECTROMETER; MARS GLOBAL SURVEYOR; CONVECTIVE
BOUNDARY-LAYER; ATMOSPHERIC TEMPERATURES; INTERANNUAL VARIABILITY;
MARTIAN ATMOSPHERE; ICE CLOUDS; EXPRESS; SIMULATIONS; OCCULTATION
AB We present a new method to retrieve column abundances and vertical extent of the water vapor from the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES) spectra. The new method enables retrievals from the nighttime TES spectra. The retrieval algorithm employs a new model of the vertical distribution of water vapor in the martian atmosphere. In this model water vapor is confined to a layer of finite height in the lower atmosphere. The atmosphere is dry above this 'wet' layer. Within the 'wet' layer the water vapor has a constant mixing ratio below the water ice cloud condensation height and is saturated above that height. The new retrieval method simultaneously fits the daytime and nighttime TES spectra for a given location using a single mixing ratio profile. We apply this new method to the TES spectra collected over the site of the Phoenix spacecraft landing during late northern spring and summer. Retrieved daytime column abundances are similar to 1-5 pr-mu m higher than in the previous TES retrieval. Nighttime column abundances are lower than the daytime abundances by similar to 5-10 pr-mu m due to assumed exchange with soil and predicted water ice cloud formation. The height of the 'wet' layer varies with season, reaching similar to 18 km around L-s = 80-100 degrees and decreasing to 7-10 km by L-s = 140 degrees. Changes in the vertical extent of vapor are consistent with seasonal changes in the intensity of the turbulent mixing in the lower atmosphere and in the water ice cloud condensation height. Water vapor extends by several kilo-meters above the top of the boundary layer at similar to 4 km, suggesting that vertical transport of vapor is not limited to the boundary layer. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Pankine, Alexey A.] Space Sci Inst, Boulder, CO 80301 USA.
[Tamppari, Leslie K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pankine, AA (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM apankine@spacescience.com
FU NASA Mars Data Analysis program [NNX13AE53G]; Jet Propulsion Laboratory
FX This research was carried out at the Space Science Institute and Jet
Propulsion Laboratory, California Institute of Technology, with funding
from the NASA Mars Data Analysis program grant NNX13AE53G and Jet
Propulsion Laboratory subcontract to Space Science Institute.
NR 57
TC 2
Z9 2
U1 1
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 MAY 15
PY 2015
VL 252
BP 107
EP 120
DI 10.1016/j.icarus.2015.01.008
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000007
ER
PT J
AU Rodriguez, JAP
Leonard, GJ
Platz, T
Tanaka, KL
Kargel, JS
Fairen, AG
Gulick, V
Baker, VR
Glines, N
Miyamoto, H
Yan, JG
Oguma, M
AF Rodriguez, J. Alexis P.
Leonard, Gregory J.
Platz, Thomas
Tanaka, Kenneth L.
Kargel, Jeffrey S.
Fairen, Alberto G.
Gulick, Virginia
Baker, Victor R.
Glines, Natalie
Miyamoto, Hideaki
Yan Jianguo
Oguma, Midori
TI New insights into the Late Amazonian zonal shrinkage of the Martian
south polar plateau (vol 248, pg 407, 2015)
SO ICARUS
LA English
DT Correction
C1 [Rodriguez, J. Alexis P.; Gulick, Virginia; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rodriguez, J. Alexis P.; Platz, Thomas] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Leonard, Gregory J.; Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Platz, Thomas] Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing, D-12249 Berlin, Germany.
[Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Gulick, Virginia] SETI Inst, Mountain View, CA 94043 USA.
[Miyamoto, Hideaki; Oguma, Midori] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
[Yan Jianguo] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
RP Rodriguez, JAP (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM alexis@psi.edu
RI Platz, Thomas/F-7539-2013; Miyamoto, Hideaki/B-9666-2008
OI Platz, Thomas/0000-0002-1253-2034;
NR 1
TC 0
Z9 0
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 MAY 15
PY 2015
VL 252
BP 228
EP 228
DI 10.1016/j.icarus.2015.01.009
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000018
ER
PT J
AU Robinson, MS
Boyd, AK
Denevi, BW
Lawrence, SJ
McEwen, AS
Moser, DE
Povilaitis, RZ
Stelling, RW
Suggs, RM
Thompson, SD
Wagner, RV
AF Robinson, Mark S.
Boyd, Aaron K.
Denevi, Brett W.
Lawrence, Samuel J.
McEwen, Alfred S.
Moser, Danielle E.
Povilaitis, Reinhold Z.
Stelling, Richard W.
Suggs, Robert M.
Thompson, Shane D.
Wagner, Robert V.
TI New crater on the Moon and a swarm of secondaries
SO ICARUS
LA English
DT Article
DE Impact processes; Geological processes; Moon, surface; Moon; Regoliths
ID ACCRETION RATE; LUNAR; METEORITES; DENSITY; FLUX
AB Lunar Reconnaissance Orbiter Camera images acquired both before and after the formation of an 18.8 m diameter crater on 17 March 2013 reveal intricate details of ejecta distribution and the structure of the top two meters of the regolith. Our observations indicate that (I) the regolith is mature down to several tens of cm and immature below one meter, (2) surface reflectivity properties are affected for distances greater than fifty crater radii, and (3) large numbers of secondary impacts (splotches) formed up to 30 km distant from this new primary crater. These observations provide new knowledge of the distribution of ejected materials from small impact craters on the Moon, the modification of the top few cm of the regolith by micrometeorite impacts, and potential hazards to future explorers. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Robinson, Mark S.; Boyd, Aaron K.; Lawrence, Samuel J.; Povilaitis, Reinhold Z.; Stelling, Richard W.; Thompson, Shane D.; Wagner, Robert V.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Moser, Danielle E.] Marshall Space Flight Ctr, Meteoroid Environm Off, MITS Dynet, Huntsville, AL 35812 USA.
[Suggs, Robert M.] Marshall Space Flight Ctr, Meteoroid Environm Off, Huntsville, AL 35812 USA.
RP Robinson, MS (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM robinson@ser.asu.edu
RI Denevi, Brett/I-6502-2012
OI Denevi, Brett/0000-0001-7837-6663
FU NASA LRO project
FX We thank the NASA LRO and LROC operations team for acquiring the images
that made this study possible; the NASA LRO project supported this
study.
NR 25
TC 10
Z9 10
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 MAY 15
PY 2015
VL 252
BP 229
EP 235
DI 10.1016/j.icarus.2015.01.019
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000019
ER
PT J
AU Vokrouhlicky, D
Farnocchia, D
Capek, D
Chesley, SR
Pravec, P
Scheirich, P
Muller, TG
AF Vokrouhlicky, David
Farnocchia, Davide
Capek, David
Chesley, Steven R.
Pravec, Petr
Scheirich, Petr
Mueller, Thomas G.
TI The Yarkovsky effect for 99942 Apophis
SO ICARUS
LA English
DT Article
DE Celestial mechanics; Asteroids, dynamics; Asteroids, rotation
ID SPIN-STATE; ASTEROIDS; YORP; EARTH; ITOKAWA; MODEL; ASTROMETRY;
STANDARDS; HAYABUSA; DENSITY
AB We use the recently determined rotation state, shape, size and thermophysical model of Apophis to predict the strength of the Yarkovsky effect in its orbit. Apophis does not rotate about the shortest principal axis of the inertia tensor, rather its rotational angular momentum vector wobbles at an average angle of similar or equal to 37 degrees from the body axis. Therefore, we pay special attention to the modeling of the Yarkovsky effect for a body in such a tumbling state, a feature that has not been described in detail so far. Our results confirm that the Yarkovsky effect is not significantly weakened by the tumbling state. The previously stated rule that the Yarkovsky effect for tumbling kilometer-size asteroids is well represented by a simple model assuming rotation about the shortest body axis in the direction of the rotational angular momentum and with rotation period close to the precession period is confirmed. Taking into account uncertainties of the model parameters, as well as the expected density distribution for Apophis' spectral class, we predict the secular change in the semimajor axis is (-12.8 +/- 3.6) x 10(-4) au/Myr (formal 1 cr uncertainty). The currently available astrometric data for Apophis do not allow an unambiguous direct detection of the Yarkovsky effect. However, the fitted secular change in semimajor axis of (-23 +/- 13) x 10(-4) au/Myr is compatible with the model prediction. We revise the Apophis' impact probability information in the second half of this century by extending the orbital uncertainty derived from the current astrometric data and by taking into account the uncertainty in the dynamical model due to the thermal recoil accelerations. This is done by mapping the combined uncertainty to the close encounter in 2029 and by determining the statistical weight of the known keyholes leading to resonant impact orbits. Whereas collision with the Earth before 2060 is ruled out, impacts are still possible from 2060 with probabilities up to a few parts in a million. More definitive analysis will be available after the Apophis apparition in 2020-2021. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Vokrouhlicky, David] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic.
[Farnocchia, Davide; Chesley, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Capek, David; Pravec, Petr; Scheirich, Petr] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic.
[Mueller, Thomas G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Vokrouhlicky, D (reprint author), Charles Univ Prague, Inst Astron, V Holesovickach 2, CZ-18000 Prague 8, Czech Republic.
EM vokrouhl@cesnet.cz
RI Pravec, Petr/G-9037-2014; Scheirich, Peter/H-4331-2014; Capek,
David/G-9005-2014
OI Scheirich, Peter/0000-0001-8518-9532;
FU Czech Grant Agency [P209/12/0229, P209-13-01308S]
FX We thank the anonymous referees for suggestions that helped to improve
the original version of this paper. This work was supported by the Czech
Grant Agency (Grants P209/12/0229 and P209-13-01308S). D. Farnocchia and
S.R. Chesley conducted this research at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 45
TC 6
Z9 6
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 15
PY 2015
VL 252
BP 277
EP 283
DI 10.1016/j.icarus.2015.01.011
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000023
ER
PT J
AU Ore, CMD
Barucci, MA
Emery, JP
Cruikshank, DP
de Bergh, C
Roush, TL
Perna, D
Merlin, F
Ore, LVD
AF Ore, C. Morea Dalle
Barucci, M. A.
Emery, J. P.
Cruikshank, D. P.
de Bergh, C.
Roush, T. L.
Perna, D.
Merlin, F.
Ore, L. V. Dalle
TI The composition of "ultra-red" TNOs and centaurs
SO ICARUS
LA English
DT Article
DE Trans-neptunian objects; Centaurs; Ices, IR spectroscopy; Photometry
ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; ESO LARGE PROGRAM; OUTER
SOLAR-SYSTEM; NEAR-INFRARED SPECTROSCOPY; 47171 1999 TC36;
TRANSNEPTUNIAN OBJECTS; 5145 PHOLUS; 90377 SEDNA; MU-M
AB We present an analysis of the colors available for seven trans-neptunian objects (TNOs) and three centaurs among the reddest known, aimed at characterizing their surface chemical properties. In particular we seek to obtain evidence in support of the proposed correlation between the visible coloration of the surface of TNOs and their surface compositions (Brown, M.E., Schaller, EL., Fraser, W.C. [2011]. Astrophys. J. 739, L60).
The analysis focuses on nine available colors in the visible-near IR (0.3-4.5 gm) spectral range scaled to the V albedo to provide a proxy for the spectral shape of the objects. The colors include Spitzer IRAC data never published before, key in providing an effective constraint in the discrimination of ices contributing to the surface composition of the objects.
Compositions are obtained by comparing the data to a grid of radiative transfer models convolved by the filter response functions of the colors adopted in the spectrum-proxies to match the resolution of the observations. We find evidence suggesting the presence of hydrocarbons and/or methanol on the surfaces of most objects in our sample, supporting the hypothesis by Brown et al. (Brown, M.E., Schaller, E.L., Fraser, W.C. [2011]. Astrophys. J. 739, L60) that the coloration of red TNOs could be linked to their methanol content.
From our finding of methanol/hydrocarbon ices on the surfaces of the objects in our sample of very red TNOs and centaurs we infer that ultra-red objects in general might contain these ices and therefore might have formed in the outer part of the Solar System. We also deduce that the surfaces of most of the very red TNOs in our dataset are probably still quite pristine, and that their organic materials could have been produced by irradiation of the volatile ices whose traces are still present on their surface. Although our sample is small, we infer that the irradiation process is still in progress, as hinted by the centaurs' slightly elevated organic amounts at smaller perihelion distances. However, considering the relatively similar amounts of organics found in our data at a wide variety of perihelion distances, we also infer that it could have started before Neptune's migration.
The technique used to constrain the composition described as part of this study introduces a new approach at investigating the surface chemistry of the very small and numerous objects that constitute the bulk of the TNO and centaur populations. This innovative method has the potential to provide constraints for irradiation theories and for models of dynamical and chemical evolution of the Solar System. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Ore, C. Morea Dalle] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Ore, C. Morea Dalle; Cruikshank, D. P.; Roush, T. L.; Ore, L. V. Dalle] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barucci, M. A.; de Bergh, C.; Perna, D.; Merlin, F.] Univ Paris Diderot, Univ Paris 06, LESIA Observ Paris, CNRS, F-92195 Meudon, France.
[Emery, J. P.] Univ Tennessee, Earth & Planetary Sci Dept, Knoxville, TN 37919 USA.
RP Ore, CMD (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM Cristina.M.DalleOre@nasa.gov
FU Outer Planets Research grant [NASA NNX12AM75G]; NASA Planetary Astronomy
grant [NNX10AB23G]; NASA
FX CMDO and JPE acknowledge support from the Outer Planets Research grant
NASA NNX12AM75G and NASA Planetary Astronomy grant NNX10AB23G. This work
is based [in part] on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.
NR 138
TC 1
Z9 1
U1 0
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 MAY 15
PY 2015
VL 252
BP 311
EP 326
DI 10.1016/j.icarus.2015.01.014
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000026
ER
PT J
AU Estrada, PR
Durisen, RH
Cuzzi, JN
Morgan, DA
AF Estrada, Paul R.
Durisen, Richard H.
Cuzzi, Jeffrey N.
Morgan, Demitri A.
TI Combined structural and compositional evolution of planetary rings due
to micrometeoroid impacts and ballistic transport
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, rings; Impact processes; Disks
ID PARTICLE EROSION MECHANISMS; SATURNS MAIN RINGS; SELF-GRAVITY WAKES;
CASSINI VIMS; NUMERICAL SIMULATIONS; VELOCITY DISPERSION; SIZE
DISTRIBUTIONS; METEOROID IMPACTS; B-RING; INSTABILITY
AB We introduce improved numerical techniques for simulating the structural and compositional evolution of planetary rings due to micrometeoroid bombardment and subsequent ballistic transport of impact ejecta. Our current, robust code is capable of modeling structural changes and pollution transport simultaneously over long times on both local and global scales. In this paper, we describe the methodology based on the original structural code of Durisen et al. (Durisen, RH. et al. [1989]. Icarus 80,136-166) and on the pollution transport code of Cuzzi and Estrada (Cuzzi, J.N., Estrada, P.R. [1998]. Icarus 132, 1-35). We provide demonstrative simulations to compare with, and extend upon previous work, as well as examples of how ballistic transport can maintain the observed structure in Saturn's rings using available Cassini occultation optical depth data. In particular, we explicitly verify the claim that the inner B (and presumably A) ring edge can be maintained over long periods of time due to an ejecta distribution that is heavily biased in the prograde direction through a balance between the sharpening effects of ballistic transport and the broadening effects of viscosity. We also see that a "ramp"-like feature forms over time just inside that edge. However, it does not remain linear for the duration of the runs presented here unless a less steep ejecta velocity distribution is adopted. We also model the C ring plateaus and find that their outer edges can be maintained at their observed sharpness for long periods due to ballistic transport. We hypothesize that the addition of a significant component of a retrograde-biased ejecta distribution may help explain the linearity of the ramp and could provide a mechanism for maintaining the sharpness of C ring plateau inner edges. This component would arise for the subset of micrometeoroid impacts which are destructive rather than merely cratering. Such a distribution will be introduced in future work. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Estrada, Paul R.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Durisen, Richard H.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Morgan, Demitri A.] NASA, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Estrada, PR (reprint author), SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave 100, Mountain View, CA 94043 USA.
EM Paul.R.Estrada@nasa.gov
FU NASA's Cassini Data Analysis Program; Cassini IDS grant
FX The authors warmly thank Henrik Latter and Jurgen Schmidt for their
thoughtful and thorough reviews of this work which has led to great
improvement in its exposition. We thank Josh Colwell and Glen Stewart
for useful discussions. This work was supported by a grant from NASA's
Cassini Data Analysis Program (PRE), and a Cassini IDS grant to JNC.
NR 78
TC 2
Z9 2
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 15
PY 2015
VL 252
BP 415
EP 439
DI 10.1016/j.icarus.2015.02.005
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000034
ER
PT J
AU Gerakines, PA
Hudson, RL
AF Gerakines, Perry A.
Hudson, Reggie L.
TI The radiation stability of glycine in solid CO2 - In situ laboratory
measurements with applications to Mars
SO ICARUS
LA English
DT Article
DE Astrobiology; Cosmochemistry; Ices, IR spectroscopy; Mars
ID SOLAR-SYSTEM BODIES; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS; WATER; ICE;
SURFACE; SPACE; RADIOLYSIS; MATRIX
AB The detection of biologically important, organic molecules on Mars is an important goal that may soon be reached. However, the current small number of organic detections at the martian surface may be due to the harsh UV and radiation conditions there. It seems likely that a successful search will require probing the subsurface of Mars, where penetrating cosmic rays and solar energetic particles dominate the radiation environment, with an influence that weakens with depth. Toward the goal of understanding the survival of organic molecules in cold radiation-rich environments on Mars, we present new kinetics data on the radiolytic destruction of glycine diluted in frozen carbon dioxide. Rate constants were measured in situ with infrared spectroscopy, without additional sample manipulation, for irradiations at 25, 50, and 75 K with 0.8-MeV protons. The resulting half-lives for glycine in CO2-ice are compared to previous results for glycine in H2O-ice and show that glycine in CO2-ice is much less stable in a radiation environment, with destruction rate constants similar to 20-40 times higher than glycine in H2O-ice. Extrapolation of these results to conditions in the martian subsurface results in half-lives estimated to be less than 100-200 Myr even at depths of a few meters. Published by Elsevier
C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
EM perty.a.gerakines@nasa.gov
RI Gerakines, Perry/D-2226-2012
OI Gerakines, Perry/0000-0002-9667-5904
NR 30
TC 3
Z9 3
U1 4
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 15
PY 2015
VL 252
BP 466
EP 472
DI 10.1016/j.icarus.2015.02.008
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE8TW
UT WOS:000352118000037
ER
PT J
AU Hume, KL
Bayes, KD
Sander, SP
AF Hume, Kelly L.
Bayes, Kyle D.
Sander, Stanley P.
TI Equilibrium Constant for the Reaction ClO plus ClO <-> ClOOCl Between
250 and 206 K
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID CHLORINE PEROXIDE; ULTRAVIOLET-ABSORPTION; SELF-REACTION; NM;
TEMPERATURE; KINETICS; OZONE; SPECTRUM; BAND; CHLOROFLUOROMETHANES
AB The chlorine peroxide molecule, ClOOCl is an important participant in the chlorine-catalyzed destruction of ozone in the stratosphere. Very few laboratory measurements have been made for the partitioning between monomer ClO and dimer ClOOCl at temperatures lower than 280 K. This paper reports absorption spectra for both ClO and ClOOCl when they are in equilibrium at 1 atm and temperatures down to 206 K. The very low ClO concentrations involved requires measuring and calibrating a differential cross section, Delta sigma(ClO), for the 10-0 band Of ClO. A third law fit of the new results gives K-eq = [(2.01 +/- 0.17) 10(-27) cm(3) molecule(-1)] e((8554 -/+ 21)K/T), where the error limits reflect the uncertainty in the entropy change. The resulting equilibrium constants. are slightly lower than currently recommended. The slope of the van't Hoff plot yields a value for the enthalpy of formation of ClOOCl at 298 K, Delta H-f(o) of 129.8 +/- 0.6 kJ mol(-1). Uncertainties in the absolute ultraviolet cross sections of ClOOCl and ClO appear to be the limiting factors in these measurements. The new K-eq parameters are consistent with the measurements of Santee et al.(42) in the stratosphere.
C1 [Hume, Kelly L.; Bayes, Kyle D.; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bayes, KD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Kyle.D.Bayes@jpl.nasa.gov
FU National Aeronautics and Space Administration; Upper Atmosphere Research
and Tropospheric Chemistry programs; JPL Postdoctoral Program
FX This work acknowledges the pioneering contributions of Mario Molina and
his colleagues in elucidating the role of ClOOCl in the catalytic
destruction of ozone in the polar stratosphere. We thank John Barker,
University of Michigan, for access to his entropy calculations for ClO
and ClOOCl and for several useful discussions. This research was carried
out by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. This work was supported by the Upper Atmosphere Research
and Tropospheric Chemistry programs and the JPL Postdoctoral Program.
NR 40
TC 2
Z9 2
U1 3
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 MAY 14
PY 2015
VL 119
IS 19
BP 4473
EP 4481
DI 10.1021/jp510100n
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CI6YV
UT WOS:000354911000020
PM 25560546
ER
PT J
AU Hwang, SA
Crucian, B
Sams, C
Actor, JK
AF Hwang, Shen-An
Crucian, Brian
Sams, Clarence
Actor, Jeffrey K.
TI Post-Spaceflight (STS-135) Mouse Splenocytes Demonstrate Altered
Activation Properties and Surface Molecule Expression
SO PLOS ONE
LA English
DT Article
ID IMMUNE-SYSTEM DYSREGULATION; EPSTEIN-BARR-VIRUS; PERIPHERAL-BLOOD
LEUKOCYTES; SHORT-DURATION SPACEFLIGHT; SPACE-FLIGHT; HUMAN-LYMPHOCYTES;
LACTOFERRIN MODULATION; CYTOKINE PRODUCTION; EPIGENETIC CHANGES; APPLIED
PHYSIOLOGY
AB Alterations in immune function have been documented during or post-spaceflight and in ground based models of microgravity. Identification of immune parameters that are dysregulated during spaceflight is an important step in mitigating crew health risks during deep space missions. The in vitro analysis of leukocyte activity post-spaceflight in both human and animal species is primarily focused on lymphocytic function. This report completes a broader spectrum analysis of mouse lymphocyte and monocyte changes post 13 days orbital flight (mission STS-135). Analysis includes an examination in surface markers for cell activation, and antigen presentation and co-stimulatory molecules. Cytokine production was measured after stimulation with T-cell mitogen or TLR-2, TLR-4, or TLR-5 agonists. Splenocyte surface marker analysis immediate post-spaceflight and after in vitro culture demonstrated unique changes in phenotypic populations between the flight mice and matched treatment ground controls. Post-spaceflight splenocytes (flight splenocytes) had lower expression intensity of CD4(+)CD25(+) and CD8(+)CD25(+) cells, lower percentage of CD11c(+)MHC II+ cells, and higher percentage of CD11c(+)MHC I+ populations compared to ground controls. The flight splenocytes demonstrated an increase in phagocytic activity. Stimulation with ConA led to decrease in CD4(+) population but increased CD4(+)CD25(+) cells compared to ground controls. Culturing with TLR agonists led to a decrease in CD11c(+) population in splenocytes isolated from flight mice compared to ground controls. Consequently, flight splenocytes with or without TLR-agonist stimulation showed a decrease in CD11c+MHC I+, CD11c(+)MHC II+, and CD11c(+)CD86(+) cells compared to ground controls. Production of IFN-gamma was decreased and IL-2 was increased from ConA stimulated flight splenocytes. This study demonstrated that expression of surface molecules can be affected by conditions of spaceflight and impaired responsiveness persists under culture conditions in vitro.
C1 [Hwang, Shen-An; Actor, Jeffrey K.] Univ Texas Houston, Sch Med, Dept Pathol & Lab Med, Houston, TX 77030 USA.
[Crucian, Brian] NASA, Lyndon B Johnson Space Ctr, Div Biomed & Environm Sci, Houston, TX 77058 USA.
[Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Space & Clin Operat Div, Houston, TX 77058 USA.
RP Actor, JK (reprint author), Univ Texas Houston, Sch Med, Dept Pathol & Lab Med, Houston, TX 77030 USA.
EM Jeffrey.K.Actor@uth.tmc.edu
OI Actor, Jeffrey/0000-0002-9265-7012
NR 63
TC 3
Z9 5
U1 0
U2 4
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAY 13
PY 2015
VL 10
IS 5
AR e0124380
DI 10.1371/journal.pone.0124380
PG 19
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CI1ZP
UT WOS:000354544200037
PM 25970640
ER
PT J
AU Goldstein, ML
Wicks, RT
Perri, S
Sahraoui, F
AF Goldstein, M. L.
Wicks, R. T.
Perri, S.
Sahraoui, F.
TI Kinetic scale turbulence and dissipation in the solar wind: key
observational results and future outlook
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE solar wind; turbulence; plasma heating; turbulent dissipation
ID ION-CYCLOTRON WAVES; INTERPLANETARY MAGNETIC-FIELD; OUTWARD PROPAGATING
WAVES; ELECTRON HEAT-CONDUCTION; FREQUENCY ALFVEN WAVES; 1 AU;
MAGNETOHYDRODYNAMIC TURBULENCE; SHELL-MODEL; HALL MAGNETOHYDRODYNAMICS;
HOMOGENEOUS TURBULENCE
AB Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbulence to solar wind dynamics.
C1 [Goldstein, M. L.; Wicks, R. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wicks, R. T.] Univ Maryland, Dept Astron, GPHI, College Pk, MD 20742 USA.
[Perri, S.] Univ Calabria, Dipartimento Fis, I-87036 Arcavacata Di Rende, Italy.
[Sahraoui, F.] Ecole Polytech, CNRS UPMC, Lab Phys Plasmas, F-91128 Palaiseau, France.
RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20771 USA.
EM melvyn.l.goldstein@nasa.gov
RI Wicks, Robert/A-1180-2009
OI Wicks, Robert/0000-0002-0622-5302
FU NASA GI grant; NASA HSR grant at Goddard Space Flight Center; Borsa
Postdoc POR Calabria FSE; project THESOW - L'Agence Nationale de la
Recherche (ANR, France)
FX R.T.W. is funded by a NASA GI grant and a NASA HSR grant at Goddard
Space Flight Center. S.P.'s research is supported by 'Borsa Postdoc POR
Calabria FSE 2007/2013'. F.S. was supported, in part, by the project
THESOW funded by L'Agence Nationale de la Recherche (ANR, France).
NR 150
TC 10
Z9 10
U1 2
U2 25
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD MAY 13
PY 2015
VL 373
IS 2041
AR 20140147
DI 10.1098/rsta.2014.0147
PG 21
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CG5BK
UT WOS:000353304500004
ER
PT J
AU Roytershteyn, V
Karimabadi, H
Roberts, A
AF Roytershteyn, Vadim
Karimabadi, Homa
Roberts, Aaron
TI Generation of magnetic holes in fully kinetic simulations of
collisionless turbulence
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE plasma turbulence; magnetic holes; fully kinetic simulations
ID SOLAR-WIND; PLASMA; FIELD
AB The results of three-dimensional fully kinetic simulations of decaying turbulence with the amplitude of the fluctuating magnetic field comparable to that of the mean field are presented. Coherent structures in the form of localized depressions in the magnitude of the magnetic field are observed to form self-consistently in the simulations. These depressions bear considerable resemblance to the so-called magnetic holes frequently reported in spacecraft observations. The structures are pressure-balanced and tend to be aligned with the local magnetic field. In the smallest structures observed, the decrease in the magnetic field strength is compensated by an increase in the electron perpendicular pressure, such that the transverse size of these structures is comparable to the electron gyroradius inside the depression. It is suggested that the structures evolve self-consistently out of the depressions in the fluctuating magnetic field, rather than being the consequence of instability growth and saturation. This is confirmed by additional, small-scale simulations, including those with realistic mass ratio between protons and electrons.
C1 [Roytershteyn, Vadim; Karimabadi, Homa] SciberQuest Inc, Del Mar, CA 92014 USA.
[Roytershteyn, Vadim] Space Sci Inst, Boulder, CO 80301 USA.
[Roberts, Aaron] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Roytershteyn, V (reprint author), SciberQuest Inc, Del Mar, CA 92014 USA.
EM vroytershteyn@spacescience.org
OI Roytershteyn, Vadim/0000-0003-1745-7587
FU NASA at SSI [NNX14AI63G]; National Science Foundation [OCI-0725070,
ACI-1238993]; State of Illinois
FX We gratefully acknowledge support from NASA grant NNX14AI63G at SSI.
This research is part of the Blue Waters sustained-petascale computing
project, which is supported by the National Science Foundation (awards
OCI-0725070 and ACI-1238993) 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. Additional simulations
were performed on the Pleiades supercomputer provided by the NASA HEC
program.
NR 21
TC 9
Z9 9
U1 1
U2 5
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 MAY 13
PY 2015
VL 373
IS 2041
AR 20140151
DI 10.1098/rsta.2014.0151
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CG5BK
UT WOS:000353304500008
ER
PT J
AU Papadopoulos, A
D'Andrea, CB
Sullivan, M
Nichol, RC
Barbary, K
Biswas, R
Brown, PJ
Covarrubias, RA
Finley, DA
Fischer, JA
Foley, RJ
Goldstein, D
Gupta, RR
Kessler, R
Kovacs, E
Kuhlmann, SE
Lidman, C
March, M
Nugent, PE
Sako, M
Smith, RC
Spinka, H
Wester, W
Abbott, TMC
Abdalla, F
Allam, SS
Banerji, M
Bernstein, JP
Bernstein, RA
Carnero, A
da Costa, LN
DePoy, DL
Desai, S
Diehl, HT
Eifler, T
Evrard, AE
Flaugher, B
Frieman, JA
Gerdes, D
Gruen, D
Honscheid, K
James, D
Kuehn, K
Kuropatkin, N
Lahav, O
Maia, MAG
Makler, M
Marshall, JL
Merritt, KW
Miller, CJ
Miquel, R
Ogando, R
Plazas, AA
Roe, NA
Romer, AK
Rykoff, E
Sanchez, E
Santiago, BX
Scarpine, V
Schubnell, M
Sevilla, I
Soares-Santos, M
Suchyta, E
Swanson, M
Tarle, G
Thaler, J
Tucker, LD
Wechsler, RH
Zuntz, J
AF Papadopoulos, A.
D'Andrea, C. B.
Sullivan, M.
Nichol, R. C.
Barbary, K.
Biswas, R.
Brown, P. J.
Covarrubias, R. A.
Finley, D. A.
Fischer, J. A.
Foley, R. J.
Goldstein, D.
Gupta, R. R.
Kessler, R.
Kovacs, E.
Kuhlmann, S. E.
Lidman, C.
March, M.
Nugent, P. E.
Sako, M.
Smith, R. C.
Spinka, H.
Wester, W.
Abbott, T. M. C.
Abdalla, F.
Allam, S. S.
Banerji, M.
Bernstein, J. P.
Bernstein, R. A.
Carnero, A.
da Costa, L. N.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Eifler, T.
Evrard, A. E.
Flaugher, B.
Frieman, J. A.
Gerdes, D.
Gruen, D.
Honscheid, K.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Maia, M. A. G.
Makler, M.
Marshall, J. L.
Merritt, K. W.
Miller, C. J.
Miquel, R.
Ogando, R.
Plazas, A. A.
Roe, N. A.
Romer, A. K.
Rykoff, E.
Sanchez, E.
Santiago, B. X.
Scarpine, V.
Schubnell, M.
Sevilla, I.
Soares-Santos, M.
Suchyta, E.
Swanson, M.
Tarle, G.
Thaler, J.
Tucker, L. D.
Wechsler, R. H.
Zuntz, J.
TI DES13S2cmm: the first superluminous supernova from the Dark Energy
Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; supernovae: general; supernovae: individual: DES13S2cmm
ID BARYON ACOUSTIC-OSCILLATIONS; HUBBLE-SPACE-TELESCOPE; IA SUPERNOVAE;
HIGH-REDSHIFT; LUMINOUS SUPERNOVAE; PAIR-INSTABILITY; LIGHT-CURVE;
COSMOLOGICAL CONSTRAINTS; ULTRALUMINOUS SUPERNOVAE; IC SUPERNOVAE
AB We present DES13S2cmm, the first spectroscopically-confirmed superluminous supernova (SLSN) from the Dark Energy Survey (DES). We briefly discuss the data and search algorithm used to find this event in the first year of DES operations, and outline the spectroscopic data obtained from the European Southern Observatory (ESO) Very Large Telescope to confirm its redshift (z = 0.663 +/- 0.001 based on the host-galaxy emission lines) and likely spectral type (Type I). Using this redshift, we find M-U(peak) = -21.05(-0.09)(+0.10) for the peak, rest-frame U-band absolute magnitude, and find DES13S2cmm to be located in a faint, low-metallicity (subsolar), low stellar-mass host galaxy (log (M/M-circle dot) = 9.3 +/- 0.3), consistent with what is seen for other SLSNe-I. We compare the bolometric light curve of DES13S2cmm to 14 similarly well-observed SLSNe-I in the literature and find that it possesses one of the slowest declining tails (beyond +30 d rest-frame past peak), and is the faintest at peak. Moreover, we find the bolometric light curves of all SLSNe-I studied herein possess a dispersion of only 0.2-0.3 mag between +25 and +30 d after peak (rest frame) depending on redshift range studied; this could be important for 'standardizing' such supernovae, as is done with the more common Type Ia. We fit the bolometric light curve of DES13S2cmm with two competing models for SLSNe-I-the radioactive decay of Ni-56, and a magnetar - and find that while the magnetar is formally a better fit, neither model provides a compelling match to the data. Although we are unable to conclusively differentiate between these two physical models for this particular SLSN-I, further DES observations of more SLSNe-I should break this degeneracy, especially if the light curves of SLSNe-I can be observed beyond 100 d in the rest frame of the supernova.
C1 [Papadopoulos, A.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Barbary, K.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Biswas, R.; Gupta, R. R.; Kovacs, E.; Kuhlmann, S. E.; Spinka, H.; Bernstein, J. P.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Brown, P. J.; DePoy, D. L.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX USA.
[Covarrubias, R. A.; Allam, S. S.; Swanson, M.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Covarrubias, R. A.; Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Finley, D. A.; Wester, W.; Diehl, H. T.; Flaugher, B.; Frieman, J. A.; Kuropatkin, N.; Merritt, K. W.; Scarpine, V.; Soares-Santos, M.; Tucker, L. D.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Fischer, J. A.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Foley, R. J.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Goldstein, D.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Goldstein, D.; Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Kessler, R.; Frieman, J. A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kessler, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Lidman, C.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Smith, R. C.; Abbott, T. M. C.; James, D.] Natl Optic Astron Observ, Ctr Tololo Interamer Observ, La Serena, Chile.
[Abdalla, F.; Banerji, M.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Allam, S. S.] Space Telescope Sci Inst STScI, Baltimore, MD 21218 USA.
[Bernstein, R. A.] Carnegie Observ, Pasadena, CA 91101 USA.
[Carnero, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carnero, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.; Santiago, B. X.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Desai, S.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Desai, S.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Eifler, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evrard, A. E.; Gerdes, D.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany.
[Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Plazas, A. A.] Brookhaven Natl Lab, Dept Phys, Upton, NY 11973 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Rykoff, E.; Sevilla, I.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Sanchez, E.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain.
[Santiago, B. X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Zuntz, J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Papadopoulos, A (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England.
EM andreas.papadopoulos@port.ac.uk
RI Ogando, Ricardo/A-1747-2010; Sanchez, Eusebio/H-5228-2015; Makler,
Martin/G-2639-2012;
OI Ogando, Ricardo/0000-0003-2120-1154; Sanchez,
Eusebio/0000-0002-9646-8198; Makler, Martin/0000-0003-2206-2651;
Suchyta, Eric/0000-0002-7047-9358; Evrard, August/0000-0002-4876-956X;
Abdalla, Filipe/0000-0003-2063-4345; Sullivan, Mark/0000-0001-9053-4820
FU SEPnet; Faculty of Technology of the University of Portsmouth; Royal
Society; EU/FP7-ERC [615929]; NASA; ESO telescopes at the La Silla
Paranal Observatory under DDT programme [ID 292.D-5013]; US Department
of Energy; US National Science Foundation; Ministry of Science and
Education of Spain; Science and Technology Facilities Council of the
United Kingdom; Higher Education Funding Council for England; National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign; Kavli Institute of Cosmological Physics at the
University of Chicago; Financiadora de Estudos e Projetos; Fundacao
Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro;
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico;
Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft;
Argonne National Laboratory; University of California at Santa Cruz;
University of Cambridge; Centro de Investigaciones Energeticas;
Medioambientales y Tecnologicas-Madrid; University of Chicago;
University College London; DES-Brazil Consortium; Eidgenossische
Technische Hochschule (ETH) Zurich; Fermi National Accelerator
Laboratory; University of Edinburgh; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat; associated Excellence Cluster Universe;
University of Michigan; National Optical Astronomy Observatory;
University of Nottingham; Ohio State University; University of
Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory; Stanford University; University of Sussex; Texas AM
University
FX We wish to thank Kate Maguire for her assistance with the ESO VLT
Directors Discretionary Time proposal. We also thank Cosimo Inserra and
Stephen Smartt for helpful discussions regarding the classification,
standardization and k-corrections of superluminous supernovae. AP
acknowledges the financial support of SEPnet (www.sepnet.ac.uk) and the
Faculty of Technology of the University of Portsmouth. Likewise, CD and
RN thank the support of the Faculty of Technology of the University of
Portsmouth during this research, and MS acknowledges support from the
Royal Society and EU/FP7-ERC grant no [615929]. Part of TE's research
was carried out at JPL/Caltech, under a contract with NASA.; Based on
observations made with ESO telescopes at the La Silla Paranal
Observatory under DDT programme ID 292.D-5013.; We are grateful for the
extraordinary contributions of our CTIO colleagues and the DES Camera,
Commissioning and Science Verification teams in achieving the excellent
instrument and telescope conditions that have made this work possible.
The success of this project also relies critically on the expertise and
dedication of the DES Data Management organization. Funding for the DES
Projects has been provided by the US Department of Energy, the US
National Science Foundation, the Ministry of Science and Education of
Spain, the Science and Technology Facilities Council of the United
Kingdom, the Higher Education Funding Council for England, the National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign, the Kavli Institute of Cosmological Physics at the
University of Chicago, Financiadora de Estudos e Projetos, Fundacao
Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro,
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the
Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft
and the Collaborating Institutions in the Dark Energy Survey.; The
Collaborating Institutions are Argonne National Laboratory, the
University of California at Santa Cruz, the University of Cambridge,
Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat and the associated Excellence Cluster
Universe, the University of Michigan, the National Optical Astronomy
Observatory, the University of Nottingham, The Ohio State University,
the University of Pennsylvania, the University of Portsmouth, SLAC
National Accelerator Laboratory, Stanford University, the University of
Sussex, and Texas A&M University.
NR 67
TC 17
Z9 17
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 MAY 11
PY 2015
VL 449
IS 2
BP 1215
EP 1227
DI 10.1093/mnras/stv174
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TN
UT WOS:000355337500003
ER
PT J
AU Shimwell, TW
Markevitch, M
Brown, S
Feretti, L
Gaensler, BM
Johnston-Hollitt, M
Lage, C
Srinivasan, R
AF Shimwell, Timothy W.
Markevitch, Maxim
Brown, Shea
Feretti, Luigina
Gaensler, B. M.
Johnston-Hollitt, M.
Lage, Craig
Srinivasan, Raghav
TI Another shock for the Bullet cluster, and the source of seed electrons
for radio relics
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE acceleration of particles; radiation mechanisms: non-thermal; shock
waves; galaxies: clusters: individual: 1E 0657-55.8; galaxies: clusters:
intracluster medium; radio continuum general
ID MERGING GALAXY CLUSTER; X-RAY OBSERVATIONS; HOTTEST KNOWN CLUSTER;
CHANDRA OBSERVATION; COMA CLUSTER; 1E 0657-56; PARTICLE-ACCELERATION;
INTRACLUSTER MEDIUM; CIZA J2242.8+5301; ABELL 2146
AB With Australia Telescope Compact Array observations, we detect a highly elongated Mpc-scale diffuse radio source on the eastern periphery of the Bullet cluster 1E 0657-55.8, which we argue has the positional, spectral and polarimetric characteristics of a radio relic. This powerful relic (2.3 +/- 0.1 x 10(25) W Hz(-1)) consists of a bright northern bulb and a faint linear tail. The bulb emits 94 per cent of the observed radio flux and has the highest surface brightness of any known relic. Exactly coincident with the linear tail, we find a sharp X-ray surface brightness edge in the deep Chandra image of the cluster - a signature of a shock front in the hot intracluster medium (ICM), located on the opposite side of the cluster to the famous bow shock. This new example of an X-ray shock coincident with a relic further supports the hypothesis that shocks in the outer regions of clusters can form relics via diffusive shock (re-) acceleration. Intriguingly, our new relic suggests that seed electrons for reacceleration are coming from a local remnant of a radio galaxy, which we are lucky to catch before its complete disruption. If this scenario, in which a relic forms when a shock crosses a well-defined region of the ICM polluted with aged relativistic plasma - as opposed to the usual assumption that seeds are uniformly mixed in the ICM - is also the case for other relics, this may explain a number of peculiar properties of peripheral relics.
C1 [Shimwell, Timothy W.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Shimwell, Timothy W.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Brown, Shea] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Feretti, Luigina] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Johnston-Hollitt, M.; Srinivasan, Raghav] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6014, New Zealand.
[Lage, Craig] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
RP Shimwell, TW (reprint author), CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia.
EM tws29@mrao.cam.ac.uk
FU Commonwealth of Australia; Australian Research Council [FL100100114];
Marsden Fund
FX The ATCA is part of the Australia Telescope National Facility which is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. BMG acknowledges the support of Australian
Laureate Fellowship FL100100114 from the Australian Research Council.
MJH acknowledges support from the Marsden Fund. MJH acknowledges support
from the Marsden Fund. We thank Douglas Clowe for kindly providing the
R-band image and we thank the anonymous referee for comments.
NR 61
TC 23
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 11
PY 2015
VL 449
IS 2
BP 1486
EP 1494
DI 10.1093/mnras/stv334
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TN
UT WOS:000355337500027
ER
PT J
AU Smith, N
Mauerhan, JC
Cenko, SB
Kasliwal, MM
Silverman, JM
Filippenko, AV
Gal-Yam, A
Clubb, KI
Graham, ML
Leonard, DC
Horst, JC
Williams, GG
Andrews, JE
Kulkarni, SR
Nugent, P
Sullivan, M
Maguire, K
Xu, D
Ben-Ami, S
AF Smith, Nathan
Mauerhan, Jon C.
Cenko, S. Bradley
Kasliwal, Mansi M.
Silverman, Jeffrey M.
Filippenko, Alexei V.
Gal-Yam, Avishay
Clubb, Kelsey I.
Graham, Melissa L.
Leonard, Douglas C.
Horst, J. Chuck
Williams, G. Grant
Andrews, Jennifer E.
Kulkarni, Shrinivas R.
Nugent, Peter
Sullivan, Mark
Maguire, Kate
Xu, Dong
Ben-Ami, Sagi
TI PTF11iqb: cool supergiant mass-loss that bridges the gap between Type
IIn and normal supernovae
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; stars: evolution; supernovae: general; supernovae:
individual: PTF11iqb; stars: winds, outflows
ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; SN 2009IP CONSTRAINTS; DIGITAL SKY
SURVEY; CIRCUMSTELLAR INTERACTION; DUST FORMATION; IA SUPERNOVAE; LIGHT
CURVES; PHOTOMETRIC CALIBRATION; LUMINOUS SUPERNOVAE; STANDARD STARS
AB The supernova (SN) PTF11iqb was initially classified as a Type IIn event caught very early after explosion. It showed narrowWolf-Rayet (WR) spectral features on day 2 (as in SN 1998S and SN 2013cu), but the narrow emission weakened quickly and the spectrum morphed to resemble Types II-L and II-P. At late times, H alpha exhibited a complex, multipeaked profile reminiscent of SN 1998S. In terms of spectroscopic evolution, we find that PTF11iqb was a near twin of SN 1998S, although with somewhat weaker interaction with circumstellar material (CSM) at early times, and stronger interaction at late times. We interpret the spectral changes as caused by early interaction with asymmetric CSM that is quickly (by day 20) enveloped by the expanding SN ejecta photosphere, but then revealed again after the end of the plateau when the photosphere recedes. The light curve can be matched with a simple model for CSM interaction (with a mass-loss rate of roughly 10(-4) M-circle dot yr(-1)) added to the light curve of a normal SN II-P. The underlying plateau requires a progenitor with an extended hydrogen envelope like a red supergiant at the moment of explosion, consistent with the slow wind speed (<80 km s(-1)) inferred from narrow H alpha emission. The cool supergiant progenitor is significant because PTF11iqb showed WR features in its early spectrum - meaning that the presence of such WR features does not necessarily indicate a WR-like progenitor. Overall, PTF11iqb bridges SNe IIn with weaker pre-SN mass-loss seen in SNe II-L and II-P, implying a continuum between these types.
C1 [Smith, Nathan; Mauerhan, Jon C.; Williams, G. Grant; Andrews, Jennifer E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Mauerhan, Jon C.; Filippenko, Alexei V.; Clubb, Kelsey I.; Graham, Melissa L.; Nugent, Peter] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cenko, S. Bradley] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kasliwal, Mansi M.; Kulkarni, Shrinivas R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Gal-Yam, Avishay; Xu, Dong; Ben-Ami, Sagi] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Leonard, Douglas C.; Horst, J. Chuck] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Williams, G. Grant] Univ Arizona, Multiple Mirror Telescope Observ, Tucson, AZ 85721 USA.
[Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA.
[Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Maguire, Kate] European Southern Observ Astron Res Southern Hemi, D-85748 Garching, Germany.
RP Smith, N (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM nathans@as.arizona.edu
OI Sullivan, Mark/0000-0001-9053-4820
FU W.M. Keck Foundation; NSF [AST-1210599, AST-1312221, AST-1211916,
AST-1009571, AST-1210311]; Willner Family Leadership Institute Ilan
Gluzman (Secaucus NJ); Israeli Ministry of Science; Israel Science
Foundation; Minerva; I-CORE Program of the Planning and Budgeting
Committee; EU/FP7 via ERC [307260]; Quantum Universe I-Core program by
the Israeli Committee; ISF; WIS-UK 'making connections'; Kimmel and
ARCHES awards; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund;
Christopher R. Redlich Fund; TABASGO Foundation; NSF Astronomy and
Astrophysics Postdoctoral Fellowship [AST-1302771]; Marie Curie
Intra-European Fellowship, within the 7th European Community Framework
Programme (FP7); Royal Society
FX We thank Iair Arcavi, Peter Blanchard, Yi Cao, Ori Fox, Paul Groot, Asaf
Horesh, Michael Kandrashoff, Pat Kelly, Nick Konidaris, Rubina Kotak,
David Levitan, Adam Miller, Yen-Chen Pan, Jarod Parrent, Paul Smith, and
WeiKang Zheng for assistance with some of the observations and data
reduction. We thank Eran Ofek for helpful discussions and assistance
with the PTF photometric data. We thank the referee, Max Stritzinger,
for a careful reading of the manuscript and helpful comments. We thank
the staffs at Lick, MMT, LBT, Keck, Palomar, and WHT for their
assistance with the observations. Observations using Steward Observatory
facilities were obtained as part of the observing program AZTEC: Arizona
Transient Exploration and Characterization. Some observations reported
here were obtained at the MMT Observatory, a joint facility of the
University of Arizona and the Smithsonian Institution. This research was
based in part on observations made with the LBT. The LBT is an
international collaboration among institutions in the United States,
Italy and Germany. The LBT Corporation partners are: the University of
Arizona on behalf of the Arizona university system; the Istituto
Nazionale di Astrofisica, Italy; the LBT Beteiligungsgesellschaft,
Germany, representing the Max-Planck Society, the Astrophysical
Institute Potsdam and Heidelberg University; the Ohio State University
and the Research Corporation, on behalf of the University of Notre Dame,
University of Minnesota and University of Virginia. The WHT is operated
on the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de AstrofAsica
de Canarias. Some of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California and
NASA; the observatory was made possible by the generous financial
support of the W.M. Keck Foundation. The authors wish to recognize and
acknowledge the very significant cultural role and reverence that the
summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain.; NS received partial support from NSF
grants AST-1210599 and AST-1312221. E.O.O. is incumbent of the Arye
Dissentshik career development chair and is grateful to support by
grants from the Willner Family Leadership Institute Ilan Gluzman
(Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation,
Minerva and the I-CORE Program of the Planning and Budgeting Committee
and The Israel Science Foundation. AGY is supported by the EU/FP7 via
ERC grant no. 307260, the Quantum Universe I-Core program by the Israeli
Committee for planning and funding, and the ISF, Minerva and ISF grants,
WIS-UK 'making connections,' and Kimmel and ARCHES awards. The supernova
research of AVF's group at U.C. Berkeley is supported by Gary & Cynthia
Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich
Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is
supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship
under award AST-1302771. KM is supported by a Marie Curie Intra-European
Fellowship, within the 7th European Community Framework Programme (FP7).
MS acknowledges support from the Royal Society. DCL and JCH are grateful
for support from NSF grants AST-1009571 and AST-1210311, under which
part of this research (photometry collected at MLO) was carried out.
NR 120
TC 25
Z9 25
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 11
PY 2015
VL 449
IS 2
BP 1876
EP 1896
DI 10.1093/mnras/stv354
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TN
UT WOS:000355337500060
ER
PT J
AU Kobayashi, MIN
Leauthaud, A
More, S
Okabe, N
Laigle, C
Rhodes, J
Takeuchi, TT
AF Kobayashi, Masato I. N.
Leauthaud, Alexie
More, Surhud
Okabe, Nobuhiro
Laigle, Clotilde
Rhodes, Jason
Takeuchi, Tsutomu T.
TI Can we use weak lensing to measure total mass profiles of galaxies on 20
kpc scales?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; galaxies: haloes; galaxies: stellar
content; galaxies: structure; cosmology: observations; large-scale
structure of Universe
ID DARK-MATTER HALOS; HUBBLE-SPACE-TELESCOPE; STELLAR POPULATION SYNTHESIS;
DENSITY PROFILES; COSMIC EVOLUTION; COSMOLOGICAL SIMULATIONS; SHAPE
MEASUREMENT; BARYONIC INFALL; ADVANCED CAMERA; ACS SURVEY
AB Current constraints on dark matter density profiles from weak lensing are typically limited to radial scales greater than 50-100 kpc. In this paper, we explore the possibility of probing the very inner regions of galaxy/halo density profiles by measuring stacked weak lensing on scales of only a few tens of kpc. Our forecasts focus on scales smaller than the 'equality radius' (R-eq), where the stellar component and the dark matter component contribute equally to the lensing signal. We compute the evolution of R-eq as a function of lens stellar mass and redshift and show that R-eq = 7-34 kpc for galaxies with M-* = 10(9.5)-10(11.5) M-circle dot. Unbiased shear measurements will be challenging on these scales. We introduce a simple metric to quantify how many source galaxies overlap with their neighbours and for which shear measurements will be challenging. Rejecting source galaxies with close-by companions results in an similar to 20 per cent decrease in the overall source density. Despite this decrease, we show that Euclid and Wide Field Infrared Survey Telescope will be able to constrain galaxy/halo density profiles at R-eq with S/N > 20 for M-* > 10(10) M-circle dot. Weak lensing measurements at R-eq, in combination with stellar kinematics on smaller scales, will be a powerful means by which to constrain both the inner slope of the dark matter density profile as well as the mass and redshift dependence of the stellar initial mass function.
C1 [Kobayashi, Masato I. N.; Takeuchi, Tsutomu T.] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.
[Leauthaud, Alexie; More, Surhud; Okabe, Nobuhiro] Univ Tokyo, WPI, Kavli IPMU, Chiba 2778582, Japan.
[Laigle, Clotilde] Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France.
[Laigle, Clotilde] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75005 Paris, France.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA.
RP Kobayashi, MIN (reprint author), Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.
EM masato.kobayashi@nagoya-u.jp
OI Kobayashi, Masato/0000-0003-3990-1204
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; Ministry of Education, Culture, Sports, Science, and
Technology of Japan [25287057, 26800097]; ILP LABEX [ANR-10-LABX-63,
ANR-11-IDEX-0004-02]; JPL, under a contract for NASA by Caltech;
[23340046]
FX We are grateful to the referee for a careful reading of the manuscript
and for providing thoughtful comments. We thank Robert Lupton for useful
discussions during the preparation of this paper and Naoshi Sugiyama for
practical advice during the data analysis. This work, AL, and SM are
supported by World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan. MINK acknowledges the financial support from
N. Sugiyama (25287057) by Grants-in-Aid from the Ministry of Education,
Culture, Sports, Science, and Technology of Japan. NO (26800097) is
supported by Grants-in-Aid from the Ministry of Education, Culture,
Sports, Science, and Technology of Japan. CL is supported by the ILP
LABEX (under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-02). JR was
supported by JPL, run under a contract for NASA by Caltech. TTT has been
supported by the Grant-in-Aid for the Scientific Research Fund
(23340046), for the Global COE Program Request for Fundamental
Principles in the Universe: from Particles to the Solar system and the
Cosmos, and for the JSPS Strategic Young Researcher Overseas Visits
Program for Accelerating Brain Circulation, commissioned by the Ministry
of Education, Culture, Sports, Science and Technology (MEXT) of Japan.
NR 85
TC 3
Z9 3
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 11
PY 2015
VL 449
IS 2
BP 2128
EP 2143
DI 10.1093/mnras/stv424
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2TN
UT WOS:000355337500078
ER
PT J
AU Allman, MS
Verma, VB
Stevens, M
Gerrits, T
Horansky, RD
Lita, AE
Marsili, F
Beyer, A
Shaw, MD
Kumor, D
Mirin, R
Nam, SW
AF Allman, M. S.
Verma, V. B.
Stevens, M.
Gerrits, T.
Horansky, R. D.
Lita, A. E.
Marsili, F.
Beyer, A.
Shaw, M. D.
Kumor, D.
Mirin, R.
Nam, S. W.
TI A near-infrared 64-pixel superconducting nanowire single photon detector
array with integrated multiplexed readout
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID CIRCUIT; SPECTROPHOTOMETER; EFFICIENCY
AB We demonstrate a 64-pixel free-space-coupled array of superconducting nanowire single photon detectors optimized for high detection efficiency in the near-infrared range. An integrated, readily scalable, multiplexed readout scheme is employed to reduce the number of readout lines to 16. The cryogenic, optical, and electronic packaging to read out the array as well as characterization measurements are discussed. (C) 2015 AIP Publishing LLC.
C1 [Allman, M. S.; Verma, V. B.; Stevens, M.; Gerrits, T.; Horansky, R. D.; Lita, A. E.; Mirin, R.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
[Marsili, F.; Beyer, A.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kumor, D.] Purdue Univ, W Lafayette, IN 47907 USA.
RP Allman, MS (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA.
EM shane.allman@boulder.nist.gov
OI Mirin, Richard/0000-0002-4472-4655
FU NIST; DARPA INPHO program
FX This work was supported by NIST and the DARPA INPHO program.
NR 27
TC 16
Z9 16
U1 6
U2 24
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAY 11
PY 2015
VL 106
IS 19
AR 192601
DI 10.1063/1.4921318
PG 4
WC Physics, Applied
SC Physics
GA CI8GI
UT WOS:000355008100024
ER
PT J
AU Stoffle, N
Pinsky, L
Kroupa, M
Hoang, S
Idarraga, J
Amberboy, C
Rios, R
Hauss, J
Keller, J
Bahadori, A
Semones, E
Turecek, D
Jakubek, J
Vykydal, Z
Pospisil, S
AF Stoffle, Nicholas
Pinsky, Lawrence
Kroupa, Martin
Hoang, Son
Idarraga, John
Amberboy, Clif
Rios, Ryan
Hauss, Jessica
Keller, John
Bahadori, Amir
Semones, Edward
Turecek, Daniel
Jakubek, Jan
Vykydal, Zdenek
Pospisil, Stanislav
TI Timepix-based radiation environment monitor measurements aboard the
International Space Station
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Timepix; Medipix; International Space Station; Ionizing radiation; Pixel
detector; Active dosimeter
ID DETECTOR
AB A number of small, single element radiation detectors, employing the CERN-based Medipix2 Collaboration's Timepix Application Specific Integrated Circuit (ASIC) coupled to a specially modified version of the USB-Lite interface for that ASIC providecl by the Institute for Experimental and Applied Physics (LEAP) at the Czech Technical University in Prague, have been developed at the University of Houston and NASA Johnson Space Center. These detectors, officially designated by NASA as Radiation Environment Monitors (REMs), were deployed aboard the International Space Station in late 2012. Six REM units are currently operating on Station Support Computers (SSCs) and returning data on a daily basis. The associated data acquisition software on the SSCs provides both automated data collection and transfer, as well as algorithms to handle adjustment of acquisition rates and recovery and restart of the acquisition software. A suite of ground software analysis tools has been developed to allow rapid analysis of the data and provides a ROOT-based framework for extending data analysis capabilities. (C) 2015 Elsevier B.V. All rights reserved,
C1 [Stoffle, Nicholas; Pinsky, Lawrence; Kroupa, Martin; Hoang, Son; Idarraga, John] Univ Houston, Houston, TX 77251 USA.
[Stoffle, Nicholas; Amberboy, Clif; Rios, Ryan; Hauss, Jessica] Lockheed Martin, Houston, TX USA.
[Keller, John] Wyle Labs, Houston, TX USA.
[Bahadori, Amir; Semones, Edward] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Turecek, Daniel; Jakubek, Jan; Vykydal, Zdenek; Pospisil, Stanislav] Czech Tech Univ, Inst Expt & Appl Phys, CR-16635 Prague, Czech Republic.
RP Stoffle, N (reprint author), Univ Houston, 3700 Calhoun, Houston, TX 77251 USA.
RI Vykydal, Zdenek/H-6426-2016
OI Vykydal, Zdenek/0000-0003-2329-0672
NR 17
TC 6
Z9 6
U1 3
U2 21
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
EI 1872-9576
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD MAY 11
PY 2015
VL 782
BP 143
EP 148
DI 10.1016/j.nima.2015.02.016
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA CD4PL
UT WOS:000351065600020
ER
PT J
AU Badnell, NR
Ferland, GJ
Gorczyca, TW
Nikolic, D
Wagle, GA
AF Badnell, N. R.
Ferland, G. J.
Gorczyca, T. W.
Nikolic, D.
Wagle, G. A.
TI BOOTSTRAPPING DIELECTRONIC RECOMBINATION FROM SECOND-ROW ELEMENTS AND
THE ORION NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic data; atomic processes; galaxies: abundances; ISM: abundances
ID FINITE-DENSITY PLASMAS; MODEL ATMOSPHERES; RATE COEFFICIENTS;
CHARGE-TRANSFER; STARS; IONS; ABUNDANCES; RADIATION; REGIONS; CLOUDY
AB Dielectronic recombination (DR) is the dominant recombination process for most heavy elements in photoionized clouds. Accurate DR rates for a species can be predicted when the positions of autoionizing states are known. Unfortunately such data are not available for most third-and higher-row elements. This introduces an uncertainty that is especially acute for photoionized clouds, where the low temperatures mean that DR occurs energetically through very low-lying autoionizing states. This paper discusses S2+ -> S+ DR, the process that is largely responsible for establishing the [S III]/[S II] ratio in nebulae. We derive an empirical rate coefficient using a novel method for second-row ions, which do have accurate data. Photoionization models are used to reproduce the [O III]/ [O II]/[O I]/[Ne III] intensity ratios in central regions of the Orion Nebula. O and Ne have accurate atomic data and can be used to derive an empirical S2+ -> S+ DR rate coefficient at similar to 10(4) K. We present new calculations of the DR rate coefficient for S2+ -> S+ and quantify how uncertainties in the autoionizing level positions affect it. The empirical and theoretical results are combined and we derive a simple fit to the resulting rate coefficient at all temperatures for incorporation into spectral synthesis codes. This method can be used to derive empirical DR rates for other ions, provided that good observations of several stages of ionization of O and Ne are available.
C1 [Badnell, N. R.] Univ Strathclyde, Glasgow G4 0NG, Lanark, Scotland.
[Ferland, G. J.; Wagle, G. A.] Univ Kentucky, Lexington, KY 40506 USA.
[Ferland, G. J.] Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland.
[Gorczyca, T. W.] Western Michigan Univ, Kalamazoo, MI 49008 USA.
[Nikolic, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Badnell, NR (reprint author), Univ Strathclyde, Glasgow G4 0NG, Lanark, Scotland.
RI Nikolic, Dragan/N-8346-2015;
OI Nikolic, Dragan/0000-0002-3810-7984; Ferland, Gary/0000-0003-4503-6333
FU NSF [1108928, 1109061, 1412155]; NASA [10-ATP10-0053, 10-ADAP10-0073,
NNX12AH73G, ATP13-0153]; STScI [HST-AR- 13245, GO-12560, HST-GO-12309,
GO-13310.002 A, HST-AR- 13914]; Leverhulme Trust via the award of a
Visiting Professorship at The Queen's University of Belfast
[VP1-2012-025]; NASA APRA grant [NNX11AF32G]; STFC UK APAP Network grant
[ST/J000892/1]
FX G.J.F. acknowledges support by NSF (1108928, 1109061, and 1412155), NASA
(10-ATP10-0053, 10-ADAP10-0073, NNX12AH73G, and ATP13-0153), STScI
(HST-AR- 13245, GO-12560, HST-GO-12309, GO-13310.002 A, and HST-AR-
13914) and is grateful to the Leverhulme Trust for support via the award
of a Visiting Professorship at The Queen's University of Belfast
(VP1-2012-025). T.W.G. was supported in part by the NASA APRA grant
NNX11AF32G. N.R.B. was supported in part the STFC UK APAP Network grant
ST/J000892/1.
NR 33
TC 1
Z9 1
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 100
DI 10.1088/0004-637X/804/2/100
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000022
ER
PT J
AU Banados, E
Venemans, BP
Morganson, E
Hodge, J
Decarli, R
Walter, F
Stern, D
Schlafly, E
Farina, EP
Greiner, J
Chambers, KC
Fan, X
Rix, HW
Burgett, WS
Draper, PW
Flewelling, J
Kaiser, N
Metcalfe, N
Morgan, JS
Tonry, JL
Wainscoat, RJ
AF Banados, E.
Venemans, B. P.
Morganson, E.
Hodge, J.
Decarli, R.
Walter, F.
Stern, D.
Schlafly, E.
Farina, E. P.
Greiner, J.
Chambers, K. C.
Fan, X.
Rix, H-W
Burgett, W. S.
Draper, P. W.
Flewelling, J.
Kaiser, N.
Metcalfe, N.
Morgan, J. S.
Tonry, J. L.
Wainscoat, R. J.
TI CONSTRAINING THE RADIO-LOUD FRACTION OF QUASARS AT z > 5.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; quasars: general
ID DIGITAL SKY SURVEY; SIMILAR-TO 6; SOUTHERN SPECTROPHOTOMETRIC STANDARDS;
OPTICALLY SELECTED QUASARS; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES;
LUMINOSITY FUNCTION; HIGH-REDSHIFT; Z-SIMILAR-TO-6 QUASARS;
HIGH-RESOLUTION
AB Radio-loud active galactic nuclei at z similar to 2-4 are typically located in dense environments and their host galaxies are among the most massive systems at those redshifts, providing key insights for galaxy evolution. Finding radio-loud quasars at the highest accessible redshifts (z similar to 6) is important to the study of their properties and environments at even earlier cosmic time. They could also serve as background sources for radio surveys intended to study the intergalactic medium beyond the epoch of reionization in HI 21 cm absorption. Currently, only five radio-loud (R= f(v,5) (GHz)/f(v,4400) (angstrom) > 10) quasars are known at z similar to 6. In this paper we search for 5.5 less than or similar to z less than or similar to 7.2 quasars by cross-matching the optical Panoramic Survey Telescope & Rapid Response System 1 and radio Faint Images of the Radio Sky at Twenty cm surveys. The radio information allows identification of quasars missed by typical color-based selections. While we find no good 6.4 less than or similar to z less than or similar to 7.2 quasar candidates at the sensitivities of these surveys, we discover two new radio-loud quasars at z similar to 6. Furthermore, we identify two additional z similar to 6 radio-loud quasars that were not previously known to be radio-loud, nearly doubling the current z similar to 6 sample. We show the importance of having infrared photometry for z > 5.5 quasars to robustly classify them as radio-quiet or radioloud. Based on this, we reclassify the quasar J0203+0012 (z = 5.72), previously considered radio-loud, to be radio-quiet. Using the available data in the literature, we constrain the radio-loud fraction of quasars at z similar to 6, using the Kaplan-Meier estimator, to be 8.1(-3.2)(+5.0)%. This result is consistent with there being no evolution of the radio-loud fraction with redshift, in contrast to what has been suggested by some studies at lower redshifts.
C1 [Banados, E.; Venemans, B. P.; Decarli, R.; Walter, F.; Schlafly, E.; Farina, E. P.; Rix, H-W] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Morganson, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hodge, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Chambers, K. C.; Burgett, W. S.; Flewelling, J.; Kaiser, N.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Fan, X.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
RP Banados, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM banados@mpia.de
OI Farina, Emanuele Paolo/0000-0002-6822-2254; Banados,
Eduardo/0000-0002-2931-7824; Chambers, Kenneth /0000-0001-6965-7789;
Schlafly, Edward Ford/0000-0002-3569-7421
FU ERC grant "Cosmic Dawn"; National Aeronautics and Space Administration
through Planetary Science Division of the NASA Science Mission
Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; NSF
[AST-9987045]; NSF Telescope System Instrumentation Program (TSIP); Ohio
Board of Regents; Ohio State University Office of Research; DFG [HA
1850/28-1]; National Aeronautics and Space Administration
FX We thank the anonymous referee for providing excellent suggestions and
comments that improved the manuscript. E. B. thanks the IMPRS for
Astronomy & Cosmic Physics at the University of Heidelberg. E. P. F. and
B. P. V. acknowledge funding through the ERC grant "Cosmic Dawn." We
thank F. Ardila, M. Balokovic J. Larson, E. Manjavacas, M. Maseda, T.
Minear, A. Place, S. Schmidl, and C. Steinhardt for their important
participation in some of our follow-up observations. The Pan-STARRS1
Surveys (PS1) have been made possible through contributions of the
Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project Office, the Max-Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, The Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astrophysics, the
Las Cumbres Observatory Global Telescope Network Incorporated, the
National Central University of Taiwan, the Space Telescope Science
Institute, the National Aeronautics and Space Administration under grant
No. NNX08AR22G issued through the Planetary Science Division of the NASA
Science Mission Directorate, the National Science Foundation under grant
No. AST-1238877, the University of Maryland, Eotvos Lorand University
(ELTE), and the Los Alamos National Laboratory. This work is based on
observations made with ESO Telescopes at the La Silla Paranal
Observatory under programs ID 092.A-0150, 093.A-0863, and 093.A-0574.
The LBT is an international collaboration among institutions in the
United States, Italy and Germany. The LBT Corporation partners are: The
University of Arizona on behalf of the Arizona university system;
Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft,
Germany, representing the Max Planck Society, the Astrophysical
Institute Potsdam, and Heidelberg University; The Ohio State University;
The Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota and University of Virginia. This paper used data
obtained with the MODS spectrographs built with funding from NSF grant
AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP),
with additional funds from the Ohio Board of Regents and the Ohio State
University Office of Research. Part of the funding for GROND (both
hardware as well as personnel) was generously granted from the
Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). 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 used the Milliquas Quasar Catalog to cross match our
candidates with known quasars (http://quasars.org/milliquas.htm; Flesch
2015) This research made use of Astropy, a community-developed core
Python package for Astronomy (Robitaille & Tollerud 2013;
http://www.astropy.org). We used the python package Lifelines
(Davidson-Pilon 2015) https://github.com/camdavidsonpilon/lifelines) to
perform the Kaplan-Meier estimates. This publication made use of TOPCAT
(Taylor et al. 2005, http://www.starlink.ac.uk/topcat). The plots in
this publication were produced using Matplotlib (Hunter 2007,
http://www.matplotlib.org).
NR 101
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 118
DI 10.1088/0004-637X/804/2/118
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000040
ER
PT J
AU Berry, CPL
Mandel, I
Middleton, H
Singer, LP
Urban, AL
Vecchio, A
Vitale, S
Cannon, K
Farr, B
Farr, WM
Graff, PB
Hanna, C
Haster, CJ
Mohapatra, S
Pankow, C
Price, LR
Sidery, T
Veitch, J
AF Berry, Christopher P. L.
Mandel, Ilya
Middleton, Hannah
Singer, Leo P.
Urban, Alex L.
Vecchio, Alberto
Vitale, Salvatore
Cannon, Kipp
Farr, Ben
Farr, Will M.
Graff, Philip B.
Hanna, Chad
Haster, Carl-Johan
Mohapatra, Satya
Pankow, Chris
Price, Larry R.
Sidery, Trevor
Veitch, John
TI PARAMETER ESTIMATION FOR BINARY NEUTRON-STAR COALESCENCES WITH REALISTIC
NOISE DURING THE ADVANCED LIGO ERA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; methods: data analysis; stars: neutron; surveys
ID GRAVITATIONAL-WAVE OBSERVATIONS; ELECTROMAGNETIC FOLLOW-UP;
MASS-DISTRIBUTION; BLACK-HOLES; BAYESIAN-INFERENCE; COMPACT BINARIES;
ASTRONOMY; MERGERS; GALAXY; TRANSIENTS
AB Advanced ground-based gravitational-wave (GW) detectors begin operation imminently. Their intended goal is not only to make the first direct detection of GWs, but also to make inferences about the source systems. Binary neutron-star mergers are among the most promising sources. We investigate the performance of the parameter-estimation (PE) pipeline that will be used during the first observing run of the Advanced Laser Interferometer Gravitational-wave Observatory (aLIGO) in 2015: we concentrate on the ability to reconstruct the source location on the sky, but also consider the ability to measure masses and the distance. Accurate, rapid sky localization is necessary to alert electromagnetic (EM) observatories so that they can perform follow-up searches for counterpart transient events. We consider PE accuracy in the presence of non-stationary, non-Gaussian noise. We find that the character of the noise makes negligible difference to the PE performance at a given signal-to-noise ratio. The source luminosity distance can only be poorly constrained, since the median 90% (50%) credible interval scaled with respect to the true distance is 0.85 (0.38). However, the chirp mass is well measured. Our chirp-mass estimates are subject to systematic error because we used gravitational-waveform templates without component spin to carry out inference on signals with moderate spins, but the total error is typically less than 10(-3) M-circle dot. The median 90% (50%) credible region for sky localization is similar to 600 deg(2) (similar to 150 deg(2)), with 3% (30%) of detected events localized within 100 deg(2). Early aLIGO, with only two detectors, will have a sky-localization accuracy for binary neutron stars of hundreds of square degrees; this makes EM follow-up challenging, but not impossible.
C1 [Berry, Christopher P. L.; Mandel, Ilya; Middleton, Hannah; Vecchio, Alberto; Farr, Ben; Farr, Will M.; Haster, Carl-Johan; Sidery, Trevor; Veitch, John] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Singer, Leo P.; Price, Larry R.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Singer, Leo P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Urban, Alex L.; Pankow, Chris] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Vitale, Salvatore; Mohapatra, Satya] MIT, Cambridge, MA 02139 USA.
[Cannon, Kipp] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Farr, Ben] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Farr, Ben] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys CI, Evanston, IL 60208 USA.
[Farr, Ben] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Graff, Philip B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Graff, Philip B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Hanna, Chad] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Hanna, Chad] Penn State Univ, University Pk, PA 16802 USA.
[Mohapatra, Satya] Syracuse Univ, Syracuse, NY 13244 USA.
RP Berry, CPL (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM cplb@star.sr.bham.ac.uk
RI Vecchio, Alberto/F-8310-2015;
OI Vecchio, Alberto/0000-0002-6254-1617; Farr, Ben/0000-0002-2916-9200;
Berry, Christopher/0000-0003-3870-7215; Mandel,
Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713
FU Science and Technology Facilities Council; NASA grant [NNX12AN10G];
National Science Foundation; LIGO Laboratory; STFC grant [ST/K005014/1];
National Science Foundation [PHY-0757058]; NSF [PHY-0923409,
PHY-0600953]
FX This work was supported by the Science and Technology Facilities
Council. P.B.G. acknowledges NASA grant NNX12AN10G. S.V. acknowledges
the support of the National Science Foundation and the LIGO Laboratory.
J.V. was supported by STFC grant ST/K005014/1. LIGO was constructed by
the California Institute of Technology and Massachusetts Institute of
Technology with funding from the National Science Foundation and
operates under cooperative agreement PHY-0757058.; Results were produced
using the computing facilities of the LIGO DataGrid including: the Nemo
computing cluster at the Center for Gravitation and Cosmology at the
University of Wisconsin-Milwauke under NSF Grants PHY-0923409 and
PHY-0600953; the Atlas computing cluster at the Albert Einstein
Institute, Hannover; the LIGO computing clusters at Caltech, and the
facilities of the Advanced Research Computing @ Cardiff (ARCCA) Cluster
at Cardiff University. We are especially grateful to Paul Hopkins of
ARCCA for assistance.
NR 88
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 114
DI 10.1088/0004-637X/804/2/114
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000036
ER
PT J
AU Brambilla, G
Kalapotharakos, C
Harding, AK
Kazanas, D
AF Brambilla, Gabriele
Kalapotharakos, Constantinos
Harding, Alice K.
Kazanas, Demosthenes
TI TESTING DISSIPATIVE MAGNETOSPHERE MODEL LIGHT CURVES AND SPECTRA WITH
FERMI PULSARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; pulsars: general; radiation mechanisms:
non-thermal
ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; SLOT GAPS;
PARTICLE-ACCELERATION; PAIR CREATION; STRIPED WIND; CRAB PULSAR; POLAR
CAPS; EMISSION; SIMULATIONS
AB We explore the emission properties of a dissipative pulsar magnetosphere model introduced by Kalapotharakos et al. comparing its high-energy light curves and spectra, due to curvature radiation, with data collected by the Fermi LAT. The magnetosphere structure is assumed to be near the force-free solution. The accelerating electric field, inside the light cylinder (LC), is assumed to be negligible, while outside the LC it rescales with a finite conductivity (sigma). In our approach we calculate the corresponding high-energy emission by integrating the trajectories of test particles that originate from the stellar surface, taking into account both the accelerating electric field components and the radiation reaction forces. First, we explore the parameter space assuming different value sets for the stellar magnetic field, stellar period, and conductivity. We show that the general properties of the model are in a good agreement with observed emission characteristics of young gamma-ray pulsars, including features of the phase-resolved spectra. Second, we find model parameters that fit each pulsar belonging to a group of eight bright pulsars that have a published phase-resolved spectrum. The sigma values that best describe each of the pulsars in this group show an increase with the spin-down rate (E) and a decrease with the pulsar age, expected if pair cascades are providing the magnetospheric conductivity. Finally, we explore the limits of our analysis and suggest future directions for improving such models.
C1 [Brambilla, Gabriele] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Brambilla, Gabriele; Kalapotharakos, Constantinos; Harding, Alice K.; Kazanas, Demosthenes] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kalapotharakos, Constantinos] Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA.
RP Brambilla, G (reprint author), Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.
EM gabriele.brambilla@nasa.gov
OI BRAMBILLA, GABRIELE/0000-0002-3692-1974
NR 40
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 84
DI 10.1088/0004-637X/804/2/84
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000006
ER
PT J
AU Holman, GD
Foord, A
AF Holman, Gordon D.
Foord, Adi
TI DIRECT SPATIAL ASSOCIATION OF AN X-RAY FLARE WITH THE ERUPTION OF A
SOLAR QUIESCENT FILAMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: filaments, prominences; Sun: flares; Sun: magnetic
fields; Sun: UV radiation; Sun: X-rays, gamma-rays
ID CORONAL MASS EJECTIONS; MICROFLARES; EVENTS; RHESSI; FLUX
AB Solar flares primarily occur in active regions. Hard X-ray flares have been found to occur only in active regions. They are often associated with the eruption of active region filaments and coronal mass ejections (CMEs). CMEs can also be associated with the eruption of quiescent filaments, not located in active regions. Here we report the first identification of a solar X-ray flare outside an active region observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The X-ray emission was directly associated with the eruption of a long, quiescent filament and fast CME. Images from RHESSI show this flare emission to be located along a section of the western ribbon of the expanding, post-eruption arcade. EUV images from the Solar Dynamics Observatory Atmospheric Imaging Assembly show no connection between this location and nearby active regions. Therefore the flare emission is found not to be located in or associated with an active region. However, a nearby, small, magnetically strong dipolar region provides a likely explanation for the existence and location of the flare X-ray emission. This emerging dipolar region may have also triggered the filament eruption.
C1 [Holman, Gordon D.; Foord, Adi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Foord, Adi] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Holman, GD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM gordon.d.holman@nasa.gov
FU NASA; RHESSI project
FX We thank the referee and Karin Muglach for helpful comments that led to
improvements in the paper, and Brian Dennis, Richard Schwartz, and Kim
Tolbert for their continuing help and support with the RHESSI data
analysis. G.H. was supported by NASA Heliophysics Guest Investigator and
Living with a Star TR & T Grants and the RHESSI project. A.F. was
supported by the RHESSI project.
NR 16
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 108
DI 10.1088/0004-637X/804/2/108
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000030
ER
PT J
AU Kashlinsky, A
Mather, JC
Helgason, K
Arendt, RG
Bromm, V
Moseley, SH
AF Kashlinsky, A.
Mather, J. C.
Helgason, K.
Arendt, R. G.
Bromm, V.
Moseley, S. H.
TI RECONSTRUCTING EMISSION FROM PRE-REIONIZATION SOURCES WITH COSMIC
INFRARED BACKGROUND FLUCTUATION MEASUREMENTS BY THE JWST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; early universe; infrared: diffuse
background; large-scale structure of universe
ID POPULATION-III STARS; COBE DIRBE MAPS; SPITZER-SPACE-TELESCOPE; ORIGINS
DEEP SURVEY; GAMMA-RAY BURSTS; 1ST BLACK-HOLES; ALL-SKY SURVEY;
PHOTOMETRIC CALIBRATION; EXPERIMENT SEARCH; INTERPLANETARY DUST
AB We present new methodology to use cosmic infrared background (CIB) fluctuations to probe sources at 10 less than or similar to z less than or similar to 30 from a James Webb Space Telescope (JWST)/NIRCam configuration that will isolate known galaxies to 28 AB mag at 0.5-5 mu m. At present significant mutually consistent source-subtracted CIB fluctuations have been identified in the Spitzer and AKARI data at similar to 2-5 mu m, but we demonstrate internal inconsistencies at shorter wavelengths in the recent CIBER data. We evaluate CIB contributions from remaining galaxies and show that the bulk of the high-z sources will be in the confusion noise of the NIRCam beam, requiring CIB studies. The accurate measurement of the angular spectrum of the fluctuations and probing the dependence of its clustering component on the remaining shot noise power would discriminate between the various currently proposed models for their origin and probe the flux distribution of its sources. We show that the contribution to CIB fluctuations from remaining galaxies is large at visible wavelengths for the current instruments precluding probing the putative Lyman-break of the CIB fluctuations. We demonstrate that with the proposed JWST configuration such measurements will enable probing the Lyman-break. We develop a Lyman-break tomography method to use the NIRCam wavelength coverage to identify or constrain, via the adjacent two-band subtraction, the history of emissions over 10 less than or similar to z less than or similar to 30 as the universe comes out of the "Dark Ages." We apply the proposed tomography to the current Spitzer/IRAC measurements at 3.6 and 4.5 mu m, to find that it already leads to interestingly low upper limit on emissions at z greater than or similar to 30.
C1 [Kashlinsky, A.; Mather, J. C.; Arendt, R. G.; Moseley, S. H.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] SSAI, Lanham, MD 20770 USA.
[Mather, J. C.; Moseley, S. H.] NASA, Greenbelt, MD USA.
[Helgason, K.] MPA, D-85748 Garching, Germany.
[Arendt, R. G.] CRESST UMBC, Baltimore, MD USA.
[Bromm, V.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Kashlinsky, A (reprint author), NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Alexander.Kashlinsky@nasa.gov
OI Arendt, Richard/0000-0001-8403-8548
NR 103
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U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 99
DI 10.1088/0004-637X/804/2/99
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000021
ER
PT J
AU Mei, S
Scarlata, C
Pentericci, L
Newman, JA
Weiner, BJ
Ashby, MLN
Castellano, M
Conselice, CJ
Finkelstein, SL
Galametz, A
Grogin, NA
Koekemoer, AM
Huertas-Company, M
Lani, C
Lucas, RA
Papovich, C
Rafelski, M
Teplitz, HI
AF Mei, Simona
Scarlata, Claudia
Pentericci, Laura
Newman, Jeffrey A.
Weiner, Benjamin J.
Ashby, Matthew L. N.
Castellano, Marco
Conselice, Chistopher J.
Finkelstein, Steven L.
Galametz, Audrey
Grogin, Norman A.
Koekemoer, Anton M.
Huertas-Company, Marc
Lani, Caterina
Lucas, Ray A.
Papovich, Casey
Rafelski, Marc
Teplitz, Harry I.
TI STAR-FORMING BLUE ETGS IN TWO NEWLY DISCOVERED GALAXY OVERDENSITIES IN
THE HUDF AT z=1.84 AND 1.9: UNVEILING THE PROGENITORS OF PASSIVE ETGS IN
CLUSTER CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution
ID COLOR-MAGNITUDE RELATION; MASS-SIZE RELATION; ULTRA DEEP FIELD;
HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; EXTRAGALACTIC LEGACY SURVEY;
FORMATION-DENSITY RELATION; LARGE-SCALE ENVIRONMENT; HIGH-REDSHIFT
CLUSTERS; LYMAN-BREAK GALAXIES
AB We present the discovery of two galaxy overdensities in the Hubble Space Telescope UDF: a proto-cluster, HUDFJ0332.4-2746.6 at z = 1.84 +/- 0.01, and a group, HUDFJ0332.5-2747.3 at z = 1.90 +/- 0.01. Assuming viralization, the velocity dispersion of HUDFJ0332.4-2746.6 implies a mass of M-200 = (2.2 +/- 1.8) x 10(14) M-circle dot, consistent with the lack of extended X-ray emission. Neither overdensity shows evidence of a red sequence. About 50% of their members show interactions and/or disturbed morphologies, which are signatures of merger remnants or disk instability. Most of their ETGs have blue colors and show recent star formation. These observations reveal for the first time large fractions of spectroscopically confirmed star-forming blue ETGs in proto-clusters at z approximate to 2. These star-forming ETGs are most likely among the progenitors of the quiescent population in clusters at more recent epochs. Their mass-size relation is consistent with that of passive ETGs in clusters at z similar to 0.7-1.5. If these galaxies are the progenitors of cluster ETGs at these lower redshifts, their size would evolve according to a similar mass-size relation. It is noteworthy that quiescent ETGs in clusters at z = 1.8-2 also do not show any significant size evolution over this redshift range, contrary to field ETGs. The ETG fraction is less than or similar to 50%, compared to the typical quiescent ETG fraction of approximate to 80% in cluster cores at z < 1. The fraction, masses, and colors of the newly discovered ETGs imply that other cluster ETGs will be formed/accreted at a later time.
C1 [Mei, Simona; Huertas-Company, Marc] Univ Paris Diderot, GEPI, Observ Paris, CNRS,PSL, F-75014 Paris, France.
[Mei, Simona; Huertas-Company, Marc] Univ Paris Sorbonne Cite PSC, Univ Paris Denis Diderot, F-75205 Paris 13, France.
[Mei, Simona; Rafelski, Marc; Teplitz, Harry I.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Pentericci, Laura; Castellano, Marco] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Newman, Jeffrey A.] Univ Pittsburgh, Pittsburgh, PA 15260 USA.
[Weiner, Benjamin J.; Ashby, Matthew L. N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Conselice, Chistopher J.; Lani, Caterina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Grogin, Norman A.; Koekemoer, Anton M.; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Finkelstein, Steven L.] Univ Texas Austin, Austin, TX 78712 USA.
[Papovich, Casey] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 78743 USA.
[Rafelski, Marc] NASA, Postdoctoral Program Fellow, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lani, Caterina] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Galametz, Audrey] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
RP Mei, S (reprint author), Univ Paris Diderot, GEPI, Observ Paris, CNRS,PSL, 61 Ave Observ, F-75014 Paris, France.
OI Castellano, Marco/0000-0001-9875-8263; Weiner,
Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048
FU NASA [NAS526555]; Institut Universitaire de France (IUF)
FX This work is based on observations taken by the CANDELS Multi-Cycle
Treasury Program and the 3D-HST Treasury Program (GO 12177 and 12328)
with the NASA/ESA HST, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS526555. This work is based in part on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. S.M. acknowledges financial support from the Institut
Universitaire de France (IUF), of which she is a senior member. We thank
the referee for very useful comments that improved the paper.
NR 152
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 117
DI 10.1088/0004-637X/804/2/117
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000039
ER
PT J
AU Richert, AJW
Lyra, W
Boley, A
Mac Low, MM
Turner, N
AF Richert, Alexander J. W.
Lyra, Wladimir
Boley, Aaron
Mac Low, Mordecai-Mark
Turner, Neal
TI ON SHOCKS DRIVEN BY HIGH-MASS PLANETS IN RADIATIVELY INEFFICIENT DISKS.
I. TWO-DIMENSIONAL GLOBAL DISK SIMULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; planet-disk interactions; planets and satellites:
formation; protoplanetary disks; shock waves; turbulence
ID DIFFERENTIALLY ROTATING-DISKS; ROSSBY-WAVE INSTABILITY; BAROCLINIC
VORTICITY PRODUCTION; PRIMORDIAL SOLAR NEBULA; PROTOPLANETARY DISKS;
MAGNETOROTATIONAL TURBULENCE; TIDAL INTERACTION; ANGULAR-MOMENTUM;
ACCRETION DISKS; MAGNETIZED ACCRETION
AB Recent observations of gaps and non-axisymmetric features in the dust distributions of transition disks have been interpreted as evidence of embedded massive protoplanets. However, comparing the predictions of planet-disk interaction models to the observed features has shown far from perfect agreement. This may be due to the strong approximations used for the predictions. For example, spiral arm fitting typically uses results that are based on low-mass planets in an isothermal gas. In this work, we describe two-dimensional, global, hydrodynamical simulations of disks with embedded protoplanets, with and without the assumption of local isothermality, for a range of planet-to-star mass ratios 1-10 M-J for a 1 M-circle dot star. We use the PENCIL CODE in polar coordinates for our models. We find that the inner and outer spiral wakes of massive protoplanets (M greater than or similar to 5 M-J) produce significant shock heating that can trigger buoyant instabilities. These drive sustained turbulence throughout the disk when they occur. The strength of this effect depends strongly on the mass of the planet and the thermal relaxation timescale; for a 10 M-J planet embedded in a thin, purely adiabatic disk, the spirals, gaps, and vortices typically associated with planet-disk interactions are disrupted. We find that the effect is only weakly dependent on the initial radial temperature profile. The spirals that form in disks heated by the effects we have described may fit the spiral structures observed in transition disks better than the spirals predicted by linear isothermal theory.
C1 [Richert, Alexander J. W.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Richert, Alexander J. W.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Richert, Alexander J. W.; Lyra, Wladimir; Turner, Neal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Richert, Alexander J. W.; Lyra, Wladimir] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Boley, Aaron] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
RP Richert, AJW (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM ajr327@psu.edu; wlyra@jpl.nasa.gov; acboley@phas.ubc.ca;
mordecai@amnh.org; neal.j.turner@jpl.nasa.gov
OI Richert, Alexander/0000-0002-9613-6863; Mac Low,
Mordecai-Mark/0000-0003-0064-4060
FU NSF AAG grant [AST10-09802]; Center for Exoplanets and Habitable Worlds
(PSU); National Aeronautics and Space Administration (NASA); Canada
Research Chairs program; University of British Columbia; NASA OSS grant
[NNX14AJ56G]; California Institute of Technology (Caltech)
FX A. R. is funded by NSF AAG grant AST10-09802, and by the Center for
Exoplanets and Habitable Worlds (PSU). W. L. is funded by the National
Aeronautics and Space Administration (NASA) through the Sagan Fellowship
Program executed by the NASA Exoplanet Science Institute. A. B. is
funded, in part, by the Canada Research Chairs program and The
University of British Columbia. M.-M. M. L. is funded, in part, by NASA
OSS grant NNX14AJ56G. This work was performed in part at the Jet
Propulsion Laboratory, under contract with the California Institute of
Technology (Caltech). The authors acknowledge discussions with Sijme-Jan
Paardekooper, Axel Brandenburg, Dhrubaditya Mitra, Thayne Currie, and
Wilhelm Kley.
NR 71
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 95
DI 10.1088/0004-637X/804/2/95
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000017
ER
PT J
AU Rivers, E
Risaliti, G
Walton, DJ
Harrison, F
Arevalo, P
Baur, FE
Boggs, SE
Brenneman, LW
Brightman, M
Christensen, FE
Craig, WW
Furst, F
Hailey, CJ
Hickox, RC
Marinucci, A
Reeves, J
Stern, D
Zhang, WW
AF Rivers, E.
Risaliti, G.
Walton, D. J.
Harrison, F.
Arevalo, P.
Baur, F. E.
Boggs, S. E.
Brenneman, L. W.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Fuerst, F.
Hailey, C. J.
Hickox, R. C.
Marinucci, A.
Reeves, J.
Stern, D.
Zhang, W. W.
TI THE MULTI-LAYER VARIABLE ABSORBERS IN NGC 1365 REVEALED BY XMM-NEWTON
AND NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 1365); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL VARIABILITY; ACCRETION DISK;
ABSORPTION; WIND; SUZAKU; AGN
AB Between 2012 July and 2013 February, NuSTAR and XMM-Newton performed four long-look joint observations of the type 1.8 Seyfert, NGC 1365. We have analyzed the variable absorption seen in these observations in order to characterize the geometry of the absorbing material. Two of the observations caught NGC 1365 in an unusually low absorption state, revealing complexity in the multi-layer absorber that had previously been hidden. We find the need for three distinct zones of neutral absorption in addition to the two zones of ionized absorption and the Compton-thick torus previously seen in this source. The most prominent absorber is likely associated with broad-line region clouds with column densities of around similar to 10(23) cm(-2) and a highly clumpy nature as evidenced by an occultation event in 2013 February. We also find evidence of a patchy absorber with a variable column around similar to 10(22) cm(-2) and a line-of-sight covering fraction of 0.3-0.9, which responds directly to the intrinsic source flux, possibly due to a wind geometry. A full-covering, constant absorber with a low column density of similar to 1 x 10(22) cm(-2) is also present, though the location of this low density haze is unknown.
C1 [Rivers, E.; Walton, D. J.; Harrison, F.; Brightman, M.; Fuerst, F.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Risaliti, G.; Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Baur, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile.
[Baur, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[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.
[Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Reeves, J.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rivers, E (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
NASA/GSFC; NASA/IPAC; NASA
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). This work has also made use of HEASARC
online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic
Database, operated by JPL/California Institute of Technology under
contract with NASA. This work also made use of data from the XMM-Newton
observatory.
NR 31
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 107
DI 10.1088/0004-637X/804/2/107
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000029
ER
PT J
AU Romani, RW
Filippenko, AV
Cenko, SB
AF Romani, Roger W.
Filippenko, Alexei V.
Cenko, S. Bradley
TI A SPECTROSCOPIC STUDY OF THE EXTREME BLACK WIDOW PSR J1311-3430
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: general
ID MILLISECOND PULSARS; DISCOVERY; COMPANION; MODEL; STAR
AB We report on a series of spectroscopic observations of PSR J1311-3430, an extreme black-widow gamma-ray pulsar with a helium-star companion. In a previous study we estimated the neutron star mass as M-NS = 2.68 +/- 0.14 M-circle dot (statistical error), based on limited spectroscopy and a basic (direct heating) light-curve model; however, much larger model-dependent systematics dominate the mass uncertainty. Our new spectroscopy reveals a range of complex source behavior. The variable He I companion wind emission lines can dominate broadband photometry, especially in red filters or near minimum brightness, and the wind flux should complete companion evaporation in a spin-down time. The heated companion face also undergoes dramatic flares, reaching similar to 40,000 K over similar to 20% of the star; this is likely powered by a magnetic field generated in the companion. The companion center-of-light radial velocity is now well measured with K-CoL = 615.4 +/- 5.1 km s(-1). We detect non-sinusoidal velocity components due to the heated face flux distribution. Using our spectra to excise flares and wind lines, we generate substantially improved light curves for companion continuum fitting. We show that the inferred inclination and neutron star mass, however, remain sensitive to the poorly constrained heating pattern. The neutron star's mass, M-NS, is likely less than the direct heating value and could range as low as 1.8 M-circle dot for extreme equatorial heating concentration. While we cannot yet pin down M-NS, our data imply that an intrabinary shock reprocesses the pulsar emission and heats the companion. Improved spectra and, especially, models that include such shock heating are needed for precise parameter measurement.
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, 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.
RP Romani, RW (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
EM rwr@astro.stanford.edu
FU NASA [NNX11AO44G, NNX12A068G]; Richard and Rhoda Goldman Fund;
Christopher R. Redlich Fund; TABASGO Foundation; NSF grant
[AST-1211916]; W. M. Keck Foundation; Gary and Cynthia Bengier
FX We thank Kelsey Clubb, Ori Fox, and Melissa Graham for assistance with
some of the Keck observations, as well as German Gimeno for help with
the Gemini campaign. We also thank the referee for many detailed
comments. This work was partially supported by NASA grants NNX11AO44G
and NNX12A068G. A.V.F. and S.B.C. were supported by Gary and Cynthia
Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich
Fund, the TABASGO Foundation, and NSF grant AST-1211916. 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
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 115
DI 10.1088/0004-637X/804/2/115
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000037
ER
PT J
AU Schneider, AC
Cushing, MC
Kirkpatrick, JD
Gelino, CR
Mace, GN
Wright, EL
Eisenhardt, PR
Skrutskie, MF
Griffith, RL
Marsh, KA
AF Schneider, Adam C.
Cushing, Michael C.
Kirkpatrick, J. Davy
Gelino, Christopher R.
Mace, Gregory N.
Wright, Edward L.
Eisenhardt, Peter R.
Skrutskie, M. F.
Griffith, Roger L.
Marsh, Kenneth A.
TI HUBBLE SPACE TELESCOPE SPECTROSCOPY OF BROWN DWARFS DISCOVERED WITH THE
WIDE-FIELD INFRARED SURVEY EXPLORER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: low-mass; brown dwarfs
ID Y DWARFS; T-DWARFS; WATER CLOUDS; WISE; PHOTOMETRY; SPECTRA; MASS;
ATMOSPHERES; TRANSITION; BINARIES
AB We present a sample of brown dwarfs identified with the Wide-field Infrared Survey Explorer (WISE) for which we have obtained Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) near-infrared grism spectroscopy. The sample (22 in total) was observed with the G141 grism covering 1.10-1.70 mu m, while 15 were also observed with the G102 grism, which covers 0.90-1.10 mu m. The additional wavelength coverage provided by the G102 grism allows us to (1) search for spectroscopic features predicted to emerge at low effective temperatures (e.g., ammonia bands) and (2) construct a smooth spectral sequence across the T/Y boundary. We find no evidence of absorption due to ammonia in the G102 spectra. Six of these brown dwarfs are new discoveries, three of which are found to have spectral types of T8 or T9. The remaining three, WISE J082507.35+280548.5 (Y0.5), WISE J120604.38+840110.6 (Y0), and WISE J235402.77+024015.0 (Y1), are the 19th, 20th, and 21st spectroscopically confirmed Y dwarfs to date. We also present HST grism spectroscopy and reevaluate the spectral types of five brown dwarfs for which spectral types have been determined previously using other instruments.
C1 [Schneider, Adam C.; Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Kirkpatrick, J. Davy; Gelino, Christopher R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Gelino, Christopher R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Mace, Gregory N.; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Mace, Gregory N.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Eisenhardt, Peter R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Griffith, Roger L.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
RP Schneider, AC (reprint author), Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA.
EM Adam.Schneider@Utoledo.edu
FU National Aeronautics and Space Administration
FX We wish to thank Caroline Morley and Didier Saumon for useful
discussions regarding low-temperature models. This publication makes use
of data products from the Wide-field Infrared Survey Explorer, which is
a joint project of the University of California, Los Angeles, and the
Jet Propulsion Laboratory/California Institute of Technology, and
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology. WISE and NEOWISE are funded by the National
Aeronautics and Space Administration. This research has benefitted from
the M, L, T, and Y dwarf compendium housed at dwarfarchives.org. This
research has benefitted from the SpeX Prism Spectral Libraries,
maintained by Adam Burgasser at http://pono.ucsd.edu/similar to
adam/browndwarfs/spexprism. HST acknowledgement needed. We thank the
STSCI help desk for useful discussions and resolution suggestions
regarding WFC3 IR photometry. The authors wish to thank Caroline Morley
for providing spectroscopic models via the webpage
http://ucolick.org/similar to cmorley/cmorley/Models.html.
NR 44
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 92
DI 10.1088/0004-637X/804/2/92
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000014
ER
PT J
AU Taquet, V
Lopez-Sepulcre, A
Ceccarelli, C
Neri, R
Kahane, C
Charnley, SB
AF Taquet, Vianney
Lopez-Sepulcre, Ana
Ceccarelli, Cecilia
Neri, Roberto
Kahane, Claudine
Charnley, Steven B.
TI CONSTRAINING THE ABUNDANCES OF COMPLEX ORGANICS IN THE INNER REGIONS OF
SOLAR-TYPE PROTOSTARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: individual objects (NGC 1333-IRAS
2A, NGC 1333-IRAS 4A); ISM: molecules; stars: formation
ID LOW-MASS PROTOSTARS; STAR-FORMING REGIONS; GRAIN-SURFACE-CHEMISTRY;
EXTRAORDINARY SOURCES ANALYSIS; SUBMILLIMETER-WAVE SPECTRUM;
INTERSTELLAR ICE ANALOGS; YOUNG STELLAR OBJECTS; MOLECULAR LINE SURVEY;
HOT-CORE; IRAS 16293-2422
AB The high abundances of Complex Organic Molecules (COMs) with respect to methanol, the most abundant COM, detected toward low-mass protostars, tend to be underpredicted by astrochemical models. This discrepancy might come from the large beam of the single-dish telescopes, encompassing several components of the studied protostar, commonly used to detect COMs. To address this issue, we have carried out multi-line observations of methanol and several COMs toward the two low-mass protostars NGC 1333-IRAS 2A and -IRAS 4A with the Plateau de Bure interferometer at an angular resolution of 2 '', resulting in the first multi-line detection of the O-bearing species glycolaldehyde and ethanol and of the N-bearing species ethyl cyanide toward low-mass protostars other than IRAS 16293. The high number of detected transitions from COMs (more than 40 methanol transitions for instance) allowed us to accurately derive the source size of their emission and the COM column densities. The COM abundances with respect to methanol derived toward IRAS 2A and IRAS 4A are slightly, but not substantitally, lower than those derived from previous single-dish observations. The COM abundance ratios do not vary significantly with the protostellar luminosity, over five orders of magnitude, implying that low-mass hot corinos are quite chemically rich as high-mass hot cores. Astrochemical models still underpredict the abundances of key COMs, such as methyl formate or di-methyl ether, suggesting that our understanding of their formation remains incomplete.
C1 [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD USA.
[Taquet, Vianney] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Lopez-Sepulcre, Ana; Ceccarelli, Cecilia; Kahane, Claudine] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Lopez-Sepulcre, Ana; Ceccarelli, Cecilia; Kahane, Claudine] CNRS, IPAG, F-38000 Grenoble, France.
[Lopez-Sepulcre, Ana] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Neri, Roberto] Inst Radioastron Millimetr, Grenoble, France.
RP Taquet, V (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mailstop 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM taquet@strw.leidenuniv.nl
FU NASA's Origins of Solar Systems and Exobiology Programs; NASA
postdoctoral program; French space agency CNES
FX The authors are grateful to the anonymous referee whose comments
contributed to improving the quality of the present paper. This work was
supported by NASA's Origins of Solar Systems and Exobiology Programs.
V.T. acknowledges support from the NASA postdoctoral program. A.L.-S.
and C.C. acknowledge financing from the French space agency CNES.
NR 97
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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 MAY 10
PY 2015
VL 804
IS 2
AR 81
DI 10.1088/0004-637X/804/2/81
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000003
ER
PT J
AU Webber, MW
Lewis, NK
Marley, M
Morley, C
Fortney, JJ
Cahoy, K
AF Webber, Matthew W.
Lewis, Nikole K.
Marley, Mark
Morley, Caroline
Fortney, Jonathan J.
Cahoy, Kerri
TI EFFECT OF LONGITUDE-DEPENDENT CLOUD COVERAGE ON EXOPLANET VISIBLE
WAVELENGTH REFLECTED-LIGHT PHASE CURVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; radiative transfer; stars: individual (Kepler-7);
techniques: photometric
ID EXTRASOLAR GIANT PLANETS; HUBBLE-SPACE-TELESCOPE; HD 189733B; HOT
JUPITERS; TRANSMISSION SPECTRUM; DWARF ATMOSPHERES; THERMAL STRUCTURE;
MEAN OPACITIES; ALBEDO; MODELS
AB We use a planetary albedo model to investigate variations in visible wavelength phase curves of exoplanets. Thermal and cloud properties for these exoplanets are derived using one-dimensional radiative-convective and cloud simulations. The presence of clouds on these exoplanets significantly alters their planetary albedo spectra. We confirm that non-uniform cloud coverage on the dayside of tidally locked exoplanets will manifest as changes to the magnitude and shift of the phase curve. In this work, we first investigate a test case of our model using a Jupiter-like planet, at temperatures consistent to 2.0 AU insolation from a solar type star, to consider the effect of H2O clouds. We then extend our application of the model to the exoplanet Kepler-7b and consider the effect of varying cloud species, sedimentation efficiency, particle size, and cloud altitude. We show that, depending on the observational filter, the largest possible shift of the phase curve maximum will be similar to 2 degrees-10 degrees for a Jupiter-like planet, and up to similar to 30 degrees (similar to 0.08 in fractional orbital phase) for hot-Jupiter exoplanets at visible wavelengths as a function of dayside cloud distribution with a uniformly averaged thermal profile. The models presented in this work can be adapted for a variety of planetary cases at visible wavelengths to include variations in planet-star separation, gravity, metallicity, and source-observer geometry. Finally, we tailor our model for comparison with, and confirmation of, the recent optical phase-curve observations of Kepler-7b with the Kepler space telescope. The average planetary albedo can vary between 0.1 and 0.6 for the 1300 cloud scenarios that were compared to the observations. Many of these cases cannot produce a high enough albedo to match the observations. We observe that smaller particle size and increasing cloud altitude have a strong effect on increasing albedo. In particular, we show that a set of models where Kepler-7b has roughly half of its dayside covered in small-particle clouds high in the atmosphere, made of bright minerals like MgSiO3 and Mg2SiO4, provide the best fits to the observed offset and magnitude of the phase-curve, whereas Fe clouds are found to be too dark to fit the observations.
C1 [Webber, Matthew W.; Lewis, Nikole K.; Cahoy, Kerri] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lewis, Nikole K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Marley, Mark] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Morley, Caroline; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Cahoy, Kerri] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
RP Webber, MW (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
OI Marley, Mark/0000-0002-5251-2943
FU NASA; Jet Propulsion Laboratory (JPL)
FX The authors thank Brice-Olivier Demory for his helpful discussion and
for providing the Kepler-7b phase curve data. This work was performed in
part under contract with the Jet Propulsion Laboratory (JPL) funded by
NASA through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute.
NR 62
TC 9
Z9 9
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2015
VL 804
IS 2
AR 94
DI 10.1088/0004-637X/804/2/94
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI6WR
UT WOS:000354905000016
ER
PT J
AU Burlaga, LF
Florinski, V
Ness, NF
AF Burlaga, L. F.
Florinski, V.
Ness, N. F.
TI IN SITU OBSERVATIONS OF MAGNETIC TURBULENCE IN THE LOCAL INTERSTELLAR
MEDIUM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: magnetic fields
ID GALACTIC COSMIC-RAYS; VOYAGER 1; ASTROPHYSICAL BODIES; FIELD; SCALE;
GENERATION; SPECTRA; MODELS; GALAXY
AB We present the first in situ observations of turbulence in the local interstellar magnetic field B, measured by Voyager 1 from 2013.36 to 2014.64. The fluctuations of the components of B, the rms of the fluctuations of the components of B, and magnitude of B have a Kolmogorov k(-5/3) spectrum in the range from 4 x 10(-6) to 3 x 10(-7) Hz. The turbulence is compressible; the variance is primarily along the average magnetic field. The turbulence is weak, the ratio of the turbulent fluctuations to the average field being 0.023. A small linear increase in the azimuthal angle lambda of B and a small linear decrease in the elevation angle delta were observed during the 468 day interval under consideration, which might be related to magnetic draping.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Florinski, V.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net; vaf000@uah.edu; nfnudel@yahoo.com
FU NASA [NNX12AC63G, NNG14PN24P, NNX10AE46, NNX12AH44G]; NSF [AGS-0955700];
NASA Marshall Space Flight Center [NNM11AA01A]
FX We thank R. Jokipii for notes on the spectrum of the interstellar
turbulence. T. McClanahan, S. Kramer, and D. Berdichevsky provided
support in the processing of the data. N. F. Ness was supported by NASA
grant NNX12AC63G to the Catholic University of America. L. F. Burlaga
was supported by NASA Contract NNG14PN24P. V. Florinski was supported by
NASA grants NNX10AE46 and NNX12AH44G, by NSF grant AGS-0955700, and a
cooperative agreement with NASA Marshall Space Flight Center NNM11AA01A.
NR 23
TC 15
Z9 15
U1 2
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAY 10
PY 2015
VL 804
IS 2
AR L31
DI 10.1088/2041-8205/804/2/L31
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH8NN
UT WOS:000354293200005
ER
PT J
AU Jennings, DE
Achterberg, RK
Cottini, V
Anderson, CM
Flasar, FM
Nixon, CA
Bjoraker, GL
Kunde, VG
Carlson, RC
Guandique, E
Kaelberer, MS
Tingley, JS
Albright, SA
Segura, ME
de Kok, R
Coustenis, A
Vinatier, S
Bampasidis, G
Teanby, NA
Calcutt, S
AF Jennings, Donald E.
Achterberg, R. K.
Cottini, V.
Anderson, C. M.
Flasar, F. M.
Nixon, C. A.
Bjoraker, G. L.
Kunde, V. G.
Carlson, R. C.
Guandique, E.
Kaelberer, M. S.
Tingley, J. S.
Albright, S. A.
Segura, M. E.
de Kok, R.
Coustenis, A.
Vinatier, S.
Bampasidis, G.
Teanby, N. A.
Calcutt, S.
TI EVOLUTION OF THE FAR-INFRARED CLOUD AT TITAN'S SOUTH POLE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE molecular processes; planets and satellites: atmospheres; planets and
satellites: composition; planets and satellites: individual (Titan);
radiation mechanisms: thermal
ID CASSINI/CIRS OBSERVATIONS; STRATOSPHERIC AEROSOLS; TEMPORAL VARIATIONS;
HCN POLYMER; ATMOSPHERE; SPECTRA; WINTER
AB A condensate cloud on Titan identified by its 220 cm(-1) far-infrared signature continues to undergo seasonal changes at both the north and south poles. In the north, the cloud, which extends from 55 N to the pole, has been gradually decreasing in emission intensity since the beginning of the Cassini mission with a half-life of 3.8 years. The cloud in the south did not appear until 2012 but its intensity has increased rapidly, doubling every year. The shape of the cloud at the south pole is very different from that in the north. Mapping in 2013 December showed that the condensate emission was confined to a ring with a maximum at 80 S. The ring was centered 4 degrees from Titan's pole. The pattern of emission from stratospheric trace gases like nitriles and complex hydrocarbons (mapped in 2014 January) was also offset by 4 degrees, but had a central peak at the pole and a secondary maximum in a ring at about 70 S with a minimum at 80 S. The shape of the gas emission distribution can be explained by abundances that are high at the atmospheric pole and diminish toward the equator, combined with correspondingly increasing temperatures. We discuss possible causes for the condensate ring. The present rapid build up of the condensate cloud at the south pole is likely to transition to a gradual decline from 2015 to 2016.
C1 [Jennings, Donald E.; Achterberg, R. K.; Cottini, V.; Anderson, C. M.; Flasar, F. M.; Nixon, C. A.; Bjoraker, G. L.; Kunde, V. G.; Carlson, R. C.; Guandique, E.; Kaelberer, M. S.; Tingley, J. S.; Albright, S. A.; Segura, M. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Achterberg, R. K.; Cottini, V.; Kunde, V. G.; Segura, M. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Carlson, R. C.] Catholic Univ Amer, IACS, Washington, DC 20064 USA.
[Guandique, E.; Kaelberer, M. S.; Tingley, J. S.] ADNET Syst Inc, Rockville, MD 20852 USA.
[Albright, S. A.] Syst & Software Designers Inc, Columbia, MD 21045 USA.
[de Kok, R.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[de Kok, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Coustenis, A.; Vinatier, S.; Bampasidis, G.] Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
[Bampasidis, G.] Univ Athens, Fac Phys, GR-15783 Athens, Greece.
[Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Calcutt, S.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM donald.e.jennings@nasa.gov
RI Flasar, F Michael/C-8509-2012; Nixon, Conor/A-8531-2009;
OI Nixon, Conor/0000-0001-9540-9121; Cottini, Valeria/0000-0003-0839-5855;
Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775
FU NASA's Cassini mission and Cassini Data Analysis Program
FX We acknowledge support from NASA's Cassini mission and Cassini Data
Analysis Program.
NR 26
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U1 2
U2 12
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 MAY 10
PY 2015
VL 804
IS 2
AR L34
DI 10.1088/2041-8205/804/2/L34
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH8NN
UT WOS:000354293200008
ER
PT J
AU Boggs, SE
Harrison, FA
Miyasaka, H
Grefenstette, BW
Zoglauer, A
Fryer, CL
Reynolds, SP
Alexander, DM
An, H
Barret, D
Christensen, FE
Craig, WW
Forster, K
Giommi, P
Hailey, CJ
Hornstrup, A
Kitaguchi, T
Koglin, JE
Madsen, KK
Mao, PH
Mori, K
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, V
Stern, D
Westergaard, NJ
Zhang, WW
AF Boggs, S. E.
Harrison, F. A.
Miyasaka, H.
Grefenstette, B. W.
Zoglauer, A.
Fryer, C. L.
Reynolds, S. P.
Alexander, D. M.
An, H.
Barret, D.
Christensen, F. E.
Craig, W. W.
Forster, K.
Giommi, P.
Hailey, C. J.
Hornstrup, A.
Kitaguchi, T.
Koglin, J. E.
Madsen, K. K.
Mao, P. H.
Mori, K.
Perri, M.
Pivovaroff, M. J.
Puccetti, S.
Rana, V.
Stern, D.
Westergaard, N. J.
Zhang, W. W.
TI Ti-44 gamma-ray emission lines from SN1987A reveal an asymmetric
explosion
SO SCIENCE
LA English
DT Article
ID CORE-COLLAPSE SUPERNOVAE; SN 1987A; LIGHT-CURVE; CHANDRA OBSERVATIONS;
NEUTRINO BURST; SN-1987A; EJECTA; PROFILES; SPECTRUM
AB In core-collapse supernovae, titanium-44 (Ti-44) is produced in the innermost ejecta, in the layer of material directly on top of the newly formed compact object. As such, it provides a direct probe of the supernova engine. Observations of supernova 1987A (SN1987A) have resolved the 67.87- and 78.32-kilo-electron volt emission lines from decay of Ti-44 produced in the supernova explosion. These lines are narrow and redshifted with a Doppler velocity of similar to 700 kilometers per second, direct evidence of large-scale asymmetry in the explosion.
C1 [Boggs, S. E.; Zoglauer, A.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Harrison, F. A.; Miyasaka, H.; Grefenstette, B. W.; Forster, K.; Madsen, K. K.; Mao, P. H.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Fryer, C. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Reynolds, S. P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[An, H.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, D.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Christensen, F. E.; Hornstrup, A.; Westergaard, N. J.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, W. W.; Pivovaroff, M. J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Giommi, P.; Perri, M.; Puccetti, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Hailey, C. J.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kitaguchi, T.] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan.
[Koglin, J. E.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Perri, M.; Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Boggs, SE (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM boggs@berkeley.edu
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; French
Space Agency (CNES); Japan Society for the Promotion of Science
[24740185]; Technical University of Denmark
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). D.B. acknowledges funding from the French
Space Agency (CNES). T.K. was supported by Japan Society for the
Promotion of Science Grant-in-Aid for Young Scientists (B) (no.
24740185). N.J.W. acknowledges funding from the Technical University of
Denmark. NuSTAR data are accessible from NASA's High Energy Astrophysics
Science Archive Research Center (HEASARC,
http://heasarc.gsfc.nasa.gov/).
NR 32
TC 20
Z9 20
U1 2
U2 4
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 MAY 8
PY 2015
VL 348
IS 6235
BP 670
EP 671
DI 10.1126/science.aaa2259
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CH5AI
UT WOS:000354045700039
PM 25954004
ER
PT J
AU Muratov, CB
Osipov, VV
Vanden-Eijnden, E
AF Muratov, C. B.
Osipov, V. V.
Vanden-Eijnden, E.
TI Energy barriers for bit-encoding states based on 360 degrees domain
walls in ultrathin ferromagnetic nanorings
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID RANDOM-ACCESS MEMORY; MICROMAGNETICS; PATH
AB A numerical thermal stability study of the bit-encoding states in a proposed multi-level magnetic storage element based on an ultrathin ferromagnetic nanoring is presented. The material parameters and the ring dimensions for which there are five distinct metastable magnetization configurations separated by energy barriers exceeding 50k(B)T at room temperature are identified. The results are obtained, using the string method for the study of rare events to locate the transition states separating the metastable states and to identify the most likely thermally activated pathways. (c) 2015 AIP Publishing LLC.
C1 [Muratov, C. B.] New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA.
[Osipov, V. V.] NASA, Intelligent Syst Div, D&SH Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Vanden-Eijnden, E.] New York Univ, Courant Inst Math Sci, New York, NY 10012 USA.
RP Muratov, CB (reprint author), New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA.
EM muratov@njit.edu
FU NSF [DMS-0908279, DMS-1313687, DMS-0708140]; ONR [N00014-11-1-0345]
FX The work of C.B.M. was supported by NSF via Grant Nos. DMS-0908279 and
DMS-1313687. E. V.-E. was supported in part by NSF Grant No. DMS-0708140
and ONR Grant No. N00014-11-1-0345.
NR 35
TC 1
Z9 1
U1 2
U2 16
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAY 7
PY 2015
VL 117
IS 17
AR 17D118
DI 10.1063/1.4914341
PG 4
WC Physics, Applied
SC Physics
GA CI7YW
UT WOS:000354984100341
ER
PT J
AU Song, XP
Huang, CQ
Saatchi, SS
Hansen, MC
Townshend, JR
AF Song, Xiao-Peng
Huang, Chengquan
Saatchi, Sassan S.
Hansen, Matthew C.
Townshend, John R.
TI Annual Carbon Emissions from Deforestation in the Amazon Basin between
2000 and 2010
SO PLOS ONE
LA English
DT Article
ID FOREST COVER CHANGE; BRAZILIAN AMAZON; TROPICAL DEFORESTATION; LAND-USE;
INTERANNUAL VARIABILITY; UNITED-STATES; DENSITY MAPS; TREE COVER;
BIOMASS; CLOUD
AB Reducing emissions fromdeforestation and forest degradation (REDD+) is considered one of themost cost-effective strategies for mitigating climate change. However, historical deforestation and emission rates. critical inputs for setting reference emission levels for REDD+. are poorly understood. Here we use multi-source, time-series satellite data to quantify carbon emissions from deforestation in the Amazon basin on a year-to-year basis between 2000 and 2010. We first derive annual deforestation indicators by using the Moderate Resolution Imaging Spectroradiometer Vegetation Continuous Fields (MODIS VCF) product. MODIS indicators are calibrated by using a large sample of Landsat data to generate accurate deforestation rates, which are subsequently combined with a spatially explicit biomass dataset to calculate committed annual carbon emissions. Across the study area, the average deforestation and associated carbon emissions were estimated to be 1.59 +/- 0.25M ha.yr(-1) and 0.18 +/- 0.07 Pg C.yr(-1) respectively, with substantially different trends and inter-annual variability in different regions. Deforestation in the Brazilian Amazon increased between 2001 and 2004 and declined substantially afterwards, whereas deforestation in the Bolivian Amazon, the Colombian Amazon, and the Peruvian Amazon increased over the study period. The average carbon density of lost forests after 2005 was 130 Mg C.ha(-1), similar to 11% lower than the average carbon density of remaining forests in year 2010 (144 Mg C.ha(-1)). Moreover, the average carbon density of cleared forests increased at a rate of 7 Mg C.ha(-1).yr(-1) from 2005 to 2010, suggesting that deforestation has been progressively encroaching into high-biomass lands in the Amazon basin. Spatially explicit, annual deforestation and emission estimates like the ones derived in this study are useful for setting baselines for REDD+ and other emission mitigation programs, and for evaluating the performance of such efforts.
C1 [Song, Xiao-Peng; Huang, Chengquan; Hansen, Matthew C.; Townshend, John R.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Song, Xiao-Peng; Huang, Chengquan; Townshend, John R.] Univ Maryland, Global Land Cover Facil, College Pk, MD 20742 USA.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Song, XP (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM xpsong@umd.edu
RI Song, Xiao-Peng/F-4894-2014
OI Song, Xiao-Peng/0000-0002-5514-0321
FU NASA's Earth and Space Science Fellowship (NESSF) Program [NNX12AN92H];
Making Earth System Data Records for Use in Research Environments
(MEaSUREs) Program [NNX08AP33A]; Land Cover and Land Use Change Program
[NNH07ZDA001N-LCLUC]; NASA's
FX This study was funded by NASA's Earth and Space Science Fellowship
(NESSF) Program (NNX12AN92H), Making Earth System Data Records for Use
in Research Environments (MEaSUREs) Program (NNX08AP33A), and Land Cover
and Land Use Change Program (NNH07ZDA001N-LCLUC). Additional support was
provided by NASA's
NR 91
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Z9 14
U1 8
U2 45
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 MAY 7
PY 2015
VL 10
IS 5
AR e0126754
DI 10.1371/journal.pone.0126754
PG 21
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CH7KF
UT WOS:000354214400108
PM 25951328
ER
PT J
AU Spitale, JN
Hurford, TA
Rhoden, AR
Berkson, EE
Platts, SS
AF Spitale, Joseph N.
Hurford, Terry A.
Rhoden, Alyssa R.
Berkson, Emily E.
Platts, Symeon S.
TI Curtain eruptions from Enceladus' south-polar terrain
SO NATURE
LA English
DT Article
ID PLUME; JETS
AB Observations of the south pole of the Saturnian moon Enceladus revealed large rifts in the south-polar terrain, informally called 'tiger stripes', named Alexandria, Baghdad, Cairo and Damascus Sulci. These fractures have been shown to be the sources of the observed jets of water vapour and icy particles(1-4) and to exhibit higher temperatures than the surrounding terrain(5,6). Subsequent observations have focused on obtaining close-up imaging of this region to better characterize these emissions. Recent work(7) examined those newer data sets and used triangulation of discrete jets3 to produce maps of jetting activity at various times. Here we show that much of the eruptive activity can be explained by broad, curtain-like eruptions. Optical illusions in the curtain eruptions resulting from a combination of viewing direction and local fracture geometry produce image features that were probably misinterpreted previously as discrete jets. We present maps of the total emission along the fractures, rather than just the jet-like component, for five times during an approximately one-year period in 2009 and 2010. An accurate picture of the style, timing and spatial distribution of the south-polar eruptions is crucial to evaluating theories for the mec(h)anism controlling the eruptions.
C1 [Spitale, Joseph N.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rhoden, Alyssa R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Berkson, Emily E.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Platts, Symeon S.] Univ Arizona, Film & Televis Dept, Tucson, AZ 85721 USA.
RP Spitale, JN (reprint author), Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
EM jnspitale@psi.edu
RI Hurford, Terry/F-2625-2012
FU Cassini Data Analysis and Participating Scientists Program [NNX13AG45G]
FX This work was funded by grant number NNX13AG45G of the Cassini Data
Analysis and Participating Scientists Program. We thank M. Hedman, P.
Thomas and C. Howett for conversations on this topic.
NR 7
TC 12
Z9 12
U1 1
U2 12
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 7
PY 2015
VL 521
IS 7550
BP 57
EP U368
DI 10.1038/nature14368
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CH4YS
UT WOS:000354040900031
PM 25951283
ER
PT J
AU Luneva, MV
Clayson, CA
Dubovikov, MS
AF Luneva, M. V.
Clayson, C. A.
Dubovikov, M. S.
TI Effects of mesoscale eddies in the active mixed layer: test of the
parametrisation in eddy resolving simulations
SO GEOPHYSICAL AND ASTROPHYSICAL FLUID DYNAMICS
LA English
DT Article; Proceedings Paper
CT Workshop on the Dynamics of Shelf Seas
CY OCT 23-24, 2013
CL Univ Liverpool, Liverpool, ENGLAND
HO Univ Liverpool
DE Mesoscale parametrisation; Active mixed layer; Eddy resolving
simulations; Restratification; Eddy diffusivity; omega-equation
ID VERTICAL VELOCITY; OCEAN; CIRCULATION; MODEL; SEA; PARAMETERIZATION;
SURFACE; FRONTS; FLUXES; DIAGNOSIS
AB In eddy resolving simulations, we test a mixed layer mesoscale parametrisation, developed recently by Canuto and Dubovikov [Ocean Model., 2011, 39, 200-207]. With no adjustable parameters, the parametrisation yields the horizontal and vertical mesoscale fluxes in terms of coarse-resolution fields and eddy kinetic energy (EKE). We compare terms of the parametrisation diagnosed from coarse-grained fields with the eddy mesoscale fluxes diagnosed directly from the high resolution model. An expression for the EKE in terms of mean fields has also been found to get a closed parametrisation in terms of the mean fields only. In 40 numerical experiments we simulated two types of flows: idealised flows driven by baroclinic instabilities only, and more realistic flows, driven by wind and surface fluxes as well as by inflow-outflow. The diagnosed quasi-instantaneous horizontal and vertical mesoscale buoyancy fluxes (averaged over 1 degrees - 2 degrees and 10 days) demonstrate a strong scatter typical for turbulent flows, however, the fluxes are positively correlated with the parametrisation with higher (0.5-0.74) correlations at the experiments with larger baroclinic radius Rossby. After being averaged over 3-4 months, diffusivities diagnosed from the eddy resolving simulations are consistent with the parametrisation for a broad range of parameters. Diagnosed vertical mesoscale fluxes restratify mixed layer and are in a good agreement with the parametrisation unless vertical turbulent mixing in the upper layer becomes strong enough in comparison with mesoscale advection. In the latter case, numerical simulations demonstrate that the deviation of the fluxes from the parametrisation is controlled by dimensionless parameter estimating the ratio of vertical turbulent mixing term to mesoscale advection. An analysis using a modified omega-equation reveals that the effects of the vertical mixing of vorticity is responsible for the two-three fold amplification of vertical mesoscale flux. Possible physical mechanisms, responsible for the amplification of vertical mesoscale flux are discussed.
C1 [Luneva, M. V.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England.
[Clayson, C. A.] Woods Hole Oceanog Inst, Phys Oceanog, Woods Hole, MA 02543 USA.
[Dubovikov, M. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dubovikov, M. S.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Luneva, MV (reprint author), Natl Oceanog Ctr, 6 Brownlow St, Liverpool L3 5DA, Merseyside, England.
EM mane1@noc.ac.uk
FU UK Natural Environment Research Council (NERC); Office of Naval Research
[N00014-03-1-0989, N00014-12-10188]; NASA High-End Computing (HEC)
Program through the NASA Center for Climate Simulation (NCCS) at the
Goddard Space Flight Center
FX The work has been dedicated to Professor John Huthnance on the occasion
of his retirement. We thank Professor V.M. Canuto for a useful
discussion of the manuscript and an anonymous reviewers for detailed
analysis of our paper and valuable criticisms. The authors acknowledge
the National Capability funding provided by the UK Natural Environment
Research Council (NERC), the Office of Naval Research under grants
N00014-03-1-0989 and N00014-12-10188, and the NASA High-End Computing
(HEC) Program through the NASA Center for Climate Simulation (NCCS) at
the Goddard Space Flight Center.
NR 44
TC 0
Z9 0
U1 1
U2 6
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0309-1929
EI 1029-0419
J9 GEOPHYS ASTRO FLUID
JI Geophys. Astrophys. Fluid Dyn.
PD MAY 4
PY 2015
VL 109
IS 3
SI SI
BP 281
EP 310
DI 10.1080/03091929.2015.1041023
PG 30
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics
GA CL6QW
UT WOS:000357093200006
ER
PT J
AU Wei, JW
Lee, ZP
Lewis, M
Pahlevan, N
Ondrusek, M
Armstrong, R
AF Wei, Jianwei
Lee, Zhongping
Lewis, Marlon
Pahlevan, Nima
Ondrusek, Michael
Armstrong, Roy
TI Radiance transmittance measured at the ocean surface
SO OPTICS EXPRESS
LA English
DT Article
ID WATER-LEAVING RADIANCE; IN-WATER; COLOR; MODEL; REFLECTANCE; FIELD
AB The radiance transmittance (T-r) is the ratio of the water-leaving radiance (L-w(0(+))) to the sub-surface upwelling radiance (L-u(0(-))), which is an important optical parameter for ocean optics and ocean color remote sensing. Historically, a constant value (similar to 0.54) based on theoretical presumptions has been adopted for Tr and is widely used. This optical parameter, however, has never been measured in the aquatic environments. With a robust setup to measure both L-u(0(-)) and L-w(0(+)) simultaneously in the field, this study presents Tr in the zenith direction between 350 and 700 nm measured in a wide range of oceanic waters. It is found that the measured T-r values are generally consistent with the long-standing theoretical value of 0.54, with mean relative difference less than 10%. In particular, the agreement within the spectral domain of 400-600 nm is found to be the best (with the averaged difference less than 5%). The largest difference is observed for wavelengths longer than 600 nm with the average difference less than 15%, which is related to the generally very small values in both L-u(0(-)) and L-w(0(+)) and rough environmental conditions. These results provide a validation of the setup for simultaneous measurements of upwelling radiance and water-leaving radiance and confidence in the theoretical T-r value used in ocean optics studies at least for oceanic waters. (C) 2015 Optical Society of America
C1 [Wei, Jianwei; Lee, Zhongping] Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA.
[Lewis, Marlon] Dalhousie Univ, Dept Oceanog, Halifax, NS B3H 4J1, Canada.
[Pahlevan, Nima] NASA Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA.
[Pahlevan, Nima] SSAI, Lanham, MD 20706 USA.
[Ondrusek, Michael] NOAA Ctr Weather & Climate Predict NCWCP, College Pk, MD 20740 USA.
[Armstrong, Roy] Univ Puerto Rico, Bioopt Oceanog Lab, Mayaguez, PR 00681 USA.
RP Wei, JW (reprint author), Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA.
EM jianwei.wei@umb.edu
RI Ondrusek, Michael/F-5617-2010; wei, Jianwei/E-8031-2016;
OI Ondrusek, Michael/0000-0002-5311-9094; wei, Jianwei/0000-0002-6872-3534;
Pahlevan, Nima/0000-0002-5454-5212
FU National Aeronautic and Space Administration (NASA) Ocean Biology and
Biogeochemistry and Water and Energy Cycle Programs; National Oceanic
and Atmospheric Administration (NOAA) JPSS VIIRS Ocean Color Cal/Val
Project; NOAA CREST Grant [NA06OAR480162]
FX This study is funded by the National Aeronautic and Space Administration
(NASA) Ocean Biology and Biogeochemistry and Water and Energy Cycle
Programs and the National Oceanic and Atmospheric Administration (NOAA)
JPSS VIIRS Ocean Color Cal/Val Project. Field measurements in Puerto
Rico were partially supported by NOAA CREST Grant # NA06OAR480162. We
thank Dr. Giuseppe Zibordi for assistance in the field campaign. Three
anonymous reviewers are thanked for their comments and suggestions.
NR 23
TC 5
Z9 5
U1 0
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD MAY 4
PY 2015
VL 23
IS 9
BP 11826
EP 11837
DI 10.1364/OE.23.011826
PG 12
WC Optics
SC Optics
GA CH9EB
UT WOS:000354337700091
PM 25969274
ER
PT J
AU DellaCorte, C
AF DellaCorte, Christopher
TI REMEMBERING EDWARD T. HANEY
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Letter
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD MAY
PY 2015
VL 71
IS 5
BP 7
EP 7
PG 1
WC Engineering, Mechanical
SC Engineering
GA CG6UF
UT WOS:000353437200011
ER
PT J
AU Nayagam, V
Dietrich, DL
Hicks, MC
Williams, FA
AF Nayagam, Vedha
Dietrich, Daniel L.
Hicks, Michael C.
Williams, Forman A.
TI Cool-flame, extinction during n-alkane droplet combustion in
microgravity
SO COMBUSTION AND FLAME
LA English
DT Article
DE Cool flame extinction; Droplet combustion; Microgravity; Normal alkane
ID SPHERICAL DIFFUSION FLAMES; SYSTEMS; HEPTANE; HYDROCARBON; OXIDATION;
IGNITION
AB Recent droplet-combustion experiments onboard the International Space Station (ISS) have revealed that large n-alkane droplets, following radiative extinction of the visible flame, can continue to burn quasisteadily in a low-temperature regime, characterized by negative-temperature-coefficient (NTC) chemistry. In this study we report experimental observations of n-heptane, n-octane, and n-decane droplets of varying initial size burning in oxygen/nitrogen, oxygen/nitrogen/carbon dioxide, and oxygen/nitrogen/helium environments at pressures from 0.5 to 1.0 atm, with oxygen concentrations from 14% to 25% by volume. These large n-alkane droplets exhibited radiative extinction of the hot flame, followed by quasi-steady low-temperature burning, which terminated with diffusive extinction accompanied by the formation of a vapor cloud, while small droplets did not exhibit radiative extinction but instead burned to completion or disruptively extinguished. Results for droplet burning rates in both the hot-flame and cool-flame regimes, as well as droplet extinction diameters at the end of each stage, are presented. The cool-flame extinction diameters for all three n-alkanes are shown to follow a similar trend as functions of the oxygen concentration, predicted here from a simplified theoretical model that is based on the reaction-rate parameters for the oxygen molecule addition to the alkyl radical and for ketohydroperoxide decomposition. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Nayagam, Vedha] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
[Dietrich, Daniel L.; Hicks, Michael C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
RP Nayagam, V (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
EM v.nayagam@grc.nasa.gov
FU NASA Space Life and Physical Sciences Research and Applications Program;
International Space Station Program
FX The authors would like to thank the FLEX team members Profs. T.
Avedisian, M.Y. Choi, T. Farouk, F. Dryer, and B. Shaw. This work was
supported by the NASA Space Life and Physical Sciences Research and
Applications Program and the International Space Station Program. Mr. J.
Mark Hickman served as the project manager.
NR 19
TC 11
Z9 11
U1 4
U2 16
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD MAY
PY 2015
VL 162
IS 5
BP 2140
EP 2147
DI 10.1016/j.combustflame.2015.01.012
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CN6RI
UT WOS:000358561500045
ER
PT J
AU Detweiler, AM
Mioni, CE
Hellier, KL
Allen, JJ
Carter, SA
Bebout, BM
Fleming, EE
Corrado, C
Prufert-Bebout, LE
AF Detweiler, Angela M.
Mioni, Cecile E.
Hellier, Katie L.
Allen, Jordan J.
Carter, Sue A.
Bebout, Brad M.
Fleming, Erich E.
Corrado, Carley
Prufert-Bebout, Leslie E.
TI Evaluation of wavelength selective photovoltaic panels on microalgae
growth and photosynthetic efficiency
SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS
LA English
DT Article
DE Microalgae cultivation; Growth rate; Wavelength selective luminescent
solar concentrators; Photovoltaic cells; Greenhouse
ID LIGHT-EMITTING-DIODES; NITROGEN LIMITATION; SOLAR CONCENTRATORS;
ENERGY-CONVERSION; DUNALIELLA-SALINA; ALGAE; ENHANCEMENT; IRRADIANCE;
RADIATION; CULTURE
AB Large-scale cultivation of microalgal biomass in open systems can benefit fromthe lowcost of using natural sun-light, as opposed to artificial light, but may encounter problems with photoinhibition, high evaporation rates, potential contamination and high energy demand. Wavelength selective luminescent solar concentrator (LSC) panels can solve some of these problems when incorporated into low-cost sheltered structures for algal biomass production that concurrently produce their own electricity by harnessing select portions of solar energy, not used for algal growth. The LSC panels in this study contained a fluorescent dye, Lumogen Red 305, which transmits blue and red wavelengths used for photosynthesis with high efficiency, while absorbing the green wavelengths and re-emitting them as red wavelengths. The fluorescently generated red wavelengths are either transmitted to boost algal growth, or waveguided and captured by photovoltaic cells to be converted into electricity. We found that different strains of microalgae (currently used commercially) grew equally well under the altered spectral conditions created by the luminescent panels, compared to growth under the full solar spectrum. Thus this technology presents a new approach wherein algae can be grown under protected, controlled conditions, while the cost of operations is offset by the structure's internal electrical production, without any loss to algal growth rate or achievable biomass density. Published by Elsevier B.V.
C1 [Detweiler, Angela M.; Bebout, Brad M.; Prufert-Bebout, Leslie E.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Detweiler, Angela M.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Mioni, Cecile E.] Calif State Univ Monterey Bay, Sci & Environm Policy Div, Seaside, CA 93955 USA.
[Hellier, Katie L.; Carter, Sue A.; Corrado, Carley] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Allen, Jordan J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Fleming, Erich E.] Calif State Univ Channel Islands, Dept Biol, Camarillo, CA 93012 USA.
RP Prufert-Bebout, LE (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4,Bldg 239,Room 334,POB 1, Moffett Field, CA 94035 USA.
EM leslie.e.bebout@nasa.gov
OI Hellier, Kaitlin/0000-0002-6328-1167
FU UC Discovery Grant "Lowcost, high efficiency luminescent solar
greenhouse" [192864]; Abengoa Solar
FX This study was funded by the UC Discovery Grant "Lowcost, high
efficiency luminescent solar greenhouse" (grant # 192864) to Dr. Sue
Carter in collaboration with the Algae for Exploration (AlEx) working
group in the Exobiology Branch at NASA ARC. Dr. Carter received
additional funding from Abengoa Solar. The authors would like to thank
Glenn Alers for making available the LSC panels used in this study,
Stuart Pilorz for the help with data analysis, and Craig Everroad and
Thomas Murphy for their insightful comments in reviewing this
manuscript.
NR 34
TC 3
Z9 3
U1 7
U2 49
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-9264
J9 ALGAL RES
JI Algal Res.
PD MAY
PY 2015
VL 9
BP 170
EP 177
DI 10.1016/j.algal.2015.03.003
PG 8
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA CM8YF
UT WOS:000357988700021
ER
PT J
AU Ciceri, S
Mancini, L
Southworth, J
Bruni, I
Nikolov, N
D'Ago, G
Schroder, T
Bozza, V
Tregloan-Reed, J
Henning, T
AF Ciceri, S.
Mancini, L.
Southworth, J.
Bruni, I.
Nikolov, N.
D'Ago, G.
Schroeder, T.
Bozza, V.
Tregloan-Reed, J.
Henning, Th.
TI Physical properties of the HAT-P-23 and WASP-48 planetary systems from
multi-colour photometry
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; stars: fundamental parameters; techniques:
photometric; stars: individual: HAT-P-23; stars: individual: WASP-48
ID TRANSITING EXTRASOLAR PLANETS; STELLAR EVOLUTION DATABASE;
HIGH-PRECISION PHOTOMETRY; LIMB-DARKENING LAW; TRANSMISSION SPECTRUM;
SURFACE GRAVITIES; LIGHT-CURVE; ATMOSPHERE MODELS; TIDAL-EVOLUTION;
PARAMETERS
AB Context. Accurate and repeated photometric follow-up observations of planetary transit events are important to precisely characterize the physical properties of exoplanets. A good knowledge of the main characteristics of the exoplanets is fundamental in order to trace their origin and evolution. Multi-band photometric observations play an important role in this process.
Aims. By using new photometric data, we computed precise estimates of the physical properties of two transiting planetary systems at equilibrium temperatures of similar to 2000 K.
Methods. We present new broadband, multi-colour photometric observations obtained using three small class telescopes and the telescope-defocussing technique. In particular we obtained 11 and 10 light curves covering 8 and 7 transits of HAT-P-23 and WASP-48, respectively. For each of the two targets, one transit event was simultaneously observed through four optical filters. One transit of WASP-48 b was monitored with two telescopes from the same observatory. The physical parameters of the systems were obtained by fitting the transit light curves with JKTEBOP and from published spectroscopic measurements.
Results. We have revised the physical parameters of the two planetary systems, finding a smaller radius for both HAT-P-23 b and WASP-48 b, R-b = 1.224 +/- 0.037 R-Jup and R-b = 1.396 +/- 0.051 R-Jup, respectively, than those measured in the discovery papers (R-b = 1.368 +/- 0.090 R-Jup and R-b = 1.67 +/- 0.10 R-Jup). The density of the two planets are higher than those previously published (rho(b) similar to 1.1 and similar to 0.3 rho(jup) for HAT-P-23 and WASP-48, respectively) hence the two hot Jupiters are no longer located in a parameter space region of highly inflated planets. An analysis of the variation of the planet's measured radius as a function of optical wavelength reveals flat transmission spectra within the experimental uncertainties. We also confirm the presence of the eclipsing contact binary NSVS-3071474 in the same field of view of WASP-48, for which we refine the value of the period to be 0.459 d.
C1 [Ciceri, S.; Mancini, L.; Schroeder, T.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Bruni, I.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Nikolov, N.] Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England.
[D'Ago, G.; Bozza, V.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy.
[D'Ago, G.; Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ciceri, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM ciceri@mpia.de
RI D'Ago, Giuseppe/N-8318-2016;
OI D'Ago, Giuseppe/0000-0001-9697-7331; Bruni, Ivan/0000-0002-1560-4590
NR 53
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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2015
VL 577
AR A54
DI 10.1051/0004-6361/201425449
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM0CN
UT WOS:000357345900006
ER
PT J
AU Guo, JN
Zeitlin, C
Wimmer-Schweingruber, RF
Hassler, DM
Posner, A
Heber, B
Kohler, J
Rafkin, S
Ehresmann, B
Appel, JK
Bohm, E
Bottcher, S
Burmeister, S
Brinza, DE
Lohf, H
Martin, C
Reitz, G
AF Guo, Jingnan
Zeitlin, Cary
Wimmer-Schweingruber, Robert F.
Hassler, Donald M.
Posner, Arik
Heber, Bernd
Koehler, Jan
Rafkin, Scot
Ehresmann, Bent
Appel, Jan K.
Boehm, Eckart
Boettcher, Stephan
Burmeister, Soenke
Brinza, David E.
Lohf, Henning
Martin, Cesar
Reitz, Goenther
TI Variations of dose rate observed by MSL/RAD in transit to Mars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: detectors; space vehicles: instruments;
solar-terrestrial relations
ID GALACTIC COSMIC-RAYS; RADIATION; MODULATION
AB Aims. To predict the cruise radiation environment related to future human missions to Mars, the correlation between solar modulation potential and the dose rate measured by the Radiation Assessment Detector (RAD) has been analyzed and empirical models have been employed to quantify this correlation.
Methods. The instrument RAD, onboard Mars Science Laboratory's (MSL) rover Curiosity, measures a broad spectrum of energetic particles along with the radiation dose rate during the 253-day cruise phase as well as on the surface of Mars. With these first ever measurements inside a spacecraft from Earth to Mars, RAD observed the impulsive enhancement of dose rate during solar particle events as well as a gradual evolution of the galactic cosmic ray (GCR) induced radiation dose rate due to the modulation of the primary GCR flux by the solar magnetic field, which correlates with long-term solar activities and heliospheric rotation.
Results. We analyzed the dependence of the dose rate measured by RAD on solar modulation potentials and estimated the dose rate and dose equivalent under different solar modulation conditions. These estimations help us to have approximate predictions of the cruise radiation environment, such as the accumulated dose equivalent associated with future human missions to Mars.
Conclusions. The predicted dose equivalent rate during solar maximum conditions could be as low as one-fourth of the current RAD cruise measurement. However, future measurements during solar maximum and minimum periods are essential to validate our estimations.
C1 [Guo, Jingnan; Wimmer-Schweingruber, Robert F.; Heber, Bernd; Koehler, Jan; Appel, Jan K.; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Lohf, Henning; Martin, Cesar] Univ Kiel, Inst Expt & Appl Phys, D-24118 Kiel, Germany.
[Zeitlin, Cary] SW Res Inst, Earth Oceans & Space Dept, Durham, NH USA.
[Hassler, Donald M.; Rafkin, Scot; Ehresmann, Bent] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA.
[Posner, Arik] NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA.
[Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Reitz, Goenther] Deutsch Zentrum Luft & Raumfahrt, Aerosp Med, D-51147 Cologne, Germany.
RP Guo, JN (reprint author), Univ Kiel, Inst Expt & Appl Phys, Olshaussenstr 40, D-24118 Kiel, Germany.
EM guo@physik.uni-kiel.de
FU National Aeronautics and Space Administration (NASA, HEOMD) under Jet
Propulsion Laboratory (JPL) [1273039]; DLR; DLR's Space Administration
[50QM0501, 50QM1201]; NASA
FX RAD is supported by the National Aeronautics and Space Administration
(NASA, HEOMD) under Jet Propulsion Laboratory (JPL) sub-contract
#1273039 to Southwest Research Institute and in Germany by DLR and DLR's
Space Administration grant numbers 50QM0501 and 50QM1201 to the
Christian Albrechts University, Kiel. Part of this research was carried
out at JPL, California Institute of Technology, under a contract with
NASA. We thank Shawn Kang at JPL for his work on the shielding model of
the spacecraft during the cruise phase. The sunspot data has been
obtained from Source: WDC-SILSO, Royal Observatory of Belgium, Brussels.
We are grateful to the Cosmic Ray Station of the University of Oulu and
Sodankyla Geophysical Observatory for sharing their Neutron Monitor
count rate data. The data used in this paper are archived in the NASA
Planetary Data System's Planetary Plasma Interactions Node at the
University of California, Los Angeles. The archival volume includes the
full binary raw data files, detailed descriptions of the structures
therein, and higher-level data products in human-readable form. The PPI
node is hosted at the following URL: http://ppi.pds.nasa.gov/
NR 22
TC 6
Z9 6
U1 3
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 MAY
PY 2015
VL 577
AR A58
DI 10.1051/0004-6361/201525680
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM0CN
UT WOS:000357345900010
ER
PT J
AU Peretz, U
Behar, E
Drake, SA
AF Peretz, Uria
Behar, Ehud
Drake, Stephen A.
TI Coronae of stars with supersolar elemental abundances
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: coronae; stars: general
ID X-RAY SPECTROSCOPY; SOLAR-TYPE STARS; PHOTOSPHERIC ABUNDANCES;
ATMOSPHERIC PARAMETERS; ENERGETIC PARTICLES; ALPHA-CENTAURI; ACTIVITY
CYCLE; BINARY-SYSTEM; CHANDRA; DWARFS
AB Coronal elemental abundances are known to deviate from the photospheric values of their parent star, with the degree of deviation depending on the first ionization potential (FIP). This study focuses on the coronal composition of stars with supersolar photospheric abundances. We present the coronal abundances of six such stars: 11 LMi, iota Hor, HR 7291, tau Boo, and alpha Cen A and B. These stars all have high-statistics X-ray spectra, three of which are presented for the first time. The abundances we measured were obtained using the line-resolved spectra of the Reflection Grating Spectrometer (RGS) in conjunction with the higher throughput EPIC-pn camera spectra onboard the XMM-Newton observatory. A collisionally ionized plasma model with two or three temperature components is found to represent the spectra well. All elements are found to be consistently depleted in the coronae compared to their respective photospheres. For 11 LMi and tau Boo no FIP effect is present, while iota Hor, HR 7291, and alpha Cen A and B show a clear FIP trend. These conclusions hold whether the comparison is made with solar abundances or the individual stellar abundances. Unlike the solar corona, where low-FIP elements are enriched, in these stars the FIP effect is consistently due to a depletion of high-FIP elements with respect to actual photospheric abundances. A comparison with solar (instead of stellar) abundances yields the same fractionation trend as on the Sun. In both cases, a similar FIP bias is inferred, but different fractionation mechanisms need to be invoked.
C1 [Peretz, Uria; Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Drake, Stephen A.] USRA, CRESST, Greenbelt, MD 20771 USA.
[Drake, Stephen A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Peretz, U (reprint author), Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
EM uperetz@tx.technion.ac.il
FU I-CORE program of the Planning and Budgeting Committee; Israel Science
Foundation [1937/12, 1163/10]; Israel's Ministry of Science and
Technology; National Science Foundation [PHYS-1066293]
FX The authors are grateful to an anonymous referee for useful comments
that led us to broaden the sample of the paper. This research is
supported by the I-CORE program of the Planning and Budgeting Committee
and the Israel Science Foundation (grant numbers 1937/12 and 1163/10),
and by a grant from Israel's Ministry of Science and Technology. This
work was supported in part by the National Science Foundation under
Grant No. PHYS-1066293 and the hospitality of the Aspen Center for
Physics.
NR 43
TC 1
Z9 1
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2015
VL 577
AR A93
DI 10.1051/0004-6361/201424769
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM0CN
UT WOS:000357345900045
ER
PT J
AU Pon, A
Caselli, P
Johnstone, D
Kaufman, M
Butler, MJ
Fontani, F
Jimenez-Serra, I
Tan, JC
AF Pon, A.
Caselli, P.
Johnstone, D.
Kaufman, M.
Butler, M. J.
Fontani, F.
Jimenez-Serra, I.
Tan, J. C.
TI Mid-J CO shock tracing observations of infrared dark clouds. I.
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; stars: formation; turbulence; shock waves; ISM: molecules
ID MASSIVE-STAR-FORMATION; MOLECULAR CLOUDS; MAGNETOHYDRODYNAMIC
TURBULENCE; DISSIPATION; CORES; DEUTERATION; CHEMISTRY; EMISSION;
VELOCITY; OUTFLOWS
AB Infrared dark clouds (IRDCs) are dense, molecular structures in the interstellar medium that can harbour sites of high-mass star formation. IRDCs contain supersonic turbulence, which is expected to generate shocks that locally heat pockets of gas within the clouds. We present observations of the CO J = 8-7, 9-8, and 10-9 transitions, taken with the Herschel Space Observatory, towards four dense, starless clumps within IRDCs (C1 in G028.37+00.07, F1 and F2 in G034.43+0007, and G2 in G034.77-0.55). We detect the CO J = 8-7 and 9-8 transitions towards three of the clumps (C1, F1, and F2) at intensity levels greater than expected from photodissociation region (PDR) models. The average ratio of the 8-7 to 9-8 lines is also found to be between 1.6 and 2.6 in the three clumps with detections, significantly smaller than expected from PDR models. These low line ratios and large line intensities strongly suggest that the C1, F1, and F2 clumps contain a hot gas component not accounted for by standard PDR models. Such a hot gas component could be generated by turbulence dissipating in low velocity shocks.
C1 [Pon, A.; Caselli, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA.
[Johnstone, D.] NRC Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada.
[Kaufman, M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Kaufman, M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Butler, M. J.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[Fontani, F.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Jimenez-Serra, I.] European So Observ, D-85748 Garching, Germany.
[Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Tan, J. C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
RP Pon, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM andyrpon@mpe.mpg.de
RI Fontani, Francesco/R-5351-2016
OI Fontani, Francesco/0000-0003-0348-3418
FU European Research Council (ERC) [PALs 320620]; Natural Sciences and
Engineering Research Council (NSERC) Discovery Grant; European Union
[PIIF-GA-2011-301538]
FX We would like to thank our referee, Dr. Goldsmith, for helping us
improve the quality of this paper. The authors would like to thank Dr.
N. Bailey, Dr. J. Bailey, and Dr. J. D. Henshaw for many insightful
conversations regarding the data presented in this paper. The authors
also thank Dr. C. McCoey and Dr. S. Beaulieu for help with HIPE. A.P.
and P.C. acknowledge the financial support of the European Research
Council (ERC; project PALs 320620). D. J. acknowledges support from a
Natural Sciences and Engineering Research Council (NSERC) Discovery
Grant. I. J. S. acknowledges the funding received from the People
Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme (FP7/2007-2013) under REA grant agreement
PIIF-GA-2011-301538. This research has made use of the Smithsonian
Astrophysical Observatory (SAO)/National Aeronautics and Space
Administration's (NASA's) Astrophysics Data System (ADS). HIFI has been
designed and built by a consortium of institutes and university
departments from across Europe, Canada and the United States under the
leadership of SRON Netherlands Institute for Space Research, Groningen,
The Netherlands and with major contributions from Germany, France and
the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR,
LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth;
Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF;
Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio
Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden:
Chalmers University of Technology - MC2, RSS & GARD; Onsala Space
Observatory; Swedish National Space Board, Stockholm University -
Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL,
NHSC. This research has made use of the astro-ph archive. Some spectral
line data were taken from the Spectral Line Atlas of Interstellar
Molecules (SLAIM; Available at http://www.splatalogue.net); (Lovas,
priv. comm.; Remijan et al. 2007).
NR 38
TC 8
Z9 8
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2015
VL 577
AR A75
DI 10.1051/0004-6361/201525681
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM0CN
UT WOS:000357345900027
ER
PT J
AU Vinas, AF
Moya, PS
Navarro, RE
Valdivia, JA
Araneda, JA
Munoz, V
AF Vinas, Adolfo F.
Moya, Pablo S.
Navarro, Roberto E.
Valdivia, J. Alejandro
Araneda, Jaime A.
Munoz, Victor
TI Electromagnetic fluctuations of the whistler-cyclotron and firehose
instabilities in a Maxwellian and Tsallis-kappa-like plasma
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND; THERMAL NOISE; ELECTRONS; DISTRIBUTIONS; STATISTICS; ION
AB Observed electron velocity distributions in the Earth's magnetosphere and the solar wind exhibit a variety of nonthermal features which deviate from thermal equilibrium, for example, in the form of temperature anisotropies, suprathermal tail extensions, and field-aligned beams. The state close to thermal equilibrium and its departure from it provides a source for spontaneous emissions of electromagnetic fluctuations, such as the whistler. Here we present a comparative analysis of the electron whistler-cyclotron and firehose fluctuations based upon anisotropic plasma modeled with Maxwellian and Tsallis-kappa-like particle distributions, to explain the correspondence relationship of the magnetic fluctuations as a function of the electron temperature and thermal anisotropy in the solar wind and magnetosphere plasmas. The analysis presented here considers correlation theory of the fluctuation-dissipation theorem and the dispersion relation of transverse fluctuations, with wave vectors parallel to the uniform background magnetic field, in a finite temperature anisotropic thermal bi-Maxwellian and nonthermal Tsallis-kappa-like magnetized electron-proton plasma. Dispersion analysis and stability thresholds are derived for these thermal and nonthermal distributions using plasma and field parameters relevant to the solar wind and magnetosphere environments. Our results indicate that there is an enhancement of the fluctuations level in the case of nonthermal distributions due to the effective higher temperature and the excess of suprathermal particles. These results suggest that a comparison of the electromagnetic fluctuations due to thermal and nonthermal distributions provides a diagnostic signature by which inferences about the nature of the particle velocity distribution function can be ascertained without in situ particle measurements.
C1 [Vinas, Adolfo F.; Moya, Pablo S.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Moya, Pablo S.; Navarro, Roberto E.; Valdivia, J. Alejandro; Munoz, Victor] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
[Navarro, Roberto E.; Araneda, Jaime A.] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Concepcion, Chile.
RP Vinas, AF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
EM adolfo.vinas@nasa.gov
RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Araneda,
Jaime/J-9245-2015; Navarro, Roberto/F-7045-2014; Munoz,
Victor/A-2255-2008
OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904;
Navarro, Roberto/0000-0003-0782-1904;
FU NASA's Wind/SWE program; Comision Nacional de Ciencia y Tecnologia
(CONICyT, Chile); FONDECYT [1110880, 3150262, 1121144, 1110135, 1110729,
1130273]
FX A. F. Vinas would like to thank the NASA's Wind/SWE program for the
support of this research. We also thank the Comision Nacional de Ciencia
y Tecnologia (CONICyT, Chile) by providing financial support for
postdoctoral (P. S. Moya) and doctoral (R. Navarro) fellows. We would
like to thank FONDECYT 1110880 (J. A. Araneda), 3150262 (R. E. Navarro),
1121144 (V. Munoz), and 1110135, 1110729, and 1130273 (J. A. Valdivia)
for providing financial support. The results of this paper do not
require any spacecraft data analysis, but the numerical data generated
to reproduce all the figures will be made available upon request.
NR 40
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Z9 19
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 MAY
PY 2015
VL 120
IS 5
BP 3307
EP 3317
DI 10.1002/2014JA020554
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600003
ER
PT J
AU Tang, XW
Cattell, C
Lysak, R
Wilson, LB
Dai, L
Thaller, S
AF Tang, Xiangwei
Cattell, Cynthia
Lysak, Robert
Wilson, Lynn B., III
Dai, Lei
Thaller, Scott
TI THEMIS observations of electrostatic ion cyclotron waves and associated
ion heating near the Earth's dayside magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID FIELD-ALIGNED CURRENTS; HYDROGEN CYCLOTRON; PLASMA-WAVES; POLAR
MAGNETOSPHERE; INSTABILITY; EXCITATION; DIFFUSION; BEAMS; MAGNETOTAIL;
INSTRUMENT
AB We present the first observations of large-amplitude electrostatic ion cyclotron (EIC) waves near the Earth's dayside magnetopause at MLT of similar to 14 using data from Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellites. The EIC waves were identified in a boundary layer in the magnetosphere adjacent to the magnetopause where reconnection was occurring. The EIC wave power was primarily at 2f(cH) (where f(cH) is the hydrogen cyclotron frequency) and simultaneously observed with perpendicular ion heating. The EIC waves had electric field amplitudes as large as 30 mV/m peak to peak with significant power both perpendicular and parallel to the magnetic field. These amplitudes were greater than those of previously observed ion cyclotron harmonics at the nightside magnetopause. The EIC waves occurred during an interval of enhancements in the quasi-static electric field and fluctuations in the background magnetic field, plasma density, and temperatures. The observations indicate that a plasma density gradient is a possible source of free energy for the EIC waves. The observed flow shears are not large enough to drive the waves. Whistler mode waves were identified near the EIC wave region but closer to the magnetopause in a region with slightly higher ion and electron temperatures.
C1 [Tang, Xiangwei; Cattell, Cynthia; Lysak, Robert; Dai, Lei; Thaller, Scott] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Wilson, Lynn B., III] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
RP Tang, XW (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM xtang@physics.umn.edu
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Cattell,
Cynthia/0000-0002-3805-320X
FU Leonard Burlaga/Arctowski Medal Fellowship; NASA [NAS5-02099]; German
Ministry for Economy and Technology; German Center for Aviation and
Space (DLR) [50 OC 0302]; [NNX08AF28]; [NNX13AE16G]
FX At the University of Minnesota, this work was supported by NNX08AF28 and
NNX13AE16G. X. Tang was partially supported by a Leonard
Burlaga/Arctowski Medal Fellowship. The data for this paper are
available at http://themis.ssl.berkeley.edu/index.shtml. The authors
acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of
data from the THEMIS Mission, specifically: J. W. Bonnell and F. S.
Mozer for the use of EFI data; D. Larson and R. P. Lin for the use of
SST data; C. W. Carlson and J. P. McFadden for the use of ESA data; A.
Roux and O. LeContel for the use of SCM data; and K. H. Glassmeier, U.
Auster, and W. Baumjohann for the use of FGM data provided under the
lead of the Technical University of Braunschweig and with financial
support through the German Ministry for Economy and Technology and the
German Center for Aviation and Space (DLR) under contract 50 OC 0302.
The authors are grateful for discussion and comments from S. J. Monson,
A. Breneman, and J. Dombeck.
NR 48
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2015
VL 120
IS 5
BP 3380
EP 3392
DI 10.1002/2015JA020984
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600008
ER
PT J
AU Collinson, GA
Grebowsky, J
Sibeck, DG
Jian, LK
Boardsen, S
Espley, J
Hartle, D
Zhang, TLL
Barabash, S
Futaana, Y
Kollmann, P
AF Collinson, Glyn A.
Grebowsky, Joseph
Sibeck, David G.
Jian, Lan K.
Boardsen, Scott
Espley, Jared
Hartle, Dick
Zhang, Tielong L.
Barabash, Stas
Futaana, Yoshifumi
Kollmann, Peter
TI The impact of a slow interplanetary coronal mass ejection on Venus
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ONE-HERTZ WAVES; BOW SHOCK; MAGNETIC-FIELD; SOLAR-WIND; IONOSPHERIC
HOLES; EXPRESS MISSION; SPACE PLASMAS; MARS EXPRESS; UPSTREAM; NIGHTSIDE
AB We present Venus Express observations of the impact of a slow interplanetary coronal mass ejection (ICME), which struck Venus on 23 December 2006, creating unusual quasi steady state upstream conditions for the 2 h close to periapsis: an enhanced (similar to 20 nT) interplanetary magnetic field (IMF), radially aligned with the Sun-Venus line; and a dense (similar to 10 cm(-3)) solar wind. Contrary to our current understanding and expectations, the ionosphere became partially demagnetized. We also find evidence for shocked sheathlike solar wind protons and electrons in the wake of Venus, and powerful (approximate to 100 nT(2)/Hz) foreshock whistler mode waves radiating from the bow shock at an unexpectedly low frequency (0.6 Hz). Given the abnormally high density of escaping heavy ions at the magnetopause boundary (295 cm(-3), one of the highest of the whole mission) and the enhanced density of escaping heavy ions in the wake, we find that even weak ICMEs with no driving shocks can increase atmospheric loss rates at Venus and suggests that the Bx component of the IMF may be a factor in atmospheric escape rates.
C1 [Collinson, Glyn A.; Grebowsky, Joseph; Sibeck, David G.; Jian, Lan K.; Boardsen, Scott; Espley, Jared; Hartle, Dick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Collinson, Glyn A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Collinson, Glyn A.] Lab Gwyddoniaeth Gofod, Cricieth, Gwynedd, Wales.
[Jian, Lan K.] Univ Maryland, College Pk, MD 20742 USA.
[Boardsen, Scott] Univ Maryland Baltimore Cty, Catonsville, MD USA.
[Zhang, Tielong L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Barabash, Stas; Futaana, Yoshifumi] Swedish Inst Space Phys, Inst Rymdfys, S-98128 Kiruna, Sweden.
[Kollmann, Peter] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Collinson, GA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM glyn.a.collinson@nasa.gov
RI Jian, Lan/B-4053-2010; Kollmann, Peter/C-2583-2016;
OI Jian, Lan/0000-0002-6849-5527; Kollmann, Peter/0000-0002-4274-9760;
Futaana, Yoshifumi/0000-0002-7056-3517
NR 54
TC 2
Z9 2
U1 2
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2015
VL 120
IS 5
BP 3489
EP 3502
DI 10.1002/2014JA020616
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600016
ER
PT J
AU Delzanno, GL
Borovsky, JE
Thomsen, MF
Moulton, JD
MacDonald, EA
AF Delzanno, G. L.
Borovsky, J. E.
Thomsen, M. F.
Moulton, J. D.
MacDonald, E. A.
TI Future beam experiments in the magnetosphere with plasma contactors: How
do we get the charge off the spacecraft?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ARTIFICIAL AURORAL STREAKS; ELECTRON-BEAM; POTENTIAL CONTROL; ACTIVE
SPACECRAFT; SOUNDING ROCKET; CODE; EMISSIONS; ORBIT
AB The idea of using a high-voltage electron beam with substantial current to actively probe magnetic field line connectivity in space has been discussed since the 1970s. However, its experimental realization onboard a magnetospheric spacecraft has never been accomplished because the tenuous magnetospheric plasma cannot provide the return current necessary to keep spacecraft charging under control. In this work, we perform Particle-In-Cell simulations to investigate the conditions under which a high-voltage electron beam can be emitted from a spacecraft and explore solutions that can mitigate spacecraft charging. The electron beam cannot simply be compensated for by an ion beam of equal current, because the Child-Langmuir space charge limit is violated under conditions of interest. On the other hand, releasing a high-density neutral contactor plasma prior and during beam emission is critical in aiding beam emission. We show that after an initial transient controlled by the size of the contactor cloud where the spacecraft potential rises, the spacecraft potential can settle into conditions that allow for electron beam emission. A physical explanation of this result in terms of ion emission into spherical geometry from the surface of the plasma cloud is presented, together with scaling laws of the peak spacecraft potential varying the ion mass and beam current. These results suggest that a strategy where the contactor plasma and the electron beam operate simultaneously might offer a pathway to perform beam experiments in the magnetosphere.
C1 [Delzanno, G. L.; Moulton, J. D.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Borovsky, J. E.] Space Sci Inst, Boulder, CO USA.
[Borovsky, J. E.] Univ Michigan, AOSS, Ann Arbor, MI 48109 USA.
[Thomsen, M. F.] Los Alamos Natl Lab, Intelligence & Space Res Div, Los Alamos, NM USA.
[MacDonald, E. A.] Nasa Goddard, Greenbelt, MD USA.
RP Delzanno, GL (reprint author), Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
EM delzanno@lanl.gov
FU Laboratory Directed Research and Development program (LDRD), U.S.
Department of Energy Office of Science, Office of Fusion Energy
Sciences, under National Nuclear Security Administration of the U.S.
Department of Energy by Los Alamos National Laboratory
[DE-AC52-06NA25396]; NASA magnetospheric GI program; NASA Geospace SRT
program; NASA LWS TRT program
FX The data used for this paper were obtained from numerical calculations
and are available from the corresponding author upon request. The
authors wish to thank Patrick Colestock and Eric Dors for useful
discussions and Ira Katz and Myron Mandell for providing useful
references on the SCATHA experiments. This work was funded by the
Laboratory Directed Research and Development program (LDRD), U.S.
Department of Energy Office of Science, Office of Fusion Energy
Sciences, under the auspices of the National Nuclear Security
Administration of the U.S. Department of Energy by Los Alamos National
Laboratory, operated by Los Alamos National Security LLC under contract
DE-AC52-06NA25396. This research used resources provided by the Los
Alamos National Laboratory Institutional Computing Program. J. E. B. was
funded by the NASA magnetospheric GI program, the NASA Geospace SRT
program, and by the NASA LWS TRT program.
NR 46
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U1 4
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2015
VL 120
IS 5
BP 3647
EP 3664
DI 10.1002/2014JA020608
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600028
ER
PT J
AU Kempf, Y
Pokhotelov, D
Gutynska, O
Wilson, LB
Walsh, BM
von Alfthan, S
Hannuksela, O
Sibeck, DG
Palmroth, M
AF Kempf, Yann
Pokhotelov, Dimitry
Gutynska, Olga
Wilson, Lynn B., III
Walsh, Brian M.
von Alfthan, Sebastian
Hannuksela, Otto
Sibeck, David G.
Palmroth, Minna
TI Ion distributions in the Earth's foreshock: Hybrid-Vlasov simulation and
THEMIS observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-FREQUENCY WAVES; COLLISIONLESS BOW SHOCKS; UPSTREAM SOLAR-WIND;
FIELD-ALIGNED BEAM; PERPENDICULAR COLLISIONLESS; GYRATING IONS;
TERRESTRIAL FORESHOCK; ULF WAVES; MAGNETOSHEATH; MACROSTRUCTURE
AB We present the ion distribution functions in the ion foreshock upstream of the terrestrial bow shock obtained with Vlasiator, a new hybrid-Vlasov simulation geared toward large-scale simulations of the Earth's magnetosphere (http://vlasiator.fmi.fi). They are compared with the distribution functions measured by the multispacecraft Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission. The known types of ion distributions in the foreshock are well reproduced by the hybrid-Vlasov model. We show that Vlasiator reproduces the decrease of the backstreaming beam speed with increasing distance from the foreshock edge, as well as the beam speed increase and density decrease with increasing radial distance from the bow shock, which have been reported before and are visible in the THEMIS data presented here. We also discuss the process by which wave-particle interactions cause intermediate foreshock distributions to lose their gyrotropy. This paper demonstrates the strength of the hybrid-Vlasov approach which lies in producing uniformly sampled ion distribution functions with good resolution in velocity space, at every spatial grid point of the simulation and at any instant. The limitations of the hybrid-Vlasov approach are also discussed.
C1 [Kempf, Yann; von Alfthan, Sebastian; Hannuksela, Otto; Palmroth, Minna] Finnish Meteorol Inst, Earth Observat Unit, FIN-00101 Helsinki, Finland.
[Kempf, Yann; Pokhotelov, Dimitry; Hannuksela, Otto] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Pokhotelov, Dimitry] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Gutynska, Olga; Wilson, Lynn B., III; Sibeck, David G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Walsh, Brian M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Kempf, Y (reprint author), Finnish Meteorol Inst, Earth Observat Unit, FIN-00101 Helsinki, Finland.
EM yann.kempf@fmi.fi
RI Wilson III, Lynn/D-4425-2012; Pokhotelov, Dimitry/H-6969-2014;
OI Wilson III, Lynn/0000-0002-4313-1970; Pokhotelov,
Dimitry/0000-0002-3712-0597; Pfau-Kempf, Yann/0000-0001-5793-7070
FU European Research Council under the European Community's Seventh
Framework Programme (FP-7/ERC) [200141-QuESpace]; Academy of Finland;
Science and Technology Facilities Council (STFC) [ST/L000563/1]
FX Y.K. acknowledges fruitful discussions with H.E.J. Koskinen and B.
Lembege. We acknowledge that the results of this research have been
achieved using the PRACE (Partnership for Advanced Computing in Europe)
Tier-0 Research Infrastructure resource Hermit based in Germany at the
High Performance Computing Center Stuttgart (HLRS) and the PRACE Tier-1
Research Infrastructure resource Abel owned by the University of Oslo
and the Norwegian metacenter for High Performance Computing (NOTUR) and
operated by the Department for Research Computing at USIT, the
University of Oslo IT department. The Quantifying Energy circulation in
Space plasmas (QuESpace) project, in which Vlasiator was initially
developed, has received funding from the European Research Council under
the European Community's Seventh Framework Programme
(FP-7/2007-2013/ERC) agreement 200141-QuESpace. The work of Y.K., D.P.,
S.A., O.H., and M.P. has been supported by the Academy of Finland. The
work of D.P. has been supported by Science and Technology Facilities
Council (STFC) grant ST/L000563/1. Simulation figures in this paper were
made using VisIt [Childs et al., 2012]. THEMIS data are available
through http://themis.ssl.berkeley.edu. Visit http://vlasiator.fmi.fi.
NR 52
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Z9 6
U1 2
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2015
VL 120
IS 5
BP 3684
EP 3701
DI 10.1002/2014JA020519
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600030
ER
PT J
AU Taguchi, S
Tawara, A
Hairston, MR
Slavin, JA
Le, G
Matzka, J
Stolle, C
AF Taguchi, S.
Tawara, A.
Hairston, M. R.
Slavin, J. A.
Le, G.
Matzka, J.
Stolle, C.
TI Response of reverse convection to fast IMF transitions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; ALIGNED CURRENT REGIONS; NORTH-SOUTH
COMPONENT; IONOSPHERIC CONVECTION; ELECTRIC-FIELDS; SUDDEN CHANGES;
SOLAR-WIND; POLAR; CURRENTS; TIME
AB The nature of the transition that high-latitude reverse convection makes in response to fast interplanetary magnetic field (IMF) changes is investigated using observations from multiple spacecraft and a ground magnetometer array. We focused on two fast IMF-transition events on 22 April 2006. Immediately after the first event, three ST5 spacecraft identified a clear change in the distribution of the polar cap field-aligned current. Coordinate observations with the Greenland magnetometer chain showed that the near-noon Hall current distribution, which is closely related to the polar cap field-aligned current or reverse convection, was in a transition state for about 10 min. For the second event, the Greenland magnetic perturbations also showed that a transition state occurred in the near-noon sector for 10-15 min. Three DMSP spacecraft that traversed the polar cap provided evidence showing that variations of the ground magnetic perturbations were produced by the transition from clockwise plasma circulation to the anticlockwise circulation over the polar cap. A simple calculation based on the Biot-Savart law shows that the near-noon transition state is consistent with the approach of a new convection region to the near-noon sector at the speed of 0.5-1 kms(-1), which is coupled with the moving away of the old convection region at a similar speed. For the higher-latitude sunward flow region, it is found that the convection takes a transition state almost simultaneously (within 1 min) with that in the near-noon sector, i.e., quasi-instantaneous response.
C1 [Taguchi, S.] Kyoto Univ, Dept Geophys, Grad Sch Sci, Kyoto, Japan.
[Tawara, A.] Univ Electrocommun, Dept Commun Engn & Informat, Tokyo, Japan.
[Hairston, M. R.] Univ Texas Dallas, William B Hanson Ctr Space Sci, Richardson, TX 75083 USA.
[Slavin, J. A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Le, G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Matzka, J.; Stolle, C.] Tech Univ Denmark, DTU Space, DK-2800 Lyngby, Denmark.
RP Taguchi, S (reprint author), Kyoto Univ, Dept Geophys, Grad Sch Sci, Kyoto, Japan.
EM taguchi@kugi.kyoto-u.ac.jp
RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012;
OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X;
Hairston, Marc/0000-0003-4524-4837; Taguchi, Satoshi/0000-0001-7419-5531
NR 36
TC 1
Z9 1
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 MAY
PY 2015
VL 120
IS 5
BP 4020
EP 4037
DI 10.1002/2015JA021002
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM7KA
UT WOS:000357869600056
ER
PT J
AU Gruen, D
Bernstein, GM
Jarvis, M
Rowe, B
Vikram, V
Plazas, AA
Seitz, S
AF Gruen, D.
Bernstein, G. M.
Jarvis, M.
Rowe, B.
Vikram, V.
Plazas, A. A.
Seitz, S.
TI Characterization and correction of charge-induced pixel shifts in DECam
SO JOURNAL OF INSTRUMENTATION
LA English
DT Article
DE Photon detectors for UV, visible and IR photons (solid-state) (PIN
diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs etc); Image
processing
ID COUPLED-DEVICES; DARK; SEXTRACTOR; FIELD
AB Interaction of charges in CCDs with the already accumulated charge distribution causes both a flux dependence of the point-spread function (an increase of observed size with flux, also known as the brighter/fatter effect) and pixel-to-pixel correlations of the Poissonian noise in flat fields. We describe these effects in the Dark Energy Camera (DECam) with charge dependent shifts of effective pixel borders, i.e. the Antilogus et al. (2014) model, which we fit to measurements of flat-field Poissonian noise correlations. The latter fall off approximately as a power-law r(-2.5) with pixel separation r, are isotropic except for an asymmetry in the direct neighbors along rows and columns, are stable in time, and are weakly dependent on wavelength. They show variations from chip to chip at the 20% level that correlate with the silicon resistivity. The charge shifts predicted by the model cause biased shape measurements, primarily due to their effect on bright stars, at levels exceeding weak lensing science requirements. We measure the flux dependence of star images and show that the effect can be mitigated by applying the reverse charge shifts at the pixel level during image processing. Differences in stellar size, however, remain significant due to residuals at larger distance from the centroid.
C1 [Gruen, D.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany.
[Gruen, D.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bernstein, G. M.; Jarvis, M.; Vikram, V.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Rowe, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Vikram, V.] Argonne Natl Lab, Lemont, IL 60439 USA.
[Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gruen, D (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany.
EM dgruen@usm.uni-muenchen.de
OI Rowe, Barnaby/0000-0002-7042-9174
FU Deutsche Forschungsgemeinschaft (DFG) [SFB-Transregio 33]; DFG cluster
of excellence 'Origin and Structure of the Universe' [DE-SC007901]; NSF
[AST-1311924]; DOE [DE-AC02-98CH10886]; JPL; NASA by Caltech; U.S.
Department of Energy; U.S. National Science Foundation; Ministry of
Science and Education of Spain; Science and Technology Facilities
Council of the United Kingdom; Higher Education Funding Council for
England; National Center for Supercomputing Applications at the
University of Illinois at Urbana-Champaign; Kavli Institute of
Cosmological Physics at the University of Chicago; Financiadora de
Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do
Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche
Forschungsgemeinschaft; Argonne National Laboratory; University of
California at Santa Cruz; University of Cambridge; Centro de
Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid;
University of Chicago; University College London; DES-Brazil Consortium;
Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National
Accelerator Laboratory; University of Edinburgh; University of Illinois
at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC);
Institut de Fisica d'Altes Energies; Lawrence Berkeley National
Laboratory; Ludwig-Maximilians Universitat; associated Excellence
Cluster Universe; University of Michigan; National Optical Astronomy
Observatory; University of Nottingham; Ohio State University; University
of Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory, Stanford University; University of Sussex; Texas AM
University
FX This project was supported by SFB-Transregio 33 'The Dark Universe' by
the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of
excellence 'Origin and Structure of the Universe'. DG thanks Pierre
Astier, Thomas Diehl, Augustin Guyonnet, Stephen Holland, Mihael Kodric,
Ralf Kosyra, and Andy Rasmussen for helpful discussions. GMB
acknowledges support for this work from NSF grant AST-1311924 and DOE
grant DE-SC007901. AAP is supported by DOE grant DE-AC02-98CH10886 and
JPL, which is run under a contract for NASA by Caltech.; Funding for the
DES Projects has been provided by the U.S. Department of Energy, the
U.S. National Science Foundation, the Ministry of Science and Education
of Spain, the Science and Technology Facilities Council of the United
Kingdom, the Higher Education Funding Council for England, the National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign, the Kavli Institute of Cosmological Physics at the
University of Chicago, Financiadora de Estudos e Projetos, Fundacao
Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro,
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the
Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft
and the Collaborating Institutions in the Dark Energy Survey.; The
Collaborating Institutions are Argonne National Laboratory, the
University of California at Santa Cruz, the University of Cambridge,
Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat and the associated Excellence Cluster
Universe, the University of Michigan, the National Optical Astronomy
Observatory, the University of Nottingham, The Ohio State University,
the University of Pennsylvania, the University of Portsmouth, SLAC
National Accelerator Laboratory, Stanford University, the University of
Sussex, and Texas A&M University.
NR 31
TC 7
Z9 7
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-0221
J9 J INSTRUM
JI J. Instrum.
PD MAY
PY 2015
VL 10
AR C05032
DI 10.1088/1748-0221/10/05/C05032
PG 22
WC Instruments & Instrumentation
SC Instruments & Instrumentation
GA CM8ZI
UT WOS:000357993300032
ER
PT J
AU Varnai, T
Marshak, A
AF Varnai, Tamas
Marshak, Alexander
TI Effect of Cloud Fraction on Near-Cloud Aerosol Behavior in the MODIS
Atmospheric Correction Ocean Color Product
SO REMOTE SENSING
LA English
DT Article
ID CALIPSO OBSERVATIONS; PARTICLES; VICINITY; CERES; MODEL; AQUA; AIR
AB Characterizing the way satellite-based aerosol statistics change near clouds is important for better understanding both aerosol-cloud interactions and aerosol direct radiative forcing. This study focuses on the question of whether the observed near-cloud increases in aerosol optical thickness and particle size may be explained by a combination of two factors: (i) Near-cloud data coming from areas with higher cloud fractions than far-from-cloud data and (ii) Cloud fraction being correlated with aerosol optical thickness and particle size. This question is addressed through a statistical analysis of aerosol parameters included in the MODIS (MODerate resolution Imaging Spectroradiometer) ocean color product. Results from ten Septembers (2002-2011) over part of the northeast Atlantic Ocean confirm that the combination of these two factors working together explains a significant but not dominant part (in our case, 15%-30%) of mean optical thickness changes near clouds. Overall, the findings show that cloud fraction plays a large role in shaping the way aerosol statistics change with distance to clouds. This implies that both cloud fraction and distance to clouds are important to consider when aerosol-cloud interactions or aerosol direct radiative effects are examined in satellite or modeling studies.
C1 [Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Varnai, Tamas; Marshak, Alexander] NASA Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
RP Varnai, T (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM varnai@umbc.edu; alexander.marshak@nasa.gov
RI Marshak, Alexander/D-5671-2012
FU NASA Radiation Sciences Program; NASA CALIPSO project
FX We gratefully acknowledge support for this research by the NASA
Radiation Sciences Program managed by Hal Maring and by the NASA CALIPSO
project supervised by Charles Trepte as the technical officer. We also
thank Ziauddin Ahmad, Bryan Franz, Gerhard Meister, and other members of
the MODIS ocean color team, as well as Bob Charlson, Larry Di Girolamo,
Robert Levy, Alexei Lyapustin, Guoyong Wen, Rob Wood, and Weidong Yang
for insightful discussions and help. We are also grateful to the three
anonymous reviewers, who helped greatly to improve the manuscript.
NR 34
TC 3
Z9 4
U1 0
U2 3
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2015
VL 7
IS 5
BP 5283
EP 5299
DI 10.3390/rs70505283
PG 17
WC Remote Sensing
SC Remote Sensing
GA CM3PW
UT WOS:000357596200015
ER
PT J
AU Chapman, B
McDonald, K
Shimada, M
Rosenqvist, A
Schroeder, R
Hess, L
AF Chapman, Bruce
McDonald, Kyle
Shimada, Masanobu
Rosenqvist, Ake
Schroeder, Ronny
Hess, Laura
TI Mapping Regional Inundation with Spaceborne L-Band SAR
SO REMOTE SENSING
LA English
DT Article
ID SYNTHETIC-APERTURE RADAR; SOUTH FLORIDA WETLANDS; AMAZON FLOODPLAIN;
SLOPE CORRECTION; WATER STORAGE; ALOS PALSAR; VEGETATION; DYNAMICS;
IMAGES; BASIN
AB Shortly after the launch of ALOS PALSAR L-band SAR by the Japan Space Exploration Agency (JAXA), a program to develop an Earth Science Data Record (ESDR) for inundated wetlands was funded by NASA. Using established methodologies, extensive multi-temporal L-band ALOS ScanSAR data acquired bi-monthly by the PALSAR instrument onboard ALOS were used to classify the inundation state for South America for delivery as a component of this Inundated Wetlands ESDR (IW-ESDR) and in collaboration with JAXA's ALOS Kyoto and Carbon Initiative science programme. We describe these methodologies and the final classification of the inundation state, then compared this with results derived from dual-season data acquired by the JERS-1 L-band SAR mission in 1995 and 1996, as well as with estimates of surface water extent measured globally every 10 days by coarser resolution sensors. Good correspondence was found when comparing open water extent classified from multi-temporal ALOS ScanSAR data with surface water fraction identified from coarse resolution sensors, except in those regions where there may be differences in sensitivity to widespread and shallow seasonal flooding event, or in areas that could be excluded through use of a continental-scale inundatable mask. It was found that the ALOS ScanSAR classification of inundated vegetation was relatively insensitive to inundated herbaceous vegetation. Inundation dynamics were examined using the multi-temporal ALOS ScanSAR acquisitions over the Pacaya-Samiria and surrounding areas in the Peruvian Amazon.
C1 [Chapman, Bruce; McDonald, Kyle; Schroeder, Ronny] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McDonald, Kyle] CUNY City Coll, CUNY Environm Crossrd Initiat, New York, NY 10031 USA.
[McDonald, Kyle] CUNY City Coll, CREST Inst, New York, NY 10031 USA.
[Shimada, Masanobu] Japan Aerosp & Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki 3058505, Japan.
[Rosenqvist, Ake] SoloEO, Tokyo 3058505, Japan.
[Schroeder, Ronny] Univ Hohenheim, Inst Bot, D-70593 Stuttgart, Germany.
[Hess, Laura] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
RP Chapman, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bruce.d.chapman@jpl.nasa.gov; kmcdonald2@ccny.cuny.edu;
shimada.masanobu@jaxa.jp; ake.rosenqvist@soloEO.com;
ronny.schroder@gmail.com; lola@eri.ucsb.edu
FU NASA MEaSUREs program; National Aeronautics and Space Administration
FX We thank the NASA MEaSUREs program and Martha Maiden for funding this
work, the NASDA/JAXA GRFM project for the JERS-1 imagery, the Alaska
Satellite Facility ALOS Data node for ancillary ALOS data, the global
classification from ESA's GlobClover land cover classification product,
and the NASA SRTM project for its near global DEM. This research was
undertaken within the framework of the ALOS Kyoto & Carbon Initiative.
The ALOS data were provided by JAXA EORC. Resources supporting this work
were provided by the NASA High-End Computing (HEC) Program through the
NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We
also thank the editor and the reviewers for their advice and suggestions
for the improvement of this paper.; This work was partially performed at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. U.S.
Government sponsorship acknowledged.
NR 41
TC 5
Z9 5
U1 5
U2 18
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2015
VL 7
IS 5
BP 5440
EP 5470
DI 10.3390/rs70505440
PG 31
WC Remote Sensing
SC Remote Sensing
GA CM3PW
UT WOS:000357596200022
ER
PT J
AU Ibrahim, YZ
Balzter, H
Kaduk, J
Tucker, CJ
AF Ibrahim, Yahaya Z.
Balzter, Heiko
Kaduk, Joerg
Tucker, Compton J.
TI Land Degradation Assessment Using Residual Trend Analysis of GIMMS
NDVI3g, Soil Moisture and Rainfall in Sub-Saharan West Africa from 1982
to 2012
SO REMOTE SENSING
LA English
DT Article
ID DIFFERENCE VEGETATION INDEX; TIME-SERIES; SOUTH-AFRICA; EAST-AFRICA;
NOAA-AVHRR; SAHEL; DESERTIFICATION; CLIMATE; PRODUCTS; VARIABILITY
AB Areas affected by land degradation in Sub-Saharan West Africa between 1982 and 2012 are identified using time-series analysis of vegetation index data derived from satellites. The residual trend (RESTREND) of a Normalized Difference Vegetation Index (NDVI) time-series is defined as the fraction of the difference between the observed NDVI and the NDVI predicted from climate data. It has been widely used to study desertification and other forms of land degradation in drylands. The method works on the assumption that a negative trend of vegetation photosynthetic capacity is an indication of land degradation if it is independent from climate variability. In the past, many scientists depended on rainfall data as the major climatic factor controlling vegetation productivity in drylands when applying the RESTREND method. However, the water that is directly available to vegetation is stored as soil moisture, which is a function of cumulative rainfall, surface runoff, infiltration and evapotranspiration. In this study, the new NDVI third generation (NDVI3g), which was generated by the National Aeronautics and Space Administration-Goddard Space Flight Center Global Inventory Modeling and Mapping Studies (NASA-GSFC GIMMS) group, was used as a satellite-derived proxy of vegetation productivity, together with the soil moisture index product from the Climate Prediction Center (CPC) and rainfall data from the Climate Research Unit (CRU). The results show that the soil moisture/NDVI pixel-wise residual trend indicates land degraded areas more clearly than rainfall/NDVI. The spatial and temporal trends of the RESTREND in the region follow the patterns of drought episodes, reaffirming the difficulties in separating the impacts of drought and land degradation on vegetation photosynthetic capacity. Therefore, future studies of land degradation and desertification in drylands should go beyond using rainfall as a sole predictor of vegetation condition, and include soil moisture index datasets in the analysis.
C1 [Ibrahim, Yahaya Z.; Balzter, Heiko; Kaduk, Joerg] Univ Leicester, Ctr Landscape & Climate Res, Dept Geog, Leicester LE1 7RH, Leics, England.
[Tucker, Compton J.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ibrahim, YZ (reprint author), Univ Leicester, Ctr Landscape & Climate Res, Dept Geog, Leicester LE1 7RH, Leics, England.
EM yzii1@le.ac.uk; hb91@le.ac.uk; jk61@le.ac.uk; compton.j.tucker@nasa.gov
OI Kaduk, Jorg/0000-0003-4051-3081
FU Royal Society, Wolfson Research Merit Award
FX The authors are grateful and wish to acknowledge the use of the new
NDVI3g provided by Jim Tucker and Jorge E. Pinzon of NASA. Special
thanks to CRU for providing the CRU v3.21 rainfall data and NOAA-NCEP
for CPC soil moisture (v2) data. Finally to R development team for
making various library packages available which were used for the data
analyses. H. Balzter was supported by the Royal Society, Wolfson
Research Merit Award.
NR 72
TC 13
Z9 13
U1 6
U2 37
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2015
VL 7
IS 5
BP 5471
EP 5494
DI 10.3390/rs70505471
PG 24
WC Remote Sensing
SC Remote Sensing
GA CM3PW
UT WOS:000357596200023
ER
PT J
AU Fagan, ME
DeFries, RS
Sesnie, SE
Arroyo-Mora, JP
Soto, C
Singh, A
Townsend, PA
Chazdon, RL
AF Fagan, Matthew E.
DeFries, Ruth S.
Sesnie, Steven E.
Arroyo-Mora, J. Pablo
Soto, Carlomagno
Singh, Aditya
Townsend, Philip A.
Chazdon, Robin L.
TI Mapping Species Composition of Forests and Tree Plantations in
Northeastern Costa Rica with an Integration of Hyperspectral and
Multitemporal Landsat Imagery
SO REMOTE SENSING
LA English
DT Article
ID MAP ACCURACY ASSESSMENT; OIL PALM; IMAGING SPECTROSCOPY; SATELLITE
IMAGERY; RAIN-FORESTS; COVER CHANGE; TIME-SERIES; ETM PLUS; RADIOMETRIC
NORMALIZATION; DISCRIMINANT-ANALYSIS
AB An efficient means to map tree plantations is needed to detect tropical land use change and evaluate reforestation projects. To analyze recent tree plantation expansion in northeastern Costa Rica, we examined the potential of combining moderate-resolution hyperspectral imagery (2005 HyMap mosaic) with multitemporal, multispectral data (Landsat) to accurately classify (1) general forest types and (2) tree plantations by species composition. Following a linear discriminant analysis to reduce data dimensionality, we compared four Random Forest classification models: hyperspectral data (HD) alone; HD plus interannual spectral metrics; HD plus a multitemporal forest regrowth classification; and all three models combined. The fourth, combined model achieved overall accuracy of 88.5%. Adding multitemporal data significantly improved classification accuracy (p < 0.0001) of all forest types, although the effect on tree plantation accuracy was modest. The hyperspectral data alone classified six species of tree plantations with 75% to 93% producer's accuracy; adding multitemporal spectral data increased accuracy only for two species with dense canopies. Non-native tree species had higher classification accuracy overall and made up the majority of tree plantations in this landscape. Our results indicate that combining occasionally acquired hyperspectral data with widely available multitemporal satellite imagery enhances mapping and monitoring of reforestation in tropical landscapes.
C1 [Fagan, Matthew E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Sesnie, Steven E.] US Fish & Wildlife Serv, Southwest Reg Off, Albuquerque, NM 87102 USA.
[Arroyo-Mora, J. Pablo; Soto, Carlomagno] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada.
[Singh, Aditya; Townsend, Philip A.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA.
[Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.
RP Fagan, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
EM matthew.e.fagan@nasa.gov; rd2402@columbia.edu; Steven_Sesnie@fws.gov;
pablo.arroyo@mcgill.ca; carlo.soto.castro@gmail.com; singh22@wisc.edu;
ptownsend@wisc.edu; robin.chazdon@uconn.edu
RI Singh, Aditya/I-3628-2013; Townsend, Philip/B-5741-2008;
OI Singh, Aditya/0000-0001-5559-9151; Townsend, Philip/0000-0001-7003-8774;
Chazdon, Robin/0000-0002-7349-5687
FU National Aeronautics and Space Administration Earth System Science
Fellowship [NNX10AP49H]; ASPRS Ta Liang Memorial Award; Earth Institute;
Columbia Institute of Latin American Studies; NASA
FX This work was supported by National Aeronautics and Space Administration
Earth System Science Fellowship NNX10AP49H, the ASPRS Ta Liang Memorial
Award, The Earth Institute, the Columbia Institute of Latin American
Studies, and 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 authors would like to
thank Margaret Kalacska for an insightful and helpful early review of
this manuscript, and to thank Chris Small for countless hours of great
remote sensing advice in small restaurants. Field research was made
possible by logistical support provided by FUNDECOR and the staff at the
Organization for Tropical Studies La Selva Biological Station, and we
would like to thank Andres Sanchun, Jose Miranda, Marvin Paniagua, and
Mauricio Gaitan for assistance in the field. We thank CENAT and Carlos
Andres Campos for providing geospatial data on Costa Rica and would like
to express our appreciation to Bonnie Tice and Sue Pirkle. Finally, the
authors wish to thank the three anonymous reviewers for their insightful
comments, which led to marked improvements in the original manuscript.
NR 136
TC 9
Z9 9
U1 7
U2 29
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2015
VL 7
IS 5
BP 5660
EP 5696
DI 10.3390/rs70505660
PG 37
WC Remote Sensing
SC Remote Sensing
GA CM3PW
UT WOS:000357596200031
ER
PT J
AU Ting, DZY
Chang, YC
Rafol, SB
Liu, JK
Hill, CJ
Keo, SA
Mumolo, J
Gunapala, SD
Bandara, SV
AF Ting, David Z. -Y.
Chang, Yia-Chung
Rafol, Sir B.
Liu, John K.
Hill, Cory J.
Keo, Sam A.
Mumolo, Jason
Gunapala, Sarath D.
Bandara, Sumith V.
TI The sub-monolayer quantum dot infrared photodetector revisited
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Infrared detector; Quantum dot; Submonolayer
ID ISLANDS; ARRAYS; WELL
AB The sub-monolayer quantum dot infrared photodetector (SML-QDIP) was proposed as an alternative to the standard QDIP based on Stranski-Krastanow (SK) quantum dots. Theoretical modeling indicates that the normal-incidence photo-response observed in the initial SML-QDIP devices, originally attributed to 3D quantum confinement effect, is most likely the result of optical cavity scattering. Modeling results also suggest candidate SML-QDIP structures with improved intrinsic normal incidence absorption. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Ting, David Z. -Y.; Rafol, Sir B.; Liu, John K.; Hill, Cory J.; Keo, Sam A.; Mumolo, Jason; Gunapala, Sarath D.; Bandara, Sumith V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chang, Yia-Chung] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, M-S 302-307,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
NR 25
TC 0
Z9 0
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 20
EP 24
DI 10.1016/j.infrared.2014.09.028
PG 5
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000005
ER
PT J
AU Sun, J
Choi, KK
Jhabvala, MD
Jhabvala, CA
Waczynski, A
Olver, K
AF Sun, J.
Choi, K. K.
Jhabvala, M. D.
Jhabvala, C. A.
Waczynski, A.
Olver, K.
TI Advanced inductively coupled plasma etching processes for fabrication of
resonator-quantum well infrared photodetector
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Inductively coupled plasma etching; Resonator-quantum well infrared;
photodetectors focal plane array; GaAs substrate removal
ID DAMAGE; GAAS; SICL4; TIME; INP
AB Resonator-quantum well infrared photodetectors (R-QWIPs) are the next generation of QWIP detectors that use resonances to increase the quantum efficiency (QE). To achieve the expected performance, the detector geometry must be produced in precise specification. In particular, the height of the diffractive elements (DE) and the thickness of the active resonator must be uniformly and accurately realized to within 0.05 mu m accuracy and the substrates of the detectors have to be removed totally. To achieve these specifications, two optimized inductively coupled plasma (ICP) etching processes are developed. Using these etching techniques, we have fabricated a number of R-QWIP test detectors and FPAs with the required dimensions and completely removed the substrates of the test detectors and FPAs. Their QE spectra were tested to be in close agreement with the theoretical predictions. The operability and spectral non-uniformity of the FPA is about 99.57% and 3% respectively. Published by Elsevier B.V.
C1 [Sun, J.] US Army, Res Lab, Adelphi, MD 20783 USA.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sun, J (reprint author), US Army, Res Lab, Adelphi, MD 20783 USA.
NR 14
TC 3
Z9 3
U1 4
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 25
EP 29
DI 10.1016/j.infrared.2014.09.022
PG 5
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000006
ER
PT J
AU Baril, N
Bandara, S
Hoeglund, L
Henry, N
Brown, A
Billman, C
Maloney, P
Nallon, E
Tidrow, M
Pellegrino, J
AF Baril, Neil
Bandara, Sumith
Hoeglund, Linda
Henry, Nathan
Brown, Alexander
Billman, Curtis
Maloney, Patrick
Nallon, Eric
Tidrow, Meimei
Pellegrino, Joseph
TI Low operating bias InAs/GaSb strain layer superlattice LWIR detector
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Superlattice; Infrared detector; Heterojunction; Band offset; InAs/GaSb;
Barrier
AB Minimization of operating bias and generation-recombination dark current in long wavelength infrared (LWIR) strained layer superlattice (SLS) detectors, consisting of a lightly doped p-type absorber layer and a wide band gap hole barrier, are investigated with respect to the band alignment between the wide band gap barrier and absorber layers. Dark current vs. bias, photoresponse, quantum efficiency, lifetime, and modeling are used to correlate device performance with the wide gap barrier composition. Decreases in dark current density and operating bias were observed as the conduction band of the wide gap barrier was lowered with respect to the absorber layer. The device achieved 95% of its maximum quantum efficiency at 0 V bias, and 100% by 0.05 V. This study demonstrates key device design parameters responsible for optimal performance of heterojunction based SLS LWIR detectors. Published by Elsevier B.V.
C1 [Baril, Neil; Bandara, Sumith; Billman, Curtis; Maloney, Patrick; Nallon, Eric; Tidrow, Meimei; Pellegrino, Joseph] US Army RDECOM CERDEC NVESD, Ft Belvoir, VA 22060 USA.
[Hoeglund, Linda] Corbin Co, Alexandria, VA 22314 USA.
[Henry, Nathan; Brown, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Baril, N (reprint author), 10221 Burbeck Rd, Ft Belvoir, VA 22060 USA.
EM info@nvl.army.mil
NR 8
TC 2
Z9 2
U1 5
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 58
EP 61
DI 10.1016/j.infrared.2014.10.013
PG 4
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000013
ER
PT J
AU Hoglund, L
Ting, DZ
Soibel, A
Fisher, A
Khoshakhlagh, A
Hill, CJ
Baker, L
Keo, S
Mumolo, J
Gunapala, SD
AF Hoeglund, L.
Ting, D. Z.
Soibel, A.
Fisher, A.
Khoshakhlagh, A.
Hill, C. J.
Baker, L.
Keo, S.
Mumolo, J.
Gunapala, S. D.
TI Influence of carrier concentration on the minority carrier lifetime in
mid-wavelength infrared InAs/InAsSb superlattices
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Infrared; Superlattice; InAs/InAsSb; Minority carrier lifetime;
Capacitance-voltage
ID DETECTORS
AB The influence of carrier concentration on the minority carrier lifetime was studied in mid-wavelength infrared InAs/InAsSb superlattices. A significant correlation between the carrier concentration and the minority carrier lifetime was observed, with lifetime decreasing from 3.6 mu s to 1 mu s when increasing the carrier concentration from 2 x 10(15) cm(-3) to 4.4 x 10(15) cm(-3). From temperature dependence studies of the minority carrier lifetime, radiative recombination has been identified as the main recombination mechanism in these superlattices. The radiative recombination rate increases with carrier concentration which is consistent with our observations. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Hoeglund, L.; Ting, D. Z.; Soibel, A.; Fisher, A.; Khoshakhlagh, A.; Hill, C. J.; Baker, L.; Keo, S.; Mumolo, J.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA.
RP Hoglund, L (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 12
TC 3
Z9 3
U1 2
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 62
EP 65
DI 10.1016/j.infrared.2014.10.011
PG 4
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000014
ER
PT J
AU Gunapala, SD
Rafol, SB
Ting, DZ
Soibel, A
Hoglund, L
Hill, CJ
Khoshakhlagh, A
Liu, JK
Mumolo, JM
Keo, SA
AF Gunapala, S. D.
Rafol, S. B.
Ting, D. Z.
Soibel, A.
Hoeglund, L.
Hill, C. J.
Khoshakhlagh, A.
Liu, J. K.
Mumolo, J. M.
Keo, S. A.
TI 1/f Noise QWIPs and nBn detectors
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Infrared detector; QWIP; nBn; Focal plane array; 1/f Noise
ID WELL INFRARED PHOTODETECTORS
AB The low-frequency noise is a ubiquitous phenomenon and the spectral power density of this fluctuation process is inversely proportional to the frequency of the signal. We have measured the 1/f noise of a 640 x 512 pixel quantum well infrared photodetector (QWIP) focal plane array (FPA) with 6.2 mu m peak wavelength. Our experimental observations show that this QWIP FPA's 1/f noise corner frequency is about 0.1 mHz. With this kind of low frequency stability, QWIPs could unveil a new class of infrared applications that have never been imagined before. Furthermore, we present the results from a similar 1/f noise measurement of bulk InAsSb absorber (lattice matched to GaSb substrate) nBn detector array with 4.0 mu m cutoff wavelength. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Gunapala, S. D.; Rafol, S. B.; Ting, D. Z.; Soibel, A.; Hoeglund, L.; Hill, C. J.; Khoshakhlagh, A.; Liu, J. K.; Mumolo, J. M.; Keo, S. A.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA.
RP Gunapala, SD (reprint author), Jet Prop Lab, M-S 302-306,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sarath.d.Gunapala@jpl.nasa.gov
NR 20
TC 0
Z9 0
U1 3
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 115
EP 120
DI 10.1016/j.infrared.2014.09.031
PG 6
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000025
ER
PT J
AU Soibel, A
Hill, CJ
Keo, SA
Hoglund, L
Rosenberg, R
Kowalczyk, R
Khoshakhlagh, A
Fisher, A
Ting, DZY
Gunapala, SD
AF Soibel, Alexander
Hill, Cory J.
Keo, Sam A.
Hoglund, Linda
Rosenberg, Robert
Kowalczyk, Robert
Khoshakhlagh, Arezou
Fisher, Anita
Ting, David Z. -Y.
Gunapala, Sarath D.
TI Room temperature performance of mid-wavelength infrared InAsSb nBn
detectors
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Quantum Structure Infrared Photodetectors
(QSIP)
CY JUN 29-JUL 03, 2014
CL Santa Fe, NM
SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off
DE Infrared detectors; Semiconductor detectors; BIRD detectors; Sb-based
detectors
ID PHOTODETECTORS; DESIGN
AB In this work we investigate the high temperature performance of mid-wavelength infrared InAsSb-AlAsSb nBn detectors with cut-off wavelengths near 4.5 mu m. The quantum efficiency of these devices is 35% without antireflection coatings and does not change with temperature in the 77-325 K temperature range, indicating potential for room temperature operation. The device dark current stays diffusion limited in the 150-325 K temperature range and becomes dominated by generation-recombination processes at lower temperatures. Detector detectivities of D*(lambda) = 1 x 10(9) (cm Hz(0.5)/W) at T= 300 K and D*(lambda)= 5 x 10(9) (cm Hz(0.5)/W) at T= 250 K, which is easily achievable with a one stage TE cooler. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Soibel, Alexander; Hill, Cory J.; Keo, Sam A.; Hoglund, Linda; Rosenberg, Robert; Kowalczyk, Robert; Khoshakhlagh, Arezou; Fisher, Anita; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA.
RP Soibel, A (reprint author), JPL, 4800 Oak Grove Dr,M-S 302-205, Pasadena, CA 91109 USA.
NR 16
TC 1
Z9 1
U1 5
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
EI 1879-0275
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAY
PY 2015
VL 70
BP 121
EP 124
DI 10.1016/j.infrared.2014.09.030
PG 4
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA CL8OM
UT WOS:000357234000026
ER
PT J
AU De Groeve, T
Thielen-del Pozo, J
Brakenridge, R
Adler, R
Alfieri, L
Kull, D
Lindsay, F
Imperiali, O
Pappenberger, F
Rudari, R
Salamon, P
Villars, N
Wyjad, K
AF De Groeve, T.
Thielen-del Pozo, J.
Brakenridge, R.
Adler, R.
Alfieri, L.
Kull, D.
Lindsay, F.
Imperiali, O.
Pappenberger, F.
Rudari, R.
Salamon, P.
Villars, N.
Wyjad, K.
TI JOINING FORCES IN A GLOBAL FLOOD PARTNERSHIP
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [De Groeve, T.; Thielen-del Pozo, J.; Alfieri, L.; Salamon, P.] Commiss European Communities, JRC, I-21027 Ispra, VA, Italy.
[Brakenridge, R.] Dartmouth Flood Observ, Boulder, CO USA.
[Adler, R.] Univ Maryland, College Pk, MD 20742 USA.
[Alfieri, L.; Pappenberger, F.] European Ctr Medium Range Weather Forecasts, Forecast Dept, Reading RG2 9AX, Berks, England.
[Kull, D.] World Bank Grp, Global Facil Disaster Reduct & Recovery, Geneva, Switzerland.
[Lindsay, F.] NASA, Washington, DC 20546 USA.
[Imperiali, O.] Commiss European Communities, European Community Humanitarian Off, B-1049 Brussels, Belgium.
[Pappenberger, F.] Hohai Univ, Coll Hydrol & Water Resources, Nanjing, Jiangsu, Peoples R China.
[Pappenberger, F.] Univ Bristol, Dept Geog, Bristol BS8 1TH, Avon, England.
[Rudari, R.] CIMA Res Fdn, Savona, Italy.
[Villars, N.] Deltares, Delft, Netherlands.
[Wyjad, K.] United Nations World Food Programme, Rome, Italy.
RP Thielen-del Pozo, J (reprint author), Commiss European Communities, JRC, Via E Fermi 2479,TP122, I-21027 Ispra, VA, Italy.
RI Pappenberger, Florian/A-2839-2009;
OI Pappenberger, Florian/0000-0003-1766-2898; Alfieri,
Lorenzo/0000-0002-3616-386X
NR 3
TC 4
Z9 4
U1 3
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 MAY
PY 2015
VL 96
IS 5
BP ES97
EP ES100
DI 10.1175/BAMS-D-14-00147.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CL3SL
UT WOS:000356870800001
ER
PT J
AU Flexas, MM
Schodlok, MP
Padman, L
Menemenlis, D
Orsi, AH
AF Flexas, M. M.
Schodlok, M. P.
Padman, L.
Menemenlis, D.
Orsi, A. H.
TI Role of tides on the formation of the Antarctic Slope Front at the
Weddell-Scotia Confluence
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article; Proceedings Paper
CT Open Science Symposium on Western Pacific Ocean Circulation and Climate
CY OCT 15-17, 2012
CL Qingdao, PEOPLES R CHINA
SP NW Pacific Ocean Circulat & Climate Expt
DE Antarctic Slope Front; Antarctic Slope Current; tides; Scotia sea;
numerical model; SASSI
ID SEA CONTINENTAL-SLOPE; BOTTOM WATER PRODUCTION; ROSS SEA; OVERTURNING
CIRCULATION; SOUTHERN-OCEAN; YERMAK PLATEAU; DIURNAL TIDES; SHELF BREAK;
DEEP-OCEAN; MODEL
AB The structure of the Antarctic Slope Front (ASF) and the associated Antarctic Slope Current (ASC) on the Scotia Sea side of the Weddell-Scotia Confluence (WSC) is described using data from a hydrographic survey and three 1 year long moorings across the continental slope. The ASC in this region flows westward along isobaths with an annual mean speed of approximate to 0.2 m s(-1), with time variability dominated by the K-1 and O-1 tidal diurnal constituents, a narrowband oscillation with approximate to 2-week period attributable to the spring/neap tidal cycle, and seasonal variability. Realistic and idealized high-resolution numerical simulations are used to determine the contribution of tides to the structure of the ASF and the speed of the ASC. Two simulations forced by realistic atmospheric forcing and boundary conditions integrated with and without tidal forcing show that tidal forcing is essential to reproduce the measured ASF/ASC cross-slope structure, the time variability at our moorings, and the reduced stratification within the WSC. Two idealized simulations run with tide-only forcing, one with a homogeneous ocean and the other with initial vertical stratification that is laterally homogeneous, show that tides can generate the ASC and ASF through volume flux convergence along the slope initiated by effects including the Lagrangian component of tidal rectification and mixing at the seabed and in the stratified ocean interior. Climate models that exclude the effects of tides will not correctly represent the ASF and ASC or their influence on the injection of intermediate and dense waters from the WSC to the deep ocean.
C1 [Flexas, M. M.; Schodlok, M. P.; Menemenlis, D.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91125 USA.
[Flexas, M. M.] UIB CSIC, IMEDEA, Palma De Mallorca, Spain.
[Schodlok, M. P.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Padman, L.] Earth & Space Res, Corvallis, OR USA.
[Orsi, A. H.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA.
RP Flexas, MM (reprint author), CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91125 USA.
EM msbert@jpl.nasa.gov
FU Spanish Research and Innovation (I+D+i) National Plan [CGL2007-28783-E/
ANT, CTM2008-04623-E/ANT, CTM2009-08287-E/ANT, CTM2011-14056-E];
National Science Foundation [ANT-0818061, ANT-0830398, OCE-0961405];
National Aeronautics and Space Administration [NNX08AN67G]; National
Aeronautics and Space Administration (ECCO2 project); NASA Postdoctoral
Program; NASA
FX We thank everyone who made the oceanographic cruises successful,
especially the scientists, technicians, officers, and crew onboard the
RV Hesperides and RV Puerto Deseado. We are grateful for the assistance
of John Walpert, Agusti Julia, Joan Puigdefabregas, and Jordi Cateura
with the mooring design, construction, and deployment. Hong Zhang kindly
provided the ECCO2 adjoint boundary conditions, and Xiaochun (Adam) Wang
helped implementing the tidal forcing. Conversations with Gary Egbert,
Eberhard Fahrbach, Andrew Thompson, and Victor Zlotnicki improved this
work. This research was supported by the Spanish Research and Innovation
(I+D+i) National Plan (CGL2007-28783-E/ ANT, CTM2008-04623-E/ANT,
CTM2009-08287-E/ANT, and CTM2011-14056-E), the National Science
Foundation (ANT-0818061, ANT-0830398, and OCE-0961405), the National
Aeronautics and Space Administration (NNX08AN67G and ECCO2 project), and
the NASA Postdoctoral Program administered by Oak Ridge Associated
Universities. Data and products are available through the Spanish Polar
Database website (http://hielo.igme.es/index.php/en/), NSF website
(http://www.nsf.gov/), and ECCO2 website (http://ecco2.jpl.nasa.gov/).
This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. This is
ESR contribution number 155. This work is dedicated to Agusti Julia
(1940-2009) and Eberhard Fahrbach (1948-2013). We are grateful to
Matthew Mazloff and one anonymous reviewer whose many perceptive
comments greatly improved this manuscript.
NR 72
TC 3
Z9 3
U1 0
U2 7
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 MAY
PY 2015
VL 120
IS 5
BP 3658
EP 3680
DI 10.1002/2014JC010372
PG 23
WC Oceanography
SC Oceanography
GA CL0JI
UT WOS:000356628100027
ER
PT J
AU Seo, KW
Wilson, CR
Scambos, T
Kim, BM
Waliser, DE
Tian, B
Kim, BH
Eom, J
AF Seo, Ki-Weon
Wilson, Clark R.
Scambos, Ted
Kim, Baek-Min
Waliser, Duane E.
Tian, Baijun
Kim, Byeong-Hoon
Eom, Jooyoung
TI Surface mass balance contributions to acceleration of Antarctic ice mass
loss during 2003-2013
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
DE ice mass balance; Antarctica; GRACE
ID SEA-LEVEL RISE; WEST ANTARCTICA; GRACE DATA; SNOW ACCUMULATION; SHEET;
GREENLAND; GLACIER; VARIABILITY; INCREASE; RADAR
AB Recent observations from satellite gravimetry (the Gravity Recovery and Climate Experiment (GRACE) mission) suggest an acceleration of ice mass loss from the Antarctic Ice Sheet (AIS). The contribution of surface mass balance changes (due to variable precipitation) is compared with GRACE-derived mass loss acceleration by assessing the estimated contribution of snow mass from meteorological reanalysis data. We find that over much of the continent, the acceleration can be explained by precipitation anomalies. However, on the Antarctic Peninsula and other parts of West Antarctica, mass changes are not explained by precipitation and are likely associated with ice discharge rate increases. The total apparent GRACE acceleration over all of the AIS between 2003 and 2013 is -13.67.2Gt/yr(2). Of this total, we find that the surface mass balance component is -8.22.0Gt/yr(2). However, the GRACE estimate appears to contain errors arising from the atmospheric pressure fields used to remove air mass effects. The estimated acceleration error from this effect is about 9.85.8Gt/yr(2). Correcting for this yields an ice discharge acceleration of -15.16.5Gt/yr(2).
C1 [Seo, Ki-Weon; Kim, Byeong-Hoon; Eom, Jooyoung] Seoul Natl Univ, Dept Earth Educ, Seoul, South Korea.
[Wilson, Clark R.] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA.
[Wilson, Clark R.] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA.
[Scambos, Ted] Univ Colorado, Nat Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Kim, Baek-Min] Korea Polar Res Inst, Div Polar Earth Syst Sci, Inchon, South Korea.
[Waliser, Duane E.; Tian, Baijun] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Seo, KW (reprint author), Seoul Natl Univ, Dept Earth Educ, Seoul, South Korea.
EM seokiweon@snu.ac.kr
RI Tian, Baijun/A-1141-2007
OI Tian, Baijun/0000-0001-9369-2373
FU National Research Foundation [NRF-2013R1A1A2008368]; Korea Polar
Research Institute [PM14020]; NASA
FX This work was supported by National Research Foundation grant
NRF-2013R1A1A2008368 and Korea Polar Research Institute research grant
PM14020. D.W. and B.T.'s contributions were carried out on behalf of the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. GRACE, ERA Interim, MERRA, and NCEP/DOE data are
available from GRACE Tellus site (http://grace.jpl.nasa.gov), ECMWF data
server (http://data-portal.ecmwf.int), Goddard Earth Sciences Data and
Information Services Center (http://disc.sci.gsfc.nasa.gov), and Earth
System Research Laboratory (http://www.esrl.noaa.gov), respectively.
RACMO2.3 data are available upon request in Institute for Marine and
Atmospheric Research Utrecht
(http://www.projects.science.uu.nl/ice-climate/models/antarctica.php).
NR 36
TC 4
Z9 4
U1 2
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAY
PY 2015
VL 120
IS 5
BP 3617
EP 3627
DI 10.1002/2014JB011755
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CK7YV
UT WOS:000356454500041
PM 27708992
ER
PT J
AU Xue, L
Schwartz, S
Liu, Z
Feng, LJ
AF Xue, Lian
Schwartz, Susan
Liu, Zhen
Feng, Lujia
TI Interseismic megathrust coupling beneath the Nicoya Peninsula, Costa
Rica, from the joint inversion of InSAR and GPS data
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
DE interseismic deformaion; subduction zone; InSAR and GPS
ID SAN-ANDREAS FAULT; SUBDUCTION ZONE; STRAIN ACCUMULATION; SLOW-SLIP;
RADAR INTERFEROMETRY; SURFACE DEFORMATION; EARTHQUAKE RUPTURE;
SEISMOGENIC ZONE; SATELLITE RADAR; P-WAVE
AB The Nicoya Peninsula, Costa Rica, was struck by a long-anticipated and gap-filling M-w 7.6 earthquake in 2012. To study interseismic strain accumulation on the megathrust beneath the Nicoya Peninsula, we present an improved interseismic coupling model by integrating interferometric synthetic aperture radar (InSAR) and GPS data. Our model reveals three strongly coupled patches. The first strongly coupled patch locates beneath the Nicoya Peninsula and ruptured during the 2012 earthquake. The second strongly coupled patch locates offshore the central Nicoya Peninsula and remained largely unbroken. However, this region is close to and possibly intermingled with shallow slow slip and tremor, suggesting that accumulated strain in this region may be released both seismically and aseismically. The third strongly coupled patch offshore of the southeastern end of Nicoya overlaps part of the coseismic rupture of the 1990 M-w 7.0 Nicoya Gulf earthquake, indicating that significant strain has re-accumulated since this event. Incorporating InSAR data provides a more refined interseismic coupling model than using GPS alone and allows for a more reliable comparison with local seismic and aseismic activities. This comparison indicates that strongly locked regions during the interseismic stage are the loci of coseismic slip, and deep slow slip and low-frequency earthquakes occur in regions of low coupling or transition zones from low to high coupling, while shallow slow slip and tremor commingle with strongly coupled regions. Our study demonstrates that InSAR data can be used to recover small long-wavelength deformation signals with refined resolution in challenging subduction zone environments when integrated with GPS observations.
C1 [Xue, Lian; Schwartz, Susan] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Liu, Zhen] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Feng, Lujia] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore.
RP Xue, L (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
EM lxue3@ucsc.edu
RI Feng, Lujia/F-2523-2012; Liu, Zhen/D-8334-2017
OI Feng, Lujia/0000-0002-3736-5025;
FU National Aeronautics and Space Administration; [OCE-0841061];
[EAR-1321550]
FX This study was supported by OCE-0841061 and EAR-1321550. ALOS PALSAR
data are copyright JAXA/METI and were provided by the GEO Supersites and
the U.S. Government Research Consortium Data pool at the Alaska
Satellite Facility (https://www.asf.alaska.edu/). The research described
in this paper was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. We greatly appreciate the support
of Emily Brodsky, and thank all the people who provided advice on this
project. Figures were created using Generic Mapping Tools [Wessel and
Smith, 1991]. We thank M.E. Prichard and an anonymous reviewer for their
very helpful comments that greatly improved this paper as well Scott
Baker, Tim Dixon, Rowena Lohman and Isabelle Ryder for their early
guidance on this project.
NR 69
TC 1
Z9 1
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAY
PY 2015
VL 120
IS 5
BP 3707
EP 3722
DI 10.1002/2014JB011844
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CK7YV
UT WOS:000356454500046
ER
PT J
AU Wu, X
Abbondanza, C
Altamimi, Z
Chin, TM
Collilieux, X
Gross, RS
Heflin, MB
Jiang, Y
Parker, JW
AF Wu, Xiaoping
Abbondanza, Claudio
Altamimi, Zuheir
Chin, T. Mike
Collilieux, Xavier
Gross, Richard S.
Heflin, Michael B.
Jiang, Yan
Parker, Jay W.
TI KALREFA Kalman filter and time series approach to the International
Terrestrial Reference Frame realization
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
DE terrestrial reference frame; Kalman filter; geodetic techniques; time
series; data combination; geocenter motion
ID MASS REDISTRIBUTION; GEODETIC DATA; SEA-LEVEL; MOTION; SYSTEM; GPS;
ITRF2008; SPACE; NOISE
AB The current International Terrestrial Reference Frame is based on a piecewise linear site motion model and realized by reference epoch coordinates and velocities for a global set of stations. Although linear motions due to tectonic plates and glacial isostatic adjustment dominate geodetic signals, at today's millimeter precisions, nonlinear motions due to earthquakes, volcanic activities, ice mass losses, sea level rise, hydrological changes, and other processes become significant. Monitoring these (sometimes rapid) changes desires consistent and precise realization of the terrestrial reference frame (TRF) quasi-instantaneously. Here, we use a Kalman filter and smoother approach to combine time series from four space geodetic techniques to realize an experimental TRF through weekly time series of geocentric coordinates. In addition to secular, periodic, and stochastic components for station coordinates, the Kalman filter state variables also include daily Earth orientation parameters and transformation parameters from input data frames to the combined TRF. Local tie measurements among colocated stations are used at their known or nominal epochs of observation, with comotion constraints applied to almost all colocated stations. The filter/smoother approach unifies different geodetic time series in a single geocentric frame. Fragmented and multitechnique tracking records at colocation sites are bridged together to form longer and coherent motion time series. While the time series approach to TRF reflects the reality of a changing Earth more closely than the linear approximation model, the filter/smoother is computationally powerful and flexible to facilitate incorporation of other data types and more advanced characterization of stochastic behavior of geodetic time series.
C1 [Wu, Xiaoping; Abbondanza, Claudio; Chin, T. Mike; Gross, Richard S.; Heflin, Michael B.; Jiang, Yan; Parker, Jay W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Abbondanza, Claudio] Univ Calif Los Angeles, Reg Earth Syst Sci & Engn, Joint Inst, Los Angeles, CA USA.
[Altamimi, Zuheir; Collilieux, Xavier] Inst Natl Informat Geog & Forestiere, Paris, France.
[Jiang, Yan] Geol Survey Canada, Sidney, BC, Canada.
RP Wu, X (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Xiaoping.Wu@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration (NASA). All data used in this study
are freely available from the ITRF Web site http://itrf.ensg.fr and
NASA's Archive of Space Geodesy Data site http://cddis.nasa.gov. The
Generic MappingTools areusedto create Figures 4 and 5. We thank two
anonymous reviewers for their constructive comments and suggestions.
NR 53
TC 5
Z9 5
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAY
PY 2015
VL 120
IS 5
BP 3775
EP 3802
DI 10.1002/2014JB011622
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CK7YV
UT WOS:000356454500049
ER
PT J
AU Fukumori, I
Wang, O
Llovel, W
Fenty, I
Forget, G
AF Fukumori, Ichiro
Wang, Ou
Llovel, William
Fenty, Ian
Forget, Gael
TI A near-uniform fluctuation of ocean bottom pressure and sea level across
the deep ocean basins of the Arctic Ocean and the Nordic Seas
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID GENERAL-CIRCULATION; DATA ASSIMILATION; ALTIMETER DATA; WIND; ATLANTIC;
MODEL; VARIABILITY; SENSITIVITY; PERFORMANCE; TRANSPORT
AB Across the Arctic Ocean and the Nordic Seas, a basin-wide mode of ocean bottom pressure and sea level fluctuation is identified using satellite and in situ observations in conjunction with a global ocean circulation model and its adjoint. The variation extends across the interconnected deep ocean basins of these semi-enclosed Arctic seas, collectively called the Arctic Mediterranean, with spatially near-uniform amplitude and phase. The basin-wide fluctuation is barotropic and dominates the region's large-scale variability from sub-monthly to interannual timescales. The fluctuation results from bifurcating coastally trapped waves generated by winds along the continental slopes of the Arctic Mediterranean and its neighboring seas, including the North Atlantic Ocean. The winds drive Ekman transport across the large bathymetric gradients, forcing mass divergence between the shallow coastal area and the deep ocean basins and creating ocean bottom pressure anomalies of opposite signs in the two regions. The anomalies rapidly propagate away as barotropic coastally trapped waves with the coast and continental slope as respective boundaries. The waves subsequently bifurcate at the shallow straits connecting the Arctic Mediterranean with the rest of the globe. The straits transmit the shallow anomalies but not the deep variations, thereby inhibiting the anomalies' mutual cancelation by geographically separating the two. Anomalies that enter the deep Arctic basins equilibrate uniformly across the domain characterized by a homogeneous depth-integrated planetary potential vorticity distribution. The potential vorticity's steep gradient that borders the basins shields the region from neighboring shallow variations, giving rise to the observed spatially confined fluctuation. Compensating anomalies outside the Arctic adjust similarly across the rest of the globe but are comparatively negligible in amplitude because of the global ocean's larger area relative to that of the deep Arctic Mediterranean. The study, from a technical perspective, illustrates the utility of a model's adjoint in identifying causal mechanisms underlying a complex system. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Fukumori, Ichiro; Wang, Ou; Llovel, William; Fenty, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Llovel, William] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Forget, Gael] MIT, Cambridge, MA 02139 USA.
RP Fukumori, I (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM fukumori@jpl.nasa.gov
RI LLOVEL, William/G-6930-2016
FU National Aeronautics and Space Administration (NASA); National Science
Foundation
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration (NASA). GRACE mascons solutions were kindly
made available by M. Watkins, D. Wiese, C. Boening, and V. Zlotnicki.
Ocean bottom pressure data in the Beaufort Sea were collected and made
available by the Beaufort Gyre Exploration Program based at the Woods
Hole Oceanographic Institution (http://www.whoi.edu/beaufortgyre) in
collaboration with researchers from Fisheries and Oceans Canada at the
Institute of Ocean Sciences. The North Pole Bottom Pressure Records were
provided by NCAR/EOL under sponsorship of the National Science
Foundation, http://data.eol.ucar.edu/. The authors thank Don Chambers
and other anonymous reviewers for providing valuable comments on this
manuscript.
NR 49
TC 8
Z9 8
U1 1
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD MAY
PY 2015
VL 134
BP 152
EP 172
DI 10.1016/j.pocean.2015.01.013
PG 21
WC Oceanography
SC Oceanography
GA CK9IN
UT WOS:000356553900008
ER
PT J
AU Williams, KE
McKay, CP
AF Williams, Kaj E.
McKay, Christopher P.
TI Comparing flow-through and static ice cave models for Shoshone Ice Cave
SO INTERNATIONAL JOURNAL OF SPELEOLOGY
LA English
DT Article
DE ice cave; latent heat; airflow; Shoshone Ice Cave; USA
ID AUSTRIA; BALANCE; MASS
AB In this paper we suggest a new ice cave type: the "flow-through" ice cave. In a flow-through ice cave external winds blow into the cave and wet cave walls chill the incoming air to the wet-bulb temperature, thereby achieving extra cooling of the cave air. We have investigated an ice cave in Idaho, located in a lava tube that is reported to have airflow through porous wet end-walls and could therefore be a flow-through cave. We have instrumented the site and collected data for one year. In order to determine the actual ice cave type present at Shoshone, we have constructed numerical models for static and flow-through caves (dynamic is not relevant here). The models are driven with exterior measurements of air temperature, relative humidity and wind speed. The model output is interior air temperature and relative humidity. We then compare the output of both models to the measured interior air temperatures and relative humidity. While both the flow-through and static cave models are capable of preserving ice year-round (a net zero or positive ice mass balance), both models show very different cave air temperature and relative humidity output. We find the empirical data support a hybrid model of the static and flow-through models: permitting a static ice cave to have incoming air chilled to the wet-bulb temperature fits the data best for the Shoshone ice cave.
C1 [Williams, Kaj E.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
[Williams, Kaj E.] Montana State Univ, Dept Earth Sci, Bozeman, MT 59717 USA.
RP Williams, KE (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Mail Stop 245-3, Moffett Field, CA 94035 USA.
EM kaj.williams@montana.edu
FU NASA; Idaho Space Grant Consortium
FX The authors would like to thank Fred Cheslik and the Shoshone Indian Ice
Caves for permitting us to instrument the cave, and for their
hospitality. We thank three anonymous reviewers who provided useful
comments and improvements to the manuscript. We also thank NASA and the
Idaho Space Grant Consortium for partial support.
NR 23
TC 0
Z9 0
U1 3
U2 3
PU SOCIETA SPELEOLOGICA ITALIANA
PI BOLOGNA
PA VIA ZAMBONI 67, BOLOGNA, 40126, ITALY
SN 0392-6672
EI 1827-806X
J9 INT J SPELEOL
JI Int. J. Speleol.
PD MAY
PY 2015
VL 44
IS 2
BP 115
EP 123
DI 10.5038/1827-806X.44.2.2
PG 9
WC Geology; Geosciences, Multidisciplinary
SC Geology
GA CK4CP
UT WOS:000356167600002
ER
PT J
AU Genova, A
Goossens, S
Lemoine, FG
Mazarico, E
Fricke, SK
Smith, DE
Zuber, MT
AF Genova, Antonio
Goossens, Sander
Lemoine, Frank G.
Mazarico, Erwan
Fricke, Susan K.
Smith, David E.
Zuber, Maria T.
TI Long-term variability of CO2 and O in the Mars upper atmosphere from MRO
radio science data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE MRO; Mars Upper Atmosphere; Radio Science
ID GLOBAL SURVEYOR; SPACECRAFT; THERMOSPHERE; ORIENTATION; AEROBRAKING;
EPHEMERIS; TRACKING; GRAVITY; ORBITS; PHOBOS
AB We estimate the annual variability of CO2 and O partial density using approximately 6years of Mars Reconnaissance Orbiter (MRO) radio science data from August 2006 to January 2012, which cover three full Martian years (from the northern hemisphere summer of 28 to the northern hemisphere summer of 31). These two elements are the dominant species at the MRO periapsis altitude, constituting about 70-80% of the total density. We report the recovered annual cycle of CO2 and the annual and seasonal cycle of O in the upper atmosphere. Although no other observations are available at those altitudes, our results are in good agreement with the density measurements of the Mars Express Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars, which uses stellar occultations between 60 and 130km to determine the CO2 variability, and with the Mars Global Reference Atmospheric Model 2010 for the O annual and seasonal variabilities. Furthermore, the updated model provides more reasonable MRO drag coefficients (C-D), which are estimated to absorb mismodeling in the atmospheric density prediction. The higher content of dust in the atmosphere due to dust storms increases the density, so the C(D)s should compensate for this effect. The correlation between the drag coefficient and the dust optical depth, measured by the Mars Odyssey Thermal Emission Imaging System (THEMIS) instrument, increases from 0.4 to 0.8 with the a priori and adjusted models, respectively. The trend of C(D)s not only confirms a substantial improvement in the prediction of the atmospheric density with the updated model but also provides useful information for local dust storms, near MRO periapsis, that cannot be measured by the opacity level since THEMIS does not always sample the southern hemisphere evenly.
C1 [Genova, Antonio; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goossens, Sander] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA.
[Fricke, Susan K.] SGT Inc, Greenbelt, MD USA.
RP Genova, A (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM antonio.genova@nasa.gov
RI Lemoine, Frank/D-1215-2013; Goossens, Sander/K-2526-2015; Mazarico,
Erwan/N-6034-2014; Genova, Antonio/M-1400-2016
OI Goossens, Sander/0000-0002-7707-1128; Mazarico,
Erwan/0000-0003-3456-427X; Genova, Antonio/0000-0001-5584-492X
NR 51
TC 1
Z9 1
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY
PY 2015
VL 120
IS 5
BP 849
EP 868
DI 10.1002/2014JE004770
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CK7TB
UT WOS:000356434600002
ER
PT J
AU Crow-Willard, EN
Pappalardo, RT
AF Crow-Willard, Emma N.
Pappalardo, Robert T.
TI Structural mapping of Enceladus and implications for formation of
tectonized regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Enceladus; tectonics; mapping
ID SOUTH-POLAR FRACTURES; UNSTABLE EXTENSION; TIGER STRIPES; ICE SHELL;
HEAT-FLUX; ORIGIN; CONVECTION; MIRANDA; GEOLOGY; SURFACE
AB Global structural mapping of high-resolution Cassini images of Enceladus reveals a richly varied surface. Most notable are three main regions of deformation each containing multiple structural units. In addition to the well known South Polar Terrain (SPT), there are two other large regions of deformation that we term Leading Hemisphere Terrain (LHT) and Trailing Hemisphere Terrain (THT). Each of these three terrains includes a circumferential belt that encloses one or more other structurally deformed units. Areal extents range from about 80,000km(2) (SPT) to 195,000km(2) (LHT) or 160 to 250km equivalent circular radius. Based on relative crater densities, the THT is inferred to be older than the LHT; the geologically active SPT is the youngest. The overall similarities in shape and dimension of the three tectonized terrains suggest similar formational processes, plausibly related to broad loading of a thin elastic shell. A viable scenario is that each tectonized terrain formed above a large-scale region of warm upwelling ice, with subsequent downwarping triggered by cooling and/or subsurface melting. However, differences in morphological detail suggest that the specific evolution of each tectonized terrain has been different.
C1 [Crow-Willard, Emma N.] Occidental Coll, Dept Geol, Los Angeles, CA 90041 USA.
[Crow-Willard, Emma N.; Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Pappalardo, RT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM robert.pappalardo@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA [NNG06GF44G];
Jupiter Europa Orbiter Pre-Project
FX 5The Cassini ISS team's global image mosaic of Enceladus is available
from the Planetary Data System or from
the ISS team website
. Our
ArcGIS map is available by email request from the corresponding author
. This work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Funding
was provided by the NASA Outer Planets Research Program (NNG06GF44G) and
the (former) Jupiter Europa Orbiter Pre-Project. We are grateful to
Geoff Collins for useful discussion and assistance, to Simon Kattenhorn
and Wes Patterson for reviews that greatly improved this manuscript, and
to D. Alex Patthoff for invaluable assistance in revision of the
manuscript.
NR 53
TC 8
Z9 8
U1 4
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY
PY 2015
VL 120
IS 5
BP 928
EP 950
DI 10.1002/2015JE004818
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CK7TB
UT WOS:000356434600006
ER
PT J
AU Jian, LK
MacNeice, PJ
Taktakishvili, A
Odstrcil, D
Jackson, B
Yu, HS
Riley, P
Sokolov, IV
Evans, RM
AF Jian, L. K.
MacNeice, P. J.
Taktakishvili, A.
Odstrcil, D.
Jackson, B.
Yu, H. -S.
Riley, P.
Sokolov, I. V.
Evans, R. M.
TI Validation for solar wind prediction at Earth: Comparison of coronal and
heliospheric models installed at the CCMC
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE models; solar wind; space weather forecasting
ID COROTATING INTERACTION REGIONS; MAGNETIC-FIELD DIRECTION; EJECTION
IMAGER SMEI; MASS EJECTIONS; INTERPLANETARY SCINTILLATION; SPACE
WEATHER; 3-DIMENSIONAL PROPAGATION; INNER HELIOSPHERE; FLUX TRANSPORT;
ALFVEN WAVES
AB Multiple coronal and heliospheric models have been recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang-Sheeley-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling Framework (SWMF), and heliospheric tomography using interplanetary scintillation data. To investigate the effects of photospheric magnetograms from different sources, different coronal models, and different model versions on the model performance, we run these models in 10 combinations. Choosing seven Carrington rotations in 2007 as the time window, we compare the modeling results with the Operating Mission as Nodes on the Internet data for near-Earth space environment during the late declining phase of solar cycle 23. Visual comparison is proved to be a necessary addition to the quantitative assessment of the models' capabilities in reproducing the time series and statistics of solar wind parameters. The MAS-Enlil model captures the time patterns of solar wind parameters better, while the WSA-Enlil model matches with the time series of normalized solar wind parameters better. Models generally overestimate slow wind temperature and underestimate fast wind temperature and magnetic field. Using improved algorithms, we have identified magnetic field sector boundaries (SBs) and slow-to-fast stream interaction regions (SIRs) as focused structures. The success rate of capturing them and the time offset vary largely with models. For this quiet period, the new version of MAS-Enlil model works best for SBs, while heliospheric tomography works best for SIRs. The new version of SWMF with more physics added needs more development. General strengths and weaknesses for each model are diagnosed to provide an unbiased reference to model developers and users.
C1 [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jian, L. K.; MacNeice, P. J.; Taktakishvili, A.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Taktakishvili, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Odstrcil, D.; Evans, R. M.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Jackson, B.; Yu, H. -S.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92103 USA.
[Riley, P.] Predictive Sci Inc, San Diego, CA USA.
[Sokolov, I. V.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Jian, LK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM lan.jian@nasa.gov
RI Sokolov, Igor/H-9860-2013; Jian, Lan/B-4053-2010;
OI Sokolov, Igor/0000-0002-6118-0469; Jian, Lan/0000-0002-6849-5527; Riley,
Pete/0000-0002-1859-456X
FU NSF [AGS 1242798, 1321493, 1259549, AGS 1257519]
FX This work is supported by NSF grants AGS 1242798, 1321493 and 1259549.
A.T. and I.V.S. are supported by NSF grant AGS 1257519. Simulation
results have been provided by the CCMC at NASA/GSFC through their public
Runs on Request system
(http://ccmc.gsfc.nasa.gov/requests/requests.php). The results of IPS
tomography are available upon request from Bernard Jackson at UCSD. The
simulation results of other models are available to the public at
http://ccmc.gsfc.nasa.gov/ungrouped/SH/Helio_main.php by searching
"Jian" as run requestor's last name and choosing 2056-2062 as the
Carrington rotation number. The CCMC is a multiagency partnership
between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. We are
grateful to the CCMC team for their work. We thank the GONG, SOHO/MDI,
MWO, and NSO teams for providing the photospheric magnetograms. We
appreciate Nick Arge for providing the WSA coronal model at the CCMC and
thank all the other modeling teams (see section 2) for providing their
models at the CCMC and for their consultation. We acknowledge the Space
Physics Data Facility at NASA/GSFC for providing OMNI data (see
http://omniweb.gsfc.nasa.gov/). L.K.J. thanks Janet Luhmann and
Christopher Russell for helpful discussion.
NR 94
TC 7
Z9 7
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAY
PY 2015
VL 13
IS 5
BP 316
EP 338
DI 10.1002/2015SW001174
PG 23
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CL0HX
UT WOS:000356623500009
ER
PT J
AU Cervini-Silva, J
Antonio-Nieto-Camacho
Ramirez-Apan, MT
Gomez-Vidales, V
Palacios, E
Montoya, A
de Jesus, ER
AF Cervini-Silva, Javiera
Antonio-Nieto-Camacho
Teresa Ramirez-Apan, Maria
Gomez-Vidales, Virginia
Palacios, Eduardo
Montoya, Ascencion
Ronquillo de Jesus, Elba
TI Anti-inflammatory, anti-bacterial, and cytotoxic activity of fibrous
clays
SO COLLOIDS AND SURFACES B-BIOINTERFACES
LA English
DT Article
DE Early anti-inflammatory response; Frequency of inversion sites; Silanol
groups
ID TRIBOLIUM-CASTANEUM; POWDER DIFFRACTION; MOUSE EAR; MAYA BLUE;
SEPIOLITE; PALYGORSKITE; EFFICACY; HALLOYSITE; AGENTS; INDIGO
AB Produced worldwide at 1.2 m tons per year, fibrous clays are used in the production of pet litter, animal feed stuff to roof parcels, construction and rheological additives, and other applications needing to replace long-fiber length asbestos. To the authors' knowledge, however, information on the beneficial effects of fibrous clays on health remains scarce. This paper reports on the anti-inflammatory, antibacterial, and cytotoxic activity by sepiolite (Vallecas, Spain) and palygorskite (Torrejon El Rubio, Spain). The anti-inflammatory activity was determined using the 12-O-tetradecanoylphorbol-13-acetate (TPA) and myeloperoxidase (MPO) methods. Histological cuts were obtained for quantifying leukocytes found in the epidermis. Palygorkite and sepiolite caused edema inhibition and migration of neutrophils ca. 68.64 and 45.54%, and 80 and 65%, respectively. Fibrous clays yielded high rates of infiltration, explained by cleavage of polysomes and exposure of silanol groups. Also, fibrous clays showed high inhibition of myeloperoxidase contents shortly after exposure, but decreased sharply afterwards. In contrast, tubular clays caused an increasing inhibition of myeloperoxidase with time. Thus, clay structure restricted the kinetics and mechanism of myeloperoxidase inhibition. Fibrous clays were screened in vitro against human cancer cell lines. Cytotoxicity was determined using the protein-binding dye sulforhodamine B (SRB). Exposing cancer human cells to sepiolite or palygorskite showed growth inhibition varying with cell line. This study shows that fibrous clays served as an effective anti-inflammatory, limited by chemical transfer and cellular-level signals responding exclusively to an early exposure to clay, and cell viability decreasing significantly only after exposure to high concentrations of sepiolite. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Cervini-Silva, Javiera; Ronquillo de Jesus, Elba] Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Mexico City 05348, DF, Mexico.
[Cervini-Silva, Javiera] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
[Cervini-Silva, Javiera] NASA, Astrobiol Inst, Mountain View, CA USA.
[Antonio-Nieto-Camacho; Teresa Ramirez-Apan, Maria] Univ Nacl Autonoma Mexico, Inst Quim, Lab Pruebas Biol, Mexico City 04510, DF, Mexico.
[Gomez-Vidales, Virginia] Univ Nacl Autonoma Mexico, Inst Quim, Lab Resonancia Paramagnet Elect, Mexico City 04510, DF, Mexico.
[Palacios, Eduardo; Montoya, Ascencion] Inst Mexicano Petr, Direcc Invest & Posgrad, Ciuadad Mexico, DF, Mexico.
RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Av Vasco de Quiroga 4871, Mexico City 05348, DF, Mexico.
EM jcervini@correo.cua.uam.mx
FU Universidad Autonoma Metropolitana Unidad Cuajimalpa [33678]
FX The authors thank Maria del Rocio Galindo Ortega and Carolina Lopez
Pacheco (UAM-Cuajimalpa), and Daniela Rodriguez Montano (Unidad de
Histologia, Instituto de Fisiologia Celular, UNAM) for technical
assistance; and Drs. Georgios D. Chyssikos (Theoretical and Physical
Chemistry Institute, National Hellenic Research Foundation, Athens,
11635, Greece), Vassilis Gionis (Institute of Materials Science,
N.C.S.R. "Demokritos", 15310, Aghia Paraskevi, Attiki, Greece); and
Stephan Kaufhold (BGR Bundensansaltfur Geowissenschaften und Rohstoffe,
Hannover, Germany) for providing insightful comments during the
preparation of this manuscript. This project was supported in part by
Universidad Autonoma Metropolitana Unidad Cuajimalpa (Grant No. 33678).
NR 35
TC 9
Z9 9
U1 6
U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-7765
EI 1873-4367
J9 COLLOID SURFACE B
JI Colloid Surf. B-Biointerfaces
PD MAY 1
PY 2015
VL 129
BP 1
EP 6
DI 10.1016/j.colsurfb.2015.03.019
PG 6
WC Biophysics; Chemistry, Physical; Materials Science, Biomaterials
SC Biophysics; Chemistry; Materials Science
GA CJ3AQ
UT WOS:000355356200001
PM 25819359
ER
PT J
AU Shaver, I
Chain-Guadarrama, A
Cleary, KA
Sanfiorenzo, A
Santiago-Garcia, RJ
Finegan, B
Hormel, L
Sibelet, N
Vierling, LA
Bosque-Perez, NA
DeClerck, F
Fagan, ME
Waits, LP
AF Shaver, Irene
Chain-Guadarrama, Adina
Cleary, Katherine A.
Sanfiorenzo, Andre
Santiago-Garcia, Ricardo J.
Finegan, Bryan
Hormel, Leontina
Sibelet, Nicole
Vierling, Lee A.
Bosque-Perez, Nilsa A.
DeClerck, Fabrice
Fagan, Matthew E.
Waits, Lisette P.
TI Coupled social and ecological outcomes of agricultural intensification
in Costa Rica and the future of biodiversity conservation in tropical
agricultural regions
SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS
LA English
DT Article
DE Agricultural intensification; Biodiversity; Non-traditional agricultural
export; Smallholder; Pineapple; Costa Rica
ID ENVIRONMENTAL SERVICE PAYMENTS; LAND-USE CHANGE; RAIN-FOREST;
AGROFORESTRY SYSTEMS; DIPTERYX-PANAMENSIS; TREE COVER; LANDSCAPES;
MANAGEMENT; SECONDARY; GLOBALIZATION
AB Tropical ecosystem conversion to agriculture has caused widespread habitat loss and created fragmented landscapes composed of remnant forest patches embedded in a matrix of agricultural land uses. Non-traditional agricultural export (NTAE) crops such as pineapple are rapidly replacing multiuse landscapes characterized by a diverse matrix of pasture and smallholder crops with intensive, large-scale, monoculture plantations. Using an interdisciplinary approach, we conduct a case study to examine the coupled social and ecological implications of agricultural intensification in this region, with larger application to regions experiencing similar patterns of agricultural intensification. Guided by frameworks from both political and landscape ecology, we: (1) describe the social and economic implications of pineapple expansion, specifically the concentration of land, labor and financial resources, (2) quantify pineapple cultivation's spatial characteristics, and (3) assess the effects of pineapple expansion on surrounding forest ecosystems, on the agricultural matrix and on biodiversity conservation. Our results indicate that pineapple production concentrates land, labor, and financial resources, which has a homogenizing effect on the agricultural economy in the study region. This constrains farm-based livelihoods, with larger implications for food security and agricultural diversity. Landscape ecology analyses further reveal how pineapple production simplifies and homogenizes the agricultural matrix between forest patches, which is likely to have a negative effect on biodiversity. To offset the effects of pineapple expansion on social and environmental systems, we recommend developing landscape level land use planning capacity. Furthermore, agricultural and conservation policy reform is needed to promote landscape heterogeneity and economic diversity within the agricultural sector. Our interdisciplinary research provides a detailed examination of the social and ecological impacts of agricultural intensification in a tropical landscape, and offers recommendations for improvement relevant not only to our study region but to the many other tropical landscapes currently undergoing non-traditional agricultural export driven agricultural intensification. (c) 2015 Elsevier Ltd. All rights reserved.
C1 [Shaver, Irene; Sanfiorenzo, Andre; Santiago-Garcia, Ricardo J.] Univ Idaho, Environm Sci Program, Moscow, ID 83844 USA.
[Chain-Guadarrama, Adina; Vierling, Lee A.] Univ Idaho, Dept Forest Rangeland & Fire Sci, Idaho Falls, ID 83441 USA.
[Shaver, Irene; Chain-Guadarrama, Adina; Cleary, Katherine A.; Sanfiorenzo, Andre; Santiago-Garcia, Ricardo J.] Trop Agr Res & Higher Educ Ctr CATIE, Grad Sch, Turrialba 30501, Costa Rica.
[Cleary, Katherine A.; Waits, Lisette P.] Univ Idaho, Dept Fish & Wildlife Sci, Moscow, ID 83844 USA.
[Bosque-Perez, Nilsa A.] Univ Idaho, Dept Plant Soil & Entomol Sci, Moscow, ID 83844 USA.
[DeClerck, Fabrice] CGIAR, Biodivers Int, Agrobiodivers & Ecosyst Serv Program, F-34950 Montpellier, France.
[Finegan, Bryan] Trop Agr Res & Higher Educ Ctr CATIE, Prod & Conservat Forests Program, Turrialba 30501, Costa Rica.
[Hormel, Leontina] Univ Idaho, Dept Sociol & Anthropol, Moscow, ID 83844 USA.
[Sibelet, Nicole] CIRAD, UMR Innovat, F-34398 Montpellier, France.
[Sibelet, Nicole] Trop Agr Res & Higher Educ Ctr CATIE, Econ & Environm Dev IDEA, Turrialba 30501, Costa Rica.
[Fagan, Matthew E.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA.
RP Shaver, I (reprint author), 13775 Nisula Rd, McCall, ID 83638 USA.
EM shaverirene@gmail.com
RI Chain-Guadarrama, Adina/K-1167-2016; Guadarrama, Mercedes/K-1155-2016
OI Chain-Guadarrama, Adina/0000-0002-6944-2064; Guadarrama,
Mercedes/0000-0002-6944-2064
FU National Science Foundation under IGERT [0903479]; National Science
Foundation under CNH [1313824]
FX This material is based upon work supported by the National Science
Foundation under IGERT grant number Award No. 0903479 and CNH grant
Award No. 1313824. Fabrice DeClerck was supported by the CGIAR research
program on Water Land and Ecosystems.
NR 121
TC 3
Z9 3
U1 21
U2 80
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 MAY
PY 2015
VL 32
BP 74
EP 86
DI 10.1016/j.gloenvcha.2015.02.006
PG 13
WC Environmental Sciences; Environmental Studies; Geography
SC Environmental Sciences & Ecology; Geography
GA CJ8RH
UT WOS:000355770700008
ER
PT J
AU Kara, E
Fabian, AC
Lohfink, AM
Parker, ML
Walton, DJ
Boggs, SE
Christensen, FE
Hailey, CJ
Harrison, FA
Matt, G
Reynolds, CS
Stern, D
Zhang, WW
AF Kara, E.
Fabian, A. C.
Lohfink, A. M.
Parker, M. L.
Walton, D. J.
Boggs, S. E.
Christensen, F. E.
Hailey, C. J.
Harrison, F. A.
Matt, G.
Reynolds, C. S.
Stern, D.
Zhang, W. W.
TI The Compton hump and variable blue wing in the extreme low-flux NuSTAR
observations of 1H0707-495
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: individual: 1H0707-495;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY REVERBERATION; LINE SEYFERT-1
GALAXY-1H-0707-495; ACCRETING BLACK-HOLES; NARROW-LINE; XMM-NEWTON; 1H
0707-495; IRON-K; SPECTRAL VARIABILITY; GALAXY MCG-6-30-15
AB The narrow-line Seyfert I galaxy, 1H0707-495, has been well observed in the 0.3-10 keV band, revealing a dramatic drop in flux in the iron K alpha band, a strong soft excess, and short time-scale reverberation lags associated with these spectral features. In this paper, we present the first results of a deep 250-ks NuSTAR (Nuclear Spectroscopic Telescope Array) observation of 1H0707-495, which includes the first sensitive observations above 10 keV. Even though the NuSTAR observations caught the source in an extreme low-flux state, the Compton hump is still significantly detected. NuSTAR, with its high effective area above 7 keV, clearly detects the drop in flux in the iron Ka band, and by comparing these observations with archival XMM-Newton observations, we find that the energy of this drop increases with increasing flux. We discuss possible explanations for this, the most likely of which is that the drop in flux is the blue wing of the relativistically broadened iron K alpha emission line. When the flux is low, the coronal source height is low, thus enhancing the most gravitationally redshifted emission.
C1 [Kara, E.; Fabian, A. C.; Lohfink, A. M.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Walton, D. J.; Harrison, F. A.] 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.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reynolds, C. S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kara, E (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England.
EM ekara@ast.cam.ac.uk
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU Gates Cambridge Scholarship; European Union [312789]; Italian Space
Agency [ASI/INAF I/037/12/0-011/13]; National Aeronautics and Space
Administration (NASA) [NNG08FD60C]; NASA
FX EK thanks Javier Garcia and Thomas Dauser for interesting discussions on
the RELXILLLP modelling. EK is supported by the Gates Cambridge
Scholarship. ACF thanks the Royal Society. EK, ACF, AML, and GM
acknowledge support from the European Union Seventh Framework Programme
(FP7/2007-2013) under grant agreement no. 312789, StrongGravity. AML and
GM acknowledge financial support from Italian Space Agency under grant
ASI/INAF I/037/12/0-011/13. This work was supported under National
Aeronautics and Space Administration (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 NASA. 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.
NR 50
TC 8
Z9 8
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2015
VL 449
IS 1
BP 234
EP 242
DI 10.1093/mnras/stv304
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2WO
UT WOS:000355345600019
ER
PT J
AU Nemmen, RS
Tchekhovskoy, A
AF Nemmen, Rodrigo S.
Tchekhovskoy, Alexander
TI On the efficiency of jet production in radio galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: active;
galaxies: jets; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; RADIATIVELY INEFFICIENT
ACCRETION; ADVECTION-DOMINATED ACCRETION; BLANDFORD-ZNAJEK PROCESS;
RELATIVISTIC JETS; SAGITTARIUS-A; ELECTROMAGNETIC EXTRACTION;
OBSERVATIONAL CONSTRAINTS; NUMERICAL SIMULATIONS
AB The mechanisms that produce and power relativistic jets are fundamental open questions in black hole (BH) astrophysics. In order to constrain these mechanisms, we analyse the energy efficiency of jet production eta based on archival Chandra observations of 27 nearby, low-luminosity active galactic nuclei. We obtain eta as the ratio of the jet power, inferred from the energetics of jet powered X-ray emitting cavities, to the BH mass accretion rate. (M) over dot(BH). The standard assumption in estimating (M) over dot(BH) is that all the gas from the Bondi radius r(B) makes it down to the BH. It is now clear, however, that only a small fraction of the gas reaches the hole. To account for this effect, we use the standard disc mass-loss scaling, (M) over dot (r) alpha (r/r(B))(s) (M) over dot(Bondi). This leads to much lower values of (M) over dot(BH) and higher values of eta than in previous studies. If hot accretion flows are characterized by 0.5 <= s <= 0.6 - on the lower end of recent theoretical and observational studies - then dynamically important magnetic fields near rapidly spinning BHs are necessary to account for the high eta approximate to 100-300 per cent in the sample. Moreover, values of s > 0.6 are essentially ruled out, or there would be insufficient energy to power the jets. We discuss the implications of our results for the distribution of massive BH spins and the possible impact of a significant extra cold gas supply on our estimates.
C1 [Nemmen, Rodrigo S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil.
[Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nemmen, Rodrigo S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Nemmen, Rodrigo S.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Tchekhovskoy, Alexander] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Tchekhovskoy, Alexander] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Tchekhovskoy, Alexander] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
RP Nemmen, RS (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil.
EM rodrigo.nemmen@iag.usp.br
FU NASA Postdoctoral Program (NPP) at Goddard Space Flight Center; NASA
[NNH10ZDA001N, NAS8-03060]; FAPESP; NASA through Einstein Postdoctoral
Fellowship - Chandra X-ray Center [PF3-140115]
FX We acknowledge useful discussions with Mihoko Yukita, Ka-Wah Wong,
Aleksander Sadowski, Helen Russell, Jonathan C. McKinney, Jeremy
Schnittman, Markos Georganopoulos, Ramesh Narayan, Jeff McClintock, Feng
Yuan and Sylvain Guiriec. RSN was partially supported by the NASA
Postdoctoral Program (NPP) at Goddard Space Flight Center, administered
by Oak Ridge Associated Universities with NASA, as well as the NASA
grant NNH10ZDA001N and FAPESP. AT was supported by NASA through Einstein
Postdoctoral Fellowship grant number PF3-140115 awarded by the Chandra
X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060, and NASA support via
High-End Computing (HEC) Program through the NASA Advanced
Super-computing (NAS) Division at Ames Research Center that provided
access to the Pleiades supercomputer, as well as NSF support through an
XSEDE computational time allocation TG-AST100040 on NICS Kraken,
Nautilus, TACC Stampede, Maverick and Ranch. This project made
considerable use of IPYTHON (Perez & Granger 2007) and the ASTROPY and
MCERP libraries.
NR 114
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2015
VL 449
IS 1
BP 316
EP 327
DI 10.1093/mnras/stv260
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2WO
UT WOS:000355345600024
ER
PT J
AU Hensley, B
Murphy, E
Staguhn, J
AF Hensley, Brandon
Murphy, Eric
Staguhn, Johannes
TI Characterizing extragalactic anomalous microwave emission in NGC 6946
with CARMA
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: general; ISM: general; radio continuum: ISM
ID SPINNING DUST EMISSION; ANISOTROPY-PROBE; GALACTIC EMISSION; NEARBY
GALAXIES; STAR-FORMATION; IMAGE ATLAS; SPITZER; RADIO; WMAP; CONTINUUM
AB Using 1 cm and 3 mm observations from the Combined Array for Research in Millimeter-wave Astronomy and 2 mm observations from the Goddard IRAM Superconducting 2 Millimeter Observer observations, we follow up the first extragalactic detection of anomalous microwave emission (AME) reported by Murphy et al. in an extranuclear region (Enuc. 4) of the nearby face-on spiral galaxy NGC 6946. We find the spectral shape and peak frequency of AME in this region to be consistent with models of spinning dust emission. However, the strength of the emission far exceeds the Galactic AME emissivity given the abundance of polycyclic aromatic hydrocarbons (PAHs) in that region. Using our galaxy-wide 1 cm map (21 arcsec resolution), we identify a total of eight 21 arcsec x 21 arcsec regions in NGC 6946 that harbour AME at > 95 per cent significance at levels comparable to that observed in Enuc. 4. The remainder of the galaxy has 1 cm emission consistent with or below the observed Galactic AME emissivity per PAH surface density. We probe relationships between the detected AME and dust surface density, PAH emission, and radiation field, though no environmental property emerges to delineate regions with strong versus weak or non-existent AME. On the basis of these data and other AME observations in the literature, we determine that the AME emissivity per unit dust mass is highly variable. We argue that the spinning dust hypothesis, which predicts the AME power to be approximately proportional to the PAH mass, is therefore incomplete.
C1 [Hensley, Brandon] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Murphy, Eric] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Staguhn, Johannes] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Staguhn, Johannes] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hensley, B (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM bhensley@princeton.edu
OI Hensley, Brandon/0000-0001-7449-4638
FU NSF Graduate Research Fellowship [DGE-0646086]; NSF [AST-1408723]; NSF
ATI [1020981, 1106284]
FX BH acknowledges support from the NSF Graduate Research Fellowship under
Grant no. DGE-0646086 and NSF grant AST-1408723. The GISMO observations
and JS were supported through NSF ATI grants 1020981 and 1106284.
NR 54
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2015
VL 449
IS 1
BP 809
EP 819
DI 10.1093/mnras/stv287
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2WO
UT WOS:000355345600059
ER
PT J
AU De Pasquale, M
Kuin, NPM
Oates, S
Schulze, S
Cano, Z
Guidorzi, C
Beardmore, A
Evans, PA
Uhm, ZL
Zhang, B
Page, M
Kobayashi, S
Castro-Tirado, A
Gorosabel, J
Sakamoto, T
Fatkhullin, T
Pandey, SB
Im, M
Chandra, P
Frail, D
Gao, H
Kopac, D
Jeon, Y
Akerlof, C
Huang, KY
Pak, S
Park, WK
Gomboc, A
Melandri, A
Zane, S
Mundell, CG
Saxton, CJ
Holland, ST
Virgili, F
Urata, Y
Steele, I
Bersier, D
Tanvir, N
Sokolov, VV
Moskvitin, AS
AF De Pasquale, Massimiliano
Kuin, N. P. M.
Oates, S.
Schulze, S.
Cano, Z.
Guidorzi, C.
Beardmore, A.
Evans, P. A.
Uhm, Z. L.
Zhang, B.
Page, M.
Kobayashi, S.
Castro-Tirado, A.
Gorosabel, J.
Sakamoto, T.
Fatkhullin, T.
Pandey, S. B.
Im, M.
Chandra, P.
Frail, D.
Gao, H.
Kopac, D.
Jeon, Y.
Akerlof, C.
Huang, K. Y.
Pak, S.
Park, W. -K.
Gomboc, A.
Melandri, A.
Zane, S.
Mundell, C. G.
Saxton, C. J.
Holland, S. T.
Virgili, F.
Urata, Y.
Steele, I.
Bersier, D.
Tanvir, N.
Sokolov, V. V.
Moskvitin, A. S.
TI The optical rebrightening of GRB100814A: an interplay of forward and
reverse shocks?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanism: non-thermal; shock waves; gamma-ray burst: general
ID GAMMA-RAY BURST; AFTERGLOW LIGHT CURVES; CONTINUOUS ENERGY INJECTION;
RELATIVISTIC BLAST WAVES; SWIFT XRT DATA; X-RAY; JET BREAKS; THEORETICAL
IMPLICATIONS; COMPREHENSIVE ANALYSIS; PHOTOMETRIC SYSTEM
AB We present a wide data set of gamma-ray, X-ray, UV/Opt/IR (UVOIR), and radio observations of the Swift GRB100814A. At the end of the slow decline phase of the X-ray and optical afterglow, this burst shows a sudden and prominent rebrightening in the optical band only, followed by a fast decay in both bands. The optical rebrightening also shows chromatic evolution. Such a puzzling behaviour cannot be explained by a single component model. We discuss other possible interpretations, and we find that a model that incorporates a long-lived reverse shock and forward shock fits the temporal and spectral properties of GRB100814 the best.
C1 [De Pasquale, Massimiliano; Kuin, N. P. M.; Oates, S.; Page, M.; Zane, S.; Saxton, C. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[De Pasquale, Massimiliano; Uhm, Z. L.; Zhang, B.; Gao, H.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[De Pasquale, Massimiliano] INAF IASF, I-90146 Palermo, Italy.
[Oates, S.; Castro-Tirado, A.; Gorosabel, J.] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain.
[Schulze, S.; Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[Schulze, S.] Pontificia Univ Catolica Chile, Dept Astronom & Astrofis, Santiago 22, Chile.
[Schulze, S.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Cano, Z.; Kopac, D.; Mundell, C. G.; Virgili, F.; Steele, I.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy.
[Beardmore, A.; Evans, P. A.; Kobayashi, S.; Tanvir, N.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain.
[Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, ETS Ingn, E-48013 Bilbao, Spain.
[Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fatkhullin, T.; Sokolov, V. V.; Moskvitin, A. S.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia.
[Pandey, S. B.] ARIES, Naini Tal 263129, Uttarakhand, India.
[Im, M.; Jeon, Y.; Park, W. -K.] Seoul Natl Univ, FPRD, Dept Phys & Astron, CEOU Astron Program, Seoul 151742, South Korea.
[Chandra, P.] Pune Univ, Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Frail, D.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Akerlof, C.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Huang, K. Y.] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan.
[Pak, S.] Kyung Hee Univ, Yongin 446701, Gyeonggi Do, South Korea.
[Park, W. -K.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Gomboc, A.] Univ Ljubljana, Fac Math & Phys, SI-1000 Ljubljana, Slovenia.
[Gomboc, A.] Ctr Excellence Space SI, SI-1000 Ljubljana, Slovenia.
[Melandri, A.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy.
[Saxton, C. J.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Holland, S. T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Urata, Y.] Natl Cent Univ, Insti Astron, Chungli 32054, Taiwan.
RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM m.depasquale@ucl.ac.uk
OI Castro-Tirado, A. J./0000-0003-2999-3563; Im,
Myungshin/0000-0002-8537-6714; Schulze, Steve/0000-0001-6797-1889
FU United Kingdom Space Agency (UKSA); Royal Society; Wolfson Foundation;
Science and Technology Facilities Council (STFC); STFC; UKSA; Slovenian
Research Agency; Centre of Excellence for Space Sciences and
Technologies SPACE-SI; European Union; European Regional Development
Fund; Republic of Slovenia; Creative Initiative programme of the
National Research Foundation of Korea (NRF) - Korea government (MSIP)
[2008-0060544]; Grant of Excellence from the Icelandic; Iniciativa
Cientifica Milenio (Millennium Center for Supernova Science)
[P10-064-F]; Basal-CATA [PFB-06/2007]; 'Fondo de Innovacion para la
Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile';
Dill Faulkes Educational Trust
FX MDP, MJP, NPK, and SRO acknowledge United Kingdom Space Agency (UKSA)
funding. MDP thanks M. A. Aloy, F. Daigne, and A. Mizuta for insightful
discussions at 'Supernovae and Gamma-Ray Burst 2013' conference, Kyoto.
CGM thanks the Royal Society, the Wolfson Foundation and the Science and
Technology Facilities Council (STFC) for support. FG acknowledges
support from STFC. APB and PAE acknowledge UKSA support. This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester. AG acknowledges funding from the Slovenian
Research Agency and from the Centre of Excellence for Space Sciences and
Technologies SPACE-SI, an operation partly financed by the European
Union, European Regional Development Fund and Republic of Slovenia. MI,
YJ, and S. Pak acknowledge the support from the Creative Initiative
programme, grant No. 2008-0060544 of the National Research Foundation of
Korea (NRF), funded by the Korea government (MSIP). SS acknowledges
financial support from support by a Grant of Excellence from the
Icelandic and the Iniciativa Cientifica Milenio grant P10-064-F
(Millennium Center for Supernova Science), with input from 'Fondo de
Innovacion para la Competitividad, del Ministerio de Economia, Fomento y
Turismo de Chile', and Basal-CATA (PFB-06/2007). The Liverpool Telescope
is operated by Liverpool John Moores University at the Observatorio del
Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The
Faulkes Telescopes, now owned by the Las Cumbres Observatory Global
Telescope network, are operated with support from the Dill Faulkes
Educational Trust.
NR 100
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2015
VL 449
IS 1
BP 1024
EP 1042
DI 10.1093/mnras/stv267
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ2WO
UT WOS:000355345600074
ER
PT J
AU Arbabi, A
Horie, Y
Ball, AJ
Bagheri, M
Faraon, A
AF Arbabi, Amir
Horie, Yu
Ball, Alexander J.
Bagheri, Mahmood
Faraon, Andrei
TI Subwavelength-thick lenses with high numerical apertures and large
efficiency based on high-contrast transmitarrays
SO NATURE COMMUNICATIONS
LA English
DT Article
ID MICRO-FRESNEL LENSES; GRATING REFLECTORS; ORDER GRATINGS; METASURFACES;
ELEMENTS; MIRROR; NM
AB Flat optical devices thinner than a wavelength promise to replace conventional free-space components for wavefront and polarization control. Transmissive flat lenses are particularly interesting for applications in imaging and on-chip optoelectronic integration. Several designs based on plasmonic metasurfaces, high-contrast transmitarrays and gratings have been recently implemented but have not provided a performance comparable to conventional curved lenses. Here we report polarization-insensitive, micron-thick, high-contrast transmitarray micro-lenses with focal spots as small as 0.57 lambda. The measured focusing efficiency is up to 82%. A rigorous method for ultrathin lens design, and the trade-off between high efficiency and small spot size (or large numerical aperture) are discussed. The micro-lenses, composed of silicon nano-posts on glass, are fabricated in one lithographic step that could be performed with high-throughput photo or nanoimprint lithography, thus enabling widespread adoption.
C1 [Arbabi, Amir; Horie, Yu; Ball, Alexander J.; Faraon, Andrei] CALTECH, Thomas J Watson Lab Appl Phys, Pasadena, CA 91125 USA.
[Bagheri, Mahmood] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Faraon, A (reprint author), CALTECH, Thomas J Watson Lab Appl Phys, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM faraon@caltech.edu
FU Caltech/JPL president and director fund (PDF); DARPA; JASSO;
'Light-Material Interactions in Energy Conversion' Energy Frontier
Research Center - US Department of Energy, Office of Science, Office of
Basic Energy Sciences [DE-SC0001293]; Summer Undergraduate Research
Fellowship (SURF) at Caltech
FX This work was supported by the Caltech/JPL president and director fund
(PDF). A.A. was also supported by DARPA. Y.H. was supported by the JASSO
fellowship and the 'Light-Material Interactions in Energy Conversion'
Energy Frontier Research Center funded by the US Department of Energy,
Office of Science, Office of Basic Energy Sciences under Award no.
DE-SC0001293. Alexander Ball was supported by the Summer Undergraduate
Research Fellowship (SURF) at Caltech. The device nanofabrication was
performed in the Kavli Nanoscience Institute at Caltech. We thank David
Fattal and Sonny Vo for useful discussion.
NR 33
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD MAY
PY 2015
VL 6
AR 7069
DI 10.1038/ncomms8069
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CJ5MG
UT WOS:000355531100005
PM 25947118
ER
PT J
AU Georgiou, CD
Sun, HJ
Mckay, CP
Grintzalis, K
Papapostolou, I
Zisimopoulos, D
Panagiotidis, K
Zhang, GS
Koutsopoulou, E
Christidis, GE
Margiolaki, I
AF Georgiou, Christos D.
Sun, Henry J.
Mckay, Christopher P.
Grintzalis, Konstantinos
Papapostolou, Ioannis
Zisimopoulos, Dimitrios
Panagiotidis, Konstantinos
Zhang, Gaosen
Koutsopoulou, Eleni
Christidis, George E.
Margiolaki, Irene
TI Evidence for photochemical production of reactive oxygen species in
desert soils
SO NATURE COMMUNICATIONS
LA English
DT Article
ID SINGLET OXYGEN; ATACAMA DESERT; MARTIAN SOIL; MOLECULAR-OXYGEN; OXIDE
SURFACES; HYDROGEN-PEROXIDE; SUPEROXIDE IONS; MOJAVE-DESERT;
PERCHLORATE; TIO2
AB The combination of intense solar radiation and soil desiccation creates a short circuit in the biogeochemical carbon cycle, where soils release significant amounts of CO2 and reactive nitrogen oxides by abiotic oxidation. Here we show that desert soils accumulate metal superoxides and peroxides at higher levels than non-desert soils. We also show the photogeneration of equimolar superoxide and hydroxyl radical in desiccated and aqueous soils, respectively, by a photo-induced electron transfer mechanism supported by their mineralogical composition. Reactivity of desert soils is further supported by the generation of hydroxyl radical via aqueous extracts in the dark. Our findings extend to desert soils the photogeneration of reactive oxygen species by certain mineral oxides and also explain previous studies on desert soil organic oxidant chemistry and microbiology. Similar processes driven by ultraviolet radiation may be operating in the surface soils on Mars.
C1 [Georgiou, Christos D.; Grintzalis, Konstantinos; Papapostolou, Ioannis; Zisimopoulos, Dimitrios; Panagiotidis, Konstantinos; Margiolaki, Irene] Univ Patras, Dept Biol, Patras 26504, Greece.
[Sun, Henry J.] Desert Res Inst, Las Vegas, NV 89119 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zhang, Gaosen] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Lanzhou 73000, Peoples R China.
[Koutsopoulou, Eleni] Univ Patras, Lab Elect Microscopy & Microanal, Patras 26500, Greece.
[Christidis, George E.] Tech Univ Crete, Dept Mineral Resources Engn, Khania 73100, Greece.
RP Georgiou, CD (reprint author), Univ Patras, Dept Biol, Patras 26504, Greece.
EM c.georgiou@upatras.gr
RI Georgiou, Christos/B-8354-2013; Grintzalis, Konstantinos/I-5124-2014
OI Georgiou, Christos/0000-0001-9707-0109; Grintzalis,
Konstantinos/0000-0002-6276-495X
FU Greek Ministry of Education; NASA Astrobiology Program [NNX07AT65];
National Science Foundation [IIA-1301726]; NASA Planetary Protection
Program
FX C.D.G. was financially supported by the Greek Ministry of Education.
H.J.S. and G.Z. were supported by a grant from the NASA Astrobiology
Program NNX07AT65. H.J.S was also in part supported by the National
Science Foundation under grant number IIA-1301726. He thanks R.
Kreidberg for editorial assistance. C.P.M. acknowledges the support from
the NASA Planetary Protection Program. We thank the ESRF for the
provision of synchrotron X-ray beamtime at the high-resolution powder
diffraction beamline (ID31). We are grateful to Professor P.V. Ioannou
(Department of Chemistry) and Associate Professor M. Kornaros
(Department of Chemical Engineering) at the University of Patras,
Greece, for HTPA synthesis and HPLC-MS identification in samples,
respectively.
NR 70
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U1 12
U2 53
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD MAY
PY 2015
VL 6
AR 7100
DI 10.1038/ncomms8100
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CJ5MN
UT WOS:000355531800001
PM 25960012
ER
PT J
AU Mostl, C
Rollett, T
Frahm, RA
Liu, YD
Long, DM
Colaninno, RC
Reiss, MA
Temmer, M
Farrugia, CJ
Posner, A
Dumbovic, M
Janvier, M
Demoulin, P
Boakes, P
Devos, A
Kraaikamp, E
Mays, ML
Vrsnak, B
AF Mostl, Christian
Rollett, Tanja
Frahm, Rudy A.
Liu, Ying D.
Long, David M.
Colaninno, Robin C.
Reiss, Martin A.
Temmer, Manuela
Farrugia, Charles J.
Posner, Arik
Dumbovic, Mateja
Janvier, Miho
Demoulin, Pascal
Boakes, Peter
Devos, Andy
Kraaikamp, Emil
Mays, Mona L.
Vrsnak, Bojan
TI Strong coronal channelling and interplanetary evolution of a solar storm
up to Earth and Mars
SO NATURE COMMUNICATIONS
LA English
DT Article
ID IN-SITU OBSERVATIONS; MASS EJECTIONS; MAGNETIC CLOUD; ARRIVAL TIMES;
WIND; PROPAGATION; SHOCK; CMES; SUN; DEFLECTION
AB The severe geomagnetic effects of solar storms or coronal mass ejections (CMEs) are to a large degree determined by their propagation direction with respect to Earth. There is a lack of understanding of the processes that determine their non-radial propagation. Here we present a synthesis of data from seven different space missions of a fast CME, which originated in an active region near the disk centre and, hence, a significant geomagnetic impact was forecasted. However, the CME is demonstrated to be channelled during eruption into a direction + 37 +/- 10 degrees (longitude) away from its source region, leading only to minimal geomagnetic effects. In situ observations near Earth and Mars confirm the channelled CME motion, and are consistent with an ellipse shape of the CME-driven shock provided by the new Ellipse Evolution model, presented here. The results enhance our understanding of CME propagation and shape, which can help to improve space weather forecasts.
C1 [Mostl, Christian; Rollett, Tanja] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Mostl, Christian; Reiss, Martin A.; Temmer, Manuela; Boakes, Peter] Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, A-8010 Graz, Austria.
[Frahm, Rudy A.] Southwest Res Inst, San Antonio, TX 78238 USA.
[Liu, Ying D.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing 100190, Peoples R China.
[Long, David M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Colaninno, Robin C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Farrugia, Charles J.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA.
[Posner, Arik] NASA Headquarters, Washington, DC 20546 USA.
[Dumbovic, Mateja; Vrsnak, Bojan] Univ Zagreb, Fac Geodesy, Hvar Observ, Zagreb 10000, Croatia.
[Janvier, Miho] Univ Dundee, Dept Math, Dundee DD1 4HN, Scotland.
[Demoulin, Pascal] CNRS, UMR 8109, LESIA, Observ Paris, F-92195 Meudon, France.
[Devos, Andy; Kraaikamp, Emil] Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, B-1180 Brussels, Belgium.
[Mays, Mona L.] Catholic Univ Amer, Washington, DC 20064 USA.
[Mays, Mona L.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Mostl, C (reprint author), Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
EM christian.moestl@oeaw.ac.at
RI Long, David/J-3227-2013;
OI Long, David/0000-0003-3137-0277; Dumbovic, Mateja/0000-0002-8680-8267;
Demoulin, Pascal/0000-0001-8215-6532; Liu, Ying/0000-0002-3483-5909
FU Austrian Science Fund (FWF) [P26174-N27, V195-N16]; Leverhulme Trust;
Croatian Science Foundation [6212]; Recruitment Program of Global
Experts of China; NSFC [41374173]; Specialized Research Fund for State
Key Laboratories of China; European Union Seventh Framework Programme
(FP7) [606692, 284461]; NASA [NNX13AP39G, NNX10AQ29G, NASW-00003];
STEREO Farside Grant; National Aeronautics and Space Administration
(NASA, HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; DLR and
DLR's Space Administration [50QM0501, 50QM1201]; Belgian Federal Science
Policy Office through the ESA-PRODEX program [4000103240]; European
Commission's Seventh Framework Programme (FP7) [263506, 263252]
FX This study was supported by the Austrian Science Fund (FWF):
[P26174-N27, V195-N16]. T.R. gratefully acknowledges the
JungforscherInnenfonds of the Council of the University Graz. D.M.L. is
a Leverhulme Early-Career Fellow funded by the Leverhulme Trust. M.D.
and B.V. acknowledge financial support by the Croatian Science
Foundation under the project 6212 SOLSTEL. Y.D.L. was supported by the
Recruitment Program of Global Experts of China, NSFC under grant
41374173 and the Specialized Research Fund for State Key Laboratories of
China. The presented work has received funding from the European Union
Seventh Framework Programme (FP7/2007-2013) under grant agreement No.
606692 [HELCATS] and No. 284461 [eHEROES]. Part of this work was
supported by NASA grants NNX13AP39G, NNX10AQ29G and STEREO Farside Grant
to UNH. MEX/ASPERA-3 is supported in the United States of America by
NASA contract NASW-00003. RAD is supported by the National Aeronautics
and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory
(JPL) subcontract #1273039 to the Southwest Research Institute and in
Germany by DLR and DLR's Space Administration grant numbers 50QM0501 and
50QM1201 to the Christian Albrechts University, Kiel. A.D. acknowledges
support from the Belgian Federal Science Policy Office through the
ESA-PRODEX program, grant No. 4000103240. E.K. acknowledges support from
the European Commission's Seventh Framework Programme (FP7/2007-2014)
under the grant agreement nr. 263506 (AFFECTS project), and grant
agreement nr. 263252 (COMESEP project). This research has made use of
the Heliophysics Event Knowledge database and the ESA JHelioviewer
software. We thank Janet G. Luhmann and Julia K. Thalmann for
discussions, and the Center for Geomagnetism in Kyoto for providing the
Dst indices.
NR 63
TC 20
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U1 0
U2 5
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD MAY
PY 2015
VL 6
AR 7135
DI 10.1038/ncomms8135
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CJ5MZ
UT WOS:000355533300005
PM 26011032
ER
PT J
AU Dunning, PD
Stanford, BK
Kim, HA
AF Dunning, Peter D.
Stanford, Bret K.
Kim, H. Alicia
TI Coupled aerostructural topology optimization using a level set method
for 3D aircraft wings
SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION
LA English
DT Article
DE Level set method; 3D unstructured mesh; Topology optimization;
Multi-disciplinary optimization
ID STRUCTURAL OPTIMIZATION; SENSITIVITY; DESIGN; VEHICLES; FEM
AB The purpose of this work is to develop a level set topology optimization method for an unstructured three-dimensional mesh and apply it to wing box design for coupled aerostructural considerations. The paper develops fast marching and upwind schemes suitable for unstructured meshes, which make the level set method robust and efficient. The method is applied to optimize a representative wing box internal structure for the NASA Common Research Model. The objective is to minimize the total compliance of the wing box. The trim condition that aerodynamic lift must balance the total weight of the aircraft is enforced by allowing the root angle of attack to change. The adjoint method is used to obtain the coupled shape sensitivities required to perform aerostructural optimization of the wing box. Optimum solutions for several aerodynamic and body force load cases, as well as a ground load case, are presented.
C1 [Dunning, Peter D.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Stanford, Bret K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Kim, H. Alicia] Univ Bath, Bath BA2 7AY, Avon, England.
RP Dunning, PD (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA.
EM en2pdd@bath.ac.uk
OI Kim, Hyunsun Alicia/0000-0002-5629-2466; Dunning,
Peter/0000-0002-7645-7598
FU Fixed Wing project under the National Aeronautics and Space
Administration's (NASA) Fundamental Aeronautics Program
FX This work is funded by the Fixed Wing project under the National
Aeronautics and Space Administration's (NASA) Fundamental Aeronautics
Program. The authors would like to thank Dr. Maxwell Blair for his
example DLM code and the Numerical Analysis Group at the Rutherford
Appleton Laboratory for their FORTRAN HSL packages (HSL, a collection of
Fortran codes for large-scale scientific computation. See
http://www.hsl.rl.ac.uk/).
NR 44
TC 5
Z9 5
U1 3
U2 23
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1615-147X
EI 1615-1488
J9 STRUCT MULTIDISCIP O
JI Struct. Multidiscip. Optim.
PD MAY
PY 2015
VL 51
IS 5
BP 1113
EP 1132
DI 10.1007/s00158-014-1200-1
PG 20
WC Computer Science, Interdisciplinary Applications; Engineering,
Multidisciplinary; Mechanics
SC Computer Science; Engineering; Mechanics
GA CJ8NP
UT WOS:000355760000010
ER
PT J
AU Montanaro, M
Gerace, A
Rohrbach, S
AF Montanaro, Matthew
Gerace, Aaron
Rohrbach, Scott
TI Toward an operational stray light correction for the Landsat 8 Thermal
Infrared Sensor
SO APPLIED OPTICS
LA English
DT Article
ID RADIOMETRIC CALIBRATION; SURFACE TEMPERATURE; TIRS
AB The Thermal Infrared Sensor (TIRS) onboard Landsat 8 was tasked with continuing thermal band measurements of Earth as part of the Landsat program. From first light in early 2013, there were obvious indications, such as non-uniform banding and varying absolute calibration errors, that stray light was contaminating the thermal image data collected from the instrument. Stray light in this case refers to unwanted radiance from outside the field-of-view entering the optical system and being recorded by the focal plane. Standard calibration techniques used to flat-field and radiometrically correct the data were not sufficient to adjust the image products to within the accuracy that the Landsat community has come to expect. The development of an operational technique to remove the effects of the stray light in the TIRS data has become a high priority. A methodology is presented that makes use of a stray light optical model developed for the instrument along with knowledge of the out-of-field area surrounding the TIRS earth scene. Two versions of the algorithm are proposed in which one method utilizes near-coincident image data from an external sensor while another novel method is proposed that makes use of TIRS image data itself without the need for external data. Preliminary results of the algorithm indicate that banding artifacts due to stray light are significantly reduced when the methods are applied. Additionally, initial absolute calibration error estimates of over 9K are reduced to within 2K when applying the correction methods. Although both variations of the proposed algorithm have significantly reduced the stray light effects, the fact that the latter method utilizing TIRS image data itself does not rely on any external data is a significant advantage toward the development of an operational stray light correction solution. Ongoing work is focused on operationalizing the algorithm and identifying and quantifying potential sources of error when applying the method. (C) 2015 Optical Society of America
C1 [Montanaro, Matthew; Gerace, Aaron] Rochester Inst Technol, Rochester, NY 14623 USA.
[Rohrbach, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Montanaro, M (reprint author), Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
EM montanaro@cis.rit.edu
FU Goddard Space Flight Center (GSFC), National Aeronautics and Space
Administration (NASA) [NNG09HP18C, NNX09AQ57A, NNX14AP40G]
FX Goddard Space Flight Center (GSFC), National Aeronautics and Space
Administration (NASA) (NNG09HP18C, NNX09AQ57A,NNX14AP40G).
NR 16
TC 4
Z9 4
U1 0
U2 7
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD MAY 1
PY 2015
VL 54
IS 13
BP 3963
EP 3978
DI 10.1364/AO.54.003963
PG 16
WC Optics
SC Optics
GA CH4DC
UT WOS:000353980900037
ER
PT J
AU Zhai, PW
Hu, YX
Trepte, CR
Winker, DM
Lucker, PL
Lee, ZP
Josset, DB
AF Zhai, Peng-Wang
Hu, Yongxiang
Trepte, Charles R.
Winker, David M.
Lucker, Patricia L.
Lee, Zhongping
Josset, Damien B.
TI Uncertainty in the bidirectional reflectance model for oceanic waters
SO APPLIED OPTICS
LA English
DT Article
ID ATMOSPHERIC CORRECTION; COLOR IMAGERY; DIFFUSE-REFLECTANCE; LEAVING
RADIANCE; PHASE FUNCTION; DETAILED VALIDATION; COUPLED ATMOSPHERE;
LIGHT-SCATTERING; SEAWIFS IMAGERY; MUELLER MATRIX
AB We study the impacts of the bio-optical model variations on the angular distribution (f/Q factor) of the upwelling radiance field in ocean waters. An ocean water bio-optical model has been combined with a vector radiative transfer model to calculate the f/Q factors systematically. The f/Q factors are compared to those in [Appl. Opt. 41, 6289 (2002)] and the differences are found to be within +/- 10% for 81% of the total number of cases covering all wavelengths, chlorophyll a concentrations, and solar and viewing geometries. The differences are attributed to the choice of ocean water scattering function and scattering coefficient biases. In addition, we study the uncertainty of f/Q factor due to three factors: (I) the absorption coefficient of the colored dissolved organic matter (CDOM), (II) the particle scattering coefficient, and (III) the ocean water depolarization. The impacts of ocean water depolarization on the f/Q variation is found to be negligible. If we perturb the CDOM absorption coefficient by a factor ranging from 0.1 to 10, the f/Q values vary within +/- 5% of the average behavior of ocean waters for 93% of the cases. If we perturb the scattering coefficients by a factor ranging from 0.5 to 2.0, the f/Q variation is within +/- 5% for 81% of the cases studied. This work contributes to understanding the uncertainty of ocean color remote sensing. (C) 2015 Optical Society of America
C1 [Zhai, Peng-Wang] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Hu, Yongxiang; Trepte, Charles R.; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Lucker, Patricia L.] NASA, Langley Res Ctr, SSAI, Hampton, VA 23681 USA.
[Lee, Zhongping] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
[Josset, Damien B.] NRL SSC, Stennis Space Ctr, MS 39529 USA.
RP Zhai, PW (reprint author), Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
EM pwzhai@umbc.edu
RI Hu, Yongxiang/K-4426-2012
FU NASA Radiation Science Program
FX This work was supported by the NASA Radiation Science Program
administrated by Hal Maring and the Biogeochemistry Program
administrated by Paula Bontempi. We appreciate the three anonymous
reviewers for their constructive comments.
NR 50
TC 4
Z9 4
U1 2
U2 8
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 MAY 1
PY 2015
VL 54
IS 13
BP 4061
EP 4069
DI 10.1364/AO.54.004061
PG 9
WC Optics
SC Optics
GA CH4DC
UT WOS:000353980900048
ER
PT J
AU Saif, B
Chaney, D
Smith, WS
Greenfield, P
Hack, W
Bluth, J
Van Otten, A
Bluth, M
Sanders, J
Keski-Kuha, R
Feinberg, L
North-Morris, M
Millerd, J
AF Saif, Babak
Chaney, David
Smith, W. Scott
Greenfield, Perry
Hack, Warren
Bluth, Josh
Van Otten, Austin
Bluth, Marcel
Sanders, James
Keski-Kuha, Ritva
Feinberg, Lee
North-Morris, Michael
Millerd, James
TI Nanometer level characterization of the James Webb Space Telescope
optomechanical systems using high-speed interferometry
SO APPLIED OPTICS
LA English
DT Article
AB The James Webb Space Telescope (JWST) Optical Telescope Element is a three mirror anastigmat consisting of a 6.5 m segmented primary mirror (PM), a secondary mirror, and a tertiary mirror. The primary mirror comprises 18 individual hexagonal segments. The telescope and instruments will be assembled at Goddard Space Flight Center (GSFC) to build the Optical Telescope Element-Integrated Science Instrument Module (OTIS). While at GSFC, the OTIS will go through a series of environmental tests. In these tests the OTIS will be exposed to launch level acoustics and vibrations. To assure that OTIS's performance has not changed due to these environmental tests, the assembly will be tested optically at the center of curvature of the PM. A high-speed interferometer has been designed and built to characterize both static and dynamic changes due to environmental exposure. This paper describes the details of these measurement techniques. To validate and develop the techniques that will be used on OTIS assembly two spare JWST PM segments were measured and the results presented here. (C) 2015 Optical Society of America
C1 [Saif, Babak; Keski-Kuha, Ritva; Feinberg, Lee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chaney, David] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
[Smith, W. Scott] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Greenfield, Perry; Hack, Warren] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bluth, Josh; Van Otten, Austin; Bluth, Marcel] ATK Space Syst, Magna, UT 84044 USA.
[Sanders, James] GSFC Vantage Syst Inc, Lanham, MD 20706 USA.
[North-Morris, Michael; Millerd, James] 4D Technol, Tucson, AZ 85706 USA.
RP Millerd, J (reprint author), 4D Technol, 3280 E Hemisphere Loop,Ste 146, Tucson, AZ 85706 USA.
EM james.millerd@4dtechnology.com
FU NASA's James Webb Space Telescope project
FX NASA's James Webb Space Telescope project.
NR 5
TC 2
Z9 2
U1 2
U2 8
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 MAY 1
PY 2015
VL 54
IS 13
BP 4285
EP 4298
DI 10.1364/AO.54.004285
PG 14
WC Optics
SC Optics
GA CH4DC
UT WOS:000353980900080
ER
PT J
AU Gundy-Burlet, K
AF Gundy-Burlet, Karen
TI The Use of Standards on the LADEE Mission
SO COMPUTER
LA English
DT Article
AB The Lunar Atmosphere Dust Environment Explorer (LADEE) software developers incorporated IEEE and other standards to achieve high reliability while adhering to strict budget and schedule guidelines.
C1 NASA, Washington, DC 20546 USA.
RP Gundy-Burlet, K (reprint author), NASA, Washington, DC 20546 USA.
EM karen.gundy-burlet@nasa.gov
NR 4
TC 0
Z9 0
U1 1
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 MAY
PY 2015
VL 48
IS 5
BP 92
EP 95
PG 4
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering
SC Computer Science
GA CJ0WV
UT WOS:000355201000018
ER
PT J
AU Yasumiishi, EM
Criddle, KR
Hillgruber, N
Mueter, FJ
Helle, JH
AF Yasumiishi, Ellen M.
Criddle, Keith R.
Hillgruber, Nicola
Mueter, Franz J.
Helle, John H.
TI Chum salmon (Oncorhynchus keta) growth and temperature indices as
indicators of the year-class strength of age-1 walleye pollock (Gadus
chalcogrammus) in the eastern Bering Sea
SO FISHERIES OCEANOGRAPHY
LA English
DT Article
DE indicators; recruitment; salmon; walleye pollock
ID OSCILLATING CONTROL HYPOTHESIS; NORTH PACIFIC-OCEAN;
THERAGRA-CHALCOGRAMMA; PINK SALMON; CLIMATE-CHANGE; SOCKEYE-SALMON;
BRISTOL BAY; ENVIRONMENT; VARIABILITY; GORBUSCHA
AB Ecosystem-based fisheries management requires the development of physical and biological time series that index ocean productivity for stock assessment and recruitment forecasts for commercially important species. As recruitment in marine fish is related to ocean condition, we developed proxies for ocean conditions based on sea surface temperature (SST) and biometric measurements of chum salmon (Oncorhynchus keta) captured in the walleye pollock (Gadus chalcogrammus) fishery in the eastern Bering Sea in three periods (July 16-30, September 1-15 and September 16-30). The main purpose of this paper was to evaluate Pacific salmon (Oncorhynchus spp.) growth as a possible indicator of ocean conditions that, in turn, may affect age-1 walleye pollock recruitment. Marine growth rates of Pacific salmon are the result of a complex interplay of physical, biological and population-based factors that fish experience as they range through oceanic habitats. These growth rates can, therefore, be viewed as indicators of recent ocean productivity. Thus, our hypothesis was that estimated intra-annual growth in body weight of immature and maturing age-4 male and female chum salmon may be used as a biological indicator of variations in rearing conditions also experienced by age-0 walleye pollock; consequently, they may be used to predict the recruitment to age-1 in walleye pollock. Summer SSTs and chum salmon growth at the end of July and September explained the largest amount of variability in walleye pollock recruitment indicating that physical and biological indices of ocean productivity can index fish recruitment.
C1 [Yasumiishi, Ellen M.; Criddle, Keith R.; Hillgruber, Nicola; Mueter, Franz J.; Helle, John H.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Yasumiishi, Ellen M.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, Juneau, AK 99801 USA.
[Hillgruber, Nicola] Thunen Inst Fisheries Ecol, D-22926 Ahrensburg, Germany.
RP Yasumiishi, EM (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM ellen.yasumiishi@noaa.gov
RI Criddle, Keith/P-7080-2016
OI Criddle, Keith/0000-0001-9347-2944
FU Auke Bay Laboratories; National Marine Fisheries, National Oceanic and
Atmospheric Administration (NOAA); NOAA Advanced Studies Program,
Professional Development program
FX Funding for this project was provided by the Auke Bay Laboratories,
National Marine Fisheries, National Oceanic and Atmospheric
Administration (NOAA) and the NOAA Advanced Studies Program,
Professional Development program. We greatly appreciate the time and
effort to collect samples made by the observers onboard the commercial
fishing vessels. We also thank the anonymous reviewers for their
comments.
NR 52
TC 0
Z9 0
U1 2
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1054-6006
EI 1365-2419
J9 FISH OCEANOGR
JI Fish Oceanogr.
PD MAY
PY 2015
VL 24
IS 3
BP 242
EP 256
DI 10.1111/fog.12108
PG 15
WC Fisheries; Oceanography
SC Fisheries; Oceanography
GA CJ1WH
UT WOS:000355275100004
ER
PT J
AU Brune, AJ
West, TK
Hosder, S
Edquist, KT
AF Brune, Andrew J.
West, Thomas K.
Hosder, Serhat
Edquist, Karl T.
TI Uncertainty Analysis of Mars Entry Flows over a Hypersonic Inflatable
Aerodynamic Decelerator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID POLYNOMIAL CHAOS; SENSITIVITY-ANALYSIS; EARTH ENTRY
AB A detailed uncertainty analysis for high-fidelity flowfield simulations over a fixed aeroshell of hypersonic inflatable aerodynamic decelerator scale for Mars entry is presented for fully laminar and turbulent flows at peak stagnation-point heating conditions. This study implements a sparse-collocation approach based on stochastic expansions for efficient and accurate uncertainty quantification under a large number of uncertainty sources in the computational model. The convective and radiative heating and shear stress uncertainties are computed over the hypersonic inflatable aerodynamic decelerator surface and are shown to vary due to a small fraction of 65 flowfield and radiation modeling parameters considered in the uncertainty analysis. The main contributors to the convective heating uncertainty near the stagnation point are the CO2-CO2, CO2-O, and CO-O binary collision interactions, freestream density, and freestream velocity for both boundary-layer flows. In laminar flow, exothermic recombination reactions are more important at the shoulder. The main contributors to radiative heating at the nose and flank were the CO2 dissociation rate and CO heavy-particle excitation rates, whereas the freestream density showed importance toward the shoulder. The CO2-CO2 interaction and freestream velocity and density control the wall shear stress uncertainty.
C1 [Brune, Andrew J.; West, Thomas K.] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[Hosder, Serhat] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Aerosp Engn, Rolla, MO 65409 USA.
[Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Engn Directorate, Hampton, VA 23681 USA.
RP Brune, AJ (reprint author), Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
FU NASA Space Technology Research Fellowship [NNX13AL58H]
FX This work was supported by a NASA Space Technology Research Fellowship
under training project grant NNX13AL58H (Serhat Hosder, principal
investigator, and Karl Edquist, research collaborator). The authors
would like to thank Christopher O. Johnston for his expert opinion and
discussions of the shock-layer radiation modeling for the current
project.
NR 19
TC 2
Z9 2
U1 0
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY
PY 2015
VL 52
IS 3
BP 776
EP 788
DI 10.2514/1.A33131
PG 13
WC Engineering, Aerospace
SC Engineering
GA CI8DC
UT WOS:000354997900013
ER
PT J
AU Milos, FS
Gasch, MJ
Prabhu, DK
AF Milos, Frank S.
Gasch, Matthew J.
Prabhu, Dinesh K.
TI Conformal Phenolic Impregnated Carbon Ablator Arcjet Testing, Ablation,
and Thermal Response
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB A new conformal type of phenolic impregnated carbon ablator was manufactured by resin impregnation of carbon felt. Based on property measurements of the conformal material and the existing model for a standard, rigid phenolic impregnated carbon ablator, a midfidelity material response model for the conformal material was developed. The rigid and conformal materials were arcjet tested simultaneously on a sphere-cone geometry in several environments with frustum heat flux up to 380W/cm2. Good agreement between the predictions and data was obtained for recession, surface temperature, and in-depth temperatures. The conformal material has a slightly greater ablation rate but significantly lower thermal diffusivity than the rigid material.
C1 [Milos, Frank S.; Gasch, Matthew J.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Prabhu, Dinesh K.] ERC Inc, Entry Syst Technol Div, Moffett Field, CA 94035 USA.
RP Milos, FS (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA.
FU Fundamental Aeronautics Program; Space Technology Program
FX This work was supported by both the Fundamental Aeronautics Program and
the Space Technology Program. The authors thank Parul Agrawal for the
arcjet test data, Robin Beck for overall management, and Mairead
Stackpoole for laboratory data.
NR 7
TC 1
Z9 1
U1 1
U2 17
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY
PY 2015
VL 52
IS 3
BP 804
EP 812
DI 10.2514/1.A33216
PG 9
WC Engineering, Aerospace
SC Engineering
GA CI8DC
UT WOS:000354997900015
ER
PT J
AU Osipov, V
Khasin, M
Hafiychuk, H
Muratov, C
Watson, M
Smelyanskiy, V
AF Osipov, Viatcheslav
Khasin, Michael
Hafiychuk, Halyna
Muratov, Cyrill
Watson, Michael
Smelyanskiy, Vadim
TI Mitigation of Solid Booster Ignition over Pressure by Water Aerosol
Sprays
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID LIQUID SHEETS; OVERPRESSURE; DROP; SIZE; SUSPENSIONS; RELAXATION;
BREAKUP; SOUND
AB Interaction of acoustic waves with water aerosol layers is analyzed in the context of the problem of solid booster ignition overpressure suppression. In contrast to the conventional approach to ignition overpressure suppression, which aims at using water to quench the sources of the ignition overpressure waves, this study focuses on blocking the ignition overpressure wave propagation, using reflection and attenuation of the wave by the water aerosol layers. The study considers interaction of the waves with aerosol layers of large mass loading for varying sizes of the droplets. The size of the droplets is shown to substantially affect the mechanisms of interaction with the waves. The criteria for the crossover between different mechanisms are established as functions of the droplet size and the ignition overpressure wave parameters. The optimal parameters and designs for water aerosol sprays are proposed that maximize the ignition overpressure suppression. These results were obtained using the nozzle and the exhaust hole geometries similar to those of the space shuttle. Remarkably, it is found that various a priori reasonable designs of the aerosol and water sprays may increase the ignition overpressure impact on the vehicle, increasing the risk of vehicle damage.
C1 [Osipov, Viatcheslav; Khasin, Michael; Hafiychuk, Halyna] NASA, Stinger Ghaffarian Technol Inc, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA.
[Muratov, Cyrill] New Jersey Inst Technol, Appl Phys Grp, Newark, NJ 07102 USA.
[Watson, Michael] NASA, George C Marshall Space Flight Ctr, Dept Math Sci, Huntsville, AL 35812 USA.
[Smelyanskiy, Vadim] NASA, Ames Res Ctr, Syst Engn, Moffett Field, CA 94035 USA.
RP Osipov, V (reprint author), NASA, Stinger Ghaffarian Technol Inc, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA.
NR 32
TC 0
Z9 0
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY
PY 2015
VL 52
IS 3
BP 928
EP 943
DI 10.2514/1.A33110
PG 16
WC Engineering, Aerospace
SC Engineering
GA CI8DC
UT WOS:000354997900025
ER
PT J
AU Qian, J
Wang, Y
Song, HJ
Pant, K
Peabody, H
Ku, JT
Butler, CD
AF Qian, Jing
Wang, Yi
Song, Hongjun
Pant, Kapil
Peabody, Hume
Ku, Jentung
Butler, Charles D.
TI Projection-Based Reduced-Order Modeling for Spacecraft Thermal Analysis
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID PIECEWISE-LINEAR APPROACH; REDUCTION; SYSTEMS; APPROXIMATIONS; DEVICES;
DESIGN; LISA
AB This paper presents a mathematically rigorous, subspace projection-based reduced-order modeling methodology and an integrated framework to automatically generate reduced-order models for spacecraft thermal analysis. Two key steps in the reduced-order modeling procedure are described: first, the acquisition of a full-scale spacecraft model in the ordinary differential equation, and differential algebraic equation, forms to resolve its dynamic thermal behavior; and second, reduced-order modeling to markedly reduce the dimension of the full-scale model. Specifically, proper orthogonal decomposition in conjunction with a discrete empirical interpolation method and trajectory piecewise-linear methods are developed to address the strong nonlinear thermal effects due to coupled conductive and radiative heat transfer in the spacecraft environment. Case studies using NASA-relevant satellite models are undertaken to verify the capability and to assess the computational performance of the reduced-order modeling technique in terms of speedup and error relative to the full-scale model. Reduced-order modeling exhibits excellent agreement in spatiotemporal thermal profiles (less than 0.5% relative error in pertinent timescales) along with salient computational acceleration (up to two orders of magnitude speedup) over the full-scale analysis. These findings establish the feasibility of reduced-order modeling to perform rational and computationally affordable thermal analysis, develop reliable thermal control strategies for spacecraft, and greatly reduce the development cycle times and costs.
C1 [Qian, Jing; Wang, Yi; Song, Hongjun; Pant, Kapil] CFD Res Corp, Biomed & Energy Technol, Huntsville, AL 35806 USA.
[Peabody, Hume; Ku, Jentung; Butler, Charles D.] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA.
RP Wang, Y (reprint author), CFD Res Corp, Biomed & Energy Technol, 701 McMillian Way, Huntsville, AL 35806 USA.
EM yi.wang@cfdrc.com
FU NASA [NNX11CB02C]
FX This research is sponsored by NASA under contract number NNX11CB02C.
NR 24
TC 2
Z9 2
U1 3
U2 7
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY
PY 2015
VL 52
IS 3
BP 978
EP 989
DI 10.2514/1.A33117
PG 12
WC Engineering, Aerospace
SC Engineering
GA CI8DC
UT WOS:000354997900029
ER
PT J
AU Bykov, AM
Churazov, EM
Ferrari, C
Forman, WR
Kaastra, JS
Klein, U
Markevitch, M
de Plaa, J
AF Bykov, A. M.
Churazov, E. M.
Ferrari, C.
Forman, W. R.
Kaastra, J. S.
Klein, U.
Markevitch, M.
de Plaa, J.
TI Structures and Components in Galaxy Clusters: Observations and Models
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Clusters of galaxies; Radiation mechanisms: non-thermal; Radio
continuum; X-rays: galaxies: clusters
ID ACTIVE GALACTIC NUCLEI; DIFFUSIVE SHOCK ACCELERATION; X-RAY-LINES;
MAGNETIC-FIELD AMPLIFICATION; XMM-NEWTON OBSERVATIONS; MASSIVE
BLACK-HOLES; COOLING FLOWS; PERSEUS CLUSTER; RESONANT SCATTERING;
ELLIPTIC GALAXIES
AB Clusters of galaxies are the largest gravitationally bounded structures in the Universe dominated by dark matter. We review the observational appearance and physical models of plasma structures in clusters of galaxies. Bubbles of relativistic plasma which are inflated by supermassive black holes of AGNs, cooling and heating of the gas, large scale plasma shocks, cold fronts, non-thermal halos and relics are observed in clusters. These constituents are reflecting both the formation history and the dynamical properties of clusters of galaxies. We discuss X-ray spectroscopy as a tool to study the metal enrichment in clusters and fine spectroscopy of Fe X-ray lines as a powerful diagnostics of both the turbulent plasma motions and the energetics of the non-thermal electron populations. The knowledge of the complex dynamical and feedback processes is necessary to understand the energy and matter balance as well as to constrain the role of the non-thermal components of clusters.
C1 [Bykov, A. M.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Bykov, A. M.] St Petersburg State Politecn Univ, St Petersburg, Russia.
[Bykov, A. M.] Int Space Sci Inst, Bern, Switzerland.
[Churazov, E. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Churazov, E. M.] Space Res Inst IKI, Moscow 117997, Russia.
[Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, CNRS,UMR7293, F-06300 Nice, France.
[Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kaastra, J. S.; de Plaa, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Klein, U.] Univ Bonn, Argelander Inst Astron, Bonn, Germany.
[Markevitch, M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Bykov, AM (reprint author), AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
EM byk@astro.ioffe.ru; churazov@mpa-garching.mpg.de; chiara.ferrari@oca.eu;
forman@cfa.harvard.edu; j.kaastra@sron.nl; uklein@astro.uni-bonn.de;
maxim.markevitch@nasa.gov; J.de.Plaa@sron.nl
RI Bykov, Andrei/E-3131-2014; Churazov, Eugene/A-7783-2013;
OI Forman, William/0000-0002-9478-1682
FU NASA [NASA-03060]; Chandra HRC project; Chandra archive grant
[AR1-12007X]; NASA observing grant [GO2-13005X]; NWO (the Netherlands
Organization for Scientific Research)
FX We would like to thank the referee for useful comments and the ISSI
staff for providing an inspiring atmosphere favorable for intense
discussions. We thank Hiroki Akamatsu for providing us with Fig. 21
before publication. W. Forman acknowledges support from NASA contract
NASA-03060 that funds the Chandra HRC project, the Chandra archive grant
AR1-12007X, and the NASA observing grant GO2-13005X. SRON is financially
supported by NWO (the Netherlands Organization for Scientific Research).
NR 202
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAY
PY 2015
VL 188
IS 1-4
BP 141
EP 185
DI 10.1007/s11214-014-0129-4
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ0FO
UT WOS:000355151400005
ER
PT J
AU Fletcher, L
Cargill, PJ
Antiochos, SK
Gudiksen, BV
AF Fletcher, L.
Cargill, P. J.
Antiochos, S. K.
Gudiksen, B. V.
TI Structures in the Outer Solar Atmosphere
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun; Corona; Hard X-rays
ID CORONAL MAGNETIC-FIELDS; X-RAY-EMISSION; FREQUENCY ACOUSTIC-WAVES; MASS
EJECTIONS; ENERGY-RELEASE; ACTIVE-REGION; FLUX ROPES; QUIET SUN;
PARTICLE-ACCELERATION; FILAMENT ERUPTIONS
AB The structure and dynamics of the outer solar atmosphere are reviewed with emphasis on the role played by the magnetic field. Contemporary observations that focus on high resolution imaging over a range of temperatures, as well as UV, EUV and hard X-ray spectroscopy, demonstrate the presence of a vast range of temporal and spatial scales, mass motions, and particle energies present. By focusing on recent developments in the chromosphere, corona and solar wind, it is shown that small scale processes, in particular magnetic reconnection, play a central role in determining the large-scale structure and properties of all regions. This coupling of scales is central to understanding the atmosphere, yet poses formidable challenges for theoretical models.
C1 [Fletcher, L.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Cargill, P. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys, London SW7 2BZ, England.
[Cargill, P. J.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gudiksen, B. V.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Gudiksen, B. V.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway.
RP Fletcher, L (reprint author), Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
EM lyndsay.fletcher@glasgow.ac.uk
FU STFC [ST/I001808/1]; NASA TRT Program; NASA SRT Program
FX We thank Andre Balogh for organizing this workshop and ISSI staff for
their hospitality. The work of L. Fletcher has been supported by STFC
grant ST/I001808/1 and that of S. Antiochos has been supported by the
NASA TR&T and SR&T Programs.
NR 202
TC 6
Z9 6
U1 2
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAY
PY 2015
VL 188
IS 1-4
BP 211
EP 249
DI 10.1007/s11214-014-0111-1
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CJ0FO
UT WOS:000355151400007
ER
PT J
AU Nathal, M
AF Nathal, Mike
TI ADVANCED TURBINE AIRFOIL DEVELOPMENT STRATEGIES: HARVESTING LOW-HANGING
FRUIT
SO ADVANCED MATERIALS & PROCESSES
LA English
DT Article
ID TENSILE PROPERTIES; BARRIER COATINGS; ALLOYS; CREEP; BEHAVIOR
C1 [Nathal, Mike] NASA Glenn Res Ctr, Adv Metall Branch, Struct & Mat Div, Cleveland, OH USA.
EM miken345@wowway.com
NR 31
TC 0
Z9 0
U1 0
U2 1
PU ASM INT
PI MATERIALS PARK
PA SUBSCRIPTIONS SPECIALIST CUSTOMER SERVICE, MATERIALS PARK, OH 44073-0002
USA
SN 0882-7958
EI 2161-9425
J9 ADV MATER PROCESS
JI Adv. Mater. Process.
PD MAY
PY 2015
VL 173
IS 5
BP 21
EP 24
PG 4
WC Materials Science, Multidisciplinary
SC Materials Science
GA CI3OL
UT WOS:000354657000003
ER
PT J
AU Righter, K
AF Righter, Kevin
TI Modeling siderophile elements during core formation and accretion, and
the role of the deep mantle and volatiles
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Core; mantle; magma ocean; siderophile; volatile; accretion
ID SILICATE PARTITION-COEFFICIENTS; TERRESTRIAL MAGMA OCEAN; HIGH-PRESSURE;
EARTHS CORE; OXYGEN FUGACITY; NITROGEN SOLUBILITY; TRACE-ELEMENTS;
LIQUID-METAL; SULFIDE MELT; REDOX STATE
AB The last decade has seen general agreement that moderately siderophile elements (MSE) in Earth's primitive upper mantle (PUM) can be explained by metal-silicate equilibrium at mid-mantle depths in an early Earth magma ocean environment. Despite the agreement, there are some differences in the detailed modeling that has been carried out. This paper will examine siderophile element metal/silicate partitioning with respect to three different topics: (1) an examination of aspects of the modeling that one might suspect leads to differences in outcomes or in comparison between models, but actually are in agreement with experimental data and between models; (2) a discussion of the role of the deep mantle in modeling efforts; and (3) the role and/or fate of volatiles in magma ocean scenarios with an emphasis on where data are lacking.
C1 NASA JSC, Mailcode KT, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA JSC, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU NASA Cosmochemistry program through an RTOP
FX The author thanks H. Watson and T. Rushmer for the invitation to write
this manuscript for the special issue. K.R. is funded by the NASA
Cosmochemistry program through an RTOP. Comments and suggestions of an
anonymous reviewer and A. Bouhifd helped improve the presentation of
this work.
NR 113
TC 5
Z9 6
U1 3
U2 21
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2015
VL 100
IS 5-6
BP 1098
EP 1109
DI 10.2138/am-2015-5052
PG 12
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CI3RS
UT WOS:000354665700013
ER
PT J
AU Martin, AM
Medard, E
Devouard, B
Keller, LP
Righter, K
Devidal, JL
Rahman, Z
AF Martin, Audrey M.
Medard, Etienne
Devouard, Bertrand
Keller, Lindsay P.
Righter, Kevin
Devidal, Jean-Luc
Rahman, Zia
TI Fayalite oxidation processes in Obsidian Cliffs rhyolite flow, Oregon
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Olivine; fayalite; laihunite; oxyfayalite; rhyolite; lithophysae;
oxidation
ID TEMPERATURE CRYSTAL-CHEMISTRY; ELECTRON-MICROPROBE; OXIDIZED OLIVINE;
TOPAZ RHYOLITES; KINETICS; STABILITY; LAIHUNITE; ENERGY; IRON;
SPECTROSCOPY
AB This study investigates the oxidation of fayalite Fe22+SiO4 that is present in lithophysae from a rhyolite flow (Obsidian Cliffs, Oregon). Textural, chemical, and structural analyses of the successive oxidation zones are used to constrain: ( I) the oxidation processes of olivine, and (2) the role of temperature, chemical diffusion, and meteoric infiltration. Petrologic analyses and thermodynamic modeling show that the rhyolite flow emplaced at 800-950 degrees C. Fayalite-bearing lithophysae formed only in the core of the lava flow. Variations in the gas composition inside the lithophysae induced the oxidation of fayalite to a laihunite-1M zone Fe12+Fe23+square(1)(SiO4)(2). This zone is made of nano-lamellae of amorphous silica SiO2 and laihunite-3MFe(1.6)(2+)Fe(1.6)(3+)square(0.8)(SiO4)(2)+ hematite Fe2O3. It probably formed by a nucleation and growth process in the fayalite fractures and defects and at fayalite crystal edges. The laihunite-1M zone then oxidized into an "oxyfayalite" zone with the composition Fe0.522+Fe2.323+square(1.16)(SiO4)(2). This second oxidation zone is made of lamellae of amorphous silica SiO2 and hematite Fe2O3, with a possible small amount of ferrosilite Fe2+SiO3. A third and outer zone, composed exclusively of hematite, is also present. The successive oxidation zones suggest that there may be a mineral in the olivine group with higher Fe3+ content than laihunite-1M. The transformation of laihunite-1M to this "oxyfayalite" phase could occur by a reaction such as
0.24Fe(M1)(2+laihunite-1M) + 0.06O(2) = 0.16 Fe-M1(3+"oxyfayalite") + 0.08 square("oxyfayalite") + 0.04 (Fe23+O3hematite)
This would imply that Fe3+ can also be incorporated in the M1 site of olivine.
C1 [Martin, Audrey M.; Keller, Lindsay P.; Righter, Kevin; Rahman, Zia] NASA, Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
[Martin, Audrey M.] Case Western Reserve Univ, Earth Environm & Planetary Sci, Cleveland, OH 44118 USA.
[Medard, Etienne; Devouard, Bertrand; Devidal, Jean-Luc] Univ Clermont Ferrand, CNRS, IRD, Lab Magmas & Volcans, F-63038 Clermont Ferrand, France.
[Devouard, Bertrand] CNRS, IRD, AMU, CEREGE,UM34, F-13545 Aix En Provence, France.
RP Martin, AM (reprint author), NASA, Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM audrey.martin@case.edu
OI Martin, Audrey/0000-0002-1165-8866; Medard, Etienne/0000-0002-7040-7442;
DEVOUARD, Bertrand/0000-0002-8774-1842
FU Johnson Space Center
FX The authors thank D. Howard for providing some of the Obsidian Cliffs
rhyolites samples. Yann Morizet, Jonathan Castro, and an anonymous
reviewer are gratefully acknowledged for their insightful and
constructive comments. This research was supported by an appointment to
the NASA Postdoctoral Program at the Johnson Space Center, administered
by Oak Ridge Associated Universities through a contract with NASA.
NR 72
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U1 6
U2 14
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2015
VL 100
IS 5-6
BP 1153
EP 1164
DI 10.2138/am-2015-5042
PG 12
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CI3RS
UT WOS:000354665700017
ER
PT J
AU Collazzi, AC
Kouveliotou, C
van der Horst, AJ
Younes, GA
Kaneko, Y
Gogus, E
Lin, L
Granot, J
Finger, MH
Chaplin, VL
Huppenkothen, D
Watts, AL
von Kienlin, A
Baring, MG
Gruber, D
Bhat, PN
Gibby, MH
Gehrels, N
McEnery, J
van der Klis, M
Wijers, RAMJ
AF Collazzi, A. C.
Kouveliotou, C.
van der Horst, A. J.
Younes, G. A.
Kaneko, Y.
Gogus, E.
Lin, L.
Granot, J.
Finger, M. H.
Chaplin, V. L.
Huppenkothen, D.
Watts, A. L.
von Kienlin, A.
Baring, M. G.
Gruber, D.
Bhat, P. N.
Gibby, M. H.
Gehrels, N.
McEnery, J.
van der Klis, M.
Wijers, R. A. M. J.
TI THE FIVE YEAR FERMI/GBM MAGNETAR BURST CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; pulsars: individual (SGR J1550-5418, SGR J0501+4516,
1E1841-045, SGR J0418+5729, SGR 1806-20, SGR J1822.3-1606, AXP 4U
0142+61, AXP 1E 2259+586, 3XMM J185246.6+0033.7); stars: neutron;
X-rays: bursts
ID SOFT GAMMA REPEATER; X-RAY PULSAR; QUASI-PERIODIC OSCILLATIONS; SGR
J1550-5418 BURSTS; HIGH-ENERGY TRANSIENT; 1E 1547.0-5408; ACTIVE
EPISODE; MONITOR; DISCOVERY; EMISSION
AB Since launch in 2008, the Fermi Gamma-ray Burst Monitor (GBM) has detected many hundreds of bursts from magnetar sources. While the vast majority of these bursts have been attributed to several known magnetars, there is also a small sample of magnetar-like bursts of unknown origin. Here, we present the Fermi/GBM magnetar catalog, providing the results of the temporal and spectral analyses of 440 magnetar bursts with high temporal and spectral resolution. This catalog covers the first five years of GBM magnetar observations, from 2008 July to 2013 June. We provide durations, spectral parameters for various models, fluences, and peak fluxes for all the bursts, as well as a detailed temporal analysis for SGR J1550-5418 bursts. Finally, we suggest that some of the bursts of unknown origin are associated with the newly discovered magnetar 3XMM J185246.6+0033.7.
C1 [Collazzi, A. C.] SciTec Inc, Princeton, NJ 08540 USA.
[Kouveliotou, C.; van der Horst, A. J.; Younes, G. A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA.
[Younes, G. A.; Finger, M. H.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Kaneko, Y.; Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Lin, L.] APC, Francois Arago Ctr, F-75205 Paris, France.
[Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel.
[Chaplin, V. L.] Vanderbilt Univ, Sch Med, Nashville, TN 37232 USA.
[Huppenkothen, D.] NYU, Ctr Data Sci, New York, NY 10003 USA.
[Huppenkothen, D.] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA.
[Watts, A. L.; van der Klis, M.; Wijers, R. A. M. J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands.
[von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Gruber, D.] Planetarium Sudtirol, I-39053 Karneid, Italy.
[Bhat, P. N.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Gibby, M. H.] Jacobs Technol Inc, Huntsville, AL USA.
[Gehrels, N.; McEnery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Collazzi, AC (reprint author), SciTec Inc, 100 Wall St, Princeton, NJ 08540 USA.
EM acollazzi@scitec.com
OI Wijers, Ralph/0000-0002-3101-1808
FU NASA [NNH07ZDA001-GLAST]; NASA Postdoctoral Program at the Marshall
Space Flight Center; Moore-Sloan Data Science Environment at New York
University; Netherlands Organization for Scientific Research (NWO) Vidi
Fellowship; Bundesministeriums fur Wirtschaft und Technologie (BMWi)
through DLR [50 OG 1101]; Netherlands Organisation for Scientific
Research (NWO); Royal Netherlands Academy of Arts and Sciences (KNAW)
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST, PI: C. Kouveliotou). A.C.C. was supported by an
appointment to the NASA Postdoctoral Program at the Marshall Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. C.K. and G.A.Y. acknowledge support from NASA
grant NNH07ZDA001-GLAST. D.H. was supported by the Moore-Sloan Data
Science Environment at New York University. A.L.W. acknowledges support
from a Netherlands Organization for Scientific Research (NWO) Vidi
Fellowship. A.v.K. was supported by the Bundesministeriums fur
Wirtschaft und Technologie (BMWi) through DLR grant 50 OG 1101. M.v.d.K.
acknowledges support from the Netherlands Organisation for Scientific
Research (NWO) and the Royal Netherlands Academy of Arts and Sciences
(KNAW).
NR 71
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U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAY
PY 2015
VL 218
IS 1
AR 11
DI 10.1088/0067-0049/218/1/11
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI8DN
UT WOS:000354999200011
ER
PT J
AU Sacchi, C
Bhasin, K
Kadowaki, N
Vong, F
AF Sacchi, Claudio
Bhasin, Kul
Kadowaki, Naoto
Vong, Fred
TI TECHNOLOGIES AND APPLICATIONS OF FUTURE SATELLITE NETWORKING
SO IEEE COMMUNICATIONS MAGAZINE
LA English
DT Editorial Material
C1 [Sacchi, Claudio] Univ Trento, Fac Engn, Trento, Italy.
[Bhasin, Kul] NASA Glenn Res Ctr, Cleveland, OH USA.
[Bhasin, Kul] Space Commun Projects NASA GRC, San Diego, CA USA.
[Bhasin, Kul] AIAA, San Diego, CA USA.
[Bhasin, Kul] SPIE, Bellingham, WA USA.
[Kadowaki, Naoto] Strateg Planning Dept NICT, Koganei, Tokyo, Japan.
[Kadowaki, Naoto] Wireless Network Res Inst NICT, Yokosuka, Kanagawa, Japan.
[Vong, Fred] Asia Satellite Telecommun Co Ltd, Engn, Hong Kong, Hong Kong, Peoples R China.
RP Sacchi, C (reprint author), Univ Trento, Dept Comp Sci & Informat Engn, Trento, Italy.
EM sacchi@disi.unitn.it
NR 0
TC 0
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U1 3
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0163-6804
EI 1558-1896
J9 IEEE COMMUN MAG
JI IEEE Commun. Mag.
PD MAY
PY 2015
VL 53
IS 5
BP 154
EP 155
PG 2
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA CI1CV
UT WOS:000354479400018
ER
PT J
AU Chen, TY
Vakilinia, K
Divsalar, D
Wesel, RD
AF Chen, Tsung-Yi
Vakilinia, Kasra
Divsalar, Dariush
Wesel, Richard D.
TI Protograph-Based Raptor-Like LDPC Codes
SO IEEE TRANSACTIONS ON COMMUNICATIONS
LA English
DT Article
DE Channel coding; low-density parity-check codes
ID PARITY-CHECK CODES; DESIGN; COMPLEXITY; CAPACITY; CONSTRUCTION;
PERFORMANCE
AB This paper proposes protograph-based Raptor-like (PBRL) codes as a class of rate-compatible low-density parity-check codes for binary-input AWGN channels. As with the Raptor codes, exclusive-OR operations on precoded bits produce additional parity bits providing extensive rate compatibility. Unlike Raptor codes, each additional parity bit in the protograph is explicitly designed to optimize the density evolution threshold. During the lifting process, approximate cycle extrinsic message degree (ACE) and circulant progressive edge growth (CPEG) constraints are used to avoid undesirable graphical structures. Some density-evolution performance is sacrificed to obtain lower error floors, particularly at short blocklengths. Simulation results are shown for information block sizes of k = 1032 and 16 384. For a target frame error rate of 10(-5), at each rate, the k = 1032 and 16 384 code families perform within 1 dB and 0.4 dB of both the Gallager bound and the normal approximation, respectively. The 16 384 code family outperforms the best known standardized code family, namely, the AR4JA codes. The PBRL codes also outperform DVB-S2 codes that have the advantages of longer blocklengths and outer BCH codes. Performance is similar to RC code families designed by Nguyen et al. that do not constrain codes to have the PBRL structure and involve simulation in the optimization process at each rate.
C1 [Chen, Tsung-Yi] SpiderCloud Wireless Inc, San Jose, CA 95134 USA.
[Vakilinia, Kasra; Divsalar, Dariush; Wesel, Richard D.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Wesel, Richard D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chen, TY (reprint author), SpiderCloud Wireless Inc, San Jose, CA 95134 USA.
EM tsungyi.chen@engineering.ucla.edu; vakiliniak@ucla.edu;
Dariush.Divsalar@jpl.nasa.gov; wesel@ee.ucla.edu
FU National Science Foundation [1162501, 1161822, 82-17473]
FX This material is based upon work supported by the National Science
Foundation under Grants 1162501 and 1161822 (JPL Task Plan 82-17473).
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. This research was carried
out in part at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Parts of this work were
presented at the Global Communications Conference 2011 and the
International Conference on Communications 2012. The editor coordinating
the review of this paper and approving it for publication was M.
Lentmaier. (Tsung-Yi Chen and Kasra Vakilinia contributed equally to
this work.)
NR 56
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U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0090-6778
EI 1558-0857
J9 IEEE T COMMUN
JI IEEE Trans. Commun.
PD MAY
PY 2015
VL 63
IS 5
BP 1522
EP 1532
DI 10.1109/TCOMM.2015.2404842
PG 11
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA CI7LE
UT WOS:000354944100003
ER
PT J
AU Choi, S
Mulfinger, DG
Robinson, JE
Capozzi, BJ
AF Choi, Seongim
Mulfinger, Daniel G.
Robinson, John E., III
Capozzi, Brian J.
TI Design of an Optimal Route Structure Using Heuristics-Based Stochastic
Schedulers
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB The purpose of the current study is to identify key parameters and provide reasonable guidelines for the design of an efficient route structure in the extended terminal airspace area under dense air traffic flows. First, various scheduling algorithms, including a first-come/first-served and mixed-integer linear programming, are compared in terms of efficiency and optimality of scheduling performance. To further improve the efficiency of the scheduling algorithms, heuristics based on the first-come/first-served and genetic algorithms are adopted and quickly predetermine the aircraft sequences at the scheduling point. Subsequently, a dynamic planning framework is constructed to provide a more practical scheduling strategy for realistic operation, and it effectively handles the dynamic situations of traffic flows under uncertainties in weather and operations. It is an integrated framework that iteratively executes a flight trajectory model and the scheduling algorithms. As a practical application of the proposed scheduling strategy to the dense terminal environment, a design of an optimal route structure is carried out where the terminal airspace is represented in Cartesian coordinates. The sensitivities of the scheduling performance with respect to the uncertainty quantification and propagation models are investigated in more general airspace topology by varying merge point locations and their numbers.
C1 [Choi, Seongim] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24060 USA.
[Mulfinger, Daniel G.; Robinson, John E., III] NASA, Ames Res Ctr, Airspace Syst Div, Moffett Field, CA 94035 USA.
[Capozzi, Brian J.] Mosa ATM, Leesburg, VA 20175 USA.
RP Choi, S (reprint author), Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24060 USA.
NR 18
TC 0
Z9 0
U1 3
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 764
EP 777
DI 10.2514/1.C032645
PG 14
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400004
ER
PT J
AU Wu, MHG
Green, SM
Jones, J
AF Wu, Minghong G.
Green, Steven M.
Jones, James
TI Strategies for Choosing Descent Flight-Path Angles for Small Jets
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID INTERNATIONAL-AIRPORT; ARRIVALS; DESIGN
AB A standard descent procedure with a fixed flight-path angle is proposed to improve trajectory predictability for arriving small jets in the transition airspace into congested terminal area. Three candidate strategies for selecting fuel-efficient and flyable descent flight-path angles are proposed. The three strategies vary in operational complexity and fuel-burn merits. To mitigate variation of wind among flights, the two simpler strategies are adapted to airport, directions of arrival, and time. Three major U.S. airports with different degrees of wind variation and disparate arrival traffic flows are analyzed. Results show that, when compared to the simple airport-static adaptation, the finest adaptation of the simpler strategies recover up to 50-75% of the extra fuel burn relative to the minimum-fuel strategy. Wind variation, descent altitude restrictions, arrival directions, and fleet composition all affect the fuel efficiency of the simple strategies. Tradeoffs between fuel burn and planned speed-brake usage in the choice of the flight-path angle are discussed. Fuel efficiency of simple strategies for the entire national airspace in the United States is estimated. Considerations and implications for air navigation service providers are discussed.
C1 [Wu, Minghong G.] Univ Calif Santa Cruz, Santa Cruz, CA 94035 USA.
[Green, Steven M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jones, James] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA.
RP Wu, MHG (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 94035 USA.
NR 34
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U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 847
EP 866
DI 10.2514/1.C032835
PG 20
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400011
ER
PT J
AU Bui, TT
AF Bui, Trong T.
TI Analysis of Stall Aerodynamics of a Swept Wing with Laminar-Flow Glove
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB Reynolds-averaged Navier-Stokes computational-fluid-dynamics analysis was conducted to study the low-speed stall aerodynamics of a business jet's swept wing modified with a laminar-flow wing glove. The stall aerodynamics of the gloved wing were analyzed and compared with the unmodified wing for the flight speed of 120 kt and altitude of 2300 ft above mean sea level. A polyhedral finite-volume unstructured Navier-Stokes computational-fluid-dynamics code was used in the analysis. This computational-fluid-dynamics code was first validated for wing stall predictions using the wing-body geometry from the First AIAA Computational Fluid Dynamics High-Lift Prediction Workshop. It was found that the computational-fluid-dynamics code under consideration can produce results that are within the scattering of other computational-fluid-dynamics codes considered at the workshop. In particular, the polyhedral computational-fluid-dynamics code was able to predict wing stall for the AIAA wing-body geometry to within 1 deg of angle of attack as compared to benchmark wind-tunnel test data. Computational-fluid-dynamics results show that the addition of the laminar-flow wing glove causes the gloved wing to stall much earlier than the unmodified wing. Furthermore, the gloved wing has a different stall characteristic than the clean wing, with no sharp lift dropoff at stall for the gloved wing.
C1 NASA, Armstrong Flight Res Ctr, Aerodynam & Prop Branch, Edwards AFB, CA 93523 USA.
RP Bui, TT (reprint author), NASA, Armstrong Flight Res Ctr, Aerodynam & Prop Branch, POB 273-MS 4840B, Edwards AFB, CA 93523 USA.
NR 6
TC 0
Z9 0
U1 1
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 867
EP 871
DI 10.2514/1.C032883
PG 5
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400012
ER
PT J
AU Landman, D
Toro, KG
Commo, SA
Lynn, KC
AF Landman, Drew
Toro, Kenneth G.
Commo, Sean A.
Lynn, Keith C.
TI Prediction Interval Development for Wind-Tunnel Balance Check-Loading
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB The current approach used to apply uncertainty intervals to balance estimated loads is based on the root mean square error from calibration. Using the root mean square error, a constant interval is applied around the estimated load and it is expected that a predetermined percentage of the check-loads applied fall within this constant uncertainty interval. However, this approach ignores additional sources of uncertainty and assumes constant uncertainty regardless of the load combination and magnitude applied to the balance. Rigorous prediction interval theory permits varying interval widths but fails to account for the additional error sources that are unrelated to the mathematical modeling. An engineered solution is proposed that combines prediction interval theory and the need to account for the additional sources of uncertainty from calibration and check loading. Results from a case study using the in-situ load system show improved probabilistic behavior in terms of uncertainty interval capture percentage when compared with the current root mean square error method.
C1 [Landman, Drew; Toro, Kenneth G.] Old Dominion Univ, Dept Mech & Aerosp Engn, Norfolk, VA 23529 USA.
[Commo, Sean A.] NASA, Langley Res Ctr, Syst Engn & Engn Methods Branch, Hampton, VA 23681 USA.
[Lynn, Keith C.] NASA, Langley Res Ctr, Adv Measurements & Data Syst Branch, Hampton, VA 23681 USA.
RP Landman, D (reprint author), Old Dominion Univ, Dept Mech & Aerosp Engn, 1300 Elkhorn Ave, Norfolk, VA 23529 USA.
FU National Force Measurement Technology Capability under NASA's
Aeronautics Test Program
FX This work has been supported and funded by the National Force
Measurement Technology Capability under NASA's Aeronautics Test Program.
The authors would like to express their sincere appreciation to the
individuals who have contributed to the many aspects of this project. In
particular, the authors would like to recognize the following for the
critical contributions: J. Greg Jones for his extensive expertise,
knowledge, and dedication to balance calibrations; Ray Rhew for his
valuable input on force measurement system design and characterization;
Peter Parker for his insight on the Single-Vector Calibration System and
consultation during the development of the in-situ load system (ILS);
and Michael Acheson and Mark Cagle for their initial work with the ILS.
NR 9
TC 0
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U1 3
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 884
EP 889
DI 10.2514/1.C032930
PG 6
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400015
ER
PT J
AU Ordaz, I
Geiselhart, KA
Fenbert, JW
AF Ordaz, Irian
Geiselhart, Karl A.
Fenbert, James W.
TI Conceptual Design of Low-Boom Aircraft with Flight Trim Requirement
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB A new low-boom target generation approach is presented that allows the introduction of a trim requirement during the early conceptual design of supersonic aircraft. The formulation provides an approximation of the center of pressure for an aircraft configuration with a reversed equivalent area matching a low-boom equivalent area target. The center of pressure is approximated from a surrogate lift distribution that is based on the lift component of the classical equivalent area. The assumptions of the formulation are verified to be sufficiently accurate for a supersonic aircraft of high fineness ratio through three case studies. The first two quantify and verify the accuracy and the sensitivity of the surrogate center of pressure corresponding to shape deformation of lifting components. The third verification case shows the capability of the approach to achieve a trim state while maintaining the low-boom characteristics of a previously untrimmed configuration. Finally, the new low-boom target generation approach is demonstrated through the early conceptual design of a demonstrator concept that is low-boom feasible, trimmed, and stable in cruise.
C1 [Ordaz, Irian; Geiselhart, Karl A.] NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA.
[Fenbert, James W.] Analytical Mech Associates Inc, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA.
RP Ordaz, I (reprint author), NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Mail Stop 442, Hampton, VA 23681 USA.
NR 18
TC 0
Z9 0
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 932
EP 939
DI 10.2514/1.C033160
PG 8
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400022
ER
PT J
AU Grauer, JA
AF Grauer, Jared A.
TI Real-Time Data-Compatibility Analysis Using Output-Error Parameter
Estimation
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID IDENTIFICATION
AB Output-error parameter estimation, normally a postflight batch technique, was applied to solve the data-compatibility problem in real time. Short segments of data were sequentially processed to enable real-time estimation, and variations on the algorithm were used to expedite convergence from arbitrary starting values of the unknown model parameters. The method was applied to flight-test data to correct the data for systematic instrumentation errors. Results showed that the method produced accurate estimates of the data-compatibility correction parameters at a rate of 0.5 Hz. A sensor fault was also introduced into the flight data, and the use of a data-forgetting algorithm showed that the method was capable of quickly adapting to the data in a way that could enable sensor fault detection.
C1 NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA.
RP Grauer, JA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, MS 308, Hampton, VA 23681 USA.
FU NASA Aviation Safety Program; Vehicle Systems Safety Technologies
project; Subsonic Fixed-Wing Project
FX This research was funded by the NASA Aviation Safety Program, Vehicle
Systems Safety Technologies project, and the Subsonic Fixed-Wing
Project. Conversations with Eugene Morelli at NASA Langley Research
Center are acknowledged and appreciated.
NR 18
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2015
VL 52
IS 3
BP 940
EP 947
DI 10.2514/1.C033182
PG 8
WC Engineering, Aerospace
SC Engineering
GA CI4VH
UT WOS:000354751400023
ER
PT J
AU Rodriguez-Fonseca, B
Mohino, E
Mechoso, CR
Caminade, C
Biasutti, M
Gaetani, M
Garcia-Serrano, J
Vizy, EK
Cook, K
Xue, YK
Polo, I
Losada, T
Druyan, L
Fontaine, B
Bader, J
Doblas-Reyes, FJ
Goddard, L
Janicot, S
Arribas, A
Lau, W
Colman, A
Vellinga, M
Rowell, DP
Kucharski, F
Voldoire, A
AF Rodriguez-Fonseca, Belen
Mohino, Elsa
Mechoso, Carlos R.
Caminade, Cyril
Biasutti, Michela
Gaetani, Marco
Garcia-Serrano, J.
Vizy, Edward K.
Cook, Kerry
Xue, Yongkang
Polo, Irene
Losada, Teresa
Druyan, Leonard
Fontaine, Bernard
Bader, Juergen
Doblas-Reyes, Francisco J.
Goddard, Lisa
Janicot, Serge
Arribas, Alberto
Lau, William
Colman, Andrew
Vellinga, M.
Rowell, David P.
Kucharski, Fred
Voldoire, Aurore
TI Variability and Predictability of West African Droughts: A Review on the
Role of Sea Surface Temperature Anomalies
SO JOURNAL OF CLIMATE
LA English
DT Article
ID TROPICAL NORTH-AFRICA; GENERAL-CIRCULATION MODELS; IDEALIZED
2-DIMENSIONAL FRAMEWORK; ATLANTIC CLIMATE VARIABILITY; EASTERN
EQUATORIAL ATLANTIC; SAHEL RAINFALL VARIABILITY; INTERANNUAL
VARIABILITY; REGIONAL CLIMATE; SUMMER RAINFALL; DECADAL PREDICTION
AB The Sahel experienced a severe drought during the 1970s and 1980s after wet periods in the 1950s and 1960s. Although rainfall partially recovered since the 1990s, the drought had devastating impacts on society. Most studies agree that this dry period resulted primarily from remote effects of sea surface temperature (SST) anomalies amplified by local land surface-atmosphere interactions. This paper reviews advances made during the last decade to better understand the impact of global SST variability on West African rainfall at interannual to decadal time scales. At interannual time scales, a warming of the equatorial Atlantic and Pacific/Indian Oceans results in rainfall reduction over the Sahel, and positive SST anomalies over the Mediterranean Sea tend to be associated with increased rainfall. At decadal time scales, warming over the tropics leads to drought over the Sahel, whereas warming over the North Atlantic promotes increased rainfall. Prediction systems have evolved from seasonal to decadal forecasting. The agreement among future projections has improved from CMIP3 to CMIP5, with a general tendency for slightly wetter conditions over the central part of the Sahel, drier conditions over the western part, and a delay in the monsoon onset. The role of the Indian Ocean, the stationarity of teleconnections, the determination of the leader ocean basin in driving decadal variability, the anthropogenic role, the reduction of the model rainfall spread, and the improvement of some model components are among the most important remaining questions that continue to be the focus of current international projects.
C1 [Rodriguez-Fonseca, Belen; Mohino, Elsa] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra Astron & Astrofis 1, E-28040 Madrid, Spain.
[Rodriguez-Fonseca, Belen] CSIC, Inst Geociencias, Madrid, Spain.
[Rodriguez-Fonseca, Belen] Univ Complutense Madrid, E-28040 Madrid, Spain.
[Mechoso, Carlos R.; Xue, Yongkang] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Caminade, Cyril] Univ Liverpool, Inst Infect & Global Hlth, Sch Environm Sci, Liverpool L69 3BX, Merseyside, England.
[Biasutti, Michela] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA.
[Gaetani, Marco] CNR, Ist Biometeorol, Rome, Italy.
[Garcia-Serrano, J.; Doblas-Reyes, Francisco J.] Inst Catala Ciencies Clima, Barcelona, Spain.
[Vizy, Edward K.; Cook, Kerry] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX USA.
[Polo, Irene] Univ Reading, Dept Meteorol, NCAS Climate, Reading, Berks, England.
[Losada, Teresa] Univ Castilla La Mancha, Inst Ciencias Ambientales, Toledo, Spain.
[Druyan, Leonard] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Druyan, Leonard] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Fontaine, Bernard] Univ Bourgogne, CNRS, Ctr Rech Climatol, Dijon, France.
[Bader, Juergen] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[Doblas-Reyes, Francisco J.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Goddard, Lisa] Columbia Univ, Int Res Inst Climate & Soc, New York, NY USA.
[Janicot, Serge] UPMC, LOCEAN IPSL, IRD, Paris, France.
[Arribas, Alberto; Colman, Andrew; Vellinga, M.; Rowell, David P.] Met Off Hadley Ctr, Exeter, Devon, England.
[Lau, William] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Kucharski, Fred] Abdus Salam Int Ctr Theoret Phys, Trieste, Italy.
[Voldoire, Aurore] CNRS, Meteo France, Grp Etud Atmosphere Meteorol, Ctr Natl Rech Meteorol, Toulouse, France.
RP Rodriguez-Fonseca, B (reprint author), Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra Astron & Astrofis 1, Ciudad Univ,Plaza Ciencias,1, E-28040 Madrid, Spain.
EM brfonsec@ucm.es
RI Mohino, Elsa/G-8620-2015; Garcia-Serrano, Javier/I-5058-2015; Biasutti,
Michela/G-3804-2012; Losada, Teresa/O-8739-2015; Vizy,
Edward/A-1577-2009;
OI Mohino, Elsa/0000-0002-4342-6349; Garcia-Serrano,
Javier/0000-0003-3913-0876; Biasutti, Michela/0000-0001-6681-1533;
Losada, Teresa/0000-0002-8430-1745; cyril, caminade/0000-0002-3846-7082
FU Spanish projects [MINECO CGL2011-13564-E, GL2012-38923-C02-01]; U.S.
National Science Foundation [SES-1048946, ATM-1036604, AGS-1041477,
AGS-1115506]; European Commission [243964, 603521, 308378]; European
Community
FX This work was supported by Spanish projects MINECO CGL2011-13564-E and
GL2012-38923-C02-01. Support from the U.S. National Science Foundation
(Awards SES-1048946, ATM-1036604, AGS-1041477, and AGS-1115506) is
gratefully acknowledged. Also gratefully acknowledged are the GCM
modeling groups, the Program for Climate Model Diagnosis and
Intercomparison (PCMDI), and the World Climate Research Programme's
Working Group on Coupled Modeling (WGCM) for their roles in making
available the WCRP CMIP5 multimodel dataset. Support of this dataset is
provided by the Office of Science, U.S. Department of Energy (DOE). We
acknowledge the EU QWECI, PREFACE, and SPECS projects both funded by the
European Commission's Seventh Framework Research Programme under Grant
Agreements 243964, 603521, and 308378 respectively. Based on a French
initiative, AMMA was built by an international scientific group and is
currently funded by a large number of agencies, especially from France,
the United Kingdom, the United States, and Africa. It has been the
beneficiary of a major financial contribution from the European
Community's Sixth Framework Research Programme. The authors are grateful
to Ashlynn Fiss for her help in improving this manuscript.
NR 197
TC 13
Z9 13
U1 4
U2 35
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAY
PY 2015
VL 28
IS 10
BP 4034
EP 4060
DI 10.1175/JCLI-D-14-00130.1
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CH9QE
UT WOS:000354370100009
ER
PT J
AU Lahsen, M
Mathews, A
Dove, MR
Orlove, B
Puri, R
Barnes, J
McElwee, P
Moore, F
O'Reilly, J
Yager, K
AF Lahsen, Myanna
Mathews, Andrew
Dove, Michael R.
Orlove, Ben
Puri, Rajindra
Barnes, Jessica
McElwee, Pamela
Moore, Frances
O'Reilly, Jessica
Yager, Karina
TI Strategies for changing the intellectual climate
SO NATURE CLIMATE CHANGE
LA English
DT Letter
C1 [Lahsen, Myanna] Brazilian Inst Space Res INPE, Ctr Earth Syst Sci, BR-12227010 Sao Paulo, Brazil.
[Mathews, Andrew] Univ Calif Santa Cruz, Anthropol, Santa Cruz, CA 95064 USA.
[Dove, Michael R.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
[Orlove, Ben] Columbia Univ, Earth & Environm Sci, New York, NY 10027 USA.
[Puri, Rajindra] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NZ, Kent, England.
[Barnes, Jessica] Univ S Carolina, Dept Geog, Columbia, SC 29208 USA.
[McElwee, Pamela] Rutgers State Univ, Dept Human Ecol, Newark, NJ 07102 USA.
[Moore, Frances] Stanford Univ, Sch Earth Sci, Stanford, CA 94305 USA.
[O'Reilly, Jessica] St Johns Univ, Coll St Benedict, Anthropol & Sociol Dept, St Joseph, MN 56321 USA.
[O'Reilly, Jessica] St Johns Univ, Coll St Benedict, Anthropol & Sociol Dept, Collegeville, MN 56321 USA.
[Yager, Karina] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lahsen, M (reprint author), Brazilian Inst Space Res INPE, Ctr Earth Syst Sci, BR-12227010 Sao Paulo, Brazil.
EM myannal@gmail.com
RI Lahsen, Myanna/E-3697-2013;
OI Puri, Rajindra/0000-0002-3442-8537; McElwee, Pamela/0000-0003-3525-9285
NR 5
TC 3
Z9 3
U1 3
U2 14
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD MAY
PY 2015
VL 5
IS 5
BP 391
EP 392
PG 3
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CI6SO
UT WOS:000354891900005
ER
PT J
AU Kok, M
Smith, JG
Wohl, CJ
Siochi, EJ
Young, TM
AF Kok, Mariana
Smith, Joseph G., Jr.
Wohl, Christopher J.
Siochi, Emilie J.
Young, Trevor M.
TI Critical considerations in the mitigation of insect residue
contamination on aircraft surfaces - A review
SO PROGRESS IN AEROSPACE SCIENCES
LA English
DT Review
DE Laminar flow; Insect mitigation; Coatings; Engineered surface testing
ID LAMINAR-FLOW CONTROL; INTERMITTENCY TRANSPORT-EQUATION; LEADING-EDGE
SURFACES; IMPACT DYNAMICS; DROSOPHILA-MELANOGASTER;
MECHANICAL-PROPERTIES; TURBULENT TRANSITION; BYPASS TRANSITION;
BOUNDARY-LAYER; DROP IMPACT
AB Mitigation of insect residue contamination on next generation aircraft is vital for the commercial exploitation of laminar flow technologies. A review of the critical entomological, meteorological and aeronautical factors affecting insect residue accumulation on aircraft leading edge surfaces is herein presented. An evaluation of a passive mitigation strategy, namely the use of anti-contamination coatings, has been conducted and the key issues in the use of these coatings highlighted. A summary of the variations in major experiments, including laboratory, wind tunnel and flight testing, is outlined. The effects of surface and material characteristics on insect residue adhesion were also investigated, with topographical features of the surface and surface chemistry shown as influential factors. The use of a substitute as an alternative to live insect testing has shown promise. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Kok, Mariana; Young, Trevor M.] Univ Limerick, Dept Mech Aeronaut & Biomed Engn, Limerick, Ireland.
[Kok, Mariana; Young, Trevor M.] Univ Limerick, Mat & Surface Sci Inst, Limerick, Ireland.
[Smith, Joseph G., Jr.; Wohl, Christopher J.; Siochi, Emilie J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Young, TM (reprint author), Univ Limerick, Dept Mech Aeronaut & Biomed Engn, Limerick, Ireland.
EM Trevor.Young@ul.ie
NR 165
TC 3
Z9 3
U1 2
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0376-0421
J9 PROG AEROSP SCI
JI Prog. Aeosp. Sci.
PD MAY
PY 2015
VL 75
BP 1
EP 14
DI 10.1016/j.paerosci.2015.02.001
PG 14
WC Engineering, Aerospace
SC Engineering
GA CI8UE
UT WOS:000355046400001
ER
PT J
AU Motagh, M
Bahroudi, A
Haghighi, MH
Samsonov, S
Fielding, E
Wetzel, HU
AF Motagh, Mahdi
Bahroudi, Abbas
Haghighi, Mahmud Haghshenas
Samsonov, Sergey
Fielding, Eric
Wetzel, Hans-Ulrich
TI The 18 August 2014 M-w 6.2 Mormon, Iran, Earthquake: A Thin-Skinned
Faulting in the Zagros Mountain Inferred from lnSAR Measurements
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID SIMPLY FOLDED BELT; MICROEARTHQUAKE SEISMICITY; CONTINENTAL COLLISION;
SPATIAL-DISTRIBUTION; SURFACE DEFORMATION; BAYESIAN INVERSION; SOURCE
PARAMETERS; QESHM EARTHQUAKE; GPS MEASUREMENTS; GEODETIC DATA
C1 [Motagh, Mahdi; Haghighi, Mahmud Haghshenas; Wetzel, Hans-Ulrich] GFZ German Res Ctr Geosci, D-14473 Potsdam, Germany.
[Bahroudi, Abbas] Univ Tehran, Fac Engn, Sch Min Engn, Explorat Dept, Tehran 51514395, Iran.
[Samsonov, Sergey] Nat Resources Canada, Canada Ctr Mapping & Earth Observat, Ottawa, ON K1A 0E4, Canada.
[Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Motagh, M (reprint author), GFZ German Res Ctr Geosci, Telegrafenberg Haus A17, D-14473 Potsdam, Germany.
EM motagh@gfz-potsdam.de
FU Initiative and Networking Fund of the Helmholtz Association
FX Original RADARSAT-2 data are copyright 2013-2014 MacDonald, Dettwiler
and Associates Ltd (MDA). Part of this research was supported by the
National Aeronautics and Space Administration's Earth Surface and
Interior focus area and performed at the Jet Propulsion Laboratory,
California Institute of Technology. We would like to thank Ziyadin
Cakir, an anonymous reviewer and the Editor in Chief, Zhigang Peng, for
their helpful comments on the original version of the manuscript. This
study was supported by the Initiative and Networking Fund of the
Helmholtz Association in the frame of Helmholtz Alliance "Remote Sensing
and Earth System Dynamics."
NR 43
TC 4
Z9 4
U1 0
U2 5
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
EI 1938-2057
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD MAY-JUN
PY 2015
VL 86
IS 3
BP 775
EP 782
DI 10.1785/0220140222
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CI3RX
UT WOS:000354666200004
ER
PT J
AU Marubashi, K
Akiyama, S
Yashiro, S
Gopalswamy, N
Cho, KS
Park, YD
AF Marubashi, K.
Akiyama, S.
Yashiro, S.
Gopalswamy, N.
Cho, K. -S.
Park, Y. -D.
TI Geometrical Relationship Between Interplanetary Flux Ropes and Their
Solar Sources
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejection (CME); Interplanetary coronal mass ejection
(ICME); Interplanetary magnetic flux rope; Magnetic cloud; Solar wind
magnetic field
ID CORONAL MASS EJECTIONS; MAGNETIC CLOUDS; WIND; MODEL; RECONNECTION;
DECREASES; FILAMENTS; ROTATION; HELIOS; SPACE
AB We investigated the physical connection between interplanetary flux ropes (IFRs) near Earth and coronal mass ejections (CMEs) by comparing the magnetic field structures of IFRs and CME source regions. The analysis is based on the list of 54 pairs of ICMEs (interplanetary coronal mass ejections) and CMEs that are taken to be the most probable solar source events. We first attempted to identify the flux rope structure in each of the 54 ICMEs by fitting models with a cylinder and torus magnetic field geometry, both with a force-free field structure. This analysis determined the possible geometries of the identified flux ropes. Then we compared the flux rope geometries with the magnetic field structure of the solar source regions. We obtained the following results: (1) Flux rope structures are seen in 51 ICMEs out of the 54. The result implies that all ICMEs have an intrinsic flux rope structure, if the three exceptional cases are attributed to unfavorable observation conditions. (2) It is possible to find flux rope geometries with the main axis orientation close to the orientation of the magnetic polarity inversion line (PIL) in the solar source regions, the differences being less than 25A degrees. (3) The helicity sign of an IFR is strongly controlled by the location of the solar source: flux ropes with positive (negative) helicity are associated with sources in the southern (northern) hemisphere (six exceptions were found). (4) Over two-thirds of the sources in the northern hemisphere are concentrated along PILs with orientations of 45A degrees A +/- 30A degrees (measured clockwise from the east), and over two-thirds in the southern hemisphere along PILs with orientations of 135A degrees A +/- 30A degrees, both corresponding to the Hale boundaries. These results strongly support the idea that a flux rope with the main axis parallel to the PIL erupts in a CME and that the erupted flux rope propagates through the interplanetary space with its orientation maintained and is observed as an IFR.
C1 [Akiyama, S.; Yashiro, S.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Akiyama, S.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Cho, K. -S.; Park, Y. -D.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
EM kmaru_bg@kzh.biglobe.ne.jp
FU "Development of Korean Space Weather Center" of KASI; KASI basic
research funds
FX This work benefited from the NASA/LWS Coordinated Data Analysis
Workshops on CME flux ropes in 2010 and 2011. We acknowledge the
workshop support provided by NASA/LWS, Predictive Sciences Inc. (San
Diego, CA), University of Alcala (Alcala de Henares, Spain), and
Ministerio de Ciencia e Innovacion (Reference number AYA2010-12439-E),
Spain. We thank the ACE, Wind, SOHO, and Yohkoh teams for providing the
data on line. SOHO is a project of international collaboration between
ESA and NASA. The Yohkoh mission was developed and launched by
ISAS/JAXA, Japan, with NASA and SERC/PPARC (UK) as international
partners. We also thank the BBSO, the MLSO, the Meudon Observatory, The
Hida Obserbatory of Kyoto University, and the Catania Astrophysical
Observatory teams for providing their H alpha data. K.M., K.-S.C., and
Y.-D. Park were supported by the "Development of Korean Space Weather
Center" of KASI and the KASI basic research funds.
NR 54
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Z9 9
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 MAY
PY 2015
VL 290
IS 5
BP 1371
EP 1397
DI 10.1007/s11207-015-0681-4
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CI1GB
UT WOS:000354490200005
ER
PT J
AU Lin, Y
Kim, JW
Connell, JW
Lebron-Colon, M
Siochi, EJ
AF Lin, Yi
Kim, Jae-Woo
Connell, John W.
Lebron-Colon, Marisabel
Siochi, Emilie J.
TI Purification of Carbon Nanotube Sheets
SO ADVANCED ENGINEERING MATERIALS
LA English
DT Article
ID SHEET/BISMALEIMIDE NANOCOMPOSITES; FIBERS; PERFORMANCE; YARNS;
TRANSPARENT; FILMS
AB Large volumes of carbon nanotube (CNT) sheets and yarns are required to enable practical applications such as structural reinforcements, electrical conductors, electromagnetic interference shielding, and energy storage. Although these macroscopic assemblages of CNTs are commercially available, reports on their handling and processing have been quite limited. In this article, we report a systematic study of the purification of commercially available CNT sheets produced directly from as-grown nanotubes. These CNT sheets contain residual metal catalysts encapsulated in graphitic carbon nanoparticles known to contaminate common powdery pristine CNT materials. Although many purification methods effective for powdery CNTs are known, they cannot be directly applied to CNT sheets because these processes often involve sonication and/or reflux, which are too aggressive and deleterious to the integrity of the sheets. Therefore, alternative physically benign processes were chosen and evaluated in detail. Assessment of the purification method included characterization of parameters such as residual metal content, weight retention, and changes in the Raman D-to-G intensity ratio. Importantly, the purification methodology was also placed in the context of the targeted application as a structural reinforcement in advanced composites. In this application, the mechanical properties of the CNT sheets are crucial, thus specific strength and modulus were evaluated and compared for the purified CNT sheets and the nanocomposites produced therefrom. Several important processing parameters were identified that resulted in purified CNT sheets with not only low catalyst content but also reasonable retention of mechanical properties. In addition, the scalability of the purification method and a procedure to prevent CNT sheet wrinkling after purification were demonstrated. Assessment criteria of CNT sheet purification techniques toward other potential applications are also discussed.
C1 [Lin, Yi; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
[Connell, John W.; Siochi, Emilie J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Lebron-Colon, Marisabel] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM yi.lin@nianet.org; emilie.j.siochi@nasa.gov
RI Kim, Jae-Woo/A-8314-2008
FU NASA Game Changing Development Program
FX The financial support from the NASA Game Changing Development Program is
gratefully acknowledged. We thank C. Chamberlain (NASA LaRC) for
assistance in thermogravimetric measurements, and Dr. W. Cao and Prof.
H. E. Elsayed-Ali (Applied Research Center at Old Dominion University)
for HR-TEM/EDS acquisitions.
NR 31
TC 2
Z9 2
U1 3
U2 42
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1438-1656
EI 1527-2648
J9 ADV ENG MATER
JI Adv. Eng. Mater.
PD MAY
PY 2015
VL 17
IS 5
BP 674
EP 688
DI 10.1002/adem.201400306
PG 15
WC Materials Science, Multidisciplinary
SC Materials Science
GA CI0HI
UT WOS:000354417300014
ER
PT J
AU Xiong, MY
Shelobolina, ES
Roden, EE
AF Xiong, Mai Yia
Shelobolina, Evgenya S.
Roden, Eric E.
TI Potential for Microbial Oxidation of Ferrous Iron in Basaltic Glass
SO ASTROBIOLOGY
LA English
DT Article
ID FE-OXIDIZING BACTERIA; NEUTRAL PH; WATER ENVIRONMENTS; OCEAN CRUST;
NITRATE; FE(II); SEQUENCES; MINERALS; ROCKS; MARS
AB Basaltic glass (BG) is an amorphous ferrous iron [Fe(II)]-containing material present in basaltic rocks, which are abundant on rocky planets such as Earth and Mars. Previous research has suggested that Fe(II) in BG can serve as an energy source for chemolithotrophic microbial metabolism, which has important ramifications for potential past and present microbial life on Mars. However, to date there has been no direct demonstration of microbially catalyzed oxidation of Fe(II) in BG. In this study, three different culture systems were used to investigate the potential for microbial oxidation of Fe(II) in BG, including (1) the chemolithoautotrophic Fe(II)-oxidizing, nitrate-reducing "Straub culture"; (2) the mixotrophic Fe(II)-oxidizing, nitrate-reducing organism Desulfitobacterium frappieri strain G2; and (3) indigenous microorganisms from a streambed Fe seep in Wisconsin. The BG employed consisted of clay and silt-sized particles of freshly quenched lava from the TEB flow in Kilauea, Hawaii. Soluble Fe(II) or chemically reduced NAu-2 smectite (RS) were employed as positive controls to verify Fe(II) oxidation activity in the culture systems. All three systems demonstrated oxidation of soluble Fe(II) and/or structural Fe(II) in RS, whereas no oxidation of Fe(II) in BG material was observed. The inability of the Straub culture to oxidize Fe(II) in BG was particularly surprising, as this culture can oxidize other insoluble Fe(II)-bearing minerals such as biotite, magnetite, and siderite. Although the reason for the resistance of the BG toward enzymatic oxidation remains unknown, it seems possible that the absence of distinct crystal faces or edge sites in the amorphous glass renders the material resistant to such attack. These findings have implications with regard to the idea that Fe(II)-Si-rich phases in basalt rocks could provide a basis for chemolithotrophic microbial life on Mars, specifically in neutral-pH environments where acid-promoted mineral dissolution and utilization of dissolved Fe(II) as an energy source is not likely to take place. Key Words: Basaltic glass-Chemolithotrophic-Microbial-Iron oxidation-Mars. Astrobiology 15, 331-340.
C1 [Roden, Eric E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA.
RP Roden, EE (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
EM eroden@geology.wisc.edu
FU NASA Astrobiology Institute
FX This work was supported by the NASA Astrobiology Institute. We
gratefully acknowledge B. Converse for assistance with the 16S rRNA gene
pyrosequencing analysis and Tao Wu for assistance with mineralogical
analysis.
NR 59
TC 0
Z9 0
U1 7
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 MAY 1
PY 2015
VL 15
IS 5
BP 331
EP 340
DI 10.1089/ast.2014.1233
PG 10
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CI2XV
UT WOS:000354612400002
PM 25915449
ER
PT J
AU Assef, RJ
Eisenhardt, PRM
Stern, D
Tsai, CW
Wu, J
Wylezalek, D
Blain, AW
Bridge, CR
Donoso, E
Gonzales, A
Griffith, RL
Jarrett, TH
AF Assef, R. J.
Eisenhardt, P. R. M.
Stern, D.
Tsai, C. -W.
Wu, J.
Wylezalek, D.
Blain, A. W.
Bridge, C. R.
Donoso, E.
Gonzales, A.
Griffith, R. L.
Jarrett, T. H.
TI HALF OF THE MOST LUMINOUS QUASARS MAY BE OBSCURED: INVESTIGATING THE
NATURE OF WISE-SELECTED HOT DUST-OBSCURED GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
infrared: galaxies; quasars: general
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; STELLAR POPULATION SYNTHESIS;
SIMILAR-TO 2; INFRARED-SURVEY-EXPLORER; SPITZER-SPACE-TELESCOPE;
LY-ALPHA EMITTERS; LESS-THAN 3.2; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES
AB The Wide-field Infrared Survey Explorer mission has unveiled a rare population of high-redshift (z = 1-4.6), dusty, hyper-luminous galaxies, with infrared luminosities L-IR > 10(13) L-circle dot, and sometimes exceeding 10(14) L-circle dot. Previous work has shown that their dust temperatures and overall far-infrared spectral energy distributions (SEDs) are significantly hotter than expected to be powered by star formation. We present here an analysis of the rest-frame optical through mid-infrared SEDs for a large sample of these so-called "hot, dust-obscured galaxies" (Hot DOGs). We find that the SEDs of Hot DOGs are generally well modeled by the combination of a luminous, yet obscured active galactic nuclei (AGNs) that dominates the rest-frame emission at lambda > 1 mu m and the bolometric luminosity output, and a less luminous host galaxy that is responsible for the bulk of the rest optical/UV emission. Even though the stellar mass of the host galaxies may be as large as 10(11) - 10(12) M-circle dot, the AGN emission, with a range of luminosities comparable to those of the most luminous QSOs known, require that either Hot DOGs have black hole masses significantly in excess of the local relations, or that they radiate significantly above the Eddington limit, at a level at least 10 times more efficiently than z similar to 2 QSOs. We show that, while rare, the number density of Hot DOGs is comparable to that of equally luminous but unobscured (i.e., Type 1) QSOs. This may be at odds with the trend suggested at lower luminosities for the fraction of obscured AGNs to decrease with increasing luminosity. That trend may, instead, reverse at higher luminosities. Alternatively, Hot DOGs may not be the torus-obscured counterparts of the known optically selected, largely unobscured, hyper-luminous QSOs, and may represent a new component of the galaxy evolution paradigm. Finally, we discuss the environments of Hot DOGs and statistically show that these objects are in regions as dense as those of known high-redshift protoclusters.
C1 [Assef, R. J.] Univ Diego Port, Nucl Astron Fac Ingn, Santiago, Chile.
[Eisenhardt, P. R. M.; Stern, D.; Tsai, C. -W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wu, J.] Univ Calif Los Angeles, Astron, Los Angeles, CA 90095 USA.
[Wylezalek, D.] European So Observ, D-85748 Garching, Germany.
[Blain, A. W.] Univ Leicester, Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bridge, C. R.; Gonzales, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Donoso, E.] ICATE, RA-5400 San Juan, Argentina.
[Gonzales, A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Gonzales, A.] Scripps Coll, Claremont, CA 91711 USA.
[Griffith, R. L.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Jarrett, T. H.] Univ Cape Town, Dept Astron, ACGC, ZA-7701 Rondebosch, South Africa.
RP Assef, RJ (reprint author), Univ Diego Port, Nucl Astron Fac Ingn, Av Ejercito Libertador 441, Santiago, Chile.
EM roberto.assef@mail.udp.cl
FU Gemini-CONICYT [32120009]; National Aeronautics and Space Administration
[13-ADAP13-0092]
FX We are indebted to all WISE team members. We thank the anonymous referee
for comments and suggestions that helped to improve this article. RJA
was supported by Gemini-CONICYT grant number 32120009. This publication
makes use of data products from the Wide-field Infrared Survey Explorer,
which is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration. This work
is based in part on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. Kitt Peak National Observatory
and CTIO, National Optical Astronomy Observatory, are operated by the
Association of Universities for Research in Astronomy (AURA) under
cooperative agreement with the National Science Foundation. The WIYN
Observatory is a joint facility of the University of Wisconsin-Madison,
Indiana University, Yale University, and the National Optical Astronomy
Observatory. The SOAR Telescope is a joint project of: Conselho Nacional
de Pesquisas Cientificas e Tecnologicas CNPq-Brazil, The University of
North Carolina at Chapel Hill, Michigan State University, and the
National Optical Astronomy Observatory. Based partly on observations
obtained at the Hale Telescope, Palomar Observatory as part of a
continuing collaboration between the California Institute of Technology,
NASA/JPL, NOAO, Oxford University, Stony Brook University, and the
National Astronomical Observatories of China. This material is based
upon work supported by the National Aeronautics and Space Administration
under Proposal No. 13-ADAP13-0092 issued through the Astrophysics Data
Analysis Program.
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J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2015
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PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CH7BB
UT WOS:000354189500027
ER
PT J
AU Crossfield, IJM
Petigura, E
Schlieder, JE
Howard, AW
Fulton, BJ
Aller, KM
Ciardi, DR
Lepine, S
Barclay, T
De Pater, I
De Kleer, K
Quintana, EV
Christiansen, JL
Schlafly, E
Kaltenegger, L
Crepp, JR
Henning, T
Obermeier, C
Deacon, N
Weiss, LM
Isaacson, HT
Hansen, BMS
Liu, MC
Greene, T
Howell, SB
Barman, T
Mordasini, C
AF Crossfield, Ian J. M.
Petigura, Erik
Schlieder, Joshua E.
Howard, Andrew W.
Fulton, B. J.
Aller, Kimberly M.
Ciardi, David R.
Lepine, Sebastien
Barclay, Thomas
De Pater, Imke
De Kleer, Katherine
Quintana, Elisa V.
Christiansen, Jessie L.
Schlafly, Eddie
Kaltenegger, Lisa
Crepp, Justin R.
Henning, Thomas
Obermeier, Christian
Deacon, Niall
Weiss, Lauren M.
Isaacson, Howard T.
Hansen, Brad M. S.
Liu, Michael C.
Greene, Tom
Howell, Steve B.
Barman, Travis
Mordasini, Christoph
TI A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; stars: individual (EPIC 201367065); techniques: photometric;
techniques: spectroscopic
ID DIGITAL SKY SURVEY; MAIN-SEQUENCE STARS; M-DWARFS; LOW-MASS; LIGHT
CURVES; SPECTROSCOPIC SURVEY; PLANET CANDIDATES; KINEMATIC GROUPS; FALSE
POSITIVES; BLEND SCENARIOS
AB Small, cool planets represent the typical end-products of planetary formation. Studying the architectures of these systems, measuring planet masses and radii, and observing these planets' atmospheres during transit directly informs theories of planet assembly, migration, and evolution. Here we report the discovery of three small planets orbiting a bright (K-s = 8.6 mag) M0 dwarf using data collected as part of K2, the new ecliptic survey using the repurposed Kepler spacecraft. Stellar spectroscopy and K2 photometry indicate that the system hosts three transiting planets with radii 1.5-2.1 R-circle plus, straddling the transition region between rocky and increasingly volatile-dominated compositions. With orbital periods of 10-45 days the planets receive just 1.5-10x the flux incident on Earth, making these some of the coolest small planets known orbiting a nearby star; planet d is located near the inner edge of the system's habitable zone. The bright, low-mass star makes this system an excellent laboratory to determine the planets' masses via Doppler spectroscopy and to constrain their atmospheric compositions via transit spectroscopy. This discovery demonstrates the ability of K2 and future space-based transit searches to find many fascinating objects of interest.
C1 [Crossfield, Ian J. M.; Barman, Travis] Univ Arizona Lunar, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Petigura, Erik; De Pater, Imke; De Kleer, Katherine; Weiss, Lauren M.; Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Schlieder, Joshua E.; Barclay, Thomas; Quintana, Elisa V.; Greene, Tom; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Howard, Andrew W.; Fulton, B. J.; Aller, Kimberly M.; Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Ciardi, David R.; Christiansen, Jessie L.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Schlafly, Eddie; Henning, Thomas; Obermeier, Christian; Mordasini, Christoph] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Deacon, Niall] Univ Hertfordshire, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Hansen, Brad M. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Kaltenegger, Lisa] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Crossfield, Ian J. M.; Mordasini, Christoph] Inst Phys, CH-3012 Bern, Switzerland.
RP Crossfield, IJM (reprint author), Univ Arizona Lunar, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA.
EM ianc@lpl.arizona.edu
OI Weiss, Lauren/0000-0002-3725-3058; Ciardi, David/0000-0002-5741-3047;
Schlafly, Edward Ford/0000-0002-3569-7421
FU NASA [NNX12AJ23G, NNH14CK55B]; NSF [AST 09-08419]
FX We thank Geoff Marcy, Evan Sinukoff, and Charles Beichman for helpful
conversations; Vishnu Reddy for swapping SpeX time; and Steve Bryson and
our referee Don Pollacco for useful comments that improved the quality
of this manuscript. A. W.H. acknowledges NASA grant No. NNX12AJ23G, and
S.L. acknowledges NSF grant No. AST 09-08419. This work made use of the
SIMBAD database (operated at CDS, Strasbourg, France); NASA's
Astrophysics Data System Bibliographic Services; the Authorea
collaborative writing website; the NASA Exoplanet Archive; and Infrared
Science Archive, and data products from the Two Micron All Sky Survey
(2MASS), the APASS database, the SDSS-III project, the Digitized Sky
Survey, and the Wide-Field Infrared Survey Explorer. Portions of this
work were performed at the California Institute of Technology under
contract with the National Aeronautics and Space Administration. Some of
the data presented herein were obtained at the W. M. Keck Observatory
(which is operated as a scientific partnership among Caltech, UC, and
NASA) and at the Infrared Telescope Facility (IRTF, operated by UH under
NASA contract NNH14CK55B). 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.
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SC Astronomy & Astrophysics
GA CH7BB
UT WOS:000354189500010
ER
PT J
AU Cucchiara, A
Fumagalli, M
Rafelski, M
Kocevski, D
Prochaska, JX
Cooke, RJ
Becker, GD
AF Cucchiara, A.
Fumagalli, M.
Rafelski, M.
Kocevski, D.
Prochaska, J. X.
Cooke, R. J.
Becker, G. D.
TI UNVEILING THE SECRETS OF METALLICITY AND MASSIVE STAR FORMATION USING
DLAS ALONG GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: general; galaxies: ISM; gamma-ray burst: general; quasars:
absorption lines; techniques: imaging spectroscopy
ID DAMPED LY-ALPHA; GRB AFTERGLOW SPECTRA; HIGH-RESOLUTION SPECTROSCOPY;
VLT/X-SHOOTER SPECTROSCOPY; COSMIC CHEMICAL EVOLUTION; MAGELLAN UNIFORM
SURVEY; HUBBLE-SPACE-TELESCOPE; HIGH COLUMN DENSITY; SIMILAR-TO 5; HOST
GALAXY
AB We present the largest, publicly available sample of damped Ly alpha systems (DLAs) along the lines of sight of Swift-discovered gamma-ray bursts (GRBs). in order to investigate the environmental properties of long GRB hosts in the z = 1.8-6 redshift range. Compared with the most recent quasar DLA sample (QSO-DLA), our analysis shows that GRB-DLAs probe a more metal-enriched environment at z greater than or similar to 3, up to [X/H] similar to -0.5. In the z = 2-3 redshift range, despite the large number of lower limits, there are hints that the two populations may be more similar (only at a 90% significance level) than at higher redshifts. Also, at high-z, the GRB-DLA average metallicity seems to decline at a lower rate than the QSO-DLAs: GRB-DLA hosts may be polluted with metals at least as far as similar to 2 kpc from the GRB explosion site, probably due to previous star formation episodes and/or supernova explosions. This shallow metallicity trend, now extended up to z similar to 5, confirms previous results that GRB hosts are star-forming and have, on average, higher metallicities. than the general QSO-DLA population. Finally, our host metallicity measurements are broadly consistent with the predictions derived from the hypothesis of two channels of GRB progenitors, one of which is mildly affected by a metallicity bias, although more data are needed to constrain the models at z greater than or similar to 4.
C1 [Cucchiara, A.; Rafelski, M.; Kocevski, D.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA.
[Fumagalli, M.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Fumagalli, M.] Carnegie Observ, Pasadena, CA 91101 USA.
[Prochaska, J. X.; Cooke, R. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Becker, G. D.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Becker, G. D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Cucchiara, A (reprint author), NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA.
EM antonino.cucchiara@nasa.gov
RI Fumagalli, Michele/K-9510-2015
OI Fumagalli, Michele/0000-0001-6676-3842
FU NASA Postdoctoral Program at the Goddard Space Flight Center; Science
and Technology Facilities Council [ST/L00075X/1]
FX This research was supported by the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. A.C. thanks M.F. and M.R. for
the incredible support and useful discussions during the writing of this
work. A.C. also thanks M.T. for fundamental discussion as well for
providing the models' curves. M.F. acknowledges support by the Science
and Technology Facilities Council (Grant #ST/L00075X/1). A.C. thanks P.
D'Avanzo for providing the spectrum of GRB 090205A.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA CH7BB
UT WOS:000354189500051
ER
PT J
AU Desert, JM
Charbonneau, D
Torres, G
Fressin, F
Ballard, S
Bryson, ST
Knutson, HA
Batalha, NM
Borucki, WJ
Brown, TM
Deming, D
Ford, EB
Fortney, JJ
Gilliland, RL
Latham, DW
Seager, S
AF Desert, Jean-Michel
Charbonneau, David
Torres, Guillermo
Fressin, Francois
Ballard, Sarah
Bryson, Stephen T.
Knutson, Heather A.
Batalha, Natalie M.
Borucki, William J.
Brown, Timothy M.
Deming, Drake
Ford, Eric B.
Fortney, Jonathan J.
Gilliland, Ronald L.
Latham, David W.
Seager, Sara
TI LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A
COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; eclipses; planetary systems; planets and
satellites: detection; techniques: polarimetric
ID TRANSIT TIMING VARIATIONS; SUN-LIKE STAR; INFRARED ARRAY CAMERA;
MULTIPLE-PLANET SYSTEMS; EXOPLANET HD 189733B; CIRCLE-PLUS PLANET;
HABITABLE-ZONE; SPACE-TELESCOPE; ECLIPSING BINARIES; EXTRASOLAR PLANET
AB NASA's Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 mu m. We use these observations to measures the candidate's transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3 sigma. This observational result, which uses the achromatic property of planetary transit signals that is not investigated by the Kepler observations, provides an independent indication that Kepler's FPR is low.
C1 [Desert, Jean-Michel; Brown, Timothy M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Desert, Jean-Michel; Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Charbonneau, David; Torres, Guillermo; Fressin, Francois; Ballard, Sarah; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA.
[Bryson, Stephen T.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA.
[Ford, Eric B.; Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Seager, Sara] MIT, Cambridge, MA 02159 USA.
RP Desert, JM (reprint author), Univ Colorado, CASA, Dept Astrophys & Planetary Sci, 389-UCB, Boulder, CO 80309 USA.
EM desert@colorado.edu
OI /0000-0001-6545-639X
FU NASA's Science Mission Directorate; NASA; NASA Kepler Mission
Participating Scientist Program [NNX09AB53G, NNX12AC77G, NNX12AC75G,
NNX14AB83G]; John Templeton Foundation; National Aeronautics and Space
Administration
FX We thank the anonymous reviewer for the careful reading of our
manuscript and the valuable comments. This work is based on observations
made with Kepler, which was competitively selected as the 10th Discovery
mission. Funding for this mission is provided by NASA's Science Mission
Directorate. The authors would like to thank the many people who
generously gave so much of their time to make this mission a success.
This work is also based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. D.C. acknowledges support for this work from grants
NNX09AB53G and NNX12AC77G, and G.T. acknowledges support from grants
NNX12AC75G and NNX14AB83G, each from the NASA Kepler Mission
Participating Scientist Program. D.C. acknowledges the support of a
grant from the John Templeton Foundation. The opinions expressed in this
publication are those of the authors and do not necessarily reflect the
views of the John Templeton Foundation. We would like to thank the
Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling
the Spitzer observations of this program. J.-M.D. and S.B. acknowledge
the Sagan Exoplanet Fellowship program supported by the National
Aeronautics and Space Administration and administered by the NASA
Exoplanet Science Institute (NExScI). We thank Samaya Nissanke for
careful reading of the manuscript.
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ER
PT J
AU Gorti, U
Hollenbach, D
Dullemond, CP
AF Gorti, U.
Hollenbach, D.
Dullemond, C. P.
TI THE IMPACT OF DUST EVOLUTION AND PHOTOEVAPORATION ON DISK DISPERSAL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; protoplanetary disks; stars:
formation; stars: winds; outflows
ID T-TAURI STARS; TURBULENT PROTOPLANETARY DISKS; GIANT-PLANET FORMATION;
HERBIG AE STARS; X-RAY-RADIATION; CIRCUMSTELLAR DISKS; FAR-ULTRAVIOLET;
EXTREME-ULTRAVIOLET; MOLECULE FORMATION; INFRARED-EMISSION
AB Protoplanetary disks are dispersed by viscous evolution and photoevaporation in a few million years; in the interim small, sub-micron-sized dust grains must grow and form planets. The time-varying abundance of small grains in an evolving disk directly affects gas heating by far-ultraviolet (FUV) photons, while dust evolution affects photoevaporation by changing the disk opacity and resulting penetration of FUV photons in the disk. Photoevaporative flows, in turn, selectively carry small dust grains, leaving the larger particles-which decouple, from the gas-behind in the disk. We study these effects by investigating the evolution of a disk subject to viscosity, photoevaporation by EUV, FUV, and X-rays, dust evolution, and radial drift using a one-dimensional (1D) multi-fluid approach (gas + different dust grain sizes) to solve for the evolving surface density distributions. The 1D evolution is augmented by 1+1D models constructed at each epoch to obtain the instantaneous disk structure and determine photoevaporation rates. The implementation of a dust coagulation/fragmentation model results in a marginal decrease in disk lifetimes when compared to models with no dust evolution; the disk lifetime is thus found to be relatively insensitive to the evolving dust opacity. We find that photoevaporation can cause significant reductions in the gas/dust mass ratio in the planet-forming regions of the disk as it evolves, and may result in a corresponding increase in heavy element abundances relative to hydrogen. We discuss implications for theories of planetesimal formation and giant planet formation, including the formation of gas-poor giants. After gas disk dispersal, similar to 3 x 10(-4) M-circle dot of mass in solids typically remain, comparable to the solids inventory of our solar system.
C1 [Gorti, U.; Hollenbach, D.] SETI Inst, Mountain View, CA 94043 USA.
[Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dullemond, C. P.] Heidelberg Univ, D-69115 Heidelberg, Germany.
RP Gorti, U (reprint author), SETI Inst, Mountain View, CA 94043 USA.
OI Dullemond, Cornelis/0000-0002-7078-5910
FU NASA [NNX09AO42G]; DFG [DU 414/9-1]
FX U.G. acknowledges several helpful discussions with Jeff Cuzzi, Chris
Ormel and Til Birnstiel. U.G. and D.H. acknowledge funding from NASA
Award NNX09AO42G which made this work possible. This project made use of
NASA HEC supercomputing resources. C.P.D. acknowledges funding from DFG
grant DU 414/9-1.
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EF