FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Colliander, A
Mckague, D
AF Colliander, Andreas
Mckague, Darren
TI The Microwave Radiometer Working Group
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
C1 [Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Mckague, Darren] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 10
TC 0
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U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD SEP
PY 2016
VL 4
IS 3
SI SI
BP 69
EP 72
DI 10.1109/MGRS.2016.2588442
PG 4
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0HY
UT WOS:000390007700009
ER
PT J
AU Eingorn, M
Kiefer, C
Zhuk, A
AF Eingorn, Maxim
Kiefer, Claus
Zhuk, Alexander
TI Scalar and vector perturbations in a universe with discrete and
continuous matter sources
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE cosmological perturbation theory; dark energy theory; gravity
ID COSMOLOGICAL PERTURBATIONS; DARK-MATTER; NETWORKS; ENERGY
AB We study a universe filled with dust-like matter in the form of discrete inhomogeneities (e.g., galaxies and their groups and clusters) and two sets of perfect fluids with linear and nonlinear equations of state, respectively. The background spacetime geometry is defined by the FLRW metric. In the weak gravitational field limit, we develop the first-order scalar and vector cosmological perturbation theory. Our approach works at all cosmological scales (i.e. sub-horizon and super-horizon ones) and incorporates linear and nonlinear effects with respect to energy density fluctuations. We demonstrate that the scalar perturbation (i.e. the gravitational potential) as well as the vector perturbation can be split into individual contributions from each matter source. Each of these contributions satisfies its own equation. The velocity-independent parts of the individual gravitational potentials are characterized by a finite time-dependent Yukawa interaction range being the same for each individual contribution. We also obtain the exact form of the gravitational potential and vector perturbation related to the discrete matter sources. The self-consistency of our approach is thoroughly checked. The derived equations can form the theoretical basis for numerical simulations for a wide class of cosmological models.
C1 [Eingorn, Maxim] North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.
[Eingorn, Maxim] NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA.
[Eingorn, Maxim; Kiefer, Claus] Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
[Zhuk, Alexander] Odessa Natl Univ, Astron Observ, Dvoryanskaya St 2, UA-65082 Odessa, Ukraine.
RP Eingorn, M (reprint author), North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
EM maxim.eingorn@gmail.com; kiefer@thp.uni-koeln.de; ai.zhuk2@gmail.com
FU Albert's Researcher Reunion Grant of the University of Cologne
FX The work of M. Eingorn was partially supported by an Albert's Researcher
Reunion Grant of the University of Cologne.
NR 39
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Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD SEP
PY 2016
IS 9
AR 032
DI 10.1088/1475-7516/2016/09/032
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EE7CM
UT WOS:000389772300017
ER
PT J
AU Eliasson, B
Speirs, DC
Daldorff, LKS
AF Eliasson, B.
Speirs, D. C.
Daldorff, L. K. S.
TI Electrostatic electron cyclotron instabilities near the upper hybrid
layer due to electron ring distributions
SO PLASMA PHYSICS AND CONTROLLED FUSION
LA English
DT Article
DE electron cyclotron instability; electron Bernstein waves; ring
distribution
ID STIMULATED ELECTROMAGNETIC EMISSION; BROAD UPSHIFTED MAXIMUM;
MAGNETIC-FIELD; PLASMA-WAVES; BERNSTEIN MODES; SIMULATION; SPACE;
HARMONICS; RADIATION; DISCHARGE
AB A theoretical study is presented of the electrostatic electron cyclotron instability involving Bernstein modes in a magnetized plasma. The presence of a tenuous thermal ring distribution in a Maxwellian plasma decreases the frequency of the upper hybrid branch of the electron Bernstein mode until it merges with the nearest lower branch with a resulting instability. The instability occurs when the upper hybrid frequency is somewhat above the third, fourth, and higher electron cyclotron harmonics, and gives rise to a narrow spectrum of waves around the electron cyclotron harmonic nearest to the upper hybrid frequency. For a tenuous cold ring distribution together with a Maxwellian distribution an instability can take place also near the second electron cyclotron harmonic. Noise-free Vlasov simulations are used to assess the theoretical linear growth-rates and frequency spectra, and to study the nonlinear evolution of the instability. The relevance of the results to laboratory and ionospheric heating experiments is discussed.
C1 [Eliasson, B.; Speirs, D. C.] Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland.
[Daldorff, L. K. S.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA.
[Daldorff, L. K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Eliasson, B (reprint author), Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland.
EM bengt.eliasson@strath.ac.uk
FU Engineering and Physical Sciences Research Council (EPSRC), U.K.
[EP/M009386/1]
FX Discussions with Thomas Leyser at the Swedish Institute of Space Physics
are gratefully acknowledged. This work was supported by the Engineering
and Physical Sciences Research Council (EPSRC), U.K., Grant no.
EP/M009386/1. Simulation data supporting the figures are available at
http://dx.doi.org/10.15129/56448d9e-adb0-4d2b-afdb-029165a40f54.
NR 50
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0741-3335
EI 1361-6587
J9 PLASMA PHYS CONTR F
JI Plasma Phys. Control. Fusion
PD SEP
PY 2016
VL 58
IS 9
AR 095002
DI 10.1088/0741-3335/58/9/095002
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA EE2TI
UT WOS:000389437000002
ER
PT J
AU Bartholomaus, TC
Stearns, LA
Sutherland, DA
Shroyer, EL
Nash, JD
Walker, RT
Catania, G
Felikson, D
Carroll, D
Fried, MJ
Noel, BPY
Van Den Broeke, MR
AF Bartholomaus, Timothy C.
Stearns, Leigh A.
Sutherland, David A.
Shroyer, Emily L.
Nash, Jonathan D.
Walker, Ryan T.
Catania, Ginny
Felikson, Denis
Carroll, Dustin
Fried, Mason J.
Noel, Brice P. Y.
Van Den Broeke, Michiel R.
TI Contrasts in the response of adjacent fjords and glaciers to ice-sheet
surface melt in West Greenland
SO ANNALS OF GLACIOLOGY
LA English
DT Article
DE atmosphere/ice/ocean interactions; ice velocity; ice/ocean interactions;
iceberg calving; subglacial processes
ID SIGNIFICANT SUBMARINE MELT; JAKOBSHAVN ISBRAE; OUTLET GLACIERS; OCEAN
WATERS; SOUTHEAST GREENLAND; TIDEWATER GLACIER; HELHEIM GLACIER;
MASS-BALANCE; DYNAMICS; TERMINUS
AB Neighboring tidewater glaciers often exhibit asynchronous dynamic behavior, despite relatively uniform regional atmospheric and oceanic forcings. This variability may be controlled by a combination of local factors, including glacier and fjord geometry, fjord heat content and circulation, and glacier surface melt. In order to characterize and understand contrasts in adjacent tidewater glacier and fjord dynamics, we made coincident ice-ocean-atmosphere observations at high temporal resolution (minutes to weeks) within a 10 000 km(2) area near Uummannaq, Greenland. Water column velocity, temperature and salinity measurements reveal systematic differences in neighboring fjords that imply contrasting circulation patterns. The observed ocean velocity and hydrography, combined with numerical modeling, suggest that subglacial discharge plays a major role in setting fjord conditions. In addition, satellite remote sensing of seasonal ice flow speed and terminus position reveal both speedup and slow-down in response to melt, as well as differences in calving style among the neighboring glaciers. Glacier force budgets and modeling also point toward subglacial discharge as a key factor in glacier behavior. For the studied region, individual glacier and fjord geometry modulate subglacial discharge, which leads to contrasts in both fjord and glacier dynamics.
C1 [Bartholomaus, Timothy C.; Catania, Ginny; Felikson, Denis; Fried, Mason J.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
[Stearns, Leigh A.] Univ Kansas, Lawrence, KS 66045 USA.
[Sutherland, David A.; Carroll, Dustin] Univ Oregon, Eugene, OR 97403 USA.
[Shroyer, Emily L.; Nash, Jonathan D.] Oregon State Univ, Corvallis, OR 97331 USA.
[Walker, Ryan T.] Univ Maryland, Greenbelt, MD USA.
[Walker, Ryan T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Noel, Brice P. Y.; Van Den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands.
RP Bartholomaus, TC (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
EM tbartholomaus@ig.utexas.edu
RI Van den Broeke, Michiel/F-7867-2011; Catania, Ginny/B-9787-2008;
OI Van den Broeke, Michiel/0000-0003-4662-7565; Bartholomaus,
Timothy/0000-0002-1470-6720; Felikson, Denis/0000-0002-3785-5112
FU National Aeronautics and Space Administration [NNX12AP50G]; University
of Texas Institute for Geophysics; Polar Program of the Netherlands
Organization for Scientific Research (NOW/ALW)
FX This work was partially supported by the National Aeronautics and Space
Administration through grant NNX12AP50G. T.C.B. was supported by a
postdoctoral fellowship from the University of Texas Institute for
Geophysics. We acknowledge field support from CH2MHill Polar Services
and the captain and crew of the R/V Sanna. We thank Ian Joughin for
deriving glacier velocities from TerraSAR-X scenes within our area and
the Polar Geospatial Center for providing World View imagery. B.N. and
M.vdB. acknowledge support of the Polar Program of the Netherlands
Organization for Scientific Research (NOW/ALW). The constructive
critiques of two anonymous reviewers significantly improved the quality
and clarity of this publication.
NR 75
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U2 8
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 0260-3055
EI 1727-5644
J9 ANN GLACIOL
JI Ann. Glaciol.
PD SEP
PY 2016
VL 57
IS 73
BP 25
EP 38
DI 10.1017/aog.2016.19
PG 14
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA ED6GJ
UT WOS:000388953800005
ER
PT J
AU Shuman, C
Scambos, T
Berthier, E
AF Shuman, Christopher
Scambos, Ted
Berthier, Etienne
TI Ice loss processes in the Seal Nunataks ice shelf region from satellite
altimetry and imagery
SO ANNALS OF GLACIOLOGY
LA English
DT Article
DE Antarctic glaciology; ice shelves; remote sensing
ID ANTARCTIC PENINSULA; MASS-BALANCE; LARSEN; SHEET; ELEVATION; GLACIERS;
DISINTEGRATION; RESOLUTION; DISCHARGE; TRIBUTARY
AB The Seal Nunataks ice shelf (SNIS, similar to 743 km(2) in 2013) is an unofficial name for a remnant area between the former Larsen A and Larsen B ice shelves off the northeastern Antarctic Peninsula. Analyses using Landsat 7 ETM+ and Terra ASTER images from 2001 to 13 and ICESat altimetry from 2003 to 09 show it has retreated and thinned following the Larsen A (1995) and Larsen B (2002) disintegrations. Despite some regional cooling and more fast ice since 2008, SNIS continues to lose ice along its margins and may be losing contact with some nunataks. Detailed analysis of data from four ICESat tracks indicates that ice shelf thinning rates range between 1.9 and 2.7 m a(-1), and generally increase from west to east. An ICESat repeat track crossing the adjacent Robertson Island shows a mean elevation loss of 1.8 m a(-1). Two tracks crossing the SNIS's remaining tributary, Rogosh Glacier, show sub-meter elevation losses. Comparing shelf remnant and grounded ice thinning rates implies that basal ocean melting augments SNIS thinning by similar to 1 m a(-1), a rate that is consistent with other estimates of ocean-driven shelf thinning in the region.
C1 [Shuman, Christopher] NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA.
[Scambos, Ted] Univ Colorado Boulder, CIRES, NSIDC, Boulder, CO USA.
[Berthier, Etienne] Univ Toulouse, UPS, CNRS, CNES,IRD,LEGOS, Toulouse, France.
RP Shuman, C (reprint author), NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA.
EM Christopher.A.Shuman@nasa.gov
RI Berthier, Etienne/B-8900-2009
OI Berthier, Etienne/0000-0001-5978-9155
FU NSF [NSF ANT-0732921]; NASA [NASA NNX10AR76G]; TOSCA program of the
French Space Agency (CNES); ISIS program of the French Space Agency
(CNES); NASA
FX The authors would like to acknowledge the support of H. Pritchard for
additional insights on a previously published analysis for the area
(Pritchard and others, 2012). The authors would also like to thank J.
Bohlander, K. Melocik, V. Suchdeo, and P. Vornberger for help with
aspects of the imagery analysis. This project also benefitted from the
help of M. Siegfried and L. Padman regarding the best available ocean
tide model for the ICESat data. The ICESat data for this paper are
available at the NASA Distributed Active Archive Center at the National
Snow and Ice Data Center (GLA12 - GLAS/ICESat L2 Antarctic and Greenland
Ice Sheet Altimetry Data). The Landsat data were acquired at no cost via
the Earth Explorer website from the US Geological Survey's Earth
Resource Observation and Science Center (EROS), home of the national
archive for Landsat imagery. The ASTER data were provided at no cost
through the Global Land Ice Measurements from Space (GLIMS) project.
This work was supported by NSF and NASA grants to T. Scambos (NSF
ANT-0732921; NASA NNX10AR76G), the TOSCA and ISIS programs of the French
Space Agency (CNES) to E. Berthier, and NASA Cryospheric Sciences
Program funds to C. Shuman. The final paper benefitted from the many
helpful comments provided by two anonymous reviewers.
NR 50
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PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 0260-3055
EI 1727-5644
J9 ANN GLACIOL
JI Ann. Glaciol.
PD SEP
PY 2016
VL 57
IS 73
BP 94
EP 104
DI 10.1017/aog.2016.29
PG 11
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA ED6GJ
UT WOS:000388953800012
ER
PT J
AU Geller, MA
Zhou, TH
Shindell, D
Ruedy, R
Aleinov, I
Nazarenko, L
Tausnev, NL
Kelley, M
Sun, S
Cheng, Y
Field, RD
Faluvegi, G
AF Geller, Marvin A.
Zhou, Tiehan
Shindell, D.
Ruedy, R.
Aleinov, I.
Nazarenko, L.
Tausnev, N. L.
Kelley, M.
Sun, S.
Cheng, Y.
Field, R. D.
Faluvegi, G.
TI Modeling the QBO-Improvements resulting from higher-model vertical
resolution
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE modeling the QBO; fine vertical resolution; other model improvements
ID QUASI-BIENNIAL OSCILLATION; STRATOSPHERIC WATER-VAPOR; TROPICAL
TROPOPAUSE; GENERAL-CIRCULATION; ATMOSPHERE MODEL; GLOBAL CLIMATE;
GRAVITY-WAVES; TRANSPORT; SIMULATION; CHEMISTRY
AB Using the NASA Goddard Institute for Space Studies (GISS) climate model, it is shown that with proper choice of the gravity wave momentum flux entering the stratosphere and relatively fine vertical layering of at least 500 m in the upper troposphere-lower stratosphere (UTLS), a realistic stratospheric quasi-biennial oscillation (QBO) is modeled with the proper period, amplitude, and structure down to tropopause levels. It is furthermore shown that the specified gravity wave momentum flux controls the QBO period whereas the width of the gravity wave momentum flux phase speed spectrum controls the QBO amplitude. Fine vertical layering is required for the proper downward extension to tropopause levels as this permits wave-mean flow interactions in the UTLS region to be resolved in the model. When vertical resolution is increased from 1000 to 500 m, the modeled QBO modulation of the tropical tropopause temperatures increasingly approach that from observations, and the tape recorder of stratospheric water vapor also approaches the observed. The transport characteristics of our GISS models are assessed using age-of-air and N2O diagnostics, and it is shown that some of the deficiencies in model transport that have been noted in previous GISS models are greatly improved for all of our tested model vertical resolutions. More realistic tropical-extratropical transport isolation, commonly referred to as the tropical pipe, results from the finer vertical model layering required to generate a realistic QBO.
C1 [Geller, Marvin A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Zhou, Tiehan; Ruedy, R.; Aleinov, I.; Nazarenko, L.; Tausnev, N. L.; Kelley, M.; Cheng, Y.; Field, R. D.; Faluvegi, G.] NASA Goddard Inst Space Studies, New York, NY USA.
[Zhou, Tiehan; Aleinov, I.; Nazarenko, L.; Cheng, Y.; Faluvegi, G.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Shindell, D.] Duke Univ, Nicholas Sch Environm, Earth & Ocean Sci, Durham, NC 27708 USA.
[Ruedy, R.; Tausnev, N. L.; Kelley, M.] Trinnovim LLC, New York, NY USA.
[Sun, S.] NOAA Earth Syst Res Lab, Boulder, CO USA.
[Field, R. D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Geller, MA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
EM marvin.geller@stonybrook.edu
FU NASA Modeling, Analysis and Prediction Program; NASA High-End Computing
(HEC) Program through NASA Center for Climate Simulation (NCCS) at
Goddard Space Flight Center
FX This work was supported by the NASA Modeling, Analysis and Prediction
Program and the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center.
Data from these runs are available from Tiehan Zhou
(tz2131@columbia.edu). We thank Jae N. Lee for kindly providing the AURA
MLS water vapor data. The authors acknowledge the two anonymous
reviewers for their helpful comments, which led to an improved paper.
NR 49
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD SEP
PY 2016
VL 8
IS 3
BP 1092
EP 1105
DI 10.1002/2016MS000699
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EC0LV
UT WOS:000387793500004
PM 27917258
ER
PT J
AU Pithan, F
Ackerman, A
Angevine, WM
Hartung, K
Ickes, L
Kelley, M
Medeiros, B
Sandu, I
Steeneveld, GJ
Sterk, HAM
Svensson, G
Vaillancourt, PA
Zadra, A
AF Pithan, Felix
Ackerman, Andrew
Angevine, Wayne M.
Hartung, Kerstin
Ickes, Luisa
Kelley, Maxwell
Medeiros, Brian
Sandu, Irina
Steeneveld, Gert-Jan
Sterk, H. A. M.
Svensson, Gunilla
Vaillancourt, Paul A.
Zadra, Ayrton
TI Select strengths and biases of models in representing the Arctic winter
boundary layer over sea ice: the Larcform 1 single column model
intercomparison
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE Arctic; boundary-layer; mixed-phase clouds; models; intercomparison;
inversion
ID LARGE-EDDY SIMULATIONS; CLIMATE MODELS; CLOUDS; PARAMETERIZATION;
PRECIPITATION; INVERSIONS; RADIATION; SYSTEM; SHEBA
AB Weather and climate models struggle to represent lower tropospheric temperature and moisture profiles and surface fluxes in Arctic winter, partly because they lack or misrepresent physical processes that are specific to high latitudes. Observations have revealed two preferred states of the Arctic winter boundary layer. In the cloudy state, cloud liquid water limits surface radiative cooling, and temperature inversions are weak and elevated. In the radiatively clear state, strong surface radiative cooling leads to the build-up of surface-based temperature inversions. Many large-scale models lack the cloudy state, and some substantially underestimate inversion strength in the clear state. Here, the transformation from a moist to a cold dry air mass is modeled using an idealized Lagrangian perspective. The trajectory includes both boundary layer states, and the single-column experiment is the first Lagrangian Arctic air formation experiment (Larcform 1) organized within GEWEX GASS (Global atmospheric system studies). The intercomparison reproduces the typical biases of large-scale models: some models lack the cloudy state of the boundary layer due to the representation of mixed-phase microphysics or to the interaction between micro- and macrophysics. In some models, high emissivities of ice clouds or the lack of an insulating snow layer prevent the build-up of surface-based inversions in the radiatively clear state. Models substantially disagree on the amount of cloud liquid water in the cloudy state and on turbulent heat fluxes under clear skies. Observations of air mass transformations including both boundary layer states would allow for a tighter constraint of model behavior.
C1 [Pithan, Felix] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Ackerman, Andrew; Kelley, Maxwell] NASA Goddard Inst Space Studies, New York, NY USA.
[Angevine, Wayne M.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Angevine, Wayne M.] NOAA Earth Syst Res Lab, Boulder, CO USA.
[Hartung, Kerstin; Svensson, Gunilla] Stockholm Univ, Dept Meteorol, Stockholm, Sweden.
[Ickes, Luisa] ETHZ, Inst Atmosphere & Climate, Zurich, Switzerland.
[Medeiros, Brian] NCAR, Boulder, CO USA.
[Sandu, Irina] ECMWF, Reading, Berks, England.
[Steeneveld, Gert-Jan; Sterk, H. A. M.] Wageningen Univ, Meteorol & Air Qual Sect, Wageningen, Netherlands.
[Vaillancourt, Paul A.; Zadra, Ayrton] Environm Canada, Rech Previs Numer Atmospher, Dorval, PQ, Canada.
RP Pithan, F (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM felix.pithan@awi.de
RI Steeneveld, Gert-Jan/B-2816-2010; Manager, CSD Publications/B-2789-2015
OI Steeneveld, Gert-Jan/0000-0002-5922-8179;
FU GASS (Global atmospheric system studies) steering group; ERC under
Marie-Curie grant UACSURF [GAP-654492]; NASA MAP program; NWO
[863.10.010, 829.09.005]; Regional and Global Climate Modeling Program
of the U.S. Department of Energy's Office of Science
[DE-FC02-97ER62402]; National Science Foundation; Swedish e-Science
Research Centre SeRC
FX We gratefully acknowledge support from the GASS (Global atmospheric
system studies) steering group. We thank the researchers involved in the
collection of SHEBA and ARM data for making their data sets available,
and the modeling groups, the Program for Climate Model Diagnosis and
Intercomparison and the World Climate Research Program's Working Group
on Coupled Modeling for making available the CMIP5 multimodel data set.
F.P. was funded by the ERC under Marie-Curie grant UACSURF (GAP-654492)
for parts of this study. AA and MK were funded by the NASA MAP program.
GJS acknowledges funding from NWO contract 863.10.010. M.S. acknowledges
the support from NWO (The Dutch Science Foundation) with grant
829.09.005 ("Quantifying contributions of surface climate feedbacks to
the Arctic amplification of greenhouse warming'' in the Sustainable
Earth program). B.M. was supported by the Regional and Global Climate
Modeling Program of the U.S. Department of Energy's Office of Science,
Cooperative Agreement DE-FC02-97ER62402. NCAR is sponsored by the
National Science Foundation. K.H. was supported by the Swedish e-Science
Research Centre SeRC. Thanks to Bert Holtslag for comments on an earlier
version of this manuscript, and to Thorsten Mauritsen for advice and
support in the development of the case. We gratefully acknowledge the
input and advice of two anonymous reviewers. Model results are available
at https://doi.org/10.1594/PANGAEA.856770.
NR 50
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD SEP
PY 2016
VL 8
IS 3
BP 1345
EP 1357
DI 10.1002/2016MS000630
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EC0LV
UT WOS:000387793500017
ER
PT J
AU Hudson, J
Spangelo, S
Hine, A
Kolosa, D
Lemmer, K
AF Hudson, Jennifer
Spangelo, Sara
Hine, Andrew
Kolosa, Daniel
Lemmer, Kristina
TI Mission Analysis for CubeSats with Micropropulsion
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID ORBIT TRANSFERS; PROPULSION; THRUSTER
AB The orbital maneuver capabilities of several CubeSat propulsion systems are analyzed using trajectory simulations. Properties of several types of developmental micropropulsion systems are reviewed, and Delta V capabilities are compared. Mission simulations are used to analyze the relationship between thrust arc length and orbit change capability in a low-thrust spiral trajectory. Constraints on power, fuel mass, and mission duration, as well as system-level constraints, are considered. Feasible CubeSat architectures and mission designs are developed for three electric propulsion systems. The most effective combinations of thruster operational modes and trajectory control strategies are discussed.
C1 [Hudson, Jennifer; Hine, Andrew; Kolosa, Daniel; Lemmer, Kristina] Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA.
[Spangelo, Sara] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Hudson, J (reprint author), Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA.
FU NASA [NNX13AR18A]
FX The authors acknowledge support from NASA cooperative agreement
NNX13AR18A.
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U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2016
VL 53
IS 5
BP 836
EP 846
DI 10.2514/1.A33564
PG 11
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400006
ER
PT J
AU Blandino, JJ
Martinez-Baquero, N
Demetriou, MA
Gatsonis, NA
Paschalidis, N
AF Blandino, John J.
Martinez-Baquero, Nicolas
Demetriou, Michael A.
Gatsonis, Nikolaos A.
Paschalidis, Nicholas
TI Feasibility for Orbital Life Extension of a CubeSat in the Lower
Thermosphere
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 54th AIAA Aerospace Sciences Meeting / AIAA Science and Technology Forum
and Exposition
CY JAN 04-08, 2016
CL San Diego, CA
SP AIAA
ID ATMOSPHERE; SATELLITE; THRUSTER; MISSION
AB Orbital flight of CubeSats at altitudes between 150 and 250 km has the potential to enable a new class of scientific, commercial, and defense-related missions. A study is presented to demonstrate the feasibility of extending the orbital lifetime of a CubeSat in a 210 km orbit. Propulsion consists of an electrospray thruster operating at a 2 W, 0.175 mN thrust, and an specific impulse (Isp) of 500 s. The mission consists of two phases. In phase 1, the CubeSat is deployed from a 414 km orbit and uses the thruster to deorbit to the target altitude of 210 km. In phase 2, the propulsion system is used to extend the mission lifetime until propellant is fully expended. A control algorithm based on maintaining a target orbital energy is presented that uses an extended Kalman filter to generate estimates of the orbital dynamic state, which are periodically updated by Global Positioning System measurements. For phase 1, the spacecraft requires 25.21 days to descend from 414 to 210 km, corresponding to a Delta V = 96.25 m/s and a propellant consumption of 77.8 g. Phase 2 lasts 57.83 days, corresponding to a Delta V = 119.15 m/s, during which the remaining 94.2 g of propellant are consumed.
C1 [Blandino, John J.; Martinez-Baquero, Nicolas; Demetriou, Michael A.; Gatsonis, Nikolaos A.] Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
[Paschalidis, Nicholas] NASA, Goddard Space Flight Ctr, Technol, Greenbelt, MD 20771 USA.
RP Blandino, JJ (reprint author), Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
NR 29
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2016
VL 53
IS 5
BP 864
EP 875
DI 10.2514/1.A33462
PG 12
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400008
ER
PT J
AU Shapiro, AA
Borgonia, JP
Chen, QN
Dillon, RP
McEnerney, B
Polit-Casillas, R
Soloway, L
AF Shapiro, A. A.
Borgonia, J. P.
Chen, Q. N.
Dillon, R. P.
McEnerney, B.
Polit-Casillas, R.
Soloway, L.
TI Additive Manufacturing for Aerospace Flight Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID INCONEL 718; LASER; STEEL; DEPOSITION; CERAMICS; PARTS; MICROSTRUCTURE;
OPTIMIZATION; ELECTRONICS; FABRICATION
AB Additive manufacturing can provide many advantages to the future of space flight. Although it has been in use for plastic prototyping applications, it is only more recently that additive technologies have been investigated to produce metal and ceramic flight parts. This review paper presents some of the specific issues that arise for space flight applications, including materials selection, processing and postprocessing parameters, and the qualification process. With these concerns in mind, there are seven main applications in which additive manufacturing can provide a benefit. These applications include innovative design strategies that use the unique parameters of additive manufacturing, as well as some specific uses such as mass reduction or in situ production in space.
C1 [Shapiro, A. A.] CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA.
[Borgonia, J. P.; Dillon, R. P.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 170-104, Pasadena, CA 91109 USA.
[Chen, Q. N.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 158-103, Pasadena, CA 91109 USA.
[McEnerney, B.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA.
[Polit-Casillas, R.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 154-410, Pasadena, CA 91109 USA.
[Soloway, L.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, 4800 Oak Grove Dr,M-S 180-502, Pasadena, CA 91109 USA.
RP Shapiro, AA (reprint author), CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA.
NR 43
TC 0
Z9 0
U1 20
U2 20
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2016
VL 53
IS 5
BP 952
EP 959
DI 10.2514/1.A33544
PG 8
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400015
ER
PT J
AU Jacobson, AR
Holzworth, RH
Pfaff, R
Heelis, R
AF Jacobson, Abram R.
Holzworth, Robert H.
Pfaff, Robert
Heelis, Roderick
TI Automated identification of discrete, lightning-generated,
multiple-dispersed whistler waves in C/NOFS-VEFI very low frequency
observations
SO RADIO SCIENCE
LA English
DT Article
ID LOW-LATITUDE IONOSPHERE; RADIATION BELT; TEMPORAL SIGNATURES; TWEEK
ATMOSPHERICS; LOCATION NETWORK; PLASMASPHERE; PROPAGATION; ORIGIN; GUIDE
AB Automated wave feature detection is required to efficiently analyze large archives of very low frequency broadband recordings for discrete whistler identification and feature extraction. We describe a new method to do this, even in the presence of simultaneous, multiple whistler phase dispersions. Previous techniques of whistler identification were unable to deal with simultaneous, multiple phase dispersions. We demonstrate the new method with data from the Vector Electric Field Investigation (VEFI) payload on the Communication/Navigation Outage Forecast System (C/NOFS) satellite, from the mission years 2008-2014.
C1 [Jacobson, Abram R.; Holzworth, Robert H.] Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA.
[Pfaff, Robert] NASA, Goddard Spaceflight Ctr, Greenbelt, MD USA.
[Heelis, Roderick] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA.
RP Jacobson, AR (reprint author), Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA.
EM abramj@u.washington.edu
FU NSF [1443011]
FX This work was partially supported by NSF grant 1443011,
"Wave-vector-resolved Study of Lightning Whistler Propagation and
Energetics in the Low-latitude Plasmasphere." Readers wishing to examine
the original data are invited to contact the corresponding author.
NR 37
TC 0
Z9 0
U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD SEP
PY 2016
VL 51
IS 9
BP 1547
EP 1569
DI 10.1002/2016RS005989
PG 23
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA ED6EI
UT WOS:000388947900009
ER
PT J
AU Wilson, SA
Howard, AD
Moore, JM
Grant, JA
AF Wilson, Sharon A.
Howard, Alan D.
Moore, Jeffrey M.
Grant, John A.
TI A cold-wet middle-latitude environment on Mars during the
Hesperian-Amazonian transition: Evidence from northern Arabia valleys
and paleolakes
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GALE CRATER; TERRA-CIMMERIA; SURFACE RUNOFF; ALLUVIAL FANS; EVOLUTION;
ORIGIN; PRECIPITATION; NETWORKS; IMPACTS; SYSTEMS
AB The growing inventory of post-Noachian fluvial valleys may represent a late, widespread episode of aqueous activity on Mars, contrary to the paradigm that fluvial activity largely ceased around the Noachian-Hesperian boundary. Fresh shallow valleys (FSVs) are widespread from similar to 30 to 45 degrees in both hemispheres with a high concentration in northern Arabia Terra. Valleys in northern Arabia Terra characteristically start abruptly on steeper slopes and terminate in topographic depressions at elevations corresponding to model-predicted lake levels. Longer valley systems flowed into and out of chains of paleolakes. Minimum discharges based on the dimensions of the incised channel assuming medium to coarse sand-size grains ranges from tens to hundreds of m(3) s(-1), respectively, consistent with formation via snowmelt from surface or sub-ice flows. Hydrologic calculations indicate the valleys likely formed in hundreds of years or less, and crater statistics constrain the timing of fluvial activity to between the Hesperian and middle Amazonian. Several craters with channels extending radially outward supports evidence for overflow of interior crater lakes possibly fed by groundwater. Most FSVs occur away from young impact craters which make an association with impact processes improbable. The widespread occurrence of FSVs along with their similar morphology and shared modest state of degradation is consistent with most forming during a global interval of favorable climate, perhaps contemporaneous with alluvial fan formation in equatorial and midlatitudes. Evidence for a snowmelt-based hydrology and considerable depths of water on the landscape in Arabia supports a cold, wet, and possibly habitable environment late in Martian history.
C1 [Wilson, Sharon A.; Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Wilson, Sharon A.; Howard, Alan D.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Wilson, SA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.; Wilson, SA (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
EM wilsons@si.edu
FU NASA [12-MDAP12-0033]
FX Thanks to Cathy Quantin-Nataf and Nick Warner for their insightful
reviews and to Caleb Fassett for his Associate Editor evaluation. This
work was supported by a NASA grant 12-MDAP12-0033 from the Mars Data
Analysis Program. The data used are listed in the figures, tables,
supplemental material, and or repository at
http://airandspace.si.edu/CEPSData.
NR 82
TC 1
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U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1667
EP 1694
DI 10.1002/2016JE005052
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400006
ER
PT J
AU Miljkovic, K
Collins, GS
Wieczorek, MA
Johnson, BC
Soderblom, JM
Neumann, GA
Zuber, MT
AF Miljkovic, K.
Collins, G. S.
Wieczorek, M. A.
Johnson, B. C.
Soderblom, J. M.
Neumann, G. A.
Zuber, M. T.
TI Subsurface morphology and scaling of lunar impact basins
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID INNER SOLAR-SYSTEM; POLE-AITKEN BASIN; HEAVY BOMBARDMENT; MASCON BASINS;
MARE BASALTS; MOON; ORIGIN; GRAVITY; GRAIL; CRUST
AB Impact bombardment during the first billion years after the formation of the Moon produced at least several tens of basins. The Gravity Recovery and Interior Laboratory (GRAIL) mission mapped the gravity field of these impact structures at significantly higher spatial resolution than previous missions, allowing for detailed subsurface and morphological analyses to be made across the entire globe. GRAIL-derived crustal thickness maps were used to define the regions of crustal thinning observed in centers of lunar impact basins, which represents a less unambiguous measure of a basin size than those based on topographic features. The formation of lunar impact basins was modeled numerically by using the iSALE-2D hydrocode, with a large range of impact and target conditions typical for the first billion years of lunar evolution. In the investigated range of impactor and target conditions, the target temperature had the dominant effect on the basin subsurface morphology. Model results were also used to update current impact scaling relationships applicable to the lunar setting (based on assumed target temperature). Our new temperature-dependent impact-scaling relationships provide estimates of impact conditions and transient crater diameters for the majority of impact basins mapped by GRAIL. As the formation of lunar impact basins is associated with the first similar to 700 Myr of the solar system evolution when the impact flux was considerably larger than the present day, our revised impact scaling relationships can aid further analyses and understanding of the extent of impact bombardment on the Moon and terrestrial planets in the early solar system.
C1 [Miljkovic, K.; Johnson, B. C.; Soderblom, J. M.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Miljkovic, K.] Curtin Univ, Dept Appl Geol, Perth, WA, Australia.
[Collins, G. S.] Imperial Coll London, Dept Earth Sci & Engn, London, England.
[Wieczorek, M. A.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, Paris, France.
[Johnson, B. C.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Neumann, G. A.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Miljkovic, K (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.; Miljkovic, K (reprint author), Curtin Univ, Dept Appl Geol, Perth, WA, Australia.
EM katarina.miljkovic@curtin.edu.au
RI Neumann, Gregory/I-5591-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Soderblom,
Jason/0000-0003-3715-6407; Collins, Gareth/0000-0002-6087-6149
FU NASA; French Space Agency (CNES); STFC [ST/N000803/1]
FX The GRAIL mission is supported by the Discovery Program of NASA and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology.
Additional support for this work was provided by the French Space Agency
(CNES). We gratefully acknowledge the developers of iSALE-2D, including
Kai Wunnemann, Dirk Elbeshausen, Boris Ivanov, and Jay Melosh. G.S.C.
was funded by STFC grant ST/N000803/1. The data used in this study are
attached as supporting information and are also available upon request
from the main author (Katarina. Miljkovic@curtin.edu.au).
NR 64
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U1 2
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1695
EP 1712
DI 10.1002/2016JE005038
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400007
ER
PT J
AU Fraeman, AA
Ehlmann, BL
Arvidson, RE
Edwards, CS
Grotzinger, JP
Milliken, RE
Quinn, DP
Rice, MS
AF Fraeman, A. A.
Ehlmann, B. L.
Arvidson, R. E.
Edwards, C. S.
Grotzinger, J. P.
Milliken, R. E.
Quinn, D. P.
Rice, M. S.
TI The stratigraphy and evolution of lower Mount Sharp from spectral,
morphological, and thermophysical orbital data sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL-CONDUCTIVITY MEASUREMENTS; GALE CRATER; REFLECTANCE
SPECTROSCOPY; LANDING SITE; PARTICULATE MATERIALS; SEDIMENTARY-ROCKS;
EARLY MARS; SULFATE; MINERALOGY; CONSTRAINTS
AB We have developed a refined geologic map and stratigraphy for lower Mount Sharp using coordinated analyses of new spectral, thermophysical, and morphologic orbital data products. The Mount Sharp group consists of seven relatively planar units delineated by differences in texture, mineralogy, and thermophysical properties. These units are (1-3) three spatially adjacent units in the Murray formation which contain a variety of secondary phases and are distinguishable by thermal inertia and albedo differences, (4) a phyllosilicate-bearing unit, (5) a hematite-capped ridge unit, (6) a unit associated with material having a strongly sloped spectral signature at visible near-infrared wavelengths, and (7) a layered sulfate unit. The Siccar Point group consists of the Stimson formation and two additional units that unconformably overlie the Mount Sharp group. All Siccar Point group units are distinguished by higher thermal inertia values and record a period of substantial deposition and exhumation that followed the deposition and exhumation of the Mount Sharp group. Several spatially extensive silica deposits associated with veins and fractures show that late-stage silica enrichment within lower Mount Sharp was pervasive. At least two laterally extensive hematitic deposits are present at different stratigraphic intervals, and both are geometrically conformable with lower Mount Sharp strata. The occurrence of hematite at multiple stratigraphic horizons suggests redox interfaces were widespread in space and/or in time, and future measurements by the Mars Science Laboratory Curiosity rover will provide further insights into the depositional settings of these and other mineral phases.
C1 [Fraeman, A. A.; Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Ehlmann, B. L.; Grotzinger, J. P.; Quinn, D. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Edwards, C. S.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Edwards, C. S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ USA.
[Milliken, R. E.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Rice, M. S.] Western Washington Univ, Dept Phys & Astron, Dept Geol, Bellingham, WA 98225 USA.
RP Fraeman, AA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM abigail.a.fraeman@jpl.nasa.gov
FU W.M. Keck Institution for Space Studies; Caltech; National Aeronautics
and Space Administration; National Aeronautics and Space Administration
through the internal Research and Technology Development program; MSL
Participating Scientist Program grant
FX We thank two anonymous reviewers for their careful reading and insight
comments that improved the quality of this manuscript. Thanks to Lulu
Pan for providing helpful advice on CRISM parameter mapping techniques,
Ara Oshagan for assistance in generating the HiRISE color mosaic, Dawn
Sumner for nomenclature guidance, and Kathryn Stack Morgan for fruitful
discussions about orbital mapping interpretations and sharing her
general knowledge of the Gale Crater geologic context. A.A.F. was
partially supported by a W.M. Keck Institution for Space Studies
Postdoctoral Fellowship and Caltech Geological and Planetary Sciences
Texaco Postdoctoral Fellowship. A portion of this research was also
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration and funded through the internal Research and Technology
Development program. B.L.E. was partially supported by an MSL
Participating Scientist Program grant. All raw data products supporting
the conclusions of this work can be obtained from the NASA Planetary
Data System (PDS).
NR 66
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1713
EP 1736
DI 10.1002/2016JE005095
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400008
PM 27867788
ER
PT J
AU Blewett, DT
Stadermann, AC
Susorney, HC
Ernst, CM
Xiao, ZY
Chabot, NL
Denevi, BW
Murchie, SL
McCubbin, FM
Kinczyk, MJ
Gillis-Davis, JJ
Solomon, SC
AF Blewett, David T.
Stadermann, Amanda C.
Susorney, Hannah C.
Ernst, Carolyn M.
Xiao, Zhiyong
Chabot, Nancy L.
Denevi, Brett W.
Murchie, Scott L.
McCubbin, Francis M.
Kinczyk, Mallory J.
Gillis-Davis, Jeffrey J.
Solomon, Sean C.
TI Analysis of MESSENGER high-resolution images of Mercury's hollows and
implications for hollow formation
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LOW-REFLECTANCE MATERIAL; DUAL IMAGING-SYSTEM; IMPACT CRATERS; SURFACE
VOLATILES; RAY SPECTROMETER; SULFUR; CARBON; MOON; EROS; STRATIGRAPHY
AB High-resolution images from MESSENGER provide morphological information on the nature and origin of Mercury's hollows, small depressions that likely formed when a volatile constituent was lost from the surface. Because graphite may be a component of the low-reflectance material that hosts hollows, we suggest that loss of carbon by ion sputtering or conversion to methane by proton irradiation could contribute to hollows formation. Measurements of widespread hollows in 565 images with pixel scales <20m indicate that the average depth of hollows is 24 +/- 16m. We propose that hollows cease to increase in depth when a volatile-depleted lag deposit becomes sufficiently thick to protect the underlying surface. The difficulty of developing a lag on steep topography may account for the common occurrence of hollows on crater central peaks and walls. Disruption of the lag, e.g., by secondary cratering, could restart growth of hollows in a location that had been dormant. Images at extremely high resolution (similar to 3 m/pixel) show that the edges of hollows are straight, as expected if the margins formed by scarp retreat. These highest-resolution images reveal no superposed impact craters, implying that hollows are very young. The width of hollows within rayed crater Balanchine suggests that the maximum time for lateral growth by 1 cm is similar to 10,000 yr. A process other than entrainment of dust by gases evolved in a steady-state sublimation-like process is likely required to explain the high-reflectance haloes that surround many hollows.
C1 [Blewett, David T.; Ernst, Carolyn M.; Chabot, Nancy L.; Denevi, Brett W.; Murchie, Scott L.; Kinczyk, Mallory J.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
[Stadermann, Amanda C.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Susorney, Hannah C.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Xiao, Zhiyong] China Univ Geosci, Wuhan, Peoples R China.
[Xiao, Zhiyong] Univ Oslo, Ctr Earth Evolut & Dynam, Oslo, Norway.
[McCubbin, Francis M.] NASA, Johnson Space Ctr, Houston, TX USA.
[Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA.
RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
EM david.blewett@jhuapl.edu
RI Murchie, Scott/E-8030-2015; Denevi, Brett/I-6502-2012
OI Murchie, Scott/0000-0002-1616-8751; Denevi, Brett/0000-0001-7837-6663
FU NASA [NAS5-97271, NASW-00002]; NASA MESSENGER Participating Scientist
grant [NNX08AN29G]; NASA/APL; NASA
FX We appreciate discussions on the physics of dust lofting with David
Jewitt (University of California, Los Angeles). Helpful reviews from
Rebecca Thomas (University of Colorado), an anonymous reviewer, and
Editor David Baratoux led us to make key improvements to this paper. The
MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory (APL) and NASW-00002 to the Carnegie Institution of
Washington. D.T.B. is supported by NASA MESSENGER Participating
Scientist grant NNX08AN29G. A.C.S. was supported by the NASA/APL
internship program. F.M.M. acknowledges support from the NASA Solar
System Workings Program. This work made use of the Integrated Software
for Imagers and Spectrometers (ISIS), which is a product maintained by
the U.S. Geological Survey Astrogeology Science Center. MESSENGER data
are available through the NASA Planetary Data System. Supporting
information "2016JE005070-ds01.txt" gives the file names of the 882
high-resolution images that contain hollows along with latitude,
longitude, and pixel scale. Supporting information
"2016JE005070-ds02.txt" contains information for the 2518 individual
depth measurements: file name, pixel scale, depth, latitude, and
longitude.
NR 64
TC 0
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1798
EP 1813
DI 10.1002/2016JE005070
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400013
ER
PT J
AU Trammell, HJ
Li, LM
Jiang, X
Pan, YF
Smith, MA
Bering, EA
Horst, SM
Vasavada, AR
Ingersoll, AP
Janssen, MA
West, RA
Porco, CC
Li, C
Simon, AA
Baines, KH
AF Trammell, Harold Justin
Li, Liming
Jiang, Xun
Pan, Yefeng
Smith, Mark A.
Bering, Edgar A., III
Horst, Sarah M.
Vasavada, Ashwin R.
Ingersoll, Andrew P.
Janssen, Michael A.
West, Robert A.
Porco, Carolyn C.
Li, Cheng
Simon, Amy A.
Baines, Kevin H.
TI Vortices in Saturn's Northern Hemisphere (2008-2015) observed by Cassini
ISS
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GROUND-BASED OBSERVATIONS; POLAR SPOT; THERMAL STRUCTURE; MOIST
CONVECTION; IMAGING SCIENCE; CLOUD STRUCTURE; VOYAGER IMAGES; JUPITER;
ATMOSPHERE; DYNAMICS
AB We use observations from the Imaging Science Subsystem on Cassini to create maps of Saturn's Northern Hemisphere (NH) from 2008 to 2015, a time period including a seasonal transition (i.e., spring equinox in 2009) and the 2010 giant storm. The processed maps are used to investigate vortices in the NH during the period of 2008-2015. All recorded vortices have diameters (east-west) smaller than 6000km except for the largest vortex that developed from the 2010 giant storm. The largest vortex decreased its diameter from similar to 11,000 km in 2011 to similar to 5000 km in 2015, and its average diameter is similar to 6500 km during the period of 2011-2015. The largest vortex lasts at least 4 years, which is much longer than the lifetimes of most vortices (less than 1 year). The largest vortex drifts to north, which can be explained by the beta drift effect. The number of vortices displays varying behaviors in the meridional direction, in which the 2010 giant storm significantly affects the generation and development of vortices in the middle latitudes (25-45 degrees N). In the higher latitudes (45-90 degrees N), the number of vortices also displays strong temporal variations. The solar flux and the internal heat do not directly contribute to the vortex activities, leaving the temporal variations of vortices in the higher latitudes (45-90 degrees N) unexplained.
C1 [Trammell, Harold Justin; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA.
[Li, Liming; Pan, Yefeng; Bering, Edgar A., III] Univ Houston, Dept Phys, Houston, TX 77004 USA.
[Smith, Mark A.] Univ Houston, Dept Chem, Houston, TX USA.
[Horst, Sarah M.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Vasavada, Ashwin R.; Janssen, Michael A.; West, Robert A.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ingersoll, Andrew P.; Li, Cheng] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Porco, Carolyn C.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
[Simon, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Li, LM (reprint author), Univ Houston, Dept Phys, Houston, TX 77004 USA.
EM lli7@central.uh.eduu
RI Simon, Amy/C-8020-2012; Horst, Sarah/A-9906-2010
OI Simon, Amy/0000-0003-4641-6186; Horst, Sarah/0000-0003-4596-0702
FU NASA ROSES Cassini Data Analysis and Participating Scientists program;
NASA ROSES Planetary Data Archiving, Restoration, and Tools program
FX We gratefully acknowledge the Cassini ISS team for recording the raw
data sets. We also acknowledge the support from the NASA ROSES Cassini
Data Analysis and Participating Scientists program and Planetary Data
Archiving, Restoration, and Tools program. Finally, we thank the two
anonymous reviewers for providing their constructive suggestions to
significantly improve the manuscript. We used the new Cassini data in
2015, which are not archived in the public Planetary Data System (PDS)
(https://pds.nasa.gov) yet. The 2015 Cassini ISS raw data will be
released by the Cassini ISS team and archived in the PDS in late 2016.
We cannot archive the processed 2015 data before the release of the ISS
raw data, so we plan to archive the data of the processed NH maps in the
atmospheres node of PDS (http://atmos.pds.nasa.gov) in the beginning of
2017 or so.
NR 48
TC 0
Z9 0
U1 5
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 SEP
PY 2016
VL 121
IS 9
BP 1814
EP 1826
DI 10.1002/2016JE005122
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400014
ER
PT J
AU Travinsky, A
Vorobiev, D
Ninkov, Z
Raisanen, AD
Pellish, J
Robberto, M
Heap, S
AF Travinsky, Anton
Vorobiev, Dmitry
Ninkov, Zoran
Raisanen, Alan D.
Pellish, Jonny
Robberto, Massimo
Heap, Sara
TI Effects of heavy ion radiation on digital micromirror device performance
SO OPTICAL ENGINEERING
LA English
DT Article
DE digital micromirror device; digital micromirror device; digital
micromirror array; multiobject spectrometer; multiple-object
spectroscopy; heavy-ion radiation
ID MULTIOBJECT SPECTROGRAPH; SPECTROMETER; SPECTROSCOPY; TELESCOPE
AB There is a pressing need in the astronomical community for space-suitable multiobject spectrometers (MOSs). Several digital micromirror device (DMD)-based prototype MOSs have been developed for ground-based observatories; however, their main use will come with deployment on a space-based mission. Therefore, the performance of DMDs under exoatmospheric radiation needs to be evaluated. DMDs were rewindowed with 2-mu m thick pellicle and tested under accelerated heavy-ion radiation (control electronics shielded from radiation), with a focus on the detection of single-event effects (SEEs) including latch-up events. Testing showed that while DMDs are sensitive to nondestructive ion-induced state changes, all SEEs are cleared with a soft reset (i.e., sending a pattern to the device). The DMDs did not experience single-event induced permanent damage or functional changes that required a hard reset (power cycle), even at high ion fluences. This suggests that the SSE rate burden will be manageable for a DMD-based instrument when exposed to solar particle fluxes and cosmic rays in orbit. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Travinsky, Anton; Vorobiev, Dmitry; Ninkov, Zoran] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
[Raisanen, Alan D.] Rochester Inst Technol, Dept Mfg & Mech Engn Technol, 78 Lomb Mem Dr, Rochester, NY 14623 USA.
[Pellish, Jonny; Heap, Sara] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Robberto, Massimo] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RP Travinsky, A (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
EM at4395@g.rit.edu
FU National Aeronautics and Space Administration (NASA) [NNX14AI62G S01]
FX This research was supported by the National Aeronautics and Space
Administration (NASA), Grant No. NNX14AI62G S01. We thank Dr. Vladimir
Horvat and Bruce Hyman from Texas A&M University Cyclotron Institute for
providing their prompt assistance during the testing and answering
practical questions about the facility. We thank Michael Douglas and
Benjamin Lee from Texas Instruments for productive discussions about DMD
performance under extreme conditions. We are also thankful to Mike
Buffalin and John "Sean" Greenslade from The Construct at RIT for
sharing their expertise in rapid manufacturing and help in producing
custom made parts for the test setup. Last but not least, we thank Emily
Berkson from Rochester Institute of Technology for her help with the
manuscript.
NR 34
TC 0
Z9 0
U1 1
U2 1
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2016
VL 55
IS 9
AR 094107
DI 10.1117/1.OE.55.9.094107
PG 8
WC Optics
SC Optics
GA EC6FV
UT WOS:000388232800037
ER
PT J
AU Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Banerjee, B
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Bilandl, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Buson, S
Carosi, A
Chatterjee, A
Clavero, R
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
da Vela, P
Dazzi, F
De Angelis, A
De Lotto, B
Wilhelmi, ED
Di Pierro, F
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Einecke, S
Glawion, DE
Elsaesser, D
Fernandez-Barra, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Giammaria, P
Godinovic, N
Munoz, AG
Gora, D
Guberman, D
Hadasch, D
Hahn, A
Hanabata, Y
Hayashida, M
Herrera, J
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kodani, K
Konno, Y
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Majumdar, P
Makariev, M
Manganaro, M
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Moretti, E
Nakajima, D
Neustroev, V
Niedzwieckil, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Nogues, L
Orito, R
Overkemping, A
Paiano, S
Palacio, J
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Pedaletti, G
Perri, L
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Saito, T
Satalecka, K
Schultz, C
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Stamerra, A
Steinbring, T
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Torres, DF
Toyama, T
Treves, A
Verguilov, V
Vovk, I
Ward, JE
Will, M
Wu, MH
Zanin, R
Blinov, DA
Chen, WP
Efimova, NV
Forne, E
Grishina, TS
Hovatta, T
Jordan, B
Kimeridze, GN
Kopatskaya, EN
Koptelova, E
Kurtanidze, OM
Kurtanidze, SO
Lahteenmaki, A
Larionov, VM
Larionova, EG
Larionova, LV
Ligustri, R
Lin, HC
McBreen, B
Morozova, DA
Nikolashvili, MG
Raiteri, CM
Ros, JA
Sadun, AC
Sigua, LA
Tornikoski, M
Troitsky, IS
Villata, M
AF Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Banerjee, B.
Bangale, P.
de Almeida, U. Barres
Barrio, J. A.
Gonzalez, J. Becerra
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Bilandl, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Buson, S.
Carosi, A.
Chatterjee, A.
Clavero, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
Wilhelmi, E. de Ona
Di Pierro, F.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Lopez, R. J. Garcia
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giammaria, P.
Godinovic, N.
Munoz, A. Gonzalez
Gora, D.
Guberman, D.
Hadasch, D.
Hahn, A.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Majumdar, P.
Makariev, M.
Manganaro, M.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Moretti, E.
Nakajima, D.
Neustroev, V.
Niedzwieckil, A.
Rosillo, M. Nievas
Nilsson, K.
Nishijima, K.
Noda, K.
Nogues, L.
Orito, R.
Overkemping, A.
Paiano, S.
Palacio, J.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Pedaletti, G.
Perri, L.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Rhode, W.
Ribo, M.
Rico, J.
Garcia, J. Rodriguez
Saito, T.
Satalecka, K.
Schultz, C.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Steinbring, T.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Torres, D. F.
Toyama, T.
Treves, A.
Verguilov, V.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Blinov, D. A.
Chen, W. P.
Efimova, N. V.
Forne, E.
Grishina, T. S.
Hovatta, T.
Jordan, B.
Kimeridze, G. N.
Kopatskaya, E. N.
Koptelova, E.
Kurtanidze, O. M.
Kurtanidze, S. O.
Lahteenmaki, A.
Larionov, V. M.
Larionova, E. G.
Larionova, L. V.
Ligustri, R.
Lin, H. C.
McBreen, B.
Morozova, D. A.
Nikolashvili, M. G.
Raiteri, C. M.
Ros, J. A.
Sadun, A. C.
Sigua, L. A.
Tornikoski, M.
Troitsky, I. S.
Villata, M.
CA Magic Collaboration
TI Long-term multi-wavelength variability and correlation study of
Markarian 421 from 2007 to 2009
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astroparticle physics; BL Lacertae objects: individual: Markarian 421;
radiation mechanisms: non-thermal
ID X-RAY; MAGIC TELESCOPES; MAJOR UPGRADE; TEV PHOTONS; CRAB-NEBULA;
EMISSION; BLAZAR; RADIO; VIEW; PERFORMANCE
AB Aims. We study the multi-band variability and correlations of the TeV blazar Mrk 421 on year timescales, which can bring additional insight on the processes responsible for its broadband emission.
Methods. We observed Mrk 421 in the very high energy (VHE) gamma-ray range with the Cherenkov telescope MAGIC-I from March 2007 to June 2009 for a total of 96 h of effective time after quality cuts. The VHE flux variability is quantified using several methods, including the Bayesian Block algorithm, which is applied to data from Cherenkov telescopes here for the first time. The 2.3 yr long MAGIC light curve is complemented with data from the Swift/BAT and RXTE/ASM satellites and the KVA, GASP-WEBT, OVRO, and Metsahovi telescopes from February 2007 to July 2009, allowing for an excellent characterisation of the multi-band variability and correlations over year timescales.
Results. Mrk 421 was found in different gamma-ray emission states during the 2.3 yr long observation period: The flux above 400 GeV spans from the minimum nightly value of (1.3 +/- 0.4) x 10(-11) cm(-2) s(-1) to the maximum flux, that is about 24 times higher, at (3.1 +/- 0.1) x 10(-10) cm(-2) s(-1). Flares and different levels of variability in the gamma-ray light curve could be identified with the Bayesian Block algorithm. The same behaviour of a quiet and active emission was found in the X-ray light curves measured by Swift/BAT and the RXTE/ASM, with a direct correlation in time. The behaviour of the optical light curve of GASP-WEBT and the radio light curves by OVRO and Metsahovi are different as they show no coincident features with the higher energetic light curves and a less variable emission. Overall, the fractional variability increases with energy. The comparable variability in the X-ray and VHE bands and their direct correlation during both high-and low-activity periods spanning many months show that the electron populations radiating the X-ray and gamma-ray photons are either the same, as expected in the synchrotron-self-Compton mechanism, or at least strongly correlated, as expected in electromagnetic cascades.
C1 [Ahnen, M. L.; Bilandl, A.; Hughes, G.; Prandini, E.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, F.; Giammaria, P.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Perri, 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 Split, Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Split, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Zagreb, Zagreb 41000, Croatia.
[Banerjee, B.; Chatterjee, A.; Majumdar, P.] Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
[Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hahn, A.; Hose, J.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moretti, E.; Noda, K.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Vovk, I.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Dominguez, A.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Rosillo, M. Nievas] Univ Complutense, E-28040 Madrid, Spain.
[Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain.
[Bednarek, W.; Idec, W.; Niedzwieckil, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; Garczarczyk, M.; Gora, D.; Pedaletti, G.; Satalecka, K.] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany.
[Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Munoz, A. Gonzalez; Guberman, D.; Lopez-Coto, R.; Martinez, M.; Moralejo, A.; Nogues, L.; Palacio, J.; Rico, J.; Ward, J. E.] Campus UAB, Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Bellaterra 08193, Barcelona, Spain.
[Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Univ Padua, I-35131 Padua, Italy.
[Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Wilhelmi, E. de Ona; Wu, M. H.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain.
[Einecke, S.; Elsaesser, D.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiat, Bellaterra 08193, Spain.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
[Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokyo, Dept Phys, ICRR, Japanese MAGIC Consortium, Tokyo 1138654, Japan.
[Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokushima, Tokai Univ, Kyoto Univ, Hakubi Ctr,KEK, Tokushima, Japan.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Oulu 90014, Finland.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Astron Div, Oulu 90014, Finland.
[Makariev, M.; Temnikov, P.; Verguilov, V.] Inst Nucl Energy Res, Sofia 1784, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, Barcelona 08193, Spain.
[Torres, D. F.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain.
[de Almeida, U. Barres] CBPF MCTI, 150 Urca, BR-22290180 Rio De Janeiro, Brazil.
[Gonzalez, J. Becerra] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bernardini, E.] Humboldt Univ, Inst Phys Newtonstr 15, D-12489 Berlin, Germany.
[Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Mazin, D.; Teshima, M.] Japanese MAGIC Consortium, Kyoto, Japan.
[Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Persic, M.] INAF Trieste, I-34143 Trieste, Italy.
[Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland.
[Blinov, D. A.; Grishina, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Blinov, D. A.] Univ Crete, Iraklion, Greece.
[Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Taoyuan 32001, Taiwan.
[Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia.
[Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Barcelona 08206, Spain.
[Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
[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.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 3000, Aalto 00076, Finland.
[Ligustri, R.] Circolo Astrofili Talmassons, Via Cadorna,57, I-33030 Talmassons, Italy.
[McBreen, B.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Raiteri, C. M.; Villata, M.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA.
RP Overkemping, A (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.; Overkemping, A (reprint author), Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain.; Tescaro, D (reprint author), Univ Padua, I-35131 Padua, Italy.; Tescaro, D (reprint author), Ist Nazl Fis Nucl, I-35131 Padua, Italy.; Manganaro, M (reprint author), Tech Univ Dortmund, D-44221 Dortmund, Germany.
EM manganaro@iac.es; ann-kristin.overkemping@tu-dortmund.de;
diego.tescaro@gmail.com
RI Lahteenmaki, Anne/L-5987-2013; Manganaro, Marina/B-7657-2011; Miranda,
Jose Miguel/F-2913-2013; Barrio, Juan/L-3227-2014; GAug,
Markus/L-2340-2014; Cortina, Juan/C-2783-2017; Morozova,
Daria/H-1298-2013; Puljak, Ivica/D-8917-2017;
OI Larionov, Valeri/0000-0002-4640-4356; Moretti,
Elena/0000-0001-5477-9097; Poutanen, Juri/0000-0002-0983-0049; Torres,
Diego F./0000-0002-1522-9065; Prandini, Elisa/0000-0003-4502-9053;
Manganaro, Marina/0000-0003-1530-3031; Miranda, Jose
Miguel/0000-0002-1472-9690; Barrio, Juan/0000-0002-0965-0259; GAug,
Markus/0000-0001-8442-7877; Cortina, Juan/0000-0003-4576-0452; Morozova,
Daria/0000-0002-9407-7804; Blinov, Dmitry/0000-0003-0611-5784;
Larionova, Elena/0000-0002-2471-6500; Grishina,
Tatiana/0000-0002-3953-6676
FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund
SNF; ERDF under the Spanish MINECO [FPA2012-39502]; Japanese JSPS;
Japanese MEXT; Centro de Excelencia Severo Ochoa of Spanish
Consolider-Ingenio programme [SEV-2012-0234]; Academy of Finland
[268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ)
Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG [SFB823/C4,
SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; NASA
[NNX08AW31G, NNX11A043G]; NFS [AST-0808050, AST-1109911]; Russian RFBR
[15-02-00949]; St. Petersburg University [6.38.335.2015]; Shota
Rustaveli National Science Foundation [FR/577/6-320/13]; CPAN Spanish
Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the
Spanish Consolider-Ingenio programme [CSD2009-00064]
FX We 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 (FPA2012-39502), 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
public data archives of Swift/BAT and RXTE/ASM are acknowledged. We
thank the OVRO telescope for making its results available for the
public. The OVRO 40 m monitoring program is supported in part by NASA
grants NNX08AW31G and NNX11A043G, and NFS grants AST-0808050 and
AST-1109911. We also thank the KVA and Metsahovi telescopes for making
their light curves available. M. Villata organized the optical-to-radio
observations by GASP-WEBT as the president of the collaboration. The
Metsahovi team acknowledges the support from the Academy of Finland to
our observing projects (numbers 212656, 210338, 121148, and others). St.
Petersburg University team acknowledges support from Russian RFBR grant
15-02-00949 and St. Petersburg University research grant 6.38.335.2015.
The Abastumani Observatory team acknowledges financial support by the
Shota Rustaveli National Science Foundation under contract
FR/577/6-320/13.
NR 52
TC 0
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U1 5
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A91
DI 10.1051/0004-6361/201628447
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100071
ER
PT J
AU Asensio-Torres, R
Janson, M
Hashimoto, J
Thalmann, C
Currie, T
Buenzli, E
Kudo, T
Kuzuhara, M
Kusakabe, N
Abe, L
Akiyama, E
Brandner, W
Brandt, TD
Carson, J
Egner, S
Feldt, M
Goto, M
Grady, C
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Kandori, R
Knapp, G
Kwon, J
Matsuo, T
McElwain, M
Mayama, S
Miyama, S
Morino, J
Moro-Martin, A
Nishimura, T
Pyo, T
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Turner, E
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Asensio-Torres, R.
Janson, M.
Hashimoto, J.
Thalmann, C.
Currie, T.
Buenzli, E.
Kudo, T.
Kuzuhara, M.
Kusakabe, N.
Abe, L.
Akiyama, E.
Brandner, W.
Brandt, T. D.
Carson, J.
Egner, S.
Feldt, M.
Goto, M.
Grady, C.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K.
Ishii, M.
Iye, M.
Kandori, R.
Knapp, G.
Kwon, J.
Matsuo, T.
McElwain, M.
Mayama, S.
Miyama, S.
Morino, J.
Moro-Martin, A.
Nishimura, T.
Pyo, T.
Serabyn, E.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y.
Takami, M.
Takato, N.
Terada, H.
Turner, E.
Watanabe, M.
Wisniewski, J.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI Polarimetry and flux distribution in the debris disk around HD 32297
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE protoplanetary disks; techniques: high angular resolution; stars:
individual: HD 32297
ID CIRCUMSTELLAR DISK; IMAGING POLARIMETRY; PROTOPLANETARY DISK; HR 4796A;
HD-32297; DISCOVERY; IMAGES; DUST; SUBTRACTION; EXOPLANETS
AB We present high-contrast angular differential imaging (ADI) observations of the debris disk around HD32297 in H-band, as well as the first polarimetric images for this system in polarized differential imaging (PDI) mode with Subaru/HICIAO. In ADI, we detect the nearly edge-on disk at > 5 sigma levels from similar to 0.45 '' to similar to 1.7 '' (50-192AU) from the star and recover the spine deviation from the midplane already found in previous works. We also find for the first time imaging and surface brightness (SB) indications for the presence of a gapped structure on both sides of the disk at distances of similar to 0.75 '' (NE side) and similar to 0.65 '' (SW side). Global forward-modelling work delivers a best-fit model disk and well-fitting parameter intervals that essentially match previous results, with high-forward scattering grains and a ring located at 110AU. However, this single ring model cannot account for the gapped structure seen in our SB profiles. We create simple double ring models and achieve a satisfactory fit with two rings located at 60 and 95AU, respectively, low-forward scattering grains and very sharp inner slopes. In polarized light we retrieve the disk extending from similar to 0.25-1.6 '', although the central region is quite noisy and high S/N are only found in the range similar to 0.75-1.2 ''. The disk is polarized in the azimuthal direction, as expected, and the departure from the midplane is also clearly observed. Evidence for a gapped scenario is not found in the PDI data. We obtain a linear polarization degree of the grains that increases from similar to 10% at 0.55 '' to similar to 25% at 1.6 ''. The maximum is found at scattering angles of similar to 90 degrees, either from the main components of the disk or from dust grains blown out to larger radii.
C1 [Asensio-Torres, R.; Janson, M.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Hashimoto, J.; Kusakabe, N.] NINS, Astrobiol Ctr, Mitaka, Tokyo 1818588, Japan.
[Thalmann, C.; Buenzli, E.] ETH, Inst Astron, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Currie, T.; Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Nishimura, T.; Pyo, T.; Takato, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Lagrange UMR 7293, CNRS, Observ Cote Azur, F-06108 Nice 2, France.
[Akiyama, E.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J.; Suto, H.; Suzuki, R.; Takahashi, Y.; Terada, H.; Takami, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Brandner, W.; Carson, J.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, T. D.; Feldt, M.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, M.] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, C.] Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hodapp, K.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Knapp, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kwon, J.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Mayama, S.] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Moro-Martin, A.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Serabyn, E.; Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Suenaga, T.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Takami, M.] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Asensio-Torres, R (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
EM ruben.torres@astro.su.se; markus.janson@astro.su.se
RI MIYAMA, Shoken/A-3598-2015;
OI Feldt, Markus/0000-0002-4188-5242
FU Knut and Alice Wallenberg foundation; US National Science Foundation
[1009203]
FX We would like to thank J.C. Augereau for providing the GraTeR code used
to create our disk models. R. Asensio-Torres and M. Janson gratefully
acknowledge funding from the Knut and Alice Wallenberg foundation. J.
Carson acknowledges support via the US National Science Foundation under
Award No. 1009203.
NR 47
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A73
DI 10.1051/0004-6361/201628543
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100081
ER
PT J
AU Drouart, G
Rocca-Volmerange, B
De Breuck, C
Fioc, M
Lehnert, M
Seymour, N
Stern, D
Vernet, J
AF Drouart, G.
Rocca-Volmerange, B.
De Breuck, C.
Fioc, M.
Lehnert, M.
Seymour, N.
Stern, D.
Vernet, J.
TI Disentangling star formation and AGN activity in powerful infrared
luminous radio galaxies at 1 < z < 4
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
galaxies: star formation; quasars: general; galaxies: starburst
ID SPECTRAL ENERGY-DISTRIBUTIONS; INITIAL MASS FUNCTION; BLACK-HOLE
ACCRETION; DEEP FIELD SOUTH; SIMILAR-TO 2; HIGH-REDSHIFT; GALACTIC
NUCLEI; ELLIPTIC GALAXIES; STELLAR POPULATIONS; STARBURST GALAXIES
AB High-redshift radio galaxies present signs of both star formation and AGN activity, making them ideal candidates to investigate the connection and coevolution of AGN and star formation in the progenitors of present-day massive galaxies. We make use of a sample of 11 powerful radio galaxies spanning 1 < z < 4 which have complete coverage of their spectral energy distribution (SED) from UV to FIR wavelengths. Using Herschel data, we disentangle the relative contribution of the AGN and star formation by combining the galaxy evolution code PEGASE.3 with an AGN torus model. We find that three components are necessary to reproduce the observed SEDs: an evolved and massive stellar component, a submm bright young starburst, and an AGN torus. We find that powerful radio galaxies form at very high-redshift, but experience episodic and important growth at 1 < z < 4 as the mass of the associated starburst varies from 5 to 50% of the total mass of the system. The properties of star formation differ from source to source, indicating no general trend of the star formation properties in the most infrared luminous high-redshift radio galaxies and no correlation with the AGN bolometric luminosity. Moreover, we find that AGN scattered light have a very limited impact on broad-band SED fitting on our sample. Finally, our analysis also suggests a wide range in origins for the observed star formation, which we partially constrain for some sources.
C1 [Drouart, G.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Drouart, G.; Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia.
[Drouart, G.; Rocca-Volmerange, B.; Fioc, M.; Lehnert, M.] Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
[De Breuck, C.; Vernet, J.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Stern, D.] CALTECH, Jet Prop Lab, Mail Stop 169-221, Pasadena, CA 91109 USA.
RP Drouart, G (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.; Drouart, G (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia.; Drouart, G (reprint author), Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
EM guillaume.drouart@curtin.edu.au
FU ARC; NASA; ESO scientific visitor programme
FX G.D. would like to warmly thank Alessandro Romeo, Kirsten Knudsen, and
Clive Tadhunter for the useful discussions that contributed to improve
this paper. The authors also thank the referee for detailed suggestions
and a thorough report that helped to clarify this paper. G.D. also
thanks Nina Hatch for providing HST fluxes for the Spiderweb galaxy and
A. Galametz for providing images for part of the sample. G.D. thanks
Philip Best for providing the 3C 368 and 3C 470 data. N.S. is the
recipient of an ARC Future Fellowship. The work of DS was carried out at
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. Based on observations made with the NASA/ESA Hubble
Space Telescope, and obtained from the Hubble Legacy Archive, which is a
collaboration between the Space Telescope Science Institute
(STScI/NASA), the Space Telescope European Coordinating Facility
(ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). GD
acknowledges the support from the ESO scientific visitor programme.
NR 161
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A109
DI 10.1051/0004-6361/201526880
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100015
ER
PT J
AU El-Marry, MR
Thomas, N
Gracia-Berna, A
Pajola, M
Lee, JC
Massironi, M
Davidsson, B
Marchi, S
Keller, HU
Hviid, SF
Besse, S
Sierks, H
Barbieri, C
Lamy, PL
Koschny, D
Rickman, H
Rodrigo, R
A'Hearn, MF
Auger, AT
Barucci, MA
Bertaux, JL
Bertini, I
Bodewits, D
Gremonese, G
Deppo, V
Cecco, M
Dehei, S
Guttler, C
Fornasier, S
Fulle, M
Giacomini, L
Groussin, O
Gutierrez, PJ
Ip, WH
Jorda, L
Knollenberg, J
Kovacs, G
Kramm, JR
Kuhrt, E
Kuppers, M
Lara, LM
Lazzarin, M
Moreno, JJL
Marschall, R
Marzari, F
Naletto, G
Oklay, N
Pommerol, A
Preusker, F
Scholten, F
Tubiana, C
Vincent, JB
AF El-Marry, M. R.
Thomas, N.
Gracia-Berna, A.
Pajola, M.
Lee, J. -C.
Massironi, M.
Davidsson, B.
Marchi, S.
Keller, H. U.
Hviid, S. F.
Besse, S.
Sierks, H.
Barbieri, C.
Lamy, P. L.
Koschny, D.
Rickman, H.
Rodrigo, R.
A'Hearn, M. F.
Auger, A. -T.
Barucci, M. A.
Bertaux, J. -L.
Bertini, I.
Bodewits, D.
Gremonese, G.
Da Deppo, V.
De Cecco, M.
Dehei, S.
Guettler, C.
Fornasier, S.
Fulle, M.
Giacomini, L.
Groussin, O.
Gutierrez, P. J.
Ip, W. -H
Jorda, L.
Knollenberg, J.
Kovacs, G.
Kramm, J. -R.
Kuehrt, E.
Kueppers, M.
Lara, L. M.
Lazzarin, M.
Moreno, J. J. Lopez
Marschall, R.
Marzari, F.
Naletto, G.
Oklay, N.
Pommerol, A.
Preusker, F.
Scholten, F.
Tubiana, C.
Vincent, J. -B.
TI Regional surface morphology of comet 67P/Churyumov-Gerasimenko from
Rosetta/OSIRIS images: The southern hemisphere
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods:
observational
ID NUCLEUS; OSIRIS; 67P
AB Aims. The OSIRIS camera on board the Rosetta spacecraft has been acquiring images of the comet 67P/Churyumov-Gerasimenko (67P)'s nucleus since August 2014. Starting in May 2015, the southern hemisphere gradually became illuminated and was imaged for the first time. Here we present the regional morphology of the southern hemisphere, which serves as a companion to an earlier paper that presented the regional morphology of the northern hemisphere.
Methods. We used OSIRIS images that were acquired at orbits similar to 45-125 km from the center of the comet (corresponding to spatial resolutions of similar to 0.8 to 2.3 m/pixel) coupled with the use of digital terrain models to define the different regions on the surface, and identify structural boundaries accurately.
Results. Seven regions have been defined in the southern hemisphere bringing the total number of defined regions on the surface of the nucleus to 26. These classifications are mainly based on morphological and/or topographic boundaries. The southern hemisphere shows a remarkable dichotomy with its northern counterpart mainly because of the absence of wide-scale smooth terrains, dust coatings and large unambiguous depressions. As a result, the southern hemisphere closely resembles previously identified consolidated regions. An assessment of the overall morphology of comet 67P suggests that the comet's two lobes show surface heterogeneities manifested in different physical/mechanical characteristics, possibly extending to local (i.e., within a single region) scales.
C1 [El-Marry, M. R.; Thomas, N.; Gracia-Berna, A.; Pommerol, A.] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Pajola, M.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy.
[Lee, J. -C.] Natl Cent Univ, Dept Earth Sci, Chungli 32054, Taiwan.
[Massironi, M.] Univ Padua, Dipartimento Geosci, Via G Gradenigo 6, I-35131 Padua, Italy.
[Davidsson, B.] Jet Prop Lab, M S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Marchi, S.] Southwest Res Inst, Solar Syst Explorat Res Virtual Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
[Keller, H. U.] TU Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Hviid, S. F.; Preusker, F.; Scholten, F.] Inst Planetenforsch, Deutsch Zentrum Luft & Raumfahrt DLR, Rutherfordstr 2, D-12489 Berlin, Germany.
[Besse, S.; Koschny, D.] European Space Agcy, Sci Support Off, NL-2201 Noordwijk, Netherlands.
[Sierks, H.; Guettler, C.; Kovacs, G.; Kramm, J. -R.; Oklay, N.; Tubiana, C.; Vincent, J. -B.] Max Planck Inst Sonnensystemforsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Barbieri, C.; Gremonese, G.; Lazzarin, M.; Marzari, F.] INAF Osservatorio Astrono, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Lamy, P. L.; Auger, A. -T.] Aix Marseille Univ, CNRS, LAM, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille, France.
[Rodrigo, R.] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Rickman, H.; Rodrigo, R.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
PAS Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[A'Hearn, M. F.; Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Barucci, M. A.] Univ Paris Diderot, Univ Paris 06, CNRS, Obs Paris,LESIA, 5 Pl J Janssen, F-92195 Meudon, France.
[Bertaux, J. -L.] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Bertini, I.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy.
[Da Deppo, V.] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[De Cecco, M.] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy.
[Dehei, S.] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy.
[Fulle, M.] INAF Osservatorio Astron, Via Tiepolo 11, I-34014 Trieste, Italy.
[Gutierrez, P. J.; Lara, L. M.; Moreno, J. J. Lopez] CSIC, Inst Astrofis Andalucia, C Glorieta Astron S-N, E-18008 Granada, Spain.
[Ip, W. -H] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan.
[Jorda, L.] Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Kueppers, M.] European Space Astron Ctr ESA, Sci Support Off, POB 78, Madrid 28691, Spain.
[Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
RP El-Marry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM mohammed.elmaarry@space.unibe.ch
RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014;
OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez,
Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi,
Matteo/0000-0002-7757-8818
FU Germany (DLR); France (CNES); Italy (ASI); Spain (MEC); Sweden (SNSB);
ESA Technical Directorate; Rosetta mission
FX OSIRIS was built by a consortium of the Max-Planck-Institut fur
Sonnensystemforschung, in Gottingen, Germany, CISAS-University of
Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the
Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the
Research and Scientific Support Department of the European Space Agency,
Noordwijk, The Netherlands, the Instituto Nacional de Tecnica
Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid,
Spain, the Department of Physics and Astronomy of Uppsala University,
Sweden, and the Institut fur Datentechnik und Kommunikationsnetze der
Technischen Universitat Braunschweig, Germany. The support of the
national funding agencies of Germany (DLR), France (CNES), Italy (ASI),
Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is
gratefully acknowledged. We thank the ESA teams at ESAC, ESOC and ESTEC
for their work in support of the Rosetta mission.
NR 26
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A110
DI 10.1051/0004-6361/201628634
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100095
ER
PT J
AU Luna, M
Diaz, AJ
Oliver, R
Terradas, J
Karpen, J
AF Luna, M.
Diaz, A. J.
Oliver, R.
Terradas, J.
Karpen, J.
TI The effects of magnetic-field geometry on longitudinal oscillations of
solar prominences: Cross-sectional area variation for thin tubes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: oscillations; Sun:
magnetic fields
ID MAGNETOHYDRODYNAMIC WAVES; FILAMENT; MODEL
AB Context. Solar prominences are subject to both field-aligned (longitudinal) and transverse oscillatory motions, as evidenced by an increasing number of observations. Large-amplitude longitudinal motions provide valuable information on the geometry of the filament-channel magnetic structure that supports the cool prominence plasma against gravity. Our pendulum model, in which the restoring force is the gravity projected along the dipped field lines of the magnetic structure, best explains these oscillations. However, several factors can influence the longitudinal oscillations, potentially invalidating the pendulum model.
Aims. The aim of this work is to study the influence of large-scale variations in the magnetic field strength along the field lines, i.e., variations of the cross-sectional area along the flux tubes supporting prominence threads.
Methods. We studied the normal modes of several flux tube configurations, using linear perturbation analysis, to assess the influence of different geometrical parameters on the oscillation properties.
Results. We found that the influence of the symmetric and asymmetric expansion factors on longitudinal oscillations is small.
Conclusions. We conclude that the longitudinal oscillations are not significantly influenced by variations of the cross-section of the flux tubes, validating the pendulum model in this context.
C1 [Luna, M.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Diaz, A. J.; Oliver, R.; Terradas, J.] Univ Illes Balears, Dept Fis, Palma de Mallorca 07122, Spain.
[Oliver, R.; Terradas, J.] Inst Appl Comp & Community Code IAC3, Palma de Mallorca 07122, Spain.
[Karpen, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Luna, M (reprint author), Inst Astrofis Canarias, Tenerife 38205, Spain.; Luna, M (reprint author), Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
EM mluna@iac.es
FU Spanish Ministry of Economy and Competitiveness [AYA2011-24808,
AYA2010-18029, AYA2014-55078-P]; FP7 European Research Council [277829];
Spanish "Ministerio de Educacion y Ciencia"; MINECO; FEDER
[AYA2014-54485-P]; International Space Science Institute (ISSI) [314]
FX M. Luna acknowledges the support by the Spanish Ministry of Economy and
Competitiveness through projects AYA2011-24808, AYA2010-18029, and
AYA2014-55078-P. This work contributes to the deliverables identified in
FP7 European Research Council grant agreement 277829, "Magnetic
Connectivity through the Solar Partially Ionized Atmosphere" (PI: E.
Khomenko). J.T. acknowledges support from the Spanish "Ministerio de
Educacion y Ciencia" through a Ramon y Cajal grant and support from
MINECO and FEDER funds through project AYA2014-54485-P. M.L., J.T., and
J.K. acknowledge support from the International Space Science Institute
(ISSI) to the Team 314 on "Large-Amplitude Oscillation in prominences"
led by M. Luna.
NR 18
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A64
DI 10.1051/0004-6361/201628845
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100124
ER
PT J
AU Montesinos, B
Eiroa, C
Krivov, AV
Marshall, JP
Pilbratt, GL
Liseau, R
Mora, A
Maldonado, J
Wolf, S
Ertel, S
Bayo, A
Augereau, JC
Heras, AM
Fridlund, M
Danchi, WC
Solano, E
Kirchschlager, F
del Burgo, C
Montes, D
AF Montesinos, B.
Eiroa, C.
Krivov, A. V.
Marshall, J. P.
Pilbratt, G. L.
Liseau, R.
Mora, A.
Maldonado, J.
Wolf, S.
Ertel, S.
Bayo, A.
Augereau, J. -C.
Heras, A. M.
Fridlund, M.
Danchi, W. C.
Solano, E.
Kirchschlager, F.
del Burgo, C.
Montes, D.
TI Incidence of debris discs around FGK stars in the solar neighbourhood
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: late-type; circumstellar matter; protoplanetary disks; infrared:
stars
ID MAIN-SEQUENCE STARS; CA-II H; ABSOLUTE FLUX CALIBRATION; SUN-LIKE STARS;
NEARBY STARS; BOLOMETRIC CORRECTIONS; PLANET-SEARCH; FIELD STARS; HOST
STARS; COOL STARS
AB Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their counterparts in the solar system are the asteroid and Edgeworth-Kuiper belts.
Aims. The aim of this paper is to provide robust numbers for the incidence of debris discs around FGK stars in the solar neighbourhood.
Methods. The full sample of 177 FGK stars with d <= 20 pc proposed for the DUst around NEarby Stars (DUNES) survey is presented. Herschel/PACS observations at 100 and 160 mu m were obtained, and were complemented in some cases with data at 70 mu m and at 250, 350, and 500 mu m SPIRE photometry. The 123 objects observed by the DUNES collaboration were presented in a previous paper. The remaining 54 stars, shared with the Disc Emission via a Bias-free Reconnaissance in IR and Sub-mm (DEBRIS) consortium and observed by them, and the combined full sample are studied in this paper. The incidence of debris discs per spectral type is analysed and put into context together with other parameters of the sample, like metallicity, rotation and activity, and age.
Results. The subsample of 105 stars with d <= 15 pc containing 23 F, 33 G, and 49 K stars is complete for F stars, almost complete for G stars, and contains a substantial number of K stars from which we draw solid conclusions on objects of this spectral type. The incidence rates of debris discs per spectral type are 0.26(-0.14)(+0.21) (6 objects with excesses out of 23 F stars), 0.21(-0.11)(+0.17) (7 out of 33 G stars), and 0.20(-0.09)(+0.14) (10 out of 49 K stars); the fraction for all three spectral types together is 0.22(-0.07)(+0.08) (23 out of 105 stars). The uncertainties correspond to a 95% confidence level. The medians of the upper limits of L-dust/L-* for each spectral type are 7.8 x 10(-7) (F), 1.4 x 10(-6) (G), and 2.2 x 10(-6) (K); the lowest values are around 4.0 x 10(-7). The incidence of debris discs is similar for active (young) and inactive (old) stars. The fractional luminosity tends to drop with increasing age, as expected from collisional erosion of the debris belts.
C1 [Montesinos, B.; Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.
[Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo 15,Campus Cantoblanco, E-28049 Madrid, Spain.
[Montesinos, B.; Eiroa, C.] UAM, Unidad Asociada CAB, Madrid, Spain.
[Krivov, A. V.] Univ Jena, Astrophys Inst & Univ, Schillergasschen 2-3, D-07745 Jena, Germany.
[Marshall, J. P.] UNSW Australia, Sch Phys, Sydney, NSW 2052, Australia.
[Marshall, J. P.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Pilbratt, G. L.; Heras, A. M.] European Space Res & Technol Ctr ESTEC SCIS, Sci Support Off, Directorate Sci, ESA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Liseau, R.; Fridlund, M.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Mora, A.] ESA ESAC Gaia SOC, POB 78, Madrid 28691, Spain.
INAF, Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Wolf, S.; Kirchschlager, F.] Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24118 Kiel, Germany.
[Ertel, S.] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Bayo, A.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Av Gran Bretana 1111,5030 Casilla, Valparaiso, Chile.
[Bayo, A.] Univ Valparaiso, ICM Nucleus Protoplanetary Disks, Av Gran Bretana 1111, Valparaiso 2360102, Chile.
[Augereau, J. -C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Augereau, J. -C.] CNRS, IPAG, F-38000 Grenoble, France.
[Fridlund, M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys, Code 667, Greenbelt, MD 20771 USA.
[Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Spanish Virtual Observ, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla, Mexico.
[Montes, D.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain.
RP Montesinos, B (reprint author), CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.; Montesinos, B (reprint author), UAM, Unidad Asociada CAB, Madrid, Spain.
EM benjamin.montesinos@cab.inta-csic.es
RI Solano, Enrique/C-2895-2017; Montesinos, Benjamin/C-3493-2017;
OI Montesinos, Benjamin/0000-0002-7982-2095; Montes,
David/0000-0002-7779-238X
FU Spanish grant [AYA2013-45347-P]; DFG [KR 2164/13-1, KR 2164/15-1, WO
857/151]; UNSW Vice-Chancellor's postdoctoral fellowship; Proyecto
Fondecyt de Iniciacion [11140572]; PNP; CNES; Mexican CONACyT
[CB-2012-183007]; [AYA2011-26202]
FX The authors are grateful to the referee for the careful revision of the
original manuscript, and for the comments and suggestions. We also thank
Francisco Galindo, Mauro Lopez del Fresno, and Pablo Riviere for their
valuable help. B. Montesinos and C. Eiroa are supported by Spanish grant
AYA2013-45347-P; they and J.P. Marshall and J. Maldonado were supported
by grant AYA2011-26202. A.V. Krivov acknowledges the DFG support under
contracts KR 2164/13-1 and KR 2164/15-1. J.P. Marshall is supported by a
UNSW Vice-Chancellor's postdoctoral fellowship. R. Liseau thanks the
Swedish National Space Board for its continued support. A. Bayo
acknowledges financial support from the Proyecto Fondecyt de Iniciacion
11140572 and scientific support from the Millenium Science Initiative,
Chilean Ministry of Economy, Nucleus RC130007. J.-C. Augereau
acknowledges support from PNP and CNES. F. Kirchschlager thanks the DFG
for finantial support under contract WO 857/151. C. del Burgo has been
supported by Mexican CONACyT research grant CB-2012-183007.
NR 95
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A51
DI 10.1051/0004-6361/201628329
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100058
ER
PT J
AU Muller, C
Burd, PR
Schulz, R
Coppejans, R
Falcke, H
Intema, H
Kadler, M
Krauss, F
Ojha, R
AF Mueller, C.
Burd, P. R.
Schulz, R.
Coppejans, R.
Falcke, H.
Intema, H.
Kadler, M.
Krauss, F.
Ojha, R.
TI The MHz-peaked radio spectrum of the unusual gamma-ray source
PMNJ1603-4904
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Letter
DE galaxies: active; galaxies: jets; galaxies: individual: PMN J1603-4904
ID LARGE-AREA TELESCOPE; COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI;
FREE-FREE ABSORPTION; SOURCE CATALOG; SYMMETRIC OBJECTS; EVOLUTION;
YOUNG; EMISSION; GALAXIES
AB Context. The majority of bright extragalactic gamma-ray sources are blazars. Only a few radio galaxies have been detected by Fermi/LAT. Recently, the GHz-peaked spectrum source PKS 1718-649 was confirmed to be gamma-ray bright, providing further evidence for the existence of a population of gamma-ray loud, compact radio galaxies. A spectral turnover in the radio spectrum in the MHz to GHz range is a characteristic feature of these objects, which are thought to be young due to their small linear sizes. The multiwavelength properties of the gamma-ray source PMNJ1603-4904 suggest that it is a member of this source class.
Aims. The known radio spectrum of PMNJ1603-4904 can be described by a power law above 1 GHz. Using observations from the Giant Metrewave Radio Telescope (GMRT) at 150, 325, and 610 MHz, we investigate the behavior of the spectrum at lower frequencies to search for a low-frequency turnover.
Methods. Data from the TIFR GMRT Sky Survey (TGSS ADR) catalog and archival GMRT observations were used to construct the first MHz to GHz spectrum of PMNJ1603-4904.
Results. We detect a low-frequency turnover of the spectrum and measure the peak position at about 490 MHz (rest-frame), which, using the known relation of peak frequency and linear size, translates into a maximum linear source size of similar to 1.4 kpc.
Conclusions. The detection of the MHz peak indicates that PMNJ1603-4904 is part of this population of radio galaxies with turnover frequencies in the MHz to GHz regime. Therefore it can be considered the second confirmed object of this kind detected in gamma-rays. Establishing this gamma-ray source class will help to investigate the gamma-ray production sites and to test broadband emission models.
C1 [Mueller, C.; Coppejans, R.; Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Burd, P. R.; Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Hubland, D-97074 Wurzburg, Germany.
[Schulz, R.] ASTRON, Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Intema, H.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Krauss, F.] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Krauss, F.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
[Ojha, R.] CRESST Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Muller, C (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM cmueller@astro.ru.nl
NR 51
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR L19
DI 10.1051/0004-6361/201629547
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100159
ER
PT J
AU Werner, K
Rauch, T
Kruk, JW
AF Werner, K.
Rauch, T.
Kruk, J. W.
TI The far-ultraviolet spectra of two hot PG1159 stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: atmospheres; stars: evolution; stars: AGB and
post-AGB; white dwarfs
ID PRE-WHITE-DWARFS; TO-OXYGEN RATIO; POST-AGB STARS; PLANETARY-NEBULAE;
INTERSTELLAR-MEDIUM; ATOMIC DATABASE; IRON ABUNDANCE; LINES;
SPECTROSCOPY; MODEL
AB PG 115(stars are hot, hydrogen-deficient (pre-) white dwarfs with atmospheres mainly composed of helium, carbon, and oxygen. The unusual surface chemistry is the result of a late helium-shell flash. Observed element abundances enable us to test stellar evolution models quantitatively with respect to their nucleosynthesis products formed near the helium-burning shell of the progenitor asymptotic giant branch stars. Because of the high effective temperatures (T-eff), abundance determinations require ultraviolet spectroscopy and non-local thermodynamic equilibrium model atmosphere analyses. Up to now, we have presented results for the prototype of this spectral class and two cooler members (T-eff in the range 85 000-140 000 K). Here we report on the results for two even hotter stars (PG 1520 + 525 and PG 1144 + 005, both with T-eff = 150 000 K) which are the only two objects in this temperature-gravity region for which useful far-ultraviolet spectra are available, and revisit the prototype star. Previous results on the abundances of some species are confirmed, while results on others (Si, P, S) are revised. In particular, a solar abundance of sulphur is measured in contrast to earlier claims of a strong S deficiency that contradicted stellar evolution models. For the first time, we assess the abundances of Na, Al, and Cl with newly constructed non-LTE model atoms. Besides the main constituents (He, C, O), we determine the abundances (or upper limits) of N, F, Ne, Na, Al, Si, P, S, Cl, Ar, and Fe. Generally, good agreement with stellar models is found.
C1 [Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Werner, K (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM werner@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [50 OR 1507]
FX We thank Amanda Karakas and Luke Shingles for reporting unpublished
results to us. T. Rauch is supported by the German Aerospace Center
(DLR) under grant 50 OR 1507. The TMAD service
(http://astro-uni-tuebingen.de/similar to TMAD) used to compile atomic
data for this paper was constructed as part of the activities of the
German Astrophysical Virtual Observatory. This research has made use of
the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's
Astrophysics Data System Bibliographic Services. Some of the data
presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). This work had been done using the profile
fitting procedure OWENS, developed by M. Lemoine and the FUSE French
Team.
NR 48
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2016
VL 593
AR A104
DI 10.1051/0004-6361/201628892
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100130
ER
PT J
AU Hopkins, FM
Ehleringer, JR
Bush, SE
Duren, RM
Miller, CE
Lai, CT
Hsu, YK
Carranza, V
Randerson, JT
AF Hopkins, Francesca M.
Ehleringer, James R.
Bush, Susan E.
Duren, Riley M.
Miller, Charles E.
Lai, Chun-Ta
Hsu, Ying-Kuang
Carranza, Valerie
Randerson, James T.
TI Mitigation of methane emissions in cities: How new measurements and
partnerships can contribute to emissions reduction strategies
SO EARTHS FUTURE
LA English
DT Article
ID GREENHOUSE-GAS EMISSIONS; WASTE-WATER TREATMENT; MUNICIPAL SOLID-WASTE;
CLIMATE-CHANGE ACTION; NATURAL-GAS; CARBON-DIOXIDE; UNITED-STATES;
NITROUS-OXIDE; LOS-ANGELES; PIPELINE LEAKS
AB Cities generate 70% of anthropogenic greenhouse gas emissions, a fraction that is growing with global urbanization. While cities play an important role in climate change mitigation, there has been little focus on reducing urban methane (CH4) emissions. Here, we develop a conceptual framework for CH4 mitigation in cities by describing emission processes, the role of measurements, and a need for new institutional partnerships. Urban CH4 emissions are likely to grow with expanding use of natural gas and organic waste disposal systems in growing population centers; however, we currently lack the ability to quantify this increase. We also lack systematic knowledge of the relative contribution of these distinct source sectors on emissions. We present new observations from four North American cities to demonstrate that CH4 emissions vary in magnitude and sector from city to city and hence require different mitigation strategies. Detections of fugitive emissions from these systems suggest that current mitigation approaches are absent or ineffective. These findings illustrate that tackling urban CH4 emissions will require research efforts to identify mitigation targets, develop and implement new mitigation strategies, and monitor atmospheric CH4 levels to ensure the success of mitigation efforts. This research will require a variety of techniques to achieve these objectives and should be deployed in cities globally. We suggest that metropolitan scale partnerships may effectively coordinate systematic measurements and actions focused on emission reduction goals.
C1 [Hopkins, Francesca M.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Hopkins, Francesca M.; Duren, Riley M.; Miller, Charles E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Ehleringer, James R.; Bush, Susan E.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Ehleringer, James R.] Univ Utah, Global Change & Sustainabil Ctr, Salt Lake City, UT USA.
[Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA.
[Hsu, Ying-Kuang] Calif Air Resources Board, Monitoring & Lab Div, Sacramento, CA USA.
[Carranza, Valerie] Univ Calif Los Angeles, Environm Sci, Los Angeles, CA USA.
RP Hopkins, FM (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.; Hopkins, FM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM francesca.m.hopkins@jpl.nasa.gov
FU U.S. Department of Energy Office of Science (BER) [DE-SC0005266]; NASA
Postdoctoral Program fellowship; NASA
FX This study was supported by U.S. Department of Energy Office of Science
(BER), Grant No. DE-SC0005266. F.M.H. also acknowledges support from a
NASA Postdoctoral Program fellowship. We thank Liz Wiggins, Gergana
Mouteva, Massimo Lupascu, Clayton Elder, Nicky Cuozzo, Ashley Braunthal,
Joshua Miu, and Simon Fahrni for collecting Fairbanks data, Joshua Rambo
for collecting San Diego data, and Bill Johnson for thermal camera
images. Portions of this work were performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. The data used are listed in the references, tables, figures, and
supplement. Raw data are available by contacting
francesca.m.hopkins@jpl.nasa.gov.
NR 123
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U1 11
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD SEP
PY 2016
VL 4
IS 9
BP 408
EP 425
DI 10.1002/2016EF000381
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA EC0BB
UT WOS:000387761400001
ER
PT J
AU Verma, M
Fisher, JB
Mallick, K
Ryu, Y
Kobayashi, H
Guillaume, A
Moore, G
Ramakrishnan, L
Hendrix, V
Wolf, S
Sikka, M
Kiely, G
Wohlfahrt, G
Gielen, B
Roupsard, O
Toscano, P
Arain, A
Cescatti, A
AF Verma, Manish
Fisher, Joshua B.
Mallick, Kaniska
Ryu, Youngryel
Kobayashi, Hideki
Guillaume, Alexandre
Moore, Gregory
Ramakrishnan, Lavanya
Hendrix, Valerie
Wolf, Sebastian
Sikka, Munish
Kiely, Gerard
Wohlfahrt, Georg
Gielen, Bert
Roupsard, Olivier
Toscano, Piero
Arain, Altaf
Cescatti, Alessandro
TI Global Surface Net-Radiation at 5 km from MODIS Terra
SO REMOTE SENSING
LA English
DT Article
DE surface net-radiation; MODIS; FLUXNET; SURFRAD; modeling; validation
ID DOWNWELLING LONGWAVE RADIATION; CLEAR-SKY DAYS; HETEROGENEOUS LANDSCAPE;
LAND; EVAPOTRANSPIRATION; VALIDATION; ATMOSPHERE; FLUX; ALGORITHMS;
PRODUCT
AB Reliable and fine resolution estimates of surface net-radiation are required for estimating latent and sensible heat fluxes between the land surface and the atmosphere. However, currently, fine resolution estimates of net-radiation are not available and consequently it is challenging to develop multi-year estimates of evapotranspiration at scales that can capture land surface heterogeneity and are relevant for policy and decision-making. We developed and evaluated a global net-radiation product at 5 km and 8-day resolution by combining mutually consistent atmosphere and land data from the Moderate Resolution Imaging Spectroradiometer (MODIS) on board Terra. Comparison with net-radiation measurements from 154 globally distributed sites (414 site-years) from the FLUXNET and Surface Radiation budget network (SURFRAD) showed that the net-radiation product agreed well with measurements across seasons and climate types in the extratropics (Wilmott's index ranged from 0.74 for boreal to 0.63 for Mediterranean sites). Mean absolute deviation between the MODIS and measured net-radiation ranged from 38.0 +/- 1.8 W.m(-2) in boreal to 72.0 +/- 4.1 W.m(-2) in the tropical climates. The mean bias was small and constituted only 11%, 0.7%, 8.4%, 4.2%, 13.3%, and 5.4% of the mean absolute error in daytime net-radiation in boreal, Mediterranean, temperate-continental, temperate, semi-arid, and tropical climate, respectively. To assess the accuracy of the broader spatiotemporal patterns, we upscaled error-quantified MODIS net-radiation and compared it with the net-radiation estimates from the coarse spatial (1 degrees x 1 degrees) but high temporal resolution gridded net-radiation product from the Clouds and Earth's Radiant Energy System (CERES). Our estimates agreed closely with the net-radiation estimates from the CERES. Difference between the two was less than 10 W center dot m(-2) in 94% of the total land area. MODIS net-radiation product will be a valuable resource for the science community studying turbulent fluxes and energy budget at the Earth's surface.
C1 [Verma, Manish; Fisher, Joshua B.; Guillaume, Alexandre; Moore, Gregory; Sikka, Munish] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mallick, Kaniska] LIST, Dept Environm Res & Innovat ERIN, L-4422 Belvaux, Luxembourg.
[Ryu, Youngryel] Seoul Natl Univ, Dept Landscape Architecture & Rural Syst Engn, Seoul 151921, South Korea.
[Kobayashi, Hideki] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan.
[Ramakrishnan, Lavanya; Hendrix, Valerie] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Wolf, Sebastian] Swiss Fed Inst Technol, Dept Environm Syst Sci, CH-8092 Zurich, Switzerland.
[Kiely, Gerard] Univ Coll, Environm Res Inst, Civil & Environm Engn Dept, Cork T12P2FY, Ireland.
[Wohlfahrt, Georg] Univ Innsbruck, Inst Ecol, Sternwartestr 15, A-6020 Innsbruck, Austria.
[Gielen, Bert] Univ Antwerp, Dept Biol, Res Grp Plant & Vegetat Ecol, B-2610 Antwerp, Belgium.
[Roupsard, Olivier] CIRAD, UMR Eco & Sols Ecol Fonct Biogeochim Sols & Agroe, F-34000 Montpellier, France.
[Roupsard, Olivier] CATIE Trop Agr Ctr Res & Higher Educ, Turrialba 937170, Costa Rica.
[Toscano, Piero] CNR, Inst Biometeorol IBIMET, Via G Caproni 8, I-50145 Florence, Italy.
[Arain, Altaf] McMaster Univ, McMaster Ctr Climate Change, Sch Geog & Earth Sci, 1280 Main St West, Hamilton, ON L8S 4K1, Canada.
[Cescatti, Alessandro] European Commiss, Joint Res Ctr, Directorate Sustainable Resources, I-21027 Ispra, Italy.
RP Verma, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM manishve@umich.edu; Joshua.B.Fisher@jpl.nasa.gov;
kaniska.mallick@gmail.com; ryuyr77@gmail.com; hkoba@jamstec.go.jp;
alexandre.guillaume@jpl.nasa.gov; Gregory.J.Moore@jpl.nasa.gov;
LRamakrishnan@lbl.gov; vchendrix@lbl.gov; sewolf@ethz.ch;
Munish.Sikka@jpl.nasa.gov; g.kiely@ucc.ie; Georg.Wohlfahrt@uibk.ac.at;
bert.gielen@uantwerpen.be; olivier.roupsard@cirad.fr;
p.toscano@ibimet.cnr.it; arainm@mcmaster.ca;
alessandro.cescatti@jrc.ec.europa.eu
RI Wohlfahrt, Georg/D-2409-2009; Wolf, Sebastian/B-4580-2010;
OI Wohlfahrt, Georg/0000-0003-3080-6702; Wolf,
Sebastian/0000-0001-7717-6993; Toscano, Piero/0000-0001-9184-0707;
Mallick, Kaniska/0000-0002-2735-930X; Fisher, Joshua/0000-0003-4734-9085
FU NASA Terrestrial Hydrology Program; Jet Propulsion Laboratory Strategic
Research & Technology Development Climate Initiative; U.S. Department of
Energy, Biological and Environmental Research, Terrestrial Carbon
Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; AfriFlux; AsiaFlux;
CarboAfrica; CarboEuropeIP; CarboItaly; CarboMont; ChinaFlux;
Fluxnet-Canada; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan;
GreenGrass; KoFlux; LBA; NECC; OzFlux; TCOS-Siberia; USCCC; Australian
Research Council [DP0451247, DP0344744, DP0772981, DP130101566];
European Commission [300083]
FX Support for this study was provided by the NASA Terrestrial Hydrology
Program and Jet Propulsion Laboratory Strategic Research & Technology
Development Climate Initiative. The research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Copyright 2015 California Institute of Technology. Government
sponsorship acknowledged. This work used net-radiation 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, USCCC. The authors gratefully acknowledge
the efforts of the FLUXNET community to compile and make available the
La Thuile data set. Data from AU-Fog-Fogg Dam, AU-How-Howard Springs,
AU-Wac-Wallaby Creek was funded by the Australian Research Council
(DP0451247, DP0344744, DP0772981 and DP130101566). Support for
collection and archiving was provided through the Australia Terrestrial
Ecosystem Research Network (TERN) (http://www.tern.org.au). SW was
supported by the European Commission with a Marie Curie International
Outgoing Fellowship (grant 300083).
NR 61
TC 0
Z9 0
U1 7
U2 7
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2016
VL 8
IS 9
AR UNSP 739
DI 10.3390/rs8090739
PG 20
WC Remote Sensing
SC Remote Sensing
GA DY9XB
UT WOS:000385488000049
ER
PT J
AU Wang, XJ
Key, J
Kwok, R
Zhang, JL
AF Wang, Xuanji
Key, Jeffrey
Kwok, Ron
Zhang, Jinlun
TI Comparison of Arctic Sea Ice Thickness from Satellites, Aircraft, and
PIOMAS Data
SO REMOTE SENSING
LA English
DT Article
DE sea ice thickness; Arctic; remote sensing; satellite; ICESat; CryoSat-2;
SMOS; IceBridge; PIOMAS; APP-x
ID SNOW DEPTH; OPERATION ICEBRIDGE; MODEL; RETRIEVAL; FREEBOARD; ALGORITHM;
CLOUD
AB In this study, six Arctic sea ice thickness products are compared: the AVHRR Polar Pathfinder-extended (APP-x), ICESat, CryoSat-2, SMOS, NASA IceBridge aircraft flights, and the Pan-Arctic Ice Ocean Modeling and Assimilation System (PIOMAS). The satellite products are based on three different retrieval methods: an energy budget approach, measurements of ice freeboard, and the relationship between passive microwave brightness temperatures and thin ice thickness. Inter-comparisons are done for the periods of overlap from 2003 to 2013. Results show that ICESat sea ice is thicker than APP-x and PIOMAS overall, particularly along the north coast of Greenland and Canadian Archipelago. The relative differences of APP-x and PIOMAS with ICESat are -0.48 m and -0.31 m, respectively. APP-x underestimates thickness relative to CryoSat-2, with a mean difference of -0.19 m. The biases for APP-x, PIOMAS, and CryoSat-2 relative to IceBridge thicknesses are 0.18 m, 0.18 m, and 0.29 m. The mean difference between SMOS and CryoSat-2 for 0 similar to 1 m thick ice is 0.13 m in March and -0.24 m in October. All satellite-retrieved ice thickness products and PIOMAS overestimate the thickness of thin ice (1 m or less) compared to IceBridge for which SMOS has the smallest bias (0.26 m). The spatial correlation between the datasets indicates that APP-x and PIOMAS are the most similar, followed by APP-x and CryoSat-2.
C1 [Wang, Xuanji] UW Madison, CIMSS, SSEC, Madison, WI 53706 USA.
[Key, Jeffrey] NOAA NESDIS, Ctr Satellite Applicat & Res, Madison, WI 53706 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, Jinlun] Univ Washington, Appl Phys Lab, Polar Sci Ctr, 1013 NE 40th St, Seattle, WA 98105 USA.
RP Wang, XJ (reprint author), UW Madison, CIMSS, SSEC, Madison, WI 53706 USA.
EM xuanjiw@ssec.wisc.edu; jeff.key@noaa.gov; ronald.kwok@jpl.nasa.gov;
zhang@apl.washington.edu
OI Wang, Xuanji/0000-0002-5893-758X; Key, Jeffrey/0000-0001-6109-3050
FU JPSS Program Office; GOES-R Program Office; National Science Foundation
[ARC-1023371]; NASA Cryosphere Program [NNX15AG68G]
FX This work was supported by the JPSS Program Office, the GOES-R Program
Office, the National Science Foundation (ARC-1023371), and the NASA
Cryosphere Program (NNX15AG68G). We thank the Alfred Wegener
Institute/Helmholtz Centre for Polar and Marine Research and the
European Space Agency for making the Cryosat-2 ice thickness product
available to the scientific community, the University of Hamburg for the
SMOS ice thicknesses, and the National Snow and Ice Data Center and NASA
for the IceBridge data. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 31
TC 2
Z9 2
U1 6
U2 6
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2016
VL 8
IS 9
AR 713
DI 10.3390/rs8090713
PG 17
WC Remote Sensing
SC Remote Sensing
GA DY9XB
UT WOS:000385488000023
ER
PT J
AU Meier, MM
Matthia, D
Forkert, T
Wirtz, M
Scheibinger, M
Hubel, R
Mertens, CJ
AF Meier, Matthias M.
Matthiae, Daniel
Forkert, Tomas
Wirtz, Michael
Scheibinger, Markus
Huebel, Robert
Mertens, Christopher J.
TI RaD-X: Complementary measurements of dose rates at aviation altitudes
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID GALACTIC COSMIC-RAYS; CALIBRATION; MODEL; DOSIMETERS
AB The RaD-X stratospheric balloon flight organized by the National Aeronautics and Space Administration was launched from Fort Sumner on 25 September 2015 and carried several instruments to measure the radiation field in the upper atmosphere at the average vertical cutoff rigidity R-c of 4.1 GV. The German Aerospace Center (Deutsches Zentrum fur Luft-und Raumfahrt) in cooperation with Lufthansa German Airlines supported this campaign with an independent measuring flight at the altitudes of civil aviation on a round trip from Germany to Japan. The goal was to measure dose rates under similar space weather conditions over an area on the Northern Hemisphere opposite to the RaD-X flight. Dose rates were measured in the target areas, i.e., around vertical cutoff rigidity Rc of 4.1 GV, at two flight altitudes for about 1 h at each position with acceptable counting statistics. The analysis of the space weather situation during the flights shows that measuring data were acquired under stable and moderate space weather conditions with a virtually undisturbed magnetosphere. The measured rates of absorbed dose in silicon and ambient dose equivalent complement the data recorded during the balloon flight. The combined measurements provide a set of experimental data suitable for validating and improving numerical models for the calculation of radiation exposure at aviation altitudes.
C1 [Meier, Matthias M.; Matthiae, Daniel; Forkert, Tomas; Wirtz, Michael] Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany.
[Scheibinger, Markus; Huebel, Robert] Lufthansa German Airlines, Lufthansa Basis, Frankfurt, Germany.
[Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Meier, MM (reprint author), Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany.
EM Matthias.Meier@dlr.de
OI Matthia, Daniel/0000-0003-1507-0143
FU Lufthansa German Airlines
FX We would like to especially express our gratitude to Lufthansa German
Airlines for their support during the preparation and performance of the
measuring flights. Furthermore, we would like to thank the Sodankyla
Geophysical Observatory and the website team (http://cosmicrays.oulu.fi)
for providing the Oulu neutron monitor data. The flight data are
available from the German Aerospace Center upon request.
NR 19
TC 3
Z9 3
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD SEP
PY 2016
VL 14
IS 9
BP 689
EP 694
DI 10.1002/2016SW001418
PG 6
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EC0PE
UT WOS:000387802300006
ER
PT J
AU Kannawadi, A
Shapiro, CA
Mandelbaum, R
Hirata, CM
Kruk, JW
Rhodes, JD
AF Kannawadi, Arun
Shapiro, Charles A.
Mandelbaum, Rachel
Hirata, Christopher M.
Kruk, Jeffrey W.
Rhodes, Jason D.
TI The Impact of Interpixel Capacitance in CMOS Detectors on PSF Shapes and
Implications for WFIRST
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE instrumentation: detectors; instrumentation: high angular resolution
ID DARK-MATTER HALOES; COSMOLOGICAL PARAMETER CONSTRAINTS; IMAGE
COMBINATION; LARGE SCALES; SDSS DR7; WEAK; CFHTLENS; CONNECTION;
EVOLUTION; GALAXIES
AB Unlike optical CCDs, near-infrared detectors, which are based on CMOS hybrid readout technology, typically suffer from electrical crosstalk between the pixels. The interpixel capacitance (IPC) responsible for the crosstalk affects the point-spread function (PSF) of the telescope, increasing the size and modifying the shape of all objects in the images while correlating the Poisson noise. Upcoming weak lensing surveys that use these detectors, such as WFIRST, place stringent requirements on the PSF size and shape (and the level at which these are known), which in turn must be translated into requirements on IPC. To facilitate this process, we present a first study of the effect of IPC on WFIRST PSF sizes and shapes. Realistic PSFs are forward-simulated from physical principles for each WFIRST bandpass. We explore how the PSF size and shape depends on the range of IPC coupling with pixels that are connected along an edge or corner; for the expected level of IPC in WFIRST, IPC increases the PSF sizes by similar to 5%. We present a linear fitting formula that describes the uncertainty in the PSF size or shape due to uncertainty in the IPC, which could arise for example due to unknown time evolution of IPC as the detectors age or due to spatial variation of IPC across the detector. We also study of the effect of a small anisotropy in the IPC, which further modifies the PSF shapes. Our results are a first, critical step in determining the hardware and characterization requirements for the detectors used in the WFIRST survey.
C1 [Kannawadi, Arun; Mandelbaum, Rachel] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Shapiro, Charles A.; Rhodes, Jason D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hirata, Christopher M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Lane, Columbus, OH 43210 USA.
[Kruk, Jeffrey W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rhodes, Jason D.] CALTECH, Pasadena, CA 91125 USA.
RP Kannawadi, A (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
EM arunkannawadi@cmu.edu
RI Mandelbaum, Rachel/N-8955-2014
OI Mandelbaum, Rachel/0000-0003-2271-1527
FU WFIRST study office; US Department of Energy; Packard Foundation; Simons
Foundation
FX The authors thank Roger Smith, Bernard Rauscher, and Andres Plazas
Malagon for many useful discussions and Mike Jarvis and Joshua Meyers
for their inputs in developing the GalSim WFIRST module. We thank Edward
Cheng of Conceptual Analytics for his comments in improving the
manuscript and the referee, David Spergel, for correcting a few minor
errors in the original version of the manuscript. This work was carried
out in part at the Jet Propulsion Laboratory (JPL), a NASA center run by
California Institute of Technology. The authors acknowledge funding from
WFIRST study office. CMH is supported by the US Department of Energy,
the Packard Foundation, and the Simons Foundation.
NR 49
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2016
VL 128
IS 967
AR 095001
DI 10.1088/1538-3873/128/967/095001
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200007
ER
PT J
AU Nguyen, HT
Zemcov, M
Battle, J
Bock, JJ
Hristov, V
Korngut, P
Meek, A
AF Nguyen, Hien T.
Zemcov, Michael
Battle, John
Bock, James J.
Hristov, Viktor
Korngut, Phillip
Meek, Andrew
TI Spatial and Temporal Stability of Airglow Measured in the Meinel Band
Window at 1191.3 nm
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE atmospheric effects; site testing; techniques: imaging spectroscopy
ID BACKGROUND-EXPERIMENT CIBER; SKY BRIGHTNESS; EMISSION; FLUCTUATIONS;
SUPPRESSION; ATMOSPHERE; MODEL; LINES
AB We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using a lambda/Delta lambda = 320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. At low airmasses, the absolute sky brightness at this wavelength is found to be 5330 +/- 30 nW m(-2) sr(-1), consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of similar to 100 s integrations the noise performance of the instrument does not appear to significantly degrade from expectations, giving a proof of concept that near-infrared line intensity mapping may be feasible from ground-based sites.
C1 [Nguyen, Hien T.; Zemcov, Michael; Bock, James J.; Korngut, Phillip] NASA, JPL, Pasadena, CA 91109 USA.
[Nguyen, Hien T.; Zemcov, Michael; Battle, John; Bock, James J.; Hristov, Viktor; Korngut, Phillip; Meek, Andrew] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
RP Nguyen, HT (reprint author), NASA, JPL, Pasadena, CA 91109 USA.; Nguyen, HT (reprint author), CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
EM htnguyen@jpl.nasa.gov
FU JPL Research and Technology Development Fund; National Aeronautics and
Space Administration; National Science Foundation
FX The authors wish to thank Jaime Luna for his help designing the LAMP
mechanical assembly, Heath Rhoades at JPL's Table Mountain Observatory
for his assistance setting up the instrument and guidance using the 24
'' telescope, and the Gemini Observatory for making their sky model
tables public. The development of LAMP was supported by the JPL Research
and Technology Development Fund. This publication makes use of data
products from the Two Micron All Sky Survey (2MASS), which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation.
NR 26
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2016
VL 128
IS 967
AR 094504
DI 10.1088/1538-3873/128/967/094504
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200006
ER
PT J
AU Stevenson, KB
Lewis, NK
Bean, JL
Beichman, C
Fraine, J
Kilpatrick, BM
Krick, JE
Lothringer, JD
Mandell, AM
Valenti, JA
Agol, E
Angerhausen, D
Barstow, JK
Birkmann, SM
Burrows, A
Charbonneau, D
Cowan, NB
Crouzet, N
Cubillos, PE
Curry, SM
Dalba, PA
de Wit, J
Deming, D
Desert, JM
Doyon, R
Dragomir, D
Ehrenreich, D
Fortney, JJ
Munoz, AG
Gibson, NP
Gizis, JE
Greene, TP
Harrington, J
Heng, K
Kataria, T
Kempton, EMR
Knutson, H
Kreidberg, L
Lafreniere, D
Lagage, PO
Line, MR
Lopez-Morales, M
Madhusudhan, N
Morley, CV
Rocchetto, M
Schlawin, E
Shkolnik, EL
Shporer, A
Sing, DK
Todorov, KO
Tucker, GS
Wakeford, HR
AF Stevenson, Kevin B.
Lewis, Nikole K.
Bean, Jacob L.
Beichman, Charles
Fraine, Jonathan
Kilpatrick, Brian M.
Krick, J. E.
Lothringer, Joshua D.
Mandell, Avi M.
Valenti, Jeff A.
Agol, Eric
Angerhausen, Daniel
Barstow, Joanna K.
Birkmann, Stephan M.
Burrows, Adam
Charbonneau, David
Cowan, Nicolas B.
Crouzet, Nicolas
Cubillos, Patricio E.
Curry, S. M.
Dalba, Paul A.
de Wit, Julien
Deming, Drake
Desert, Jean-Michel
Doyon, Rene
Dragomir, Diana
Ehrenreich, David
Fortney, Jonathan J.
Munoz, Antonio Garcia
Gibson, Neale P.
Gizis, John E.
Greene, Thomas P.
Harrington, Joseph
Heng, Kevin
Kataria, Tiffany
Kempton, Eliza M. -R.
Knutson, Heather
Kreidberg, Laura
Lafreniere, David
Lagage, Pierre-Olivier
Line, Michael R.
Lopez-Morales, Mercedes
Madhusudhan, Nikku
Morley, Caroline V.
Rocchetto, Marco
Schlawin, Everett
Shkolnik, Evgenya L.
Shporer, Avi
Sing, David K.
Todorov, Kamen O.
Tucker, Gregory S.
Wakeford, Hannah R.
TI Transiting Exoplanet Studies and Community Targets for JWST's Early
Release Science Program
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual;
telescopes
ID WEBB-SPACE-TELESCOPE; FIELD CAMERA 3; HOT JUPITERS; MIDINFRARED
INSTRUMENT; RESOLUTION SPECTROMETER; TRANSMISSION SPECTRUM; GIANT
PLANET; KEPLER FIELD; HD 149026B; WASP-SOUTH
AB The James Webb Space Telescope (JWST) will likely revolutionize transiting exoplanet atmospheric science, due to a combination of its capability for continuous, long duration observations and its larger collecting area, spectral coverage, and spectral resolution compared to existing space-based facilities. However, it is unclear precisely how well JWST will perform and which of its myriad instruments and observing modes will be best suited for transiting exoplanet studies. In this article, we describe a prefatory JWST Early Release Science (ERS) Cycle. 1 program that focuses on testing specific observing modes to quickly give the community the data and experience it needs to plan more efficient and successful transiting exoplanet characterization programs in later cycles. We propose a multi-pronged approach wherein one aspect of the program focuses on observing transits of a single target with all of the recommended observing modes to identify and understand potential systematics, compare transmission spectra at overlapping and neighboring wavelength regions, confirm throughputs, and determine overall performances. In our search for transiting exoplanets that are well suited to achieving these goals, we identify 12 objects (dubbed "community targets") that meet our defined criteria. Currently, the most favorable target is WASP-62b because of its large predicted signal size, relatively bright host star, and location in JWST's continuous viewing zone. Since most of the community targets do not have well-characterized atmospheres, we recommend initiating preparatory observing programs to determine the presence of obscuring clouds/hazes within their atmospheres. Measurable spectroscopic features are needed to establish the optimal resolution and wavelength regions for exoplanet characterization. Other initiatives from our proposed ERS program include testing the instrument brightness limits and performing phase-curve observations. The latter are a unique challenge compared to transit observations because of their significantly longer durations. Using only a single mode, we propose to observe a full-orbit phase curve of one of the previously characterized, short-orbital-period planets to evaluate the facility-level aspects of long, uninterrupted time-series observations.
C1 [Stevenson, Kevin B.; Bean, Jacob L.; Dragomir, Diana; Kreidberg, Laura] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Beichman, Charles] CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, Pasadena, CA USA.
[Fraine, Jonathan; Schlawin, Everett] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kilpatrick, Brian M.; Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Krick, J. E.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91106 USA.
[Lothringer, Joshua D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Mandell, Avi M.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Agol, Eric] Univ Washington, Box 351580, Seattle, WA 98195 USA.
[Angerhausen, Daniel; Wakeford, Hannah R.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barstow, Joanna K.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Birkmann, Stephan M.] European Space Agcy, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Charbonneau, David; Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Cowan, Nicolas B.] McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 1A1, Canada.
[Crouzet, Nicolas] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada.
[Cubillos, Patricio E.] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
[Curry, S. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Dalba, Paul A.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Desert, Jean-Michel] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Doyon, Rene; Lafreniere, David] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, CP 6128,Succ Ctr Vile, Montreal, PQ H3C 3J7, Canada.
[Ehrenreich, David] Observ Univ Geneve, 51 Chemin Maillettes, CH-1290 Versoix, Switzerland.
[Fortney, Jonathan J.; Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Munoz, Antonio Garcia] Tech Univ Berlin, Zentrum Astron & Astrophys, D-10623 Berlin, Germany.
[Gibson, Neale P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Gizis, John E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Greene, Thomas P.; Line, Michael R.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Harrington, Joseph] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA.
[Heng, Kevin] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Kataria, Tiffany; Sing, David K.] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Kempton, Eliza M. -R.] Grinnell Coll, Dept Phys, Noyce Sci Bldg, Grinnell, IA 50112 USA.
[Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lagage, Pierre-Olivier] Paris Saclay Univ, Irfu AIM, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Rocchetto, Marco] UCL, Dept Phys & Astron, London NW1 2PS, England.
[Shkolnik, Evgenya L.] Arizona State Univ, Sch Earth & Space Explorat, 781 S Terrace Rd, Tempe, AZ 85281 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Todorov, Kamen O.] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
RP Stevenson, KB (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kbs@uchicago.edu
RI Harrington, Joseph/E-6250-2011;
OI Gibson, Neale/0000-0002-9308-2353
FU Sagan Fellowship Program - NASA
FX K.B.S. recognizes support from the Sagan Fellowship Program, supported
by NASA and administered by the NASA Exoplanet Science Institute
(NExScI).
NR 50
TC 4
Z9 4
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2016
VL 128
IS 967
AR 094401
DI 10.1088/1538-3873/128/967/094401
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200002
ER
PT J
AU Brown, PJ
Yang, Y
Cooke, J
Olaes, M
Quimby, RM
Baade, D
Gehrels, N
Hoeflich, P
Maund, J
Mould, J
Wang, LF
Wheeler, JC
AF Brown, Peter J.
Yang, Yi
Cooke, Jeff
Olaes, Melanie
Quimby, Robert M.
Baade, Dietrich
Gehrels, Neil
Hoeflich, Peter
Maund, Justyn
Mould, Jeremy
Wang, Lifan
Wheeler, J. Craig
TI ASASSN-15LH: A SUPERLUMINOUS ULTRAVIOLET REBRIGHTENING OBSERVED BY SWIFT
AND HUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; supernovae: individual (ASASSN-15lh, SN2015L);
ultraviolet: general; X-rays: general
ID X-RAY OBSERVATIONS; PAIR-INSTABILITY SUPERNOVAE; MASSIVE BLACK-HOLE;
CORE-COLLAPSE SUPERNOVAE; TIDAL DISRUPTION; SPACE-TELESCOPE; IIN
SUPERNOVA; LUMINOUS SUPERNOVAE; LINEAR-POLARIZATION; MAGNETAR BIRTH
AB We present and discuss ultraviolet and optical photometry from the Ultraviolet/Optical Telescope, X-ray limits from the X-Ray Telescope on Swift, and imaging polarimetry and ultraviolet/optical spectroscopy with the Hubble Space Telescope, all from observations of ASASSN-15lh. It has been classified as a hydrogen-poor superluminous supernova (SLSN I), making it more luminous than any other supernova observed. ASASSN-15lh is not detected in the X-rays in individual or co-added observations. From the polarimetry we determine that the explosion was only mildly asymmetric. We find the flux of ASASSN-15lh to increase strongly into the ultraviolet, with an ultraviolet luminosity 100 times greater than the hydrogen-rich, ultraviolet-bright SLSN II SN 2008es. We find that objects as bright as ASASSN-15lh are easily detectable beyond redshifts of similar to 4 with the single-visit depths planned for the Large Synoptic Survey Telescope. Deep near-infrared surveys could detect such objects past a redshift of similar to 20, enabling a probe of the earliest star formation. A late rebrightening-most prominent at shorter wavelengths -is seen about two months after the peak brightness, which is itself as bright as an SLSN. The ultraviolet spectra during the rebrightening are dominated by the continuum without the broad absorption or emission lines seen in SLSNe or tidal disruption events (TDEs) and the early optical spectra of ASASSN-15lh. Our spectra show no strong hydrogen emission, showing only Lya absorption near the redshift previously found by optical absorption lines of the presumed host. The properties of ASASSN-15lh are extreme when compared to either SLSNe or TDEs.
C1 [Brown, Peter J.; Yang, Yi; Wang, Lifan] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA.
[Cooke, Jeff; Mould, Jeremy] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Olaes, Melanie; Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Quimby, Robert M.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Baade, Dietrich] Southern Hemisphere ESO, European Org Astron Res, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hoeflich, Peter] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Maund, Justyn] Dept Phys & Astron, F39 Hicks Bldg,Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England.
[Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Brown, PJ (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA.
OI Maund, Justyn/0000-0003-0733-7215
FU NASA from Space Telescope Science Institute [NASA 5-26555,
HST-GO-14450.001-A]; NASA [NAS5-26555]; STSCi by STScI
[HST-AR-13276.02-A]; Swift GI program [NNX15AR41G]; NASA's Astrophysics
Data Analysis Program [NNX13AF35G]; [14348]; [14450]
FX We thank the HST director for approving the DDT requests. We thank Matt
McMaster and Dean Hines for helping with the calibration of the ACS/WFC
polarizers. This work is based on observations made with the NASA/ESA
Hubble Space Telescope, obtained from the data archive at the Space
Telescope Science Institute. STScI is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NASA
5-26555. These observations are associated with programs #14348 and
#14450. Support for this work was provided by NASA through grant number
HST-GO-14450.001-A from the Space Telescope Science Institute, which is
operated by AURA, Inc., under NASA contract NAS5-26555. J.C.W. was
supported by STSCi by STScI grant HST-AR-13276.02-A. This work is
supported by the Swift GI program through grant NNX15AR41G. The Swift
Optical/ Ultraviolet Supernova Archive (SOUSA) is supported by NASA's
Astrophysics Data Analysis Program through grant NNX13AF35G. This work
made use of public data in the Swift data archive from observations
requested by several others (PIs: Dong, Godoy, Holoien, Leloudas,
Jonker). This research has made use of NASA's Astrophysics Data System
Bibliographic Services.
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 SEP 1
PY 2016
VL 828
IS 1
AR 3
DI 10.3847/0004-637X/828/1/3
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900003
ER
PT J
AU Cordiner, MA
Boogert, ACA
Charnley, SB
Justtanont, K
Cox, NLJ
Smith, RG
Tielens, AGGM
Wirstrom, ES
Milam, SN
Keane, JV
AF Cordiner, M. A.
Boogert, A. C. A.
Charnley, S. B.
Justtanont, K.
Cox, N. L. J.
Smith, R. G.
Tielens, A. G. G. M.
Wirstrom, E. S.
Milam, S. N.
Keane, J. V.
TI ON THE NATURE OF THE ENIGMATIC OBJECT IRAS 19312+1950: A RARE PHASE OF
MASSIVE STAR FORMATION?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: molecules; masers; stars: AGB and post-AGB; stars: formation;
stars: protostars; stars: winds, outflows
ID YOUNG STELLAR OBJECTS; POSTASYMPTOTIC GIANT BRANCH; WIDE-FIELD CAMERA;
HI-GAL SURVEY; FORMING REGIONS; HERSCHEL OBSERVATIONS; MOLECULAR CLOUDS;
MASER SURVEY; H2O MASERS; CLASS-I
AB IRAS 19312+1950 is a peculiar object that has eluded firm characterization since its discovery, with combined maser properties similar to an evolved star and a young stellar object (YSO). To help determine its true nature, we obtained infrared spectra of IRAS 19312+1950 in the range 5-550 mu m using the Herschel and Spitzer space observatories. The Herschel PACS maps exhibit a compact, slightly asymmetric continuum source at 170 mu m, indicative of a large, dusty circumstellar envelope. The far-IR CO emission line spectrum reveals two gas temperature components: approximate to 0.22 Me of material at 280 +/- 18 K, and approximate to 1.6 M-circle dot of material at 157 +/- 3 K. The O I 63 mu m line is detected on-source but no significant emission from atomic ions was found. The HIFI observations display shocked, high-velocity gas with outflow speeds up to 90 km s(-1) along the line of sight. From Spitzer spectroscopy, we identify ice absorption bands due to H2O at 5.8 mu m and CO2 at 15 mu m. The spectral energy distribution is consistent with a massive, luminous (similar to 2 x 10(4) Le) central source surrounded by a dense, warm circumstellar disk and envelope of total mass similar to 500-700 Me, with large bipolar outflow cavities. The combination of distinctive far-IR spectral features suggest that IRAS 19312+1950 should be classified as an accreting, highmass YSO rather than an evolved star. In light of this reclassification, IRAS 19312+1950 becomes only the fifth high-mass protostar known to exhibit SiO maser activity, and demonstrates that 18 cm OH maser line ratios may not be reliable observational discriminators between evolved stars and YSOs.
C1 [Cordiner, M. A.; Charnley, S. B.; Milam, S. N.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Boogert, A. C. A.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, MS 232-11, Moffett Field, CA 94035 USA.
[Justtanont, K.; Wirstrom, E. S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Cox, N. L. J.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D,Bus 2401, B-3001 Leuven, Belgium.
[Cox, N. L. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Smith, R. G.] Univ New South Wales, Australian Def Force Acad, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia.
[Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Cordiner, MA (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Cordiner, MA (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM martin.cordiner@nasa.gov
OI Wirstrom, Eva/0000-0002-0656-876X; /0000-0003-1689-9201
FU NASA through JPL/Caltech; NASA through NASA's Origins of Solar Systems
program
FX Support for this work was provided by NASA through an award issued by
JPL/Caltech and through NASA's Origins of Solar Systems program. We
gratefully acknowledge the work of Thomas Robitaille for providing and
supporting the Hyperion radiative transfer code.
NR 95
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2016
VL 828
IS 1
AR 51
DI 10.3847/0004-637X/828/1/51
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900051
ER
PT J
AU D'Angelo, G
Bodenheimer, P
AF D'Angelo, Gennaro
Bodenheimer, Peter
TI IN SITU AND EX SITU FORMATION MODELS OF KEPLER 11 PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; planetary systems; planets and satellites:
formation; planets and satellites: individual (Kepler 11); planets and
satellites: interiors; protoplanetary disks
ID MEAN-MOTION RESONANCES; EQUATION-OF-STATE; X-RAY-DIFFRACTION;
DISK-SATELLITE INTERACTION; ISOTHERMAL GASEOUS DISK; TERRESTRIAL MAGMA
OCEAN; EARTHS CORE CONDITIONS; LOW-MASS STARS; SUPER-EARTHS; GIANT
PLANETS
AB We present formation simulations of the six Kepler 11 planets. Models assume either in situ or ex situ assembly, the latter with migration, and are evolved to the estimated age of the system, approximate to 8 Gyr. Models combine detailed calculations of both the gaseous envelope and the condensed core structures, including accretion of gas and solids, of the disk's viscous and thermal evolution, including photo-evaporation and disk-planet interactions, and of the planet's evaporative mass loss after disk dispersal. Planet-planet interactions are neglected. Both sets of simulations successfully reproduce measured radii, masses, and orbital distances of the planets, except for the radius of Kepler 11b, which loses its entire gaseous envelope shortly after formation. Gaseous (H+ He) envelopes account for less than or similar to 18% of the planet masses, and between approximate to 35 and approximate to 60% of the planet radii. In situ models predict a very massive inner disk, whose solid surface density (sigma(Z)) varies from over 10(4) to approximate to 10(3) g cm(-2) at stellocentric distances 0.1 less than or similar to r less than or similar to 0.5 au. Initial gas densities would be in excess of 10(5) g cm(-2) if solids formed locally. Given the high disk temperatures (greater than or similar to 1000 K), planetary interiors can only be composed of metals and highly refractory materials. Sequestration of hydrogen by the core and subsequent outgassing is required to account for the observed radius of Kepler 11b. Ex situ models predict a relatively low-mass disk, whose initial sigma(Z) varies from approximate to 10 to approximate to 5 g cm(-2) at 0.5 less than or similar to r less than or similar to 7 au and whose initial gas density ranges from approximate to 10(3) to approximate to 100 g cm(-2). All planetary interiors are expected to be rich in H2O, as core assembly mostly occurs exterior to the ice condensation front. Kepler 11b is expected to have a steam atmosphere, and H2O is likely mixed with H+He in the envelopes of the other planets. Results indicate that Kepler. 11g may not be more massive than Kepler. 11e.
C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
[D'Angelo, Gennaro] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Bodenheimer, Peter] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.; D'Angelo, G (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM gennaro.dangelo@nasa.gov; peter@ucolick.org
OI D'Angelo, Gennaro/0000-0002-2064-0801; Bodenheimer,
Peter/0000-0001-6093-3097
FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins
of Solar Systems Program [NNX14AG92G]; NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center
FX We thank Uma Gorti for numerous helpful discussions and for her precious
guidance during the implementation of the disk photo-evaporation module.
We are grateful to an anonymous referee, whose insightful comments
helped improve several parts of this paper. G.D. thanks the Los Alamos
National Laboratory for its hospitality. G.D. acknowledges support from
NASA Outer Planets Research Program grant 202844.02.02.01.75 and from
NASA Origins of Solar Systems Program grant 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 186
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U1 3
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2016
VL 828
IS 1
AR 33
DI 10.3847/0004-637X/828/1/33
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900033
ER
PT J
AU Deller, AT
Vigeland, SJ
Kaplan, DL
Goss, WM
Brisken, WF
Chatterjee, S
Cordes, JM
Janssen, GH
Lazio, TJW
Petrov, L
Stappers, BW
Lyne, A
AF Deller, A. T.
Vigeland, S. J.
Kaplan, D. L.
Goss, W. M.
Brisken, W. F.
Chatterjee, S.
Cordes, J. M.
Janssen, G. H.
Lazio, T. J. W.
Petrov, L.
Stappers, B. W.
Lyne, A.
TI MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSR pi. I. TWO BINARY
MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; pulsars: individual (PSR J1022+1001, J2145-0750); stars:
neutron; techniques: high angular resolution; white dwarfs
ID BASE-LINE ARRAY; DATA RELEASE; SPECTROSCOPIC ANALYSIS; SOFTWARE
CORRELATOR; PROPER MOTION; PARALLAXES; SKY; DISTANCE; MASS;
INTERFEROMETRY
AB Model-independent distance constraints to binary millisecond pulsars (MSPs) are of great value to both the timing observations of the radio pulsars and multiwavelength observations of their companion stars. Astrometry using very long baseline interferometry (VLBI) can be employed to provide these model-independent distances with very high precision via the detection of annual geometric parallax. Using the Very Long Baseline Array, we have observed two binary MSPs, PSR J1022+1001 and J2145-0750, over a two-year period and measured their distances to be 700(10)(+14) pc and 613(-14)(+16) pc respectively. We use the well-calibrated distance in conjunction with revised analysis of optical photometry to tightly constrain the nature of their massive (M similar to 0.85 M-circle dot) white dwarf companions. Finally, we show that several measurements of the parallax and proper motion of PSR J1022 + 1001 and PSR J2145-0750 obtained by pulsar timing array projects are incorrect, differing from the more precise VLBI values by up to 5 sigma. We investigate possible causes for the discrepancy, and find that imperfect modeling of the solar wind is a likely candidate for the errors in the timing model given the low ecliptic latitude of these two pulsars.
C1 [Deller, A. T.; Janssen, G. H.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Vigeland, S. J.; Kaplan, D. L.] Univ Wisconsin Milwaukee, POB 413, Milwaukee, WI 53201 USA.
[Goss, W. M.; Brisken, W. F.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chatterjee, S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Petrov, L.] Astrogeo Ctr, Falls Church, VA 22043 USA.
[Stappers, B. W.; Lyne, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Deller, AT (reprint author), Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
OI Deller, Adam/0000-0001-9434-3837
FU NWO Veni Fellowship; NANOGrav project through National Science
Foundation (NSF) PIRE program [0968296]; NSF Physics Frontiers Center
[1430284]; National Aeronautics and Space Administration; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of Energy
Office of Science
FX A.T.D. was supported by an NWO Veni Fellowship. D.L.K. an d S.J.V.
receive support from the NANOGrav project through National Science
Foundation (NSF) PIRE program award number 0968296 and NSF Physics
Frontiers Center award number 1430284. Part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. The authors thank David Nice and Pierre Bergeron for
useful discussions. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. Pulsar research at the
Jodrell Bank Centre for Astrophysics and the observations using the
Lovell Telescope are supported by a consolidated grant from the STFC in
the UK. Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/.
NR 55
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2016
VL 828
IS 1
AR 8
DI 10.3847/0004-637X/828/1/8
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900008
ER
PT J
AU Furst, F
Grinberg, V
Tomsick, JA
Bachetti, M
Boggs, SE
Brightman, M
Christensen, FE
Craig, WW
Gandhi, P
Grefenstette, B
Hailey, CJ
Harrison, FA
Madsen, KK
Parker, ML
Pottschmidt, K
Stern, D
Walton, DJ
Wilms, J
Zhang, WW
AF Furst, F.
Grinberg, V.
Tomsick, J. A.
Bachetti, M.
Boggs, S. E.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Grefenstette, B.
Hailey, C. J.
Harrison, F. A.
Madsen, K. K.
Parker, M. L.
Pottschmidt, K.
Stern, D.
Walton, D. J.
Wilms, J.
Zhang, W. W.
TI SPECTRO-TIMING STUDY OF GX 339-4 IN A HARD INTERMEDIATE STATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: black holes; X-rays: binaries;
X-rays: individual (GX 339-4)
ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; BLACK-HOLE CANDIDATES;
ADVECTION-DOMINATED ACCRETION; RELATIVISTIC PRECESSION MODEL;
LENS-THIRRING PRECESSION; NOVA XTE J1550-564; LOW/HARD STATE; CYGNUS
X-1; FREQUENCY CORRELATION
AB We present an analysis of Nuclear Spectroscopic Telescope Array. observations of a hard intermediate state of the transient. black hole GX 339-4 taken in 2015 January. With. the source softening significantly over the course of the 1.3 day long observation we split the data into 21 sub-sets and find that the spectrum of all of them can be well described by a power-law continuum with an additional relativistically blurred reflection component. The photon index increases from similar to 1.69 to similar to 1.77 over the course of the observation. The accretion disk is truncated at around nine gravitational radii in all spectra. We also perform timing analysis on the same 21 individual data sets, and find a strong type-C quasi-periodic oscillation (QPO), which increases. in frequency from similar to 0.68 to similar to 1.05 Hz with time. The frequency change is well correlated with the softening of the spectrum. We discuss possible scenarios for the production of the QPO and calculate predicted inner radii in the relativistic precession model as well as the global disk mode oscillations model. We find discrepancies with respect to the observed values in both models unless we allow for a black hole mass of similar to 100 M-circle dot, which is highly unlikely. We discuss possible systematic uncertainties, in particular with the measurement of the inner accretion disk radius in the relativistic reflection model. We conclude that the combination of observed QPO frequencies and inner accretion disk radii, as obtained from spectral fitting,. is difficult to reconcile with current models.
C1 [Furst, F.; Brightman, M.; Grefenstette, B.; Harrison, F. A.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Grinberg, V.] MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bachetti, M.] INAF, Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
[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.
[Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Parker, M. L.] Inst Astron, Cambridge CB3 0HA, England.
[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.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU NASA [NNG08FD60C, NAS8-03060]; National Aeronautics and Space
Administration; NASA through Smithsonian Astrophysical Observatory (SAO)
[SV3-73016]
FX We thank the anonymous referee for the constructive and helpful
comments. We thank the NuSTAR schedulers and SOC, in particular Karl
Forster, for making this observation possible. We thank Javier Garcia
and Thomas Dauser for helpful discussions about the reflection models.
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. Support for
this work was provided by NASA through the Smithsonian Astrophysical
Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra
X-ray Center (CXC) and Science Instruments; CXC is operated by SAO for
and on behalf of NASA under contract NAS8-03060. We 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 a collection of ISIS
functions (ISISscripts) provided by ECAP/Remeis observatory and MIT
(http://www.sternwarte.uni-erlangen.de/isis/). We would like to thank
John E. Davis for the slxfig module, which was used to produce all
figures in this work. This research has made use of MAXI data provided
by RIKEN, JAXA and the MAXI team.
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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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SC Astronomy & Astrophysics
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UT WOS:000386894900034
ER
PT J
AU Hamren, K
Beaton, RL
Guhathakurta, P
Gilbert, KM
Tollerud, EJ
Boyer, ML
Rockosi, CM
Smith, GH
Majewski, SR
Howley, K
AF Hamren, Katherine
Beaton, Rachael L.
Guhathakurta, Puragra
Gilbert, Karoline M.
Tollerud, Erik J.
Boyer, Martha L.
Rockosi, Constance M.
Smith, Graeme H.
Majewski, Steven R.
Howley, Kirsten
TI CARBON STARS IN THE SATELLITES AND HALO OF M31
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); stars: AGB and post-AGB; stars: carbon
ID ASYMPTOTIC GIANT BRANCH; DIGITAL-SKY-SURVEY; LOCAL GROUP GALAXIES; DWARF
SPHEROIDAL GALAXIES; SPITZER-SPACE-TELESCOPE; SURVEY STELLAR SPECTRA;
LARGE-MAGELLANIC-CLOUD; AGB STARS; SPLASH SURVEY; METAL-POOR
AB We spectroscopically identify a sample of carbon stars in the satellites and halo of M31 using moderate-resolution optical spectroscopy from the Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo survey. We present the photometric properties of our sample of 41 stars, including their brightness with respect to the tip of the red giant branch (TRGB) and their distributions in various color-color spaces. This analysis reveals a bluer population of carbon stars fainter than the TRGB and a redder population of carbon stars brighter than the TRGB. We then apply principal component analysis to determine the sample's eigenspectra and eigencoefficients. Correlating the eigencoefficients with various observable properties reveals the spectral features that trace effective temperature and metallicity. Putting the spectroscopic and photometric information together, we find the carbon stars in the satellites and halo of M31 to be minimally impacted by dust and internal dynamics. We also find that while there is evidence to suggest that the sub-TRGB stars are extrinsic in origin, it is also possible that they are are particularly faint members of the asymptotic giant branch.
C1 [Hamren, Katherine; Guhathakurta, Puragra; Rockosi, Constance M.; Smith, Graeme H.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
[Beaton, Rachael L.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Gilbert, Karoline M.; Tollerud, Erik J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gilbert, Karoline M.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Howley, Kirsten] Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA.
RP Hamren, K (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
EM khamren@ucolick.org
OI Guhathakurta, Puragra/0000-0001-8867-4234
FU NSF [AST-1010039, AST-1412648, AST-1413269]; NASA [HST-GO-12055]; NSF
Graduate Research Fellowship; Giacconi Fellowship
FX The authors would like to thank Bernhard Aringer and Leo Girardi for
helpful conversations and an early look at the 2016 cool star models. We
would also like to thank Marla Geha, James Bullock, and Jason Kalirai
for their work on the SPLASH survey over the years. and their
willingness to provide data for this paper. P.G. and K.H. acknowledge
NSF grants AST-1010039 and AST-1412648 and NASA grant HST-GO-12055.
R.L.B. and S.R.M. thank NSF grant AST-1413269. K. H. was supported by an
NSF Graduate Research Fellowship, and E.J.T. was supported by a Giacconi
Fellowship. We appreciate the very significant cultural role and
reverence that the summit of Mauna Kea has always held within the
indigenous Hawaiian community. We are most grateful to have had the
opportunity 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.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900015
ER
PT J
AU Han, C
Udalski, A
Gould, A
Zhu, W
Street, RA
Yee, JC
Beichman, C
Bryden, C
Novati, SC
Carey, S
Fausnaugh, M
Gaudi, BS
Henderson, CB
Shvartzvald, Y
Wibking, B
Szymanski, MK
Soszynski, I
Skowron, J
Mroz, P
Poleski, R
Pietrukowicz, P
Kozlowski, S
Ulaczyk, K
Wyrzykowski, L
Pawlak, M
Tsapras, Y
Hundertmark, M
Bachelet, E
Dominik, M
Bramich, DM
Cassan, A
Jaimes, RF
Horne, K
Ranc, C
Schmidt, R
Snodgrass, C
Wambsganss, J
Steele, IA
Menzies, J
Mao, S
Bozza, V
Jorgensen, UG
Alsubai, KA
Ciceri, S
D'Ago, G
Haugbolle, T
Hessman, FV
Hinse, TC
Juncher, D
Korhonen, H
Mancini, L
Popovas, A
Rabus, M
Rahvar, S
Scarpetta, G
Skottfelt, J
Southworth, J
Starkey, D
Surdej, J
Wertz, O
Zarucki, M
Pogge, RW
DePpoy, DL
AF Han, C.
Udalski, A.
Gould, A.
Zhu, Wei
Street, R. A.
Yee, J. C.
Beichman, C.
Bryden, C.
Novati, S. Calchi
Carey, S.
Fausnaugh, M.
Gaudi, B. S.
Henderson, Calen B.
Shvartzvald, Y.
Wibking, B.
Szymanski, M. K.
Soszynski, I.
Skowron, J.
Mroz, P.
Poleski, R.
Pietrukowicz, P.
Kozlowski, S.
Ulaczyk, K.
Wyrzykowski, L.
Pawlak, M.
Tsapras, Y.
Hundertmark, M.
Bachelet, E.
Dominik, M.
Bramich, D. M.
Cassan, A.
Jaimes, R. Figuera
Horne, K.
Ranc, C.
Schmidt, R.
Snodgrass, C.
Wambsganss, J.
Steele, I. A.
Menzies, J.
Mao, S.
Bozza, V.
Jorgensen, U. G.
Alsubai, K. A.
Ciceri, S.
D'Ago, G.
Haugbolle, T.
Hessman, F. V.
Hinse, T. C.
Juncher, D.
Korhonen, H.
Mancini, L.
Popovas, A.
Rabus, M.
Rahvar, S.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Starkey, D.
Surdej, J.
Wertz, O.
Zarucki, M.
Pogge, R. W.
DePpoy, D. L.
CA Spitzer Microlensing Team
OGLE Collaboration
RoboNet Collaboration
MINDSTEp Consortium
Fun Collaboration
TI OGLE-2015-BLG-0479LA,B: BINARY GRAVITATIONAL MICROLENS CHARACTERIZED BY
SIMULTANEOUS GROUND-BASED AND SPACE-BASED OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID DIFFERENCE IMAGE-ANALYSIS; PARALLAX SATELLITE MASS; LENSING EXPERIMENT;
PLANET PHOTOMETRY; GALACTIC BULGE; OGLE-III; SPITZER; EVENTS; STARS;
DISTANCES
AB We present a combined analysis of the observations of the gravitational microlensing event OGLE-2015-BLG-0479 taken both from the ground and by the Spitzer Space Telescope. The light curves seen from the ground and from space exhibit a time offset of similar to 13 days between the caustic spikes, indicating that the relative lens-source positions seen from the two places are displaced by parallax effects. From modeling the light curves, we measure the space-based microlens parallax. Combined with the angular Einstein radius measured by analyzing the caustic crossings, we determine the mass and distance of the lens. We find that the lens is a binary composed of two G-type stars with masses of similar to 1.0 M-circle dot and similar to 0.9 M-circle dot located at a distance. of similar to 3 kpc. In addition, we are able to constrain the complete orbital parameters of the lens thanks to the precise measurement of the microlens parallax derived from the joint analysis. In contrast to the binary event OGLE-2014-BLG-1050, which was also observed by Spitzer, we find that the interpretation of OGLE-2015-BLG-0479 does not suffer from the degeneracy between (+/-, +/-) and (+/-, -/+) solutions, confirming that the four-fold parallax degeneracy in single-lens events collapses into the two-fold degeneracy for the general case of binary-lens events. The location of the blend in the color-magnitude diagram is consistent with the lens properties, suggesting that the blend is the lens itself. The blend is bright enough for spectroscopy and thus this possibility can be checked from future follow-up observations.
C1 [Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Udalski, A.; Szymanski, M. K.; Soszynski, I.; Skowron, J.; Mroz, P.; Poleski, R.; Pietrukowicz, P.; Kozlowski, S.; Ulaczyk, K.; Wyrzykowski, L.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Gould, A.; Zhu, Wei; Gaudi, B. S.; Wibking, B.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Gould, A.; Ciceri, S.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Street, R. A.] Queen Mary Univ London, Sch Phys & Astron, Mile End Rd, London E1 4NS, England.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
[Bryden, C.; Henderson, Calen B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, S.] CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
[Tsapras, Y.; Jaimes, R. Figuera; Schmidt, R.; Wambsganss, J.] Univ Heidelberg ZAH, Zentrum Astron, Astronom Rechen Inst, D-69120 Heidelberg, Germany.
[Hundertmark, M.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Bachelet, E.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Bachelet, E.; Bramich, D. M.; Alsubai, K. A.] Qatar Fdn, HBKU, QEERI, Doha, Qatar.
[Dominik, M.; Jaimes, R. Figuera; Horne, K.; Starkey, D.] Univ St Andrews, Sch Phys Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Ranc, C.] UPMC Univ Paris 6, Sorbonne Univ, CNRS, Inst Astrophys Paris,UMR 7095, 98 Bis Bd Arago, F-75014 Paris, France.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Menzies, J.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Jorgensen, U. G.; Haugbolle, T.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Hessman, F. V.] Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
[Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 305348, South Korea.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[DePpoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016
OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago, Giuseppe/0000-0001-9697-7331
FU Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; National Science Centre, Poland [MAESTRO
2014/14/A/ST9/00121]; JPL grant [1500811]; NASA through the Sagan
Fellowship Program; NASA
FX Work by C. Han was supported by the Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea. The OGLE
project has received funding from the National Science Centre, Poland,
grant MAESTRO 2014/14/A/ST9/00121 to A.U. The OGLE Team thanks Profs.
M.. Kubiak and G.. Pietrzynski, former members of the OGLE team, for
their contribution to the collection of the OGLE photometric data over
the past years. Work by A.G. was supported by JPL grant 1500811. Work by
J.C.Y. was performed under contract with the California Institute of
Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA
through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute. Work by C.B.H. and Y.S. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Universities Space Research Association
through a contract with NASA. The Spitzer Team thanks Christopher S.
Kochanek for graciously trading us his allocated observing time on the
CTIO 1.3m during the Spitzer campaign. We acknowledge the high-speed
internet service (KREONET) provided by Korea Institute of Science and
Technology Information (KISTI).
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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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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900053
ER
PT J
AU Lieman-Sifry, J
Hughes, AM
Carpenter, JM
Gorti, U
Hales, A
Flaherty, KM
AF Lieman-Sifry, Jesse
Hughes, A. Meredith
Carpenter, John M.
Gorti, Uma
Hales, Antonio
Flaherty, Kevin M.
TI DEBRIS DISKS IN THE SCORPIUS-CENTAURUS OB ASSOCIATION RESOLVED BY ALMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planets and satellites:
formation; protoplanetary disks; submillimeter: planetary systems
ID TERRESTRIAL PLANET FORMATION; CIRCLE-DOT STARS; ANALOG HD 107146; A-TYPE
STARS; BETA-PICTORIS; DUSTY DEBRIS; MOLECULAR GAS; MILLIMETER EMISSION;
CIRCUMSTELLAR DISK; SCATTERED-LIGHT
AB We present a CO(2-1) and 1240 mu m continuum survey of 23 debris disks with spectral types B9-G1, observed at an angular resolution of 0.5 ''-1 '' with the Atacama Large Millimeter/Submillimeter Array (ALMA). The sample was selected for large infrared excess and age similar to 10 Myr, to characterize the prevalence of molecular gas emission in young debris disks. We identify three CO-rich debris disks, plus two additional tentative (3 sigma) CO detections. Twenty disks were detected in the continuum at the >3 sigma level. For the 12 disks in the sample that are spatially resolved by our observations, we perform an independent analysis of the interferometric continuum visibilities to constrain the basic dust disk geometry, as well as a simultaneous analysis of the visibilities and broadband spectral energy distribution to constrain the characteristic grain size and disk mass. The gas-rich debris disks exhibit preferentially larger outer radii in their dust disks, and a higher prevalence of characteristic grain sizes smaller than the blowout size. The gas-rich disks do not exhibit preferentially larger dust masses, contrary to expectations for a scenario in which a higher cometary destruction rate would be expected to result in a larger mass of both CO and dust. The three debris disks in our sample with strong CO detections are all around A stars: the conditions in disks around intermediate-mass stars appear to be the most conducive to the survival or formation of CO.
C1 [Lieman-Sifry, Jesse; Hughes, A. Meredith; Flaherty, Kevin M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
[Carpenter, John M.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA.
[Carpenter, John M.; Hales, Antonio] Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile.
[Gorti, Uma] SETI Inst, Mountain View, CA USA.
[Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hales, Antonio] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
RP Lieman-Sifry, J (reprint author), Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
FU NSF [AST-1412647, CNS-0619508]; NASA CT Space Grant Directed Campus
Scholarship
FX The authors thank Angelo Ricarte for his contributions to the code base
and helpful comments, and the anonymous referee for a careful commentary
that improved the paper. J.L.S. and A.M.H. gratefully acknowledge
support from NSF grant AST-1412647. J.L.S. was also supported in part by
a NASA CT Space Grant Directed Campus Scholarship. We acknowledge
Wesleyan University for time on its high-performance computing cluster,
supported by the NSF under grant number CNS-0619508. This work makes use
of the following ALMA data: ADS/JAO. ALMA#2012.1.00688. S. ALMA is a
partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/ NRAO, and NAOJ. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. This
research has made use of NASA's Astrophysics Data System Bibliographic
Services, as well as Astropy, a community-developed core Python package
for Astronomy (Astropy Collaboration et al. 2013).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900025
ER
PT J
AU Lomax, JR
Wisniewski, JP
Grady, CA
McElwain, MW
Hashimoto, J
Kudo, T
Kusakabe, N
Okamoto, YK
Fukagawa, M
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Currie, TM
Egner, S
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Inoue, A
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
Mayama, S
Miyama, S
Momose, M
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Schneider, GH
Serabyn, E
Sitko, ML
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Lomax, Jamie R.
Wisniewski, John P.
Grady, Carol A.
McElwain, Michael W.
Hashimoto, Jun
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Okamoto, Yoshiko K.
Fukagawa, Misato
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Currie, Thayne M.
Egner, Sebastian
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Inoue, Akio
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
Mayama, Satoshi
Miyama, Shoken
Momose, Munetake
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Schneider, Glenn H.
Serabyn, Eugene
Sitko, Michael L.
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF
PLANETARY BODIES WITHIN THE AB AUR SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; planetary systems; protoplanetary disks;
radiative transfer; stars: individual (AB Aur); stars: pre-main sequence
ID YOUNG STELLAR OBJECTS; HERBIG AE STARS; SPECTRAL ENERGY-DISTRIBUTIONS;
CIRCUMSTELLAR DUST; PROTOPLANETARY DISK; RADIATION TRANSFER;
INTERSTELLAR DUST; SIZE DISTRIBUTION; HIGH-RESOLUTION; TAURUS-AURIGA
AB We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.
C1 [Lomax, Jamie R.; Wisniewski, John P.; Hashimoto, Jun] Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
[Grady, Carol A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Grady, Carol A.] Goddard Ctr Astrobiol, Pasadena, CA USA.
[McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Code 6681, Greenbelt, MD 20771 USA.
[Kudo, Tomoyuki; Currie, Thayne M.; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Kusakabe, Nobuhiko; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Tamura, Motohide] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Okamoto, Yoshiko K.] Ibaraki Univ, Fac Sci, Inst Astrophys & Planetary Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange UMR 7293, 28 Ave Valrose, F-06108 Nice 2, France.
[Brandner, Wolfgang] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Turner, Edwin L.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Kwon, Jungmi; Usuda, Tomonori; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama Cho, Hayama, Kanagawa 2400193, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima 7398511, Japan.
[Momose, Munetake] Ibaraki Univ, Coll Sci, Bunkyo 2-1-1, Mito, Ibaraki 3108512, Japan.
[Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Schneider, Glenn H.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Sitko, Michael L.] Space Sci Inst, 475 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23141, Taipei 10617, Taiwan.
[Thalmann, Christian] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Lomax, JR (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
EM Jamie.R.Lomax@ou.edu; wisniewski@ou.edu; carol.a.grady@nasa.gov
RI MIYAMA, Shoken/A-3598-2015
FU NASA Origins of Solar System program [NNX13AK17G, RTOP 12-OSS12-0045,
NNG13PB64P]; MEXT Japan; Mitsubishi Foundation; [NSF-AST 1009203];
[1008440]; [1009314]
FX We acknowledge support from NSF-AST 1009203 (J.C.), 1008440 (C.G.), and
1009314 (E.R., J.W., J.H.) and the NASA Origins of Solar System program
under NNX13AK17G (J.W.), RTOP 12-OSS12-0045 (M.M.), and NNG13PB64P
(C.G.). This work is partly supported by a Grant-in-Aid for Science
Research in a Priority Area from MEXT Japan and by the Mitsubishi
Foundation. The authors recognize and acknowledge the significant
cultural role and reverence that the summit of Mauna Kea has always had
within the indigenous Hawaiian community. We are most fortunate to have
the opportunity to conduct observations from this mountain. We wish to
extend special thanks to those of Hawaiian ancestry on whose sacred
mountain we are privileged to be guests. This work is based in part on
data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan. We also thank Barbara
Whitney for providing us with helpful feedback that improved our paper
and for clarifying aspects of her HOCHUNK3D code, and Anthony Paat for
helping run models. Additionally, we would like to thank the anonymous
reviewer for providing comments that led to an improved paper.
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J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900002
ER
PT J
AU Nelson, EJ
van Dokkum, PG
Schreiber, NMF
Franx, M
Brammer, GB
Momcheva, IG
Wuyts, S
Whitaker, KE
Skelton, RE
Fumagalli, M
Hayward, CC
Kriek, M
Labbe, I
Leja, J
Rix, HW
Tacconi, LJ
van der Wel, A
van den Bosch, FC
Oesch, PA
Dickey, C
Lange, JU
AF Nelson, Erica June
van Dokkum, Pieter G.
Schreiber, Natascha M. Foerster
Franx, Marijn
Brammer, Gabriel B.
Momcheva, Ivelina G.
Wuyts, Stijn
Whitaker, Katherine E.
Skelton, Rosalind E.
Fumagalli, Mattia
Hayward, Christopher C.
Kriek, Mariska
Labbe, Ivo
Leja, Joel
Rix, Hans-Walter
Tacconi, Linda J.
van der Wel, Arjen
van den Bosch, Frank C.
Oesch, Pascal A.
Dickey, Claire
Lange, Johannes Ulf
TI WHERE STARS FORM: INSIDE-OUT GROWTH AND COHERENT STAR FORMATION FROM HST
H alpha MAPS OF 3200 GALAXIES ACROSS THE MAIN SEQUENCE AT 0.7 < z < 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
galaxies: star formation; galaxies: structure
ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; SINS/ZC-SINF SURVEY; INTEGRAL
FIELD SPECTROSCOPY; LYMAN BREAK GALAXIES; ULTRA-DEEP FIELD;
EXTRAGALACTIC LEGACY SURVEY; COMPACT QUIESCENT GALAXIES;
MASS-METALLICITY RELATION; KILOPARSEC-SCALE CLUMPS
AB We present H alpha maps at 1 kpc spatial resolution for star-forming galaxies at z similar to 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked H alpha images, we reach surface brightness limits of 1 x 10(-18) erg s(-1) cm(-2) arc sec(-2), allowing us to map the distribution of ionized gas to similar to 10 kpc for typical L* galaxies at this epoch. We find that the spatial extent of the H alpha distribution increases with stellar mass as r(H alpha) = 1.5(M-*/10(10) M-circle dot)(0.23) kpc. The H alpha emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as r(H alpha)/r(*) = 1.1(M-*/10(10) M-circle dot)(0.054). We map the H alpha distribution as a function of SFR(IR+UV) and find evidence for "coherent star formation" across the SFR-M-* plane: above the main sequence (MS), H alpha is enhanced at all radii; below the MS, H alpha is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (10(10.5) < M-*/M-circle dot < 10(11)), above the MS, H alpha is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(H alpha), as well as. the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M-* plane, the absolute SFR as traced by H alpha is always centrally peaked, even in galaxies below the MS.
C1 [Nelson, Erica June; van Dokkum, Pieter G.; Momcheva, Ivelina G.; Leja, Joel; van den Bosch, Frank C.; Oesch, Pascal A.; Dickey, Claire; Lange, Johannes Ulf] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Schreiber, Natascha M. Foerster; Wuyts, Stijn; Tacconi, Linda J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Franx, Marijn; Fumagalli, Mattia; Labbe, Ivo] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Brammer, Gabriel B.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Wuyts, Stijn] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England.
[Whitaker, Katherine E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Skelton, Rosalind E.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Hayward, Christopher C.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Hayward, Christopher C.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA.
[Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rix, Hans-Walter; van der Wel, Arjen] MPIA, Konigstuhl 17, Heidelberg, Germany.
RP Nelson, EJ (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RI Skelton, Rosalind/S-1845-2016
OI Skelton, Rosalind/0000-0001-7393-3336
FU 3D-HST Treasury Program [GO 12177, 12328]; NASA [NAS5-26555]; National
Science Foundation Graduate Research Fellowship
FX We thank the referee for their thoughtful report,. which improved the
paper. This work is based on observations taken by the 3D-HST Treasury
Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by
the Associations of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. E.J.N. gratefully acknowledges support from
the National Science Foundation Graduate Research Fellowship.
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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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PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900027
ER
PT J
AU Odegard, N
Kogut, A
Chuss, DT
Miller, NJ
AF Odegard, N.
Kogut, A.
Chuss, D. T.
Miller, N. J.
TI ASSESSMENT OF MODELS OF GALACTIC THERMAL DUST EMISSION USING COBE/FIRAS
AND COBE/DIRBE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; submillimeter: ISM
ID BACKGROUND EXPERIMENT SEARCH; TEMPERATURE-DEPENDENCE; AMORPHOUS SOLIDS;
COBE FIRAS; ABSORPTION-COEFFICIENT; SPECTRAL OBSERVATIONS;
INFRARED-EMISSION; GAL OBSERVATIONS; COLD CLUMPS; PLANCK
AB Accurate modeling of the spectrum of thermal dust emission at millimeter wavelengths is important for improving the accuracy of foreground subtraction for cosmic microwave background (CMB) measurements, for improving the accuracy with which the contributions of different foreground emission components can be determined, and for improving our understanding of dust composition and dust physics. We fit four models of dust emission to high Galactic latitude COBE/FIRAS and COBE/DIRBE observations from 3 mm to 100 mu m and compare the quality of the fits. We consider the two-level systems (TLS) model because it provides a physically motivated explanation for the observed long wavelength flattening of the dust spectrum and the anti-correlation between emissivity index and dust temperature. We consider the model of Finkbeiner et al. because it has been widely used for CMB studies, and the generalized version of this model that was recently applied to Planck data by Meisner and Finkbeiner. For comparison we have also fit a phenomenological model consisting of the sum of two graybody components. We find that the two-graybody model gives the best fit and the FDS model gives a significantly poorer fit than the other models. The Meisner and Finkbeiner model and the TLS model remain viable for use in Galactic foreground subtraction, but the FIRAS data do not have a sufficient signal-to-noise ratio to provide a strong test of the predicted spectrum at millimeter wavelengths.
C1 [Odegard, N.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA.
[Kogut, A.; Miller, N. J.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
[Chuss, D. T.] Villanova Univ, Dept Phys, 800 E Lancaster Ave, Villanova, PA 19085 USA.
[Miller, N. J.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RP Odegard, N (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA.
EM Nils.Odegard@nasa.gov
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J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900016
ER
PT J
AU Parmentier, V
Fortney, JJ
Showman, AP
Morley, C
Marley, MS
AF Parmentier, Vivien
Fortney, Jonathan J.
Showman, Adam P.
Morley, Caroline
Marley, Mark S.
TI TRANSITIONS IN THE CLOUD COMPOSITION OF HOT JUPITERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: gaseous
planets; radiative transfer; scattering
ID 3-DIMENSIONAL ATMOSPHERIC CIRCULATION; EXTRASOLAR GIANT PLANETS; GREY
ANALYTICAL-MODEL; EXOPLANET HD 189733B; OPTICAL-PHASE CURVES; MASS DWARF
STARS; BROWN DWARFS; IRRADIATED ATMOSPHERES; THERMAL STRUCTURE;
TRANSMISSION SPECTRUM
AB Over a large range of equilibrium temperatures, clouds shape the transmission spectrum of hot Jupiter atmospheres, yet their composition remains unknown. Recent observations show that the Kepler light. curves of some hot Jupiters are asymmetric: for the hottest planets, the light. curve peaks before secondary eclipse, whereas for planets cooler than similar to 1900 K, it peaks after secondary eclipse. We use the thermal structure from 3D global circulation models to determine the expected cloud distribution and Kepler light. curves of hot Jupiters. We demonstrate that the change from an optical light. curve dominated by thermal emission to one dominated by scattering (reflection) naturally explains the observed trend from negative to positive offset. For the cool planets the presence of an asymmetry in the Kepler light curve is a telltale sign of the cloud composition, because each cloud species can produce an offset only over a narrow range of effective temperatures. By comparing our models and the observations, we show that the cloud composition of hot Jupiters likely varies with equilibrium temperature. We suggest that a transition occurs between silicate and manganese sulfide clouds at a temperature near 1600 K, analogous to the L/T transition on brown dwarfs. The cold trapping of cloud species below the photosphere naturally produces such a transition and predicts similar transitions for other condensates, including TiO. We predict that most hot Jupiters should have cloudy nightsides, that partial cloudiness should be common at the limb, and that the dayside hot spot should often be cloud-free.
C1 [Parmentier, Vivien; Fortney, Jonathan J.; Morley, Caroline] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA.
RP Parmentier, V (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.; Parmentier, V (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.; Parmentier, V (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
OI Marley, Mark/0000-0002-5251-2943
FU Sagan Postdoctoral Fellowship through NASA Exoplanet Science Institute;
Origins grant [NNX12AI196]
FX We thank Mike Line for reading the manuscript and providing useful
comments and Kevin Stevenson for useful discussions. V. P. acknowledges
support from the Sagan Postdoctoral Fellowship through the NASA
Exoplanet Science Institute. A.P.S. was supported by Origins grant
NNX12AI196.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000386894900022
ER
PT J
AU Sadykov, VM
Kosovichev, AG
Sharykin, IN
Zimovets, IV
Dominguez, SV
AF Sadykov, Viacheslav M.
Kosovichev, Alexander G.
Sharykin, Ivan N.
Zimovets, Ivan V.
Vargas Dominguez, Santiago
TI RELATIONSHIP BETWEEN CHROMOSPHERIC EVAPORATION AND MAGNETIC FIELD
TOPOLOGY IN AN M-CLASS SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: magnetic fields;
Sun: UV radiation; techniques: spectroscopic
ID LOOP RADIATIVE HYDRODYNAMICS; QUASI-SEPARATRIX LAYERS;
REGION-IMAGING-SPECTROGRAPH; SLIP-RUNNING RECONNECTION; THICK-TARGET;
RESOLUTION OBSERVATIONS; MODEL; IRIS; DYNAMICS; PLASMA
AB Chromospheric evaporation is observed as Doppler blueshift during solar flares. It plays a key role in the dynamics and energetics of solar flares; however, its mechanism is still unknown. In this paper,. we present a detailed analysis of spatially resolved multi-wavelength observations of chromospheric evaporation during an M 1.0-class solar flare (SOL2014-06-12T21:12) using data from NASA's Interface Region Imaging Spectrograph and HMI/SDO (the. Helioseismic and Magnetic Imager on. board. the. Solar Dynamics Observatory), and high-resolution observations from VIS/NST (the. Visible Imaging Spectrometer at the. New Solar Telescope). The results show that the averaged over the flare region Fe XXI blueshift of the hot (10(7) K) evaporating plasma is delayed relative to the C II redshift of the relatively cold (10(4) K) chromospheric plasma by about one minute. The spatial distribution of the delays is not uniform across the region and can be as long as two minutes in several zones. Using vector magnetograms from HMI, we reconstruct the magnetic field topology and the quasi-separatrix layer, and find that the blueshift delay regions as well as the Ha flare ribbons are connected to the region of the. magnetic polarity inversion line (PIL) and an expanding flux rope via a system of low-lying loop arcades with a. height of less than or similar to 4.5 Mm. As a result, the chromospheric evaporation may be driven by the energy release in the vicinity of PIL, and has the observed properties due to a local magnetic field topology.
C1 [Sadykov, Viacheslav M.; Kosovichev, Alexander G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
[Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kosovichev, Alexander G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Sharykin, Ivan N.; Zimovets, Ivan V.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Vargas Dominguez, Santiago] Univ Nacl Colombia, Observ Astron, Sede Bogota, Carrera 45 26-85, Bogota, Colombia.
RP Sadykov, VM (reprint author), New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
RI Zimovets, Ivan/E-4431-2017
OI Zimovets, Ivan/0000-0001-6995-3684
FU NJIT; US NSF [AGS-1250818]; NASA [NNX13AG14G, NNX14AB68G, NNX14AB70G,
NNX11AO736]; Korea Astronomy and Space Science Institute; Seoul National
University; strategic priority research program of CAS [XDB09000000];
ESA; Norwegian Space Centre; NSF [AGS-1250818]; RFBR [15-32-21078,
16-32-00462]
FX The authors acknowledge the BBSO, IRIS, and SDO mission teams for their
contribution and support. The BBSO operation is supported by NJIT, US
NSF AGS-1250818, and NASA NNX13AG14G grants, and the NST operation is
partly supported by the Korea Astronomy and Space Science Institute and
Seoul National University and by the strategic priority research program
of CAS with grant No. XDB09000000. IRIS is a NASA small explorer mission
developed and operated by LMSAL with mission operations executed at the
NASA Ames Research Center and major contributions to downlink
communications funded by ESA and the Norwegian Space Centre. The authors
thank NASA's SDO HMI team for the availability of the high-quality
scientific data. The authors also thank the. anonymous referee for
valuable comments. The work was partially supported by NASA grants
NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant AGS-1250818; RFBR
grants 15-32-21078 and 16-32-00462; and an NJIT grant.
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JI Astrophys. J.
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PG 9
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900004
ER
PT J
AU Watson, DM
Calvet, NP
Fischer, WJ
Forrest, WJ
Manoj, P
Megeath, ST
Melnick, GJ
Najita, J
Neufeld, DA
Sheehan, PD
Stutz, AM
Tobin, JJ
AF Watson, Dan M.
Calvet, Nuria P.
Fischer, William J.
Forrest, W. J.
Manoj, P.
Megeath, S. Thomas
Melnick, Gary J.
Najita, Joan
Neufeld, David A.
Sheehan, Patrick D.
Stutz, Amelia M.
Tobin, John J.
TI EVOLUTION OF MASS OUTFLOW IN PROTOSTARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Herbig-Haro objects; ISM: jets and outflows; shock waves; stars: jets;
stars: pre-main sequence stars: protostars
ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS;
T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; PROTOSTELLAR ACCRETION
DISCS; FAST INTERSTELLAR SHOCKS; O I LINE; 63 MU-M; C-II
AB We have surveyed 84 Class 0, Class I, and flat-spectrum protostars in mid-infrared [Si II], [Fe II], and [S I] line emission, and 11 of these in far-infrared [O I] emission. We use the results to derive their mass. outflow rates, (M) over dot(w). Thereby we observe a strong correlation of (M) over dot(w) with bolometric luminosity, and with the inferred mass accretion rates of the central objects, (M) over dot(a), which continues through the Class 0 range the trend observed in Class II young stellar objects. Along this trend from large to small mass. flow rates, the different classes of young stellar objects lie in the sequence Class 0-Class I/flat-spectrum-Class II, indicating that the trend is an evolutionary sequence in which (M) over dot(a) and (M) over dot(w) decrease together with increasing age, while maintaining rough proportionality. The survey results include two that. are key tests of magnetocentrifugal outflow-acceleration mechanisms: the distribution of the outflow/accretion branching ratio b = (M) over dot(w)/(M) over dot(a), and limits on the distribution of outflow speeds. Neither rules out any of the three leading outflow-acceleration, angular-momentum-ejection mechanisms, but they provide some evidence that disk winds and accretion-powered stellar winds (APSWs) operate in many protostars. An upper edge observed in the branching-ratio distribution is consistent with the upper bound of b = 0.6 found in models of APSWs, and a large fraction (31%) of the sample have a. branching ratio sufficiently small that only disk winds, launched on scales as large as several au, have been demonstrated to account for them.
C1 [Watson, Dan M.; Forrest, W. J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Calvet, Nuria P.] Univ Michigan, Dept Astron, 825 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
[Fischer, William J.; Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA.
[Fischer, William J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Manoj, P.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Najita, Joan] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
[Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Sheehan, Patrick D.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Stutz, Amelia M.] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
[Tobin, John J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Watson, DM (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
EM dmw@pas.rochester.edu
FU NASA [NNX14AF79G]
FX We are grateful to Ingrid Koch for her help with the IRS data reduction.
This work was supported in part by NASA grant NNX14AF79G.
NR 77
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2016
VL 828
IS 1
AR 52
DI 10.3847/0004-637X/828/1/52
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900052
ER
PT J
AU Koster, RD
Brocca, L
Crow, WT
Burgin, MS
De Lannoy, GJM
AF Koster, Randal D.
Brocca, Luca
Crow, Wade T.
Burgin, Mariko S.
De Lannoy, Gabrielle J. M.
TI Precipitation estimation using L-band and C-band soil moisture
retrievals
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE precipitation; soil moisture; remote sensing
ID TIME SATELLITE PRECIPITATION; DATA SETS; RAINFALL
AB An established methodology for estimating precipitation amounts from satellite-based soil moisture retrievals is applied to L-band products from the Soil Moisture Active Passive (SMAP) and Soil Moisture and Ocean Salinity (SMOS) satellite missions and to a C-band product from the Advanced Scatterometer (ASCAT) mission. The precipitation estimates so obtained are evaluated against in situ (gauge-based) precipitation observations from across the globe. The precipitation estimation skill achieved using the L-band SMAP and SMOS data sets is higher than that obtained with the C-band product, as might be expected given that L-band is sensitive to a thicker layer of soil and thereby provides more information on the response of soil moisture to precipitation. The square of the correlation coefficient between the SMAP-based precipitation estimates and the observations (for aggregations to approximate to 100 km and 5 days) is on average about 0.6 in areas of high rain gauge density. Satellite missions specifically designed to monitor soil moisture thus do provide significant information on precipitation variability, information that could contribute to efforts in global precipitation estimation.
C1 [Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Brocca, Luca] CNR, Res Inst Geohydrol Protect, Perugia, Italy.
[Crow, Wade T.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Burgin, Mariko S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[De Lannoy, Gabrielle J. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Heverlee, Belgium.
RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM randal.d.koster@nasa.gov
RI Brocca, Luca/F-2854-2010; Koster, Randal/F-5881-2012
OI Brocca, Luca/0000-0002-9080-260X; Koster, Randal/0000-0001-6418-6383
FU NASA SMAP mission; SMAP Science Team; Italian Department of Civil
Protection
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). This work (mainly carried
out at the NASA Goddard Space Flight Center) was supported by the NASA
SMAP mission and the SMAP Science Team. Author Brocca appreciates
support from the Italian Department of Civil Protection. Qing Liu and
Clara Draper assisted with the processing of the data. SMAP data are
available from https://nsidc.org/data/smap, SMOS data from
https://smos-ds-02.eo.esa.int/oads/access/, and ASCAT data from
http://www.eumetsat.int/website/home/index.htm. Precipitation data are
available from
ftp://ftp.cpc.ncep.noaa.gov/precip/CPC_UNI_PRCP/GAUGE_GLB.
NR 28
TC 4
Z9 4
U1 8
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7213
EP 7225
DI 10.1002/2016WR019024
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900029
ER
PT J
AU Wiese, DN
Landerer, FW
Watkins, MM
AF Wiese, David N.
Landerer, Felix W.
Watkins, Michael M.
TI Quantifying and reducing leakage errors in the JPL RL05M GRACE mascon
solution
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE GRACE; postprocessing; mascon; leakage errors; gain factors
ID SEA-LEVEL; MASS; DECADE; OCEAN; SYSTEM
AB Recent advances in processing data from the Gravity Recovery and Climate Experiment (GRACE) have led to a new generation of gravity solutions constrained within a Bayesian framework to remove correlated errors rather than relying on empirical filters. The JPL RL05M mascon solution is one such solution, solving for mass variations using spherical cap mass concentration elements (mascons), while relying on external information provided by near-global geophysical models to constrain the solution. This new gravity solution is fundamentally different than the traditional spherical harmonic gravity solution, and as such, requires different care when postprocessing. Here we discuss two classes of postprocessing considerations for the JPL RL05M GRACE mascon solution: (1) reducing leakage errors across land/ocean boundaries, and (2) scaling the solutions to account for leakage errors introduced through parameterizing the gravity solution in terms of mascons. A Coastline Resolution Improvement (CRI) filter is developed to reduce leakage errors across coastlines. Synthetic simulations reveal a reduction in leakage errors of approximate to 50%, such that residual leakage errors are approximate to 1 cm equivalent water height (EWH) averaged globally. A set of gain factors is derived to reduce leakage errors for continental hydrology applications. The combined effect of the CRI filter coupled with application of the gain factors, is shown to reduce leakage errors when determining the mass balance of large (>160,000 km(2)) hydrological basins from 11% to 30% (0.6-1.5 mm EWH) averaged globally, with local improvements up to 38%-81% (9-19 mm EWH).
C1 [Wiese, David N.; Landerer, Felix W.; Watkins, Michael M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Wiese, DN (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.n.wiese@jpl.nasa.gov
NR 31
TC 2
Z9 2
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7490
EP 7502
DI 10.1002/2016WR019344
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900044
ER
PT J
AU Molotch, NP
Barnard, DM
Burns, SP
Painter, TH
AF Molotch, Noah P.
Barnard, David M.
Burns, Sean P.
Painter, Thomas H.
TI Measuring spatiotemporal variation in snow optical grain size under a
subalpine forest canopy using contact spectroscopy
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE snow; forests; snow grain size; spectroscopy; snow temperature;
snow-forest interactions
ID INFRARED REFLECTANCE; SURFACE-AREA; WATER EQUIVALENT; NUMERICAL-MODEL;
COVERED AREA; STRATIGRAPHY; ACCUMULATION; COVARIANCE; ABLATION; DENSITY
AB The distribution of forest cover exerts strong controls on the spatiotemporal distribution of snow accumulation and snowmelt. The physical processes that govern these controls are poorly understood given a lack of detailed measurements of snow states. In this study, we address one of many measurement gaps by using contact spectroscopy to measure snow optical grain size at high spatial resolution in trenches dug between tree boles in a subalpine forest. Trenches were collocated with continuous measurements of snow depth and vertical profiles of snow temperature and supplemented with manual measurements of snow temperature, geometric grain size, grain type, and density from trench walls. There was a distinct difference in snow optical grain size between winter and spring periods. In winter and early spring, when facetted snow crystal types were dominant, snow optical grain size was 6% larger in canopy gaps versus under canopy positions; a difference that was smaller than the measurement uncertainty. By midspring, the magnitude of snow optical grain size differences increased dramatically and patterns of snow optical grain size became highly directional with 34% larger snow grains in areas south versus north of trees. In winter, snow temperature gradients were up to 5-15 degrees C m(-1) greater under the canopy due to shallower snow accumulation. However, in canopy gaps, snow depths were greater in fall and early winter and therefore more significant kinetic growth metamorphism occurred relative to under canopy positions, resulting in larger snow grains in canopy gaps. Our findings illustrate the novelty of our method of measuring snow optical grain size, allowing for future studies to advance the understanding of how forest and meteorological conditions interact to impact snowpack evolution.
C1 [Molotch, Noah P.; Barnard, David M.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Molotch, Noah P.; Burns, Sean P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.; Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Burns, Sean P.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.; Molotch, NP (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA.; Molotch, NP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM noah.molotch@colorado.edu
RI Molotch, Noah/C-8576-2009; Painter, Thomas/B-7806-2016
FU U.S. National Aeronautics and Space Administration [NNXIIAK35A]; U.S.
National Science Foundation (NSF) [EAR 1141764]; U.S. Department of
Agriculture [2012-67003-19802]; NSF Niwot Ridge Long Term Ecological
Research program; Department of Energy Ameriflux program
FX This work was supported by the U.S. National Aeronautics and Space
Administration under grant NNXIIAK35A, by the U.S. National Science
Foundation (NSF) under grant EAR 1141764, and by the U.S. Department of
Agriculture under grant 2012-67003-19802. Additional support was
provided by the NSF Niwot Ridge Long Term Ecological Research program
and by the Department of Energy Ameriflux program. Part of this work was
conducted at the Jet Propulsion Laboratory, California Institute of
Technology under contract from NASA. Snow grain size data sets can be
downloaded from
ftp://snowserver.colorado.edu/pub/NWT_snow_grain_size_trenches2006/grain
-Size.zip. All meteorological data can be obtained from
http://fluxnet.ornl.gov/site/997.
NR 40
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7513
EP 7522
DI 10.1002/2016WR018954
PG 10
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900046
PM 27917006
ER
PT J
AU Jung-Kubiak, C
Reck, TJ
Siles, JV
Lin, R
Lee, C
Gill, J
Cooper, K
Mehdi, I
Chattopadhyay, G
AF Jung-Kubiak, Cecile
Reck, Theodore J.
Siles, Jose V.
Lin, Robert
Lee, Choonsup
Gill, John
Cooper, Ken
Mehdi, Imran
Chattopadhyay, Goutam
TI A Multistep DRIE Process for Complex Terahertz Waveguide Components
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Deep reactive-ion etching (DRIE); orthomode transducer (OMT); silicon
dioxide (SiO2); silicon micromachining; submillimeter waves; terahertz
(THz)
ID SATELLITE; GHZ
AB Asilicon deep reactive-ion etching (DRIE) process has been developed, using multiple SiO2 masks to enable multidepth waveguide features with +/- 2% tolerance. The unique capability of this process is demonstrated by designing, fabricating, and testing an orthomode transducer working in the 500-600 GHz frequency range. Straight waveguide measurements are also performed to characterize the losses associated with the multistep DRIE process, giving results slightly better than expected for metal-machined waveguides. This process enables the integration of multiple terahertz waveguide components such as mixers, multipliers, quadrature hybrids, and polarization twists onto a single silicon package.
C1 [Jung-Kubiak, Cecile; Reck, Theodore J.; Siles, Jose V.; Lin, Robert; Lee, Choonsup; Gill, John; Cooper, Ken; Mehdi, Imran; Chattopadhyay, Goutam] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jung-Kubiak, C (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov;
Jose.V.Siles@jpl.nasa.gov; Robert.H.Lin@jpl.nasa.gov;
Choonsup.Lee@jpl.nasa.gov; John.J.Gill@jpl.nasa.gov;
Ken.B.Cooper@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov;
goutam.chattopadhyay@jpl.nasa.gov
FU National Aeronautical and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology supported under a contract with the National
Aeronautical and Space Administration.
NR 19
TC 1
Z9 1
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2016
VL 6
IS 5
BP 690
EP 695
DI 10.1109/TTHZ.2016.2593793
PG 6
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DZ7QF
UT WOS:000386060200007
ER
PT J
AU Shah, U
Decrossas, E
Jung-Kubiak, C
Reck, T
Chattopadhyay, G
Mehdi, I
Oberhammer, J
AF Shah, Umer
Decrossas, Emmanuel
Jung-Kubiak, Cecile
Reck, Theodore
Chattopadhyay, Goutam
Mehdi, Imran
Oberhammer, Joachim
TI Submillimeter-Wave 3.3-bit RF MEMS Phase Shifter Integrated in
Micromachined Waveguide
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Micromachined waveguide; phase shifter; radio-frequency (RF)
microelectromechanical system (MEMS); rectangular waveguide;
submillimeter-wave; terahertz (THz)
ID E-PLANE; BAND; TECHNOLOGY; COMPONENTS; FILTERS
AB This paper presents a submillimeter-wave 500-550-GHz MEMS-reconfigurable phase shifter, which is based on loading a micromachined rectangular waveguide with 9 E-plane stubs. The phase shifter uses MEMS-reconfigurable surfaces to individually block/unblock the E-plane stubs from the micromachined waveguide. Each MEMS-reconfigurable surface is designed so that in the nonblocking state, it allows the electromagnetic wave to pass freely through it into the stub, while in the blocking state, it serves as the roof of the main waveguide and blocks the wave propagation into the stub. The phase-shifter design comprises three micromachined chips that are mounted in the H-plane cuts of the rectangular waveguide. Experimental results of the first device prototypes show that the microelectromechanical system (MEMS)- reconfigurable phase shifter has a linear phase shift of 20 degrees in ten discrete steps (3.3 bits). The measured insertion loss is better than 3 dB, of which only 0.5-1.5 dB is attributed to the MEMS surfaces and switched stubs, and the measured return loss is better than 15 dB in the design frequency band of 500-550 GHz. It is also shown that the major part of the insertion loss is attributed to misalignment and assembly uncertainties of the micromachined chips and the waveguide flanges, shown by simulations and reproducibility measurements. The MEMS-reconfigurable phase shifter is also operated in an analog tuning mode for high phase resolution. Furthermore, a detailed study has been carried out identifying the reason for the discrepancy between the simulated (90 degrees) and the measured (20 degrees) phase shift. Comb-drive actuators with spring constant variations between 2.13 and 8.71 N/m are used in the phase shifter design. An actuation voltage of 21.94 V with a reproducibility better than sigma = 0.0503 V is measured for the actuator design with a spring constant of 2.13 N/m. Reliability measurement on this actuator was performed in an uncontrolled laboratory environment and showed no deterioration in the functioning of the actuator observed over one hundred million cycles.
C1 [Shah, Umer; Oberhammer, Joachim] KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden.
[Decrossas, Emmanuel; Jung-Kubiak, Cecile; Reck, Theodore; Chattopadhyay, Goutam; Mehdi, Imran] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Shah, U (reprint author), KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden.
EM umers@kth.se; Emmanuel.Decrossas@jpl.nasa.gov;
Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov;
goutam.chattopadhyay@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov;
joachim.oberhammer@ee.kth.se
OI Oberhammer, Joachim/0000-0003-3339-9137
FU European Research Council Consolidator Grant [616846]; Swedish
Foundation for Strategic Research Synergy Grant Electronics [SE13-007];
Nils and Hans Backmark scholarship
FX The contribution by KTH to this work was supported under the European
Research Council Consolidator Grant 616846, under the Swedish Foundation
for Strategic Research Synergy Grant Electronics SE13-007, and under a
Nils and Hans Backmark scholarship.
NR 19
TC 0
Z9 0
U1 7
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2016
VL 6
IS 5
BP 706
EP 715
DI 10.1109/TTHZ.2016.2584924
PG 10
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DZ7QF
UT WOS:000386060200009
ER
PT J
AU Kempes, CP
Wang, L
Amend, JP
Doyle, J
Hoehler, T
AF Kempes, Christopher P.
Wang, Lawrence
Amend, Jan P.
Doyle, John
Hoehler, Tori
TI Evolutionary tradeoffs in cellular composition across diverse bacteria
SO ISME JOURNAL
LA English
DT Article
ID ESCHERICHIA-COLI; AEROBACTER-AEROGENES; UNIFYING THEORY; SIZE CONTROL;
GROWTH; PROTEIN; CELLS; RATES; RNA; EUKARYOTES
AB One of the most important classic and contemporary interests in biology is the connection between cellular composition and physiological function. Decades of research have allowed us to understand the detailed relationship between various cellular components and processes for individual species, and have uncovered common functionality across diverse species. However, there still remains the need for frameworks that can mechanistically predict the tradeoffs between cellular functions and elucidate and interpret average trends across species. Here we provide a comprehensive analysis of how cellular composition changes across the diversity of bacteria as connected with physiological function and metabolism, spanning five orders of magnitude in body size. We present an analysis of the trends with cell volume that covers shifts in genomic, protein, cellular envelope, RNA and ribosomal content. We show that trends in protein content are more complex than a simple proportionality with the overall genome size, and that the number of ribosomes is simply explained by cross-species shifts in biosynthesis requirements. Furthermore, we show that the largest and smallest bacteria are limited by physical space requirements. At the lower end of size, cell volume is dominated by DNA and protein content-the requirement for which predicts a lower limit on cell size that is in good agreement with the smallest observed bacteria. At the upper end of bacterial size, we have identified a point at which the number of ribosomes required for biosynthesis exceeds available cell volume. Between these limits we are able to discuss systematic and dramatic shifts in cellular composition. Much of our analysis is connected with the basic energetics of cells where we show that the scaling of metabolic rate is surprisingly superlinear with all cellular components.
C1 [Kempes, Christopher P.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Kempes, Christopher P.; Wang, Lawrence; Doyle, John] CALTECH, Control & Dynam Syst, Pasadena, CA 91125 USA.
[Kempes, Christopher P.; Hoehler, Tori] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Amend, Jan P.] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA.
[Amend, Jan P.] Univ Southern Calif, Dept Biol Sci, Los Angeles, CA USA.
RP Kempes, CP (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
EM ckempes@gmail.com
FU 'Life Underground' NASA Astrobiology Institute [NNA13AA92A]; Gordon and
Betty Moore Foundation
FX CPK acknowledges the support of the 'Life Underground' NASA Astrobiology
Institute (NNA13AA92A) and the Gordon and Betty Moore Foundation.
NR 41
TC 4
Z9 4
U1 13
U2 13
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 SEP
PY 2016
VL 10
IS 9
BP 2145
EP 2157
DI 10.1038/ismej.2016.21
PG 13
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA EA5MK
UT WOS:000386664600007
PM 27046336
ER
PT J
AU Saghaian, SM
Karaca, HE
Tobe, H
Pons, J
Santamarta, R
Chumlyakov, YI
Noebe, RD
AF Saghaian, S. M.
Karaca, H. E.
Tobe, H.
Pons, J.
Santamarta, R.
Chumlyakov, Y. I.
Noebe, R. D.
TI Effects of Ni content on the shape memory properties and microstructure
of Ni-rich NiTi-20Hf alloys
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE Ni-rich NiTiHf; high temperature shape memory alloys; martensite
morphology; high strength
ID NITIHFPD SINGLE-CRYSTALS; MARTENSITIC-TRANSFORMATION; COMPRESSIVE
RESPONSE; BEHAVIOR; PHASE; TEMPERATURES; STRENGTH
AB Shape memory properties and microstructure of four Ni-rich NiTiHf alloys (Ni50.3Ti29.7Hf20, Ni50.7Ti29.3Hf20, Ni51.2Ti28.8Hf20, and Ni52Ti28Hf20 (at.%)) were systematically characterized in the furnace cooled condition. H-phase precipitates were formed during furnace cooling in compositions with greater than 50.3Ni and the driving force for nucleation increased with Ni content. Alloy strength increased while recoverable strain decreased with increasing Ni content due to changes in precipitate characteristics. When the precipitates were small (similar to 5-15 nm), they were readily absorbed by martensite plates, which resulted in maximum recoverable strain of 2% in Ni50.7Ti29.3Hf20. With increasing Ni content, the size (>100 nm) and volume fraction of precipitates increased and the growth of martensite plates was constrained between the precipitates when the Ni concentration was greater than 50.7 at.%. Near perfect dimensional stability with negligible irrecoverable strain was observed at stress levels as high as 2 GPa in the Ni52Ti28Hf20 alloy, though the recoverable strain was rather small. In general, strong local stress fields were created at precipitate/matrix interphases, which lead to high stored elastic energy during the martensitic transformation.
C1 [Saghaian, S. M.; Karaca, H. E.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Pons, J.; Santamarta, R.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
[Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
[Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH USA.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karacahaluk@uky.edu
RI Chumlyakov, Yuriy/R-6496-2016
FU NASA Transformative Aeronautics Concepts Program (TACP),
Transformational Tools and Technologies Project; NASA EPSCOR program
[NNX11AQ31A]; RFBR [10-03-0154-a]; RSF program [14-29-00012]; Spanish
MINECO [MAT2011-28217-C02-01]; MECOMP-DGICT [MAT2014-56116-C4-1-R];
FEDER
FX This work was supported in part by the NASA Transformative Aeronautics
Concepts Program (TACP), Transformational Tools and Technologies Project
and the NASA EPSCOR program under grant No: NNX11AQ31A and RFBR project
with grant No: 10-03-0154-a and RSF program under grant No: 14-29-00012.
J Pons and R Santamarta also acknowledge the financial support from the
Spanish MINECO (ref. MAT2011-28217-C02-01), MECOMP-DGICT (ref.
MAT2014-56116-C4-1-R) and FEDER.
NR 42
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Z9 0
U1 12
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2016
VL 25
IS 9
AR 095029
DI 10.1088/0964-1726/25/9/095029
PG 11
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA DZ6UJ
UT WOS:000385997500029
ER
PT J
AU Meskhidze, N
Johnson, MS
Hurley, D
Dawson, K
AF Meskhidze, Nicholas
Johnson, Matthew S.
Hurley, David
Dawson, Kyle
TI Influence of measurement uncertainties on fractional solubility of iron
in mineral aerosols over the oceans
SO AEOLIAN RESEARCH
LA English
DT Article
DE Soluble iron; Mineral dust; Measurement techniques; 3-D chemical
transport model
ID DRY DEPOSITION; SIZE DISTRIBUTION; SAHARAN DUST; DISSOLUTION; MODEL;
DISTRIBUTIONS; TRANSPORT; PACIFIC; CYCLE; FE
AB The atmospheric supply of mineral dust iron (Fe) plays a crucial role in the Earth's biogeochemical cycle and is of specific importance as a micronutrient in the marine environment. Observations show several orders of magnitude variability in the fractional solubility of Fe in mineral dust aerosols, making it hard to assess the role of mineral dust in the global ocean biogeochemical Fe cycle. In this study we compare the operational solubility of mineral dust aerosol Fe associated with the flow-through leaching protocol to the results of the global 3-D chemical transport model GEOS-Chem. According to the protocol, aerosol Fe is defined as soluble by first deionized water leaching of mineral dust through a 0.45 mu m pore size membrane followed by acidification and storage of the leachate over a long period of time prior to analysis. To estimate the uncertainty in soluble Fe results introduced by the flow-through leaching protocol, we prescribe an average 50% (range of 30-70%) fractional solubility to sub-0.45 mu m sized mineral dust particles that may inadvertently pass the filter and end up in the acidified (at pH similar to 1.7) leachate for a couple of month period. In the model, the fractional solubility of Fe is either explicitly calculated using a complex mineral aerosol Fe dissolution equations; or prescribed to be 1% and 4% often used by global ocean biogeochemical Fe cycle models to reproduce the broad characteristics of the presently observed ocean dissolved iron distribution. Calculations show that the fractional solubility of Fe derived through the flow-through leaching is higher compared to the model results. The largest differences (similar to 40%) are predicted to occur farther away from the dust source regions, over the areas where sub-0.45 mu m sized mineral dust particles contribute a larger fraction of the total mineral dust mass. This study suggests that different methods used in soluble Fe measurements and inconsistences in the operational definition of filterable Fe in marine environment and soluble Fe in atmospheric aerosols are likely to contribute to the wide range of fractional solubility of aerosol Fe reported in the literature. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Meskhidze, Nicholas; Hurley, David; Dawson, Kyle] North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
[Johnson, Matthew S.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Meskhidze, N (reprint author), North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
EM nmeskhidze@ncsu.edu
RI Chem, GEOS/C-5595-2014;
OI Dawson, Kyle/0000-0003-3175-0456
FU NCSU Faculty Research & Professional Development Fund; Office of
Undergraduate Research at North Carolina State University; NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at NASA Ames Research Center
FX This research was supported by NCSU Faculty Research & Professional
Development Fund and the grant from the Office of Undergraduate Research
at North Carolina State University. The authors would like to thank
Daniel Jacob and the Harvard University Atmospheric Chemistry Modeling
Group for providing the base GEOS-Chem model used during our research.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at NASA Ames Research Center. We also thank Dr. Akinori Ito
from the Japan Agency for Marine-Earth Science and Technology (JAMSTEC)
for providing the dust-Fe dissolution code used in Ito and Xu (2014).
NR 79
TC 1
Z9 1
U1 6
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1875-9637
EI 2212-1684
J9 AEOLIAN RES
JI Aeolian Res.
PD SEP
PY 2016
VL 22
BP 85
EP 92
DI 10.1016/j.aeolia.2016.07.002
PG 8
WC Geography, Physical
SC Physical Geography
GA DZ1NP
UT WOS:000385605400008
ER
PT J
AU Nicolas, MJ
Sullivan, RW
Richards, WL
AF Nicolas, Matthew J.
Sullivan, Rani W.
Richards, W. Lance
TI Large Scale Applications Using FBG Sensors: Determination of In-Flight
Loads and Shape of a Composite Aircraft Wing
SO AEROSPACE
LA English
DT Article
DE fiber Bragg grating; FBG; carbon composite wing; optical fiber strain
measurement; flight loads; wing deflection; wing shape; structural
health monitoring
ID FIBER-OPTIC SENSORS; BRAGG GRATING SENSORS; STRAIN
AB Technological advances have enabled the development of a number of optical fiber sensing methods over the last few years. The most prevalent optical technique involves the use of fiber Bragg grating (FBG) sensors. These small, lightweight sensors have many attributes that enable their use for a number of measurement applications. Although much literature is available regarding the use of FBGs for laboratory level testing, few publications in the public domain exist of their use at the operational level. Therefore, this paper gives an overview of the implementation of FBG sensors for large scale structures and applications. For demonstration, a case study is presented in which FBGs were used to determine the deflected wing shape and the out-of-plane loads of a 5.5-m carbon-composite wing of an ultralight aerial vehicle. The in-plane strains from the 780 FBG sensors were used to obtain the out-of-plane loads as well as the wing shape at various load levels. The calculated out-of-plane displacements and loads were within 4.2% of the measured data. This study demonstrates a practical method in which direct measurements are used to obtain critical parameters from the high distribution of FBG sensors. This procedure can be used to obtain information for structural health monitoring applications to quantify healthy vs. unhealthy structures.
C1 [Nicolas, Matthew J.] PACCAR Engine Co, Dept Mfg Engn, Columbus, MS 39701 USA.
[Sullivan, Rani W.] Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
[Richards, W. Lance] NASA Langley Res Ctr, NASA Engn & Safety Ctr, Hampton, VA 23681 USA.
RP Sullivan, RW (reprint author), Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
EM matthewnicolas52@gmail.com; sullivan@ae.msstate.edu;
lance.richards-1@nasa.gov
OI Nicolas, Matthew/0000-0001-9807-5817
FU NASA Armstrong Flight Research Center [AERO532 11020161]; Raspet Flight
Research Laboratory; NASA/Mississippi Space Grant Consortium [12040456
12070825]
FX The support provided for this study by the NASA Armstrong Flight
Research Center (Award No. AERO532 11020161), Raspet Flight Research
Laboratory, and the NASA/Mississippi Space Grant Consortium (Award No.
12040456 12070825) is gratefully acknowledged.
NR 38
TC 0
Z9 0
U1 5
U2 5
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2226-4310
J9 AEROSPACE
JI Aerospace
PD SEP
PY 2016
VL 3
IS 3
AR 18
DI 10.3390/aerospace3030018
PG 15
WC Engineering, Aerospace
SC Engineering
GA DZ0LQ
UT WOS:000385531300001
ER
PT J
AU Sree, D
Stephens, DB
AF Sree, Dave
Stephens, David B.
TI Improved Separation of Tone and Broadband Noise Components from Open
Rotor Acoustic Data
SO AEROSPACE
LA English
DT Article
DE acoustic; broadband; open rotor; phase-shift; segment-pair; separation;
spectrum; spike; tone
AB The term open rotor refers to unducted counter-rotating dual rotors or propellers used for propulsion. The noise generated by an open rotor is very complicated and requires special techniques for its analysis. The determination of its tone and broadband components is vital for properly assessing the noise control parameters and also for validating open rotor noise prediction codes. The data analysis technique developed by Sree for processing raw acoustic data of open rotors has been modified to yield much better results of tone and broadband separation particularly for the case when the two rotor speeds are approximately the same. The modified algorithm is found to eliminate most or all of the spikes previously observed in the broadband spectra computed from the original algorithm. A full description of the modified algorithm and examples of improved results from its application are presented in this paper.
C1 [Sree, Dave] Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA.
[Stephens, David B.] NASA, Acoust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sree, D (reprint author), Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA.
EM dave.sree@gmail.com; david.stephens@nasa.gov
FU NASA Environmentally Responsible Aviation project; GE Aviation,
Evendale, OH, USA; NASA Advanced Air Transportation Technology project
FX Sincere thanks and appreciation are expressed to Acoustics Branch at
NASA GRC for providing the non-proprietary open rotor acoustic data used
in this work, in particular to Daniel L. Sutliff regarding the mini-open
rotor data. The open rotor wind tunnel test campaign was funded by the
NASA Environmentally Responsible Aviation project, in collaboration with
GE Aviation, Evendale, OH, USA. The NASA Advanced Air Transportation
Technology project funded David B. Stephens during the preparation of
this report.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2226-4310
J9 AEROSPACE
JI Aerospace
PD SEP
PY 2016
VL 3
IS 3
AR 29
DI 10.3390/aerospace3030029
PG 15
WC Engineering, Aerospace
SC Engineering
GA DZ0LQ
UT WOS:000385531300012
ER
PT J
AU Righter, K
Sutton, SR
Danielson, L
Pando, K
Newville, M
AF Righter, Kevin
Sutton, Steve R.
Danielson, Lisa
Pando, Kellye
Newville, Matt
TI Redox variations in the inner solar system with new constraints from
vanadium XANES in spinels
SO AMERICAN MINERALOGIST
LA English
DT Review
DE Oxygen fugacity; meteorites; solar nebula; spinel; chromite; vanadium;
Invited Centennial article
ID INTERPLANETARY DUST PARTICLES; COMET 81P/WILD 2; OXYGEN FUGACITY;
OXIDATION-STATE; CARBONACEOUS CHONDRITES; ENSTATITE CHONDRITES; MARTIAN
BASALTS; ELECTROCHEMICAL MEASUREMENTS; THERMODYNAMIC CONSTRAINTS;
LAYERED INTRUSION
AB Many igneous rocks contain mineral assemblages that are not appropriate for application of common mineral equilibria or oxybarometers to estimate oxygen fugacity. Spinel-structured oxides, common minerals in 1916 z A 2016 many igneous rocks, typically contain sufficient V for XANES measurements, allowing use of the correlation between oxygen fugacity and V K pre-edge peak intensity. Here we report V pre-edge peak intensities for a wide range of spinels from source rocks ranging from terrestrial basalt to achondrites to oxidized chondrites. The XANES measurements are used to calculate oxygen fugacity from experimentally produced spinels of known f(o2). We obtain values, in order of increasing f(o2), from IW-3 for lodranites and acapulcoites, to diogenites, brachinites (near IW), ALH 84001, terrestrial basalt, hornblende-bearing R chondrite LAP 04840 (IW+1.6), and finally ranging up to IW+3.1 for CK chondrites (where the Delta IW notation = logf(o2), of a sample relative to the logf(o2), of the IW buffer at specific 7). To place the significance of these new measurements into context we then review the range of oxygen fugacities recorded in major achondrite groups, chondritic and primitive materials, and planetary materials. This range extends from IW-8 to IW+2. Several chondrite groups associated with aqueous alteration exhibit values that are slightly higher than this range, suggesting that water and oxidation may be linked. The range in planetary materials is even wider than that defined by meteorite groups. Earth and Mars exhibit values higher than IW+2, due to a critical role played by pressure. Pressure allows dissolution of volatiles into magmas, which can later cause oxidation or reduction during fractionation, cooling, and degassing. Fluid mobility, either in the sub-arc mantle and crust, or in regions of metasomatism, can generate values >IW+2, again suggesting an important link between water and oxidation. At the very least, Earth exhibits a higher range of oxidation than other planets and astromaterials due to the presence of an O-rich atmosphere, liquid water, and hydrated interior. New analytical techniques and sample suites will revolutionize our understanding of oxygen fugacity variation in the inner solar system, and the origin of our solar system in general.
C1 [Righter, Kevin] NASA, JSC, NASA Pkwy, Houston, TX 77058 USA.
[Sutton, Steve R.; Newville, Matt] Univ Chicago, GSECARS, 9700 South Cass Ave,Bldg 434A, Argonne, IL 60439 USA.
[Danielson, Lisa; Pando, Kellye] Jacobs Engn, ESCG, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA, JSC, NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP from the NASA Cosmochemistry/Emerging Worlds programs; National
Science Foundation, Earth Sciences [EAR-1128799]; Department of
Energy-GeoSciences [DE-FG02-94ER14466]; DOE Office of Science
[DE-AC02-06CH11357]
FX This work was supported by an RTOP from the NASA Cosmochemistry/Emerging
Worlds programs. Portions of this work were performed at
GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne
National Laboratory. GeoSoilEnviroCARS is supported by the National
Science Foundation, Earth Sciences (EAR-1128799) and Department of
Energy-GeoSciences (DE-FG02-94ER14466). 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 No. DE-AC02-06CH11357. All meteorite
samples were provided by the Meteorite Working Group except for the
acapulcoites/lodranites (J. Herrin), GRA 06128 (A. Treiman), and ALH
84001 (M. Righter). The manuscript benefitted from the careful reviews
and constructive comments of P. Burger, S. Paque, and AE S. Simon. We
thank K. Putirka for the invitation to contribute a paper in celebration
of the American Mineralogist centennial, and K.R. acknowledges the
enormous and continuing influence the Mineralogical Society of America
has had on his science and understanding of the natural world.
NR 140
TC 1
Z9 1
U1 8
U2 8
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 1928
EP 1942
DI 10.2138/am-2016-5638
PG 15
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100003
ER
PT J
AU Lee, S
Shen, ZZ
Xu, HF
AF Lee, Seungyeol
Shen, Zhizhang
Xu, Huifang
TI Study on nanophase iron oxyhydroxides in freshwater ferromanganese
nodules from Green Bay, Lake Michigan, with implications for the
adsorption of As and heavy metals
SO AMERICAN MINERALOGIST
LA English
DT Article
DE XRD; HRTEM; Z-contrast imaging; ab initio; two-line ferrihydrite;
proto-goethite; nanophase goethite; feroxyhyte; ferromanganese nodule;
arsenic
ID AB-INITIO; POWDER DIFFRACTION; STRUCTURAL MODEL; AKDALAITE MODEL;
FERRIHYDRITE; SPECIATION; SEDIMENTS; MANGANESE; FEOOH; MN
AB Nanophase Fe-oxyhydroxides in freshwater ferromanganese nodules (FFN) from Green Bay, Lake Michigan, and adsorbed arsenate have been investigated by X-ray powder diffraction (XRD), high-resolution transmission electron microscopy (HRTEM), Z-contrast imaging, and ab initio calculations using the density functional theory (DFT). The samples from northern Green Bay can be divided into two types: Fe-Mn nodules and Fe-rich nodules. The manganese-bearing phases are todorokite, birnessite, and buserite. The iron-bearing phases are feroxyhyte, nanophase goethite, two-line ferrihydrite, and nanophase FeOOH with guyanaite structure. Z-contrast images of the Fe-oxyhydroxides show ordered FeOOH nano-domains with guyanaite structure intergrown with nanophase goethite. The FeOOH nanophase is a precursor to the goethite. Henceforth, we will refer to it as "proto-goethite." DFT calculations indicate that goethite is more stable than proto-goethite. Our results suggest that ordering between Fe and vacancies in octahedral sites result in the transformation from feroxyhyte to goethite through a proto-goethite intermediate phase. Combining Z-contrast images and TEM-EDS reveals that arsenate (AsO43-) tetrahedra are preferentially adsorbed on the proto-goethite (001) surface via tridentate adsorption. Our study directly shows the atomic positions of Fe-oxyhydroxides with associated trace elements. The methods can be applied for identifying structures of nano-phases and adsorbed trace elements and heavy metals.
C1 [Lee, Seungyeol; Shen, Zhizhang; Xu, Huifang] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
RP Xu, HF (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NASA Astrobiology Institute [N07-5489]
FX The authors acknowledge the financial support from NASA Astrobiology
Institute (N07-5489). The authors thank Carl Bowser for providing the
samples and their locations, Hiromi Konishi for assistance in acquiring
Z-contrast images, Izabela Szlufarska for allowing us to access
computing facility, Gabor J. Kemeny of Middleton Spectral Vision and
Michael Beauchaine of Bruker AXS for XRF mapping. The authors also thank
Philip E. Brown, John W. Valley, Clark M. Johnson, Eric E. Roden, and
Franklin Hobbs for their helpful suggestions.
NR 53
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U1 8
U2 8
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 1986
EP 1995
DI 10.2138/am-2016-5729
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100007
ER
PT J
AU Chan, QHS
Zolensky, ME
Martinez, JE
Tsuchiyama, A
Miyake, A
AF Chan, Queenie H. S.
Zolensky, Michael E.
Martinez, James E.
Tsuchiyama, Akira
Miyake, Akira
TI Magnetite plaquettes are naturally asymmetric materials in meteorites
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Magnetite; plaquettes; carbonaceous chondrites; symmetry-breaking;
scanning electron microscopy; SEM; electron backscatter diffraction;
EBSD; synchrotron X-ray computed microtomography; SXRCT; aqueous
alteration; crystal structure
ID EXTRATERRESTRIAL AMINO-ACIDS; CARBONACEOUS CHONDRITE; TAGISH LAKE;
ADSORPTION; HOMOCHIRALITY; MINERALOGY; EVOLUTION; CRYSTALS; PARTICLES;
CHEMISTRY
AB Life on Earth shows preference toward the set of organics with particular spatial configurations. Enantiomeric excesses have been observed for a-methyl amino acids in meteorites, which suggests that chiral asymmetry might have an abiotic origin. A possible abiotic mechanism that could produce chiral asymmetry in meteoritic amino acids is their formation under the influence of asymmetric catalysts, as mineral crystallization can produce spatially asymmetric structures. Although magnetite plaquettes have been proposed to be a possible candidate for an asymmetric catalyst, based on the suggestion that they have a spiral structure, a comprehensive description of their morphology and interpretation of the mechanism associated with symmetry-breaking in biomolecules remain elusive. Here we report observations of magnetite plaquettes in carbonaceous chondrites (CC) that were made with scanning electron microscopy and synchrotron X-ray computed microtomography (SXRCT). We obtained the crystal orientation of the plaquettes using electron backscatter diffraction (EBSD) analysis. SXRCT permits visualization of the internal features of the plaquettes. It provides an unambiguous conclusion that the plaquettes are devoid of a spiral feature and, rather that they are stacks of individual magnetite disks that do not join to form a continuous spiral. Despite the lack of spiral features, our EBSD data show significant changes in crystal orientation between adjacent magnetite disks. The magnetite disks are displaced in a consistent relative direction that lead to an overall crystallographic rotational mechanism. This work offers an explicit understanding of the structures of magnetite plaquettes in CC, which provides a fundamental basis for future interpretation of the proposed symmetry-breaking mechanism.
C1 [Chan, Queenie H. S.; Zolensky, Michael E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
[Martinez, James E.] Jacobs Engn, Houston, TX 77058 USA.
[Tsuchiyama, Akira; Miyake, Akira] Kyoto Univ, Grad Sch Sci, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
RP Chan, QHS (reprint author), NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
EM hschan@nasa.gov
FU NASA Cosmochemistry Program; NASA Postdoctoral Program at the Johnson
Space Center; Japan Ministry of Education, Culture, Sports, Science and
Technology [15H05695]
FX We acknowledge CAPTEM for loan of the Bench Crater sample, which is an
Apollo lunar sample. We thank Field Museum for Orgueil, Murchison,
Mighei, Renazzo, National Museum of Natural History for the Alais
meteorite sample, and American Museum of Natural History for the Ivuna
sample. This study was supported by the NASA Cosmochemistry Program
(M.E.Z. is the PI). Q.H.S.C. acknowledges support from the NASA
Postdoctoral Program at the Johnson Space Center, administered by the
Universities Space Research Association. A.T. was supported by a
Grant-in-aid of the Japan Ministry of Education, Culture, Sports,
Science and Technology (15H05695). We thank Tomoki Nakamura, John
Bradley, and Rhian Jones for careful reviews of the manuscript, and
Sandra Pizzarello, Jose Aponte, and Aaron Burton for the helpful
comments and insightful discussions. The microtomography experiment was
made by the project at SPring-8 (proposal no. 2015A1413) with help of
Kentaro Uesugi and Tsukasa Nakano.
NR 58
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U1 4
U2 4
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 2041
EP 2050
DI 10.2138/am-2016-5604
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100012
ER
PT J
AU Gullikson, AL
Hagerty, JJ
Reid, MR
Rapp, JF
Draper, DS
AF Gullikson, Amber L.
Hagerty, Justin J.
Reid, Mary R.
Rapp, Jennifer F.
Draper, David S.
TI Silicic lunar volcanism: Testing the crustal melting model
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Moon; silicic volcanism; crustal melting; partial melting experiments;
silicate liquid immiscibility
ID LIQUID IMMISCIBILITY; QUARTZ MONZODIORITE; MAIRAN DOMES; MOON; GRANITE;
PETROLOGY; GEOCHEMISTRY; GRUITHUISEN; CHEMISTRY; ROCKS
AB Lunar silicic rocks were first identified by granitic fragments found in samples brought to Earth by the Apollo missions, followed by the discovery of silicic domes on the lunar surface through remote sensing. Although these silicic lithologies are thought to make up a small portion of the lunar crust, their presence indicates that lunar crustal evolution is more complex than originally thought. Models currently used to describe the formation of silicic lithologies on the Moon include in situ differentiation of a magma, magma differentiation with silicate liquid immiscibility, and partial melting of the crust. This study focuses on testing a crustal melting model through partial melting experiments on compositions representing lithologies spatially associated with the silicic domes. The experiments were guided by the results of modeling melting temperatures and residual melt compositions of possible protoliths for lunar silicic rocks using the thermodynamic modeling software, rhyolite-MELTS.
Rhyolite-MELTS simulations predict liquidus temperatures of 950-1040 degrees C for lunar granites under anhydrous conditions, which guided the temperature range for the experiments. Monzogabbro, alkali gabbronorite, and KREEP basalt were identified as potential protoliths due to their ages, locations on the Moon (i.e., located near observed silicic domes), chemically evolved compositions, and the results from rhyolite-MELTS modeling. Partial melting experiments, using mixtures of reagent grade oxide powders representing bulk rock compositions of these rock types, were carried out at atmospheric pressure over the temperature range of 900-1100 degrees C. Because all lunar granite samples and remotely sensed domes have an elevated abundance of Th, some of the mixtures were doped with Th to observe its partitioning behavior.
Run products show that at temperatures of 1050 and 1100 degrees C, melts of the three protoliths are not silicic in nature (i.e., they have <63 wt% SiO2). By 1000 degrees C, melts of both monzogabbro and alkali gabbronorite approach the composition of granite, but are also characterized by immiscible Si-rich and Fe-rich liquids. Furthermore, Th strongly partitions into the Fe-rich, and not the Si-rich glass in all experimental runs.
Our work provides important constraints on the mechanism of silicic melt formation on the Moon. The observed high-Th content of lunar granite is difficult to explain by silicate liquid immiscibility, because through this process, Th is not fractionated into the Si-rich phase. Results of our experiments and modeling suggests that silicic lunar rocks could be produced from monzogabbro and alkali gabbronorite protoliths by partial melting at T < 1000 degrees C. Additionally, we speculate that at higher pressures (P >= 0.005 GPa), the observed immiscibility in the partial melting experiments would be suppressed.
C1 [Gullikson, Amber L.; Reid, Mary R.] Northern Univ Arizona, Flagstaff, AZ 86011 USA.
[Hagerty, Justin J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Rapp, Jennifer F.] NASA, Johnson Space Ctr, Jacobs, Mail Code JE20, Houston, TX 77058 USA.
[Draper, David S.] NASA, Astromat Res Off, ARES Directorate, Johnson Space Ctr, Houston, TX USA.
RP Gullikson, AL (reprint author), Northern Univ Arizona, Flagstaff, AZ 86011 USA.
EM agullikson@usgs.gov
FU Geological Society of America; Sigma Xi; NAU Support for Graduate
Students program; Tom and Rose Bedwell Earth Physics Scholarship
FX We thank Brad Jolliff and Malcolm Rutherford for their insightful
comments, which greatly improved this paper. Funding for this work was
provided by the Geological Society of America research grant, Sigma Xi
Grants-in-Aid Research, the NAU Support for Graduate Students program,
and the Tom and Rose Bedwell Earth Physics Scholarship.
NR 68
TC 0
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U1 6
U2 6
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD SEP-OCT
PY 2016
VL 101
IS 9-10
BP 2312
EP 2321
DI 10.2138/am-2016-5619
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100034
ER
PT J
AU Singer, LP
Chen, HY
Holz, DE
Farr, WM
Price, LR
Raymond, V
Cenko, SB
Gehrels, N
Cannizzo, J
Kasliwal, MM
Nissanke, S
Coughlin, M
Farr, B
Urban, AL
Vitale, S
Veitch, J
Graff, P
Berry, CPL
Mohapatra, S
Mandel, I
AF Singer, Leo P.
Chen, Hsin-Yu
Holz, Daniel E.
Farr, Will M.
Price, Larry R.
Raymond, Vivien
Cenko, S. Bradley
Gehrels, Neil
Cannizzo, John
Kasliwal, Mansi M.
Nissanke, Samaya
Coughlin, Michael
Farr, Ben
Urban, Alex L.
Vitale, Salvatore
Veitch, John
Graff, Philip
Berry, Christopher P. L.
Mohapatra, Satya
Mandel, Ilya
TI SUPPLEMENT: "GOING THE DISTANCE: MAPPING HOST GALAXIES OF LIGO AND VIRGO
SOURCES IN THREE DIMENSIONS USING LOCAL COSMOGRAPHY AND TARGETED
FOLLOW-UP" (2016, ApJL, 829, L15)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: distances and redshifts; gravitational waves;
surveys
AB This is a supplement to the Letter of Singer et al., in which we demonstrated a rapid algorithm for obtaining joint 3D estimates of sky location and luminosity distance from observations of binary neutron star mergers with Advanced LIGO and Virgo. We argued that combining the reconstructed volumes with positions and redshifts of possible host galaxies can provide large-aperture but small field of view instruments with a manageable list of targets to search for optical or infrared emission. In this Supplement, we document the new HEALPix-based file format for 3D localizations of gravitational-wave transients. We include Python sample code to show the reader how to perform simple manipulations of the 3D sky maps and extract ranked lists of likely host galaxies. Finally, we include mathematical details of the rapid volume reconstruction algorithm.
C1 [Singer, Leo P.; Cenko, S. Bradley; Gehrels, Neil; Cannizzo, John] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
[Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Farr, Will M.; Veitch, John; Berry, Christopher P. L.; Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Price, Larry R.; Raymond, Vivien] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Raymond, Vivien] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Kasliwal, Mansi M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Nissanke, Samaya] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
[Coughlin, Michael] Harvard Univ, Dept Phys & Astron, Cambridge, MA 02138 USA.
[Urban, Alex L.] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Vitale, Salvatore; Mohapatra, Satya] MIT, LIGO Lab, 185 Albany St, Cambridge, MA 02139 USA.
[Graff, Philip] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Singer, LP (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
OI Singer, Leo/0000-0001-9898-5597; Chen, Hsin-Yu/0000-0001-5403-3762
FU NSF [1066293]
FX We thank the Aspen Center for Physics and NSF grant #1066293 for
hospitality during the conception, writing, and editing of this paper.
We thank P. Shawhan and F. Tombesi for detailed feedback on the
manuscript. The online data release is available at
https://dcc.ligo.org/P1500071/public/html. This is LIGO document
P1500071-v7.
NR 16
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2016
VL 226
IS 1
AR 10
DI 10.3847/0067-0049/226/1/10
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY8SH
UT WOS:000385400500001
ER
PT J
AU Jensen, MP
Petersen, WA
Bansemer, A
Bharadwaj, N
Carey, LD
Cecil, DJ
Collis, SM
Del Genio, AD
Dolan, B
Gerlach, J
Giangrande, SE
Heymsfield, A
Heymsfield, G
Kollias, P
Lang, TJ
Nesbitt, SW
Neumann, A
Poellot, M
Rutledge, SA
Schwaller, M
Tokay, A
Williams, CR
Wolff, DB
Xie, S
Zipser, EJ
AF Jensen, M. P.
Petersen, W. A.
Bansemer, A.
Bharadwaj, N.
Carey, L. D.
Cecil, D. J.
Collis, S. M.
Del Genio, A. D.
Dolan, B.
Gerlach, J.
Giangrande, S. E.
Heymsfield, A.
Heymsfield, G.
Kollias, P.
Lang, T. J.
Nesbitt, S. W.
Neumann, A.
Poellot, M.
Rutledge, S. A.
Schwaller, M.
Tokay, A.
Williams, C. R.
Wolff, D. B.
Xie, S.
Zipser, E. J.
TI THE MIDLATITUDE CONTINENTAL CONVECTIVE CLOUDS EXPERIMENT (MC3E)
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID RADIATION MEASUREMENT PROGRAM; ATMOSPHERIC RADIATION; POLARIMETRIC
RADAR; WIND PROFILERS; PRECIPITATION; RADIOMETER; RESOLUTION; MESOSCALE;
SYSTEMS; GHZ
AB The Midlatitude Continental Convective Clouds Experiment (MC3E), a field program jointly led by the U.S. Department of Energy's Atmospheric Radiation Measurement (ARM) Program and the National Aeronautics and Space Administration's (NASA) Global Precipitation Measurement (GPM) mission, was conducted in south-central Oklahoma during April-May 2011. MC3E science objectives were motivated by the need to improve our understanding of midlatitude continental convective cloud system life cycles, microphysics, and GPM precipitation retrieval algorithms. To achieve these objectives, a multi scale surface- and aircraft-based in situ and remote sensing observing strategy was employed. A variety of cloud and precipitation events were sampled during MC3E, of which results from three deep convective events are highlighted. Vertical structure, air motions, precipitation drop size distributions, and ice properties were retrieved from multiwavelength radar, profiler, and aircraft observations for a mesoscale convective system (MCS) on 11 May. Aircraft observations for another MCS observed on 20 May were used to test agreement between observed radar reflectivities and those calculated with forward-modeled reflectivity and microwave brightness temperatures using in situ particle size distributions and ice water content. Multiplatform observations of a supercell that occurred on 23 May allowed for an integrated analysis of kinematic and microphysical interactions. A core updraft of 25 m supported growth of hail and large raindrops. Data collected during the MC3E campaign are being used in a number of current and ongoing research projects and are available through the ARM and NASA data archives.
C1 [Jensen, M. P.; Giangrande, S. E.] Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA.
[Petersen, W. A.; Gerlach, J.; Heymsfield, G.; Schwaller, M.; Tokay, A.; Wolff, D. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Petersen, W. A.; Gerlach, J.; Wolff, D. B.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Bansemer, A.; Heymsfield, A.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Bharadwaj, N.] Pacific Northwest Natl Lab, Richland, WA USA.
[Carey, L. D.] Univ Alabama, Huntsville, AL 35899 USA.
[Cecil, D. J.; Lang, T. J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Collis, S. M.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Del Genio, A. D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dolan, B.; Rutledge, S. A.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Kollias, P.] McGill Univ, Montreal, PQ, Canada.
[Nesbitt, S. W.] Univ Illinois, Urbana, IL USA.
[Neumann, A.; Poellot, M.] Univ North Dakota, Grand Forks, ND USA.
[Tokay, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Williams, C. R.] Univ Colorado, Boulder, CO 80309 USA.
[Xie, S.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Zipser, E. J.] Univ Utah, Salt Lake City, UT USA.
RP Jensen, MP (reprint author), Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA.
EM mjensen@bnl.gov
RI Xie, Shaocheng/D-2207-2013
OI Xie, Shaocheng/0000-0001-8931-5145
FU U.S. Department of Energy's ARM Program; NASA's Global Precipitation
Measurement mission's Ground Validation Program; NASA [NNX10AN38G,
NNX10AH67G, NNX14AH06G]; U.S. Department of Energy, Office of Science,
Office of Biological and Environmental Research (BER), as part of the
Atmospheric System Research (ASR) program; U.S. Department of Energy,
Office of Science, Office of Biological and Environmental Research
(BER), as part of the ARM program; DOE [DE-SC0007016]; U.S. Department
of Energy [DE-AC02-98CH10886]
FX The MC3E field campaign was jointly funded by the U.S. Department of
Energy's ARM Program and NASA's Global Precipitation Measurement
mission's Ground Validation Program. We acknowledge the important
contributions of the ARM SGP site operations staff members for their
contributions to the siting, deployment, and maintenance of NASA MC3E
and SGP ARM Climate Facility instrumentation. We also acknowledge the
UND Citation flight and support crews for their excellent conduct of
airborne microphysical sampling, and Offutt AFB and Ponca City Regional
Airport for their hosting and field support of the NASA ER-2 and UND
Citation, respectively. Operations of the UND Citation aircraft were
funded under NASA Grant NNX10AN38G. MJ and SG were funded by the U.S.
Department of Energy, Office of Science, Office of Biological and
Environmental Research (BER), as part of the Atmospheric System Research
(ASR) and ARM programs. AH and AB were funded by NASA Grant NNX10AH67G.
SR and BD were funded by DOE Grant DE-SC0007016 and NASA Grant
NNX14AH06G. This paper has been coauthored by employees of Brookhaven
Science Associates, LLC, under Contract DE-AC02-98CH10886 with the U.S.
Department of Energy.
NR 56
TC 10
Z9 10
U1 6
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD SEP
PY 2016
VL 97
IS 9
BP 1667
EP +
DI 10.1175/BAMS-D-14-00228.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ5PG
UT WOS:000385913400016
ER
PT J
AU Wood, R
Jensen, MP
Wang, J
Bretherton, CS
Burrows, SM
Del Genio, AD
Fridlind, AM
Ghan, SJ
Ghate, VP
Kollias, P
Krueger, SK
McGraw, RL
Miller, MA
Painemal, D
Russell, LM
Yuter, SE
Zuidema, P
AF Wood, Robert
Jensen, Michael P.
Wang, Jian
Bretherton, Christopher S.
Burrows, Susannah M.
Del Genio, Anthony D.
Fridlind, Ann M.
Ghan, Steven J.
Ghate, Virendra P.
Kollias, Pavlos
Krueger, Steven K.
McGraw, Robert L.
Miller, Mark A.
Painemal, David
Russell, Lynn M.
Yuter, Sandra E.
Zuidema, Paquita
TI PLANNING THE NEXT DECADE OF COORDINATED RESEARCH TO BETTER UNDERSTAND
AND SIMULATE MARINE LOW CLOUDS
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
ID STRATOCUMULUS
C1 [Wood, Robert; Bretherton, Christopher S.] Univ Washington, Seattle, WA 98195 USA.
[Jensen, Michael P.; Wang, Jian; McGraw, Robert L.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Burrows, Susannah M.; Ghan, Steven J.] Pacific Northwest Natl Lab, Richland, WA USA.
[Del Genio, Anthony D.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ghate, Virendra P.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Kollias, Pavlos] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Krueger, Steven K.] Univ Utah, Salt Lake City, UT USA.
[Miller, Mark A.] Rutgers State Univ, New Brunswick, NJ USA.
[Painemal, David] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Russell, Lynn M.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Yuter, Sandra E.] North Carolina State Univ, Raleigh, NC USA.
[Zuidema, Paquita] Univ Miami, Miami, FL USA.
RP Wood, R (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM robwood2@uw.edu
RI Ghan, Steven/H-4301-2011; Zuidema, Paquita/C-9659-2013; Wang,
Jian/G-9344-2011; Burrows, Susannah/A-7429-2011; Wood,
Robert/A-2989-2008
OI Ghan, Steven/0000-0001-8355-8699; Zuidema, Paquita/0000-0003-4719-372X;
Burrows, Susannah/0000-0002-0745-7252; Wood, Robert/0000-0002-1401-3828
NR 12
TC 0
Z9 0
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD SEP
PY 2016
VL 97
IS 9
BP 1699
EP 1702
DI 10.1175/BAMS-D-16-0160.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ5PG
UT WOS:000385913400018
ER
PT J
AU Ichoku, C
Ellison, LT
Willmot, KE
Matsui, T
Dezfuli, AK
Gatebe, CK
Wang, J
Wilcox, EM
Lee, J
Adegoke, J
Okonkwo, C
Bolten, J
Policelli, FS
Habib, S
AF Ichoku, Charles
Ellison, Luke T.
Willmot, K. Elena
Matsui, Toshihisa
Dezfuli, Amin K.
Gatebe, Charles K.
Wang, Jun
Wilcox, Eric M.
Lee, Jejung
Adegoke, Jimmy
Okonkwo, Churchill
Bolten, John
Policelli, Frederick S.
Habib, Shahid
TI Biomass burning, land-cover change, and the hydrological cycle in
Northern sub-Saharan Africa
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE sub-Saharan Africa; biomass burning; water cycle; land cover change;
precipitation; fire
ID WESTERN EQUATORIAL AFRICA; FIRE DETECTION; CLIMATE-CHANGE; RAINFALL
VARIABILITY; TROPICAL OCEANS; SAHEL RAINFALL; SOIL-MOISTURE; LAKE CHAD;
PART I; SURFACE
AB The Northern Sub-Saharan African (NSSA) region, which accounts for 20%-25% of the global carbon emissions from biomass burning, also suffers from frequent drought episodes and other disruptions to the hydrological cycle whose adverse societal impacts have been widely reported during the last several decades. This paper presents a conceptual framework of the NSSA regional climate system components that may be linked to biomass burning, as well as detailed analyses of a variety of satellite data for 2001-2014 in conjunction with relevant model-assimilated variables. Satellite fire detections in NSSA show that the vast majority (>75%) occurs in the savanna and woody savanna land-cover types. Starting in the 2006-2007 burning season through the end of the analyzed data in 2014, peak burning activity showed a net decrease of 2-7%/yr in different parts of NSSA, especially in the savanna regions. However, fire distribution shows appreciable coincidence with land-cover change. Although there is variable mutual exchange of different land cover types, during 2003-2013, cropland increased at an estimated rate of 0.28%/yr of the total NSSA land area, with most of it (0.18%/yr) coming from savanna. During the last decade, conversion to croplands increased in some areas classified as forests and wetlands, posing a threat to these vital and vulnerable ecosystems. Seasonal peak burning is anti-correlated with annual water-cycle indicators such as precipitation, soil moisture, vegetation greenness, and evapotranspiration, except in humid West Africa (5 degrees-10 degrees latitude), where this anti-correlation occurs exclusively in the dry season and burning virtually stops when monthly mean precipitation reaches 4 mm d(-1). These results provide observational evidence of changes in land-cover and hydrological variables that are consistent with feedbacks from biomass burning in NSSA, and encourage more synergistic modeling and observational studies that can elaborate this feedback mechanism.
C1 [Ichoku, Charles; Ellison, Luke T.; Matsui, Toshihisa; Dezfuli, Amin K.; Gatebe, Charles K.; Bolten, John; Policelli, Frederick S.; Habib, Shahid] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Willmot, K. Elena] Vanderbilt Univ, Nashville, TN 37235 USA.
[Matsui, Toshihisa] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Dezfuli, Amin K.; Gatebe, Charles K.] USRA, Columbia, MD USA.
[Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
[Wang, Jun] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
[Wang, Jun] Univ Iowa, Dept Chem & Biochem Engn, Iowa City, IA 52242 USA.
[Wilcox, Eric M.] Desert Res Inst, Reno, NV USA.
[Lee, Jejung; Adegoke, Jimmy] Univ Missouri, Kansas City, MO 64110 USA.
[Okonkwo, Churchill] Howard Univ, Beltsville Ctr Climate Syst Observat, Washington, DC 20059 USA.
RP Ichoku, C (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
EM Charles.Ichoku@nasa.gov
RI Wang, Jun/A-2977-2008
OI Wang, Jun/0000-0002-7334-0490
FU NASA under its Research Opportunities in Space and Earth Sciences
(ROSES) through the Radiation Sciences Program; NASA under its
Interdisciplinary Studies (IDS) Program through the Radiation Sciences
Program
FX This research was fully funded by NASA under its Research Opportunities
in Space and Earth Sciences (ROSES)-2009 and 2013 Interdisciplinary
Studies (IDS) Program (Dr Jack Kaye, Earth Science Research Director)
through the Radiation Sciences Program managed by Dr Hal Maring. We also
appreciate the efforts of providers of the large diversity of data
products used for this study from various satellite sensors and global
models.
NR 72
TC 1
Z9 1
U1 15
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2016
VL 11
IS 9
AR 095005
DI 10.1088/1748-9326/11/9/095005
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PW
UT WOS:000385393300001
ER
PT J
AU Marchand, P
Carr, JA
Dell'Angelo, J
Fader, M
Gephart, JA
Kummu, M
Magliocca, NR
Porkka, M
Puma, MJ
Ratajczak, Z
Rulli, MC
Seekell, DA
Suweis, S
Tavoni, A
D'Odorico, P
AF Marchand, Philippe
Carr, Joel A.
Dell'Angelo, Jampel
Fader, Marianela
Gephart, Jessica A.
Kummu, Matti
Magliocca, Nicholas R.
Porkka, Miina
Puma, Michael J.
Ratajczak, Zak
Rulli, Maria Cristina
Seekell, David A.
Suweis, Samir
Tavoni, Alessandro
D'Odorico, Paolo
TI Reserves and trade jointly determine exposure to food supply shocks
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Letter
DE food systems; resilience; food crises
ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION;
DISPLACEMENT; SECURITY; NATIONS; WATER
AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations.
C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
[Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany.
[Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland.
[Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy.
[Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Ume, Sweden.
[Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy.
[Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England.
RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
NR 44
TC 0
Z9 0
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2016
VL 11
IS 9
AR 095009
DI 10.1088/1748-9326/11/9/095009
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DZ2XT
UT WOS:000385707100001
ER
PT J
AU Marchand, P
Carr, JA
Dell'Angelo, J
Fader, M
Gephart, JA
Kummu, M
Magliocca, NR
Porkka, M
Puma, MJ
Ratajczak, Z
Rulli, MC
Seekell, DA
Suweis, S
Tavoni, A
D'Odorico, P
AF Marchand, Philippe
Carr, Joel A.
Dell'Angelo, Jampel
Fader, Marianela
Gephart, Jessica A.
Kummu, Matti
Magliocca, Nicholas R.
Porkka, Miina
Puma, Michael J.
Ratajczak, Zak
Rulli, Maria Cristina
Seekell, David A.
Suweis, Samir
Tavoni, Alessandro
D'Odorico, Paolo
TI Reserves and trade jointly determine exposure to food supply shocks
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE food systems; resilience; food crises
ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION;
DISPLACEMENT; SECURITY; NATIONS; WATER
AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations.
C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
[Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany.
[Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland.
[Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy.
[Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden.
[Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy.
[Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England.
RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
RI Kummu, Matti/C-4797-2011
OI Kummu, Matti/0000-0001-5096-0163
FU National Socio-Environmental Synthesis Center (SESYNC) under National
Science Foundation (NSF) [DBI-1052875]; Academy of Finland SRC project
Winland; Academy of Finland project SCART; Columbia University Center
for Climate and Life; Interdisciplinary Global Change Research under
NASA [NNX08AJ75A]; Carl Trygger Foundation for Scientific Research; NSF
[DBI-1402033]; Centre for Climate Change Economics and Policy - ESRC;
Grantham Foundation for the Protection of the Environment
FX We thank Roberto Patricio Korzeniewicz and Christina Prell for their
participation in early discussions on this project. This work was
supported by the National Socio-Environmental Synthesis Center (SESYNC)
under funding received from the National Science Foundation (NSF) grant
DBI-1052875. M Kummu received support from Academy of Finland SRC
project Winland and Academy of Finland project SCART. M J Puma is
supported by a fellowship from the Columbia University Center for
Climate and Life and the Interdisciplinary Global Change Research under
NASA cooperative agreement NNX08AJ75A. D A Seekell was supported by the
Carl Trygger Foundation for Scientific Research. Z Ratajczak received
support from NSF grant DBI-1402033. A Tavoni is supported by the Centre
for Climate Change Economics and Policy, funded by the ESRC, and the
Grantham Foundation for the Protection of the Environment.
NR 44
TC 0
Z9 0
U1 4
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2016
VL 11
IS 9
AR 095009
DI 10.1088/1748-9326/11/9/095009
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PW
UT WOS:000385393300005
ER
PT J
AU Sedano, F
Silva, JA
Machoco, R
Meque, CH
Sitoe, A
Ribeiro, N
Anderson, K
Ombe, ZA
Baule, SH
Tucker, CJ
AF Sedano, F.
Silva, J. A.
Machoco, R.
Meque, C. H.
Sitoe, A.
Ribeiro, N.
Anderson, K.
Ombe, Z. A.
Baule, S. H.
Tucker, C. J.
TI The impact of charcoal production on forest degradation: a case study in
Tete, Mozambique
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE forest degradation; charcoal; carbon emissions; remote sensing; very
high-resolution; Africa
ID DEVELOPING-COUNTRIES; DEVELOPING-WORLD; DEFORESTATION; IMAGERY; POLICY;
LIVELIHOODS; EMISSIONS; AFRICA; MAPS
AB Charcoal production for urban energy consumption is a main driver of forest degradation in sub Saharan Africa. Urban growth projections for the continent suggest that the relevance of this process will increase in the coming decades. Forest degradation associated to charcoal production is difficult to monitor and commonly overlooked and underrepresented in forest cover change and carbon emission estimates. We use a multitemporal dataset of very high-resolution remote sensing images to map kiln locations in a representative study area of tropical woodlands in central Mozambique. The resulting maps provided a characterization of the spatial extent and temporal dynamics of charcoal production. Using an indirect approach we combine kiln maps and field information on charcoal making to describe the magnitude and intensity of forest degradation linked to charcoal production, including aboveground biomass and carbon emissions. Our findings reveal that forest degradation associated to charcoal production in the study area is largely independent from deforestation driven by agricultural expansion and that its impact on forest cover change is in the same order of magnitude as deforestation. Our work illustrates the feasibility of using estimates of urban charcoal consumption to establish a link between urban energy demands and forest degradation. This kind of approach has potential to reduce uncertainties in forest cover change and carbon emission assessments in sub-Saharan Africa.
C1 [Sedano, F.; Silva, J. A.; Anderson, K.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Machoco, R.; Sitoe, A.; Ribeiro, N.] UEM, Fac Agron & Forest Engn, Dept Forest Engn, Maputo, Mozambique.
[Meque, C. H.] Mozambican Minist Sci & Technol, Zambezia, Mozambique.
[Ombe, Z. A.] Univ Pedagog, Fac Earth Sci & Environm, Maputo, Mozambique.
[Baule, S. H.] Univ Pedagog, Dept Language Commun & Arts, Beira, Mozambique.
[Tucker, C. J.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
RP Sedano, F (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM fsedano@umd.edu
FU National Science Foundation-Dynamics of Coupled Natural and Human
Systems program [1413999]
FX This research is part of the 'CNH-Ex: Investigating the Dynamic
Intersections Among Economic Development, Urbanization, and Forest
Degradation' project, funded under the National Science
Foundation-Dynamics of Coupled Natural and Human Systems program (Award
number 1413999). The authors express their gratitude to students and
representatives of the Universidade Eduardo Mondlane, Universidade
Pegagogica-Tete branch and the personnel of the provincial Forest
Services of Tete whose contribution and support made possible field data
collection.
NR 39
TC 0
Z9 0
U1 10
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2016
VL 11
IS 9
AR 094020
DI 10.1088/1748-9326/11/9/094020
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PU
UT WOS:000385393100008
ER
PT J
AU Rani, B
Krichbaum, T
Hodgson, JA
Koyama, S
Zensus, AJ
Fuhramnn, L
Marscher, A
Jorstad, S
AF Rani, Bindu
Krichbaum, Thomas
Hodgson, Jeff A.
Koyama, Shoko
Zensus, Anton J.
Fuhramnn, Lars
Marscher, Alan
Jorstad, Svetlana
TI Exploring the Magnetic Field Configuration in BL Lac Using GMVA
SO GALAXIES
LA English
DT Article
DE active galaxies; BL Lacertae object: BL Lac; jets; GMVA; high-resolution
VLBI; magnetic field; polarization
ID JET
AB The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. To explore the the magnetic field configuration at the base of jets in blazars, we took advantage of the full polarization capabilities of the Global Millimeter VLBI Array (GMVA). With an angular resolution of similar to 50 micro-arcseconds (m as) at 86 GHz, one could resolve scales up to similar to 450 gravitational radii (for a 10(9) solar mass black hole at a redshift of 0.1). We present here the preliminary results of our study on the blazar BL Lac. Our results suggest that on sub-mas scales the core and the central jet of BL Lac are significantly polarized with two distinct regions of polarized intensity. We also noted a great morphological similarity between the 7 mm/3 mm VLBI images at very similar angular resolution.
C1 [Rani, Bindu] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rani, Bindu; Krichbaum, Thomas; Koyama, Shoko; Zensus, Anton J.; Fuhramnn, Lars] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Hodgson, Jeff A.] Korea Astron & Space Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea.
[Marscher, Alan; Jorstad, Svetlana] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
RP Rani, B (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Rani, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM bindu.rani@nasa.gov; tkrichbaum@mpifr-bonn.mpg.de; jhodgo@gmail.com;
skoyama@mpifr-bonn.mpg.de; azensus@mpifr-bonn.mpg.de;
fuhrmann.lars@googlemail.com; marscher@bu.edu; jorstad@bu.edu
OI Jorstad, Svetlana/0000-0001-6158-1708
NR 18
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2075-4434
J9 GALAXIES
JI Galaxies
PD SEP
PY 2016
VL 4
IS 3
AR 32
DI 10.3390/galaxies4030032
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9UM
UT WOS:000385480600024
ER
PT J
AU Wilder, FD
Ergun, RE
Schwartz, SJ
Newman, DL
Eriksson, S
Stawarz, JE
Goldman, MV
Goodrich, KA
Gershman, DJ
Malaspina, DM
Holmes, JC
Sturner, AP
Burch, JL
Torbert, RB
Lindqvist, PA
Marklund, GT
Khotyaintsev, Y
Strangeway, RJ
Russell, CT
Pollock, CJ
Giles, BL
Dorrelli, JC
Avanov, LA
Patterson, WR
Plaschke, F
Magnes, W
AF Wilder, F. D.
Ergun, R. E.
Schwartz, S. J.
Newman, D. L.
Eriksson, S.
Stawarz, J. E.
Goldman, M. V.
Goodrich, K. A.
Gershman, D. J.
Malaspina, D. M.
Holmes, J. C.
Sturner, A. P.
Burch, J. L.
Torbert, R. B.
Lindqvist, P. -A.
Marklund, G. T.
Khotyaintsev, Y.
Strangeway, R. J.
Russell, C. T.
Pollock, C. J.
Giles, B. L.
Dorrelli, J. C.
Avanov, L. A.
Patterson, W. R.
Plaschke, F.
Magnes, W.
TI Observations of large-amplitude, parallel, electrostatic waves
associated with the Kelvin-Helmholtz instability by the magnetospheric
multiscale mission
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Kelvin-Helmholtz; electrostatic waves; boundary layer; turbulence
ID LATITUDE BOUNDARY-LAYER; MAGNETIC RECONNECTION; PLASMA TRANSPORT
AB On 8 September 2015, the four Magnetospheric Multiscale spacecraft encountered a Kelvin-Helmholtz unstable magnetopause near the dusk flank. The spacecraft observed periodic compressed current sheets, between which the plasma was turbulent. We present observations of large-amplitude (up to 100mV/m) oscillations in the electric field. Because these oscillations are purely parallel to the background magnetic field, electrostatic, and below the ion plasma frequency, they are likely to be ion acoustic-like waves. These waves are observed in a turbulent plasma where multiple particle populations are intermittently mixed, including cold electrons with energies less than 10eV. Stability analysis suggests a cold electron component is necessary for wave growth.
C1 [Wilder, F. D.; Ergun, R. E.; Schwartz, S. J.; Eriksson, S.; Stawarz, J. E.; Goodrich, K. A.; Malaspina, D. M.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Ergun, R. E.; Stawarz, J. E.; Goodrich, K. A.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Schwartz, S. J.] Imperial Coll London, Dept Phys, London, England.
[Newman, D. L.; Goldman, M. V.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Gershman, D. J.; Pollock, C. J.; Giles, B. L.; Dorrelli, J. C.; Avanov, L. A.; Patterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
[Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Lindqvist, P. -A.; Marklund, G. T.] Royal Inst Technol, Stockholm, Sweden.
[Khotyaintsev, Y.] Swedish Inst Space Phys, Uppsala, Sweden.
[Strangeway, R. J.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Plaschke, F.; Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
RP Wilder, FD (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM frederick.wilder@lasp.colorado.edu
RI Stawarz, Julia/L-7387-2016; NASA MMS, Science Team/J-5393-2013;
OI Stawarz, Julia/0000-0002-5702-5802; NASA MMS, Science
Team/0000-0002-9504-5214; Eriksson, Stefan/0000-0002-5619-1577
FU NASA MMS project; Leverhulme Trust
FX This work was funded by the NASA MMS project. S.J.S. thanks the
Leverhulme Trust for the award of a research fellowship. We thank the
MMS search coil magnetometer team for providing burst data and comments
on our analyses. Level 2 spacecraft data are available via the MMS
Science Data Center (https://lasp.colorado.edu/mms/sdc/public/).
NR 22
TC 0
Z9 0
U1 1
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 SEP
PY 2016
VL 43
IS 17
BP 8859
EP 8866
DI 10.1002/2016GL070404
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200005
ER
PT J
AU Xu, SS
Mitchell, D
Liemohn, M
Dong, CF
Bougher, S
Fillingim, M
Lillis, R
McFadden, J
Mazelle, C
Connerney, J
Jakosky, B
AF Xu, Shaosui
Mitchell, David
Liemohn, Michael
Dong, Chuanfei
Bougher, Stephen
Fillingim, Matthew
Lillis, Robert
McFadden, James
Mazelle, Christian
Connerney, Jack
Jakosky, Bruce
TI Deep nightside photoelectron observations by MAVEN SWEA: Implications
for Martian northern hemispheric magnetic topology and nightside
ionosphere source
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; photoelectrons; nightside ionosphere; magnetic topology; weak
crustal fields; MAVEN
ID SOLAR-WIND INTERACTION; ELECTRON REFLECTOMETRY; MARS; FIELD; ATMOSPHERE;
MODEL; INSTRUMENT; MISSION; FLUXES; ATOMS
AB The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission samples the Mars ionosphere down to altitudes of approximate to 150km over a wide range of local times and solar zenith angles. On 5 January 2015 (Orbit 520) when the spacecraft was in darkness at high northern latitudes (solar zenith angle, SZA>120 degrees; latitude>60 degrees), the Solar Wind Electron Analyzer (SWEA) instrument observed photoelectrons at altitudes below 200km. Such observations imply the presence of closed crustal magnetic field loops that cross the terminator and extend thousands of kilometers to the deep nightside. This occurs over the weak northern crustal magnetic source regions, where the magnetic field has been thought to be dominated by draped interplanetary magnetic fields (IMF). Such a day-night magnetic connectivity also provides a source of plasma and energy to the deep nightside. Simulations with the SuperThermal Electron Transport (STET) model show that photoelectron fluxes measured by SWEA precipitating onto the nightside atmosphere provide a source of ionization that can account for the O(2)(+)density measured by the Suprathermal and Thermal Ion Composition (STATIC) instrument below 200km. This finding indicates another channel for Martian energy redistribution to the deep nightside and consequently localized ionosphere patches and potentially aurora.
C1 [Xu, Shaosui; Mitchell, David; Fillingim, Matthew; Lillis, Robert; McFadden, James] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Xu, Shaosui; Liemohn, Michael; Dong, Chuanfei; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Dong, Chuanfei] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dong, Chuanfei] Princeton Univ, Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA.
[Mazelle, Christian] CNRS, IRAP, Toulouse, France.
[Mazelle, Christian] Univ Toulouse 3, Toulouse, France.
[Connerney, Jack] GSFC, Greenbelt, MD USA.
[Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Xu, SS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Xu, SS (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM shaosui.xu@ssl.berkeley.edu
RI Dong, Chuanfei/E-6485-2010;
OI Dong, Chuanfei/0000-0002-8990-094X; Xu, Shaosui/0000-0002-5121-600X;
connerney, jack/0000-0001-7478-6462
FU NASA; NSF [NNX13AG26G, AST-0908311]; NASA Mars Scout Program; Rackham
graduate school of University of Michigan; NASA Living With a Star Jack
Eddy Postdoctoral Fellowship Program
FX The authors would like to thank NASA and NSF for their support of this
project under grants NNX13AG26G and AST-0908311. This work was also
supported by the NASA Mars Scout Program. The authors thank the Rackham
graduate school of University of Michigan for the research grant that
supports S. Xu's visit at SSL, University of California, Berkeley, which
makes this study possible. C.F. Dong is supported by the NASA Living
With a Star Jack Eddy Postdoctoral Fellowship Program, administered by
the University Corporation for Atmospheric Research. The MAVEN data used
in this study are available through Planetary Data System. The BATS-R-US
code is publicly available from http://csem.engin.umich.edu/tools/swmf.
For distribution of the model results used in this study, please contact
C. Dong (dcfy@pppl.gov).
NR 53
TC 1
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U1 8
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP
PY 2016
VL 43
IS 17
BP 8876
EP 8884
DI 10.1002/2016GL070527
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200007
ER
PT J
AU Edwards, CS
Piqueux, S
AF Edwards, Christopher S.
Piqueux, Sylvain
TI The water content of recurring slope lineae on Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; recurring slope lineae; water budget; THEMIS; thermophysics
ID THERMAL-CONDUCTIVITY MEASUREMENTS; EMISSION SPECTROMETER; PARTICULATE
MATERIALS; REFLECTANCE; STABILITY; SURFACE; THEMIS; ICE
AB Observations of recurring slope lineae (RSL) from the High-Resolution Imaging Science Experiment have been interpreted as present-day, seasonally variable liquid water flows; however, orbital spectroscopy has not confirmed the presence of liquid H2O, only hydrated salts. Thermal Emission Imaging System (THEMIS) temperature data and a numerical heat transfer model definitively constrain the amount of water associated with RSL. Surface temperature differences between RSL-bearing and dry RSL-free terrains are consistent with no water associated with RSL and, based on measurement uncertainties, limit the water content of RSL to at most 0.5-3wt %. In addition, distinct high thermal inertia regolith signatures expected with crust-forming evaporitic salt deposits from cyclical briny water flows are not observed, indicating low water salinity (if any) and/or low enough volumes to prevent their formation. Alternatively, observed salts may be preexisting in soils at low abundances (i.e., near or below detection limits) and largely immobile. These RSL-rich surfaces experience similar to 100K diurnal temperature oscillations, possible freeze/thaw cycles and/or complete evaporation on time scales that challenge their habitability potential. The unique surface temperature measurements provided by THEMIS are consistent with a dry RSL hypothesis or at least significantly limit the water content of Martian RSL.
C1 [Edwards, Christopher S.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Edwards, Christopher S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
[Piqueux, Sylvain] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Edwards, CS (reprint author), US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.; Edwards, CS (reprint author), Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
EM Christopher.Edwards@nau.edu
FU National Aeronautics and Space Administration
FX The authors thank the 2001 Mars Odyssey THEMIS team, who aided in the
collection of needed seasonal data. We thank Joshua Bandfield, Shane
Byrne, and two anonymous reviewers that greatly improved the manuscript.
All THEMIS, CTX, and HiRISE data presented in this work are available on
the Planetary Data System (http://pds-geosciences.wustl.edu), data
processing software was completed using davinci (http://davinci.asu.edu)
and the Integrated Software for Imaging Spectrometers
(http://isis.astrogeology.usgs.gov), and modeling was conducted using
the KRC thermal model (http://krc.mars.asu.edu). Work at the Jet
Propulsion Laboratory, California Institute of Technology was performed
under a contract with the National Aeronautics and Space Administration.
NR 59
TC 2
Z9 2
U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP
PY 2016
VL 43
IS 17
BP 8912
EP 8919
DI 10.1002/2016GL070179
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200011
ER
PT J
AU Coats, S
Mankin, JS
AF Coats, Sloan
Mankin, Justin S.
TI The challenge of accurately quantifying future megadrought risk in the
American Southwest
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE hydroclimate; drought; North America; climate; megadrought; projections
ID LAST MILLENNIUM; NORTH-AMERICA; DROUGHT; RECONSTRUCTIONS; VARIABILITY;
FREQUENCY; EVENTS; WATER
AB American Southwest (ASW) megadroughts represent decadal-scale periods of dry conditions the near-term risks of which arise from natural low-frequency hydroclimate variability and anthropogenic forcing. A large single-climate-model ensemble indicates that anthropogenic forcing increases near-term ASW megadrought risk by a factor of 100; however, accurate risk assessment remains a challenge. At the global-scale we find that anthropogenic forcing may alter the variability driving megadroughts over 55% of land areas, undermining accurate assessments of their risk. For the remaining areas, current ensembles are too small to characterize megadroughts' driving variability. For example, constraining uncertainty in near-term ASW megadrought risk to 5 percentage points with high confidence requires 287 simulations. Such ensemble sizes are beyond current computational and storage resources, and these limitations suggest that constraining errors in near-term megadrought risk projections with high confidenceeven in places where underlying variability is stationaryis not currently possible.
C1 [Coats, Sloan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Mankin, Justin S.] Columbia Univ, Ocean & Climate Phys, Lamont Doherty Earth Observ, Palisades, NY USA.
[Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Coats, S (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM sloan.coats@colorado.edu
FU Center for International Security and Cooperation at Stanford
University; Earth Institute Fellowship at Columbia University;
Cooperative Institute for Research in Environmental Sciences at the
University of Colorado, Boulder
FX The authors would like to thank the National Center for Atmospheric
Research's CESM1 (CAM5) Large Ensemble Community Project (LENS) and
supercomputing resources provided by Stanford Center for Computational
Earth and Environmental Science in the School of Earth, Energy, and
Environmental Sciences at Stanford University. The model output employed
from the LENS can be accessed at
https://www2.cesm.ucar.edu/models/experiments/LENS. Our work was
supported by the Center for International Security and Cooperation at
Stanford University and the Earth Institute Fellowship at Columbia
University to J.S.M. and the Cooperative Institute for Research in
Environmental Sciences at the University of Colorado, Boulder, and
Kristopher B. Karnauskas to S.C. LDEO publication 8051.
NR 31
TC 0
Z9 0
U1 5
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP
PY 2016
VL 43
IS 17
BP 9225
EP 9233
DI 10.1002/2016GL070445
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200049
ER
PT J
AU Tong, D
Pan, L
Chen, WW
Lamsal, L
Lee, P
Tang, YH
Kim, H
Kondragunta, S
Stajner, I
AF Tong, Daniel
Pan, Li
Chen, Weiwei
Lamsal, Lok
Lee, Pius
Tang, Youhua
Kim, Hyuncheol
Kondragunta, Shobha
Stajner, Ivanka
TI Impact of the 2008 Global Recession on air quality over the United
States: Implications for surface ozone levels from changes in NOx
emissions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone; recession; NO2; air quality
ID NITROGEN-OXIDES; NORTH-AMERICA; SATELLITE; POLLUTION; MODEL; CAPABILITY;
SYSTEM; TRENDS; CITIES; SPACE
AB Satellite and ground observations detected large variability in nitrogen oxides (NOx) during the 2008 economic recession, but the impact of the recession on air quality has not been quantified. This study combines observed NOx trends and a regional chemical transport model to quantify the impact of the recession on surface ozone (O-3) levels over the continental United States. The impact is quantified by simulating O-3 concentrations under two emission scenarios: business-as-usual (BAU) and recession. In the BAU case, the emission projection from the Cross-State Air Pollution Rule is used to estimate the would-be NOx emission level in 2011. In the recession case, the actual NO2 trends observed from Air Quality System ground monitors and the Ozone Monitoring Instrument on the Aura satellite are used to obtain realistic changes in NOx emissions. The model prediction with the recession effect agrees better with ground O-3 observations over time and space than the prediction with the BAU emission. The results show that the recession caused a 1-2ppbv decrease in surface O-3 concentration over the eastern United States, a slight increase (0.5-1ppbv) over the Rocky Mountain region, and mixed changes in the Pacific West. The gain in air quality benefits during the recession, however, could be quickly offset by the much slower emission reduction rate during the post-recession period.
C1 [Tong, Daniel] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.
[Tong, Daniel; Pan, Li; Tang, Youhua; Kim, Hyuncheol] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.
[Tong, Daniel; Pan, Li; Chen, Weiwei; Lee, Pius; Tang, Youhua; Kim, Hyuncheol] NOAA, Air Resources Lab, College Pk, MD 20740 USA.
[Lamsal, Lok] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lamsal, Lok] Univ Space Res Assoc, Greenbelt, MD USA.
[Kondragunta, Shobha] NOAA, Satellite & Informat Serv, Ctr Satellite Res & Applicat, College Pk, MD USA.
[Stajner, Ivanka] NOAA, Natl Weather Serv, Off Sci & Technol Integrat, Silver Spring, MD 20910 USA.
RP Tong, D (reprint author), Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.; Tong, D (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.; Tong, D (reprint author), NOAA, Air Resources Lab, College Pk, MD 20740 USA.
EM daniel.tong@noaa.gov
RI Kondragunta, Shobha/F-5601-2010; Tong, Daniel/A-8255-2008; Kim,
Hyun/G-1315-2012
OI Kondragunta, Shobha/0000-0001-8593-8046; Tong,
Daniel/0000-0002-4255-4568; Kim, Hyun/0000-0003-3968-6145
FU NOAA's US Weather Research Program (USWRP); Joint Polar Satellite System
(JPSS) Proving Ground and Risk Reduction Programs
FX This work has been financially supported by grants from the NOAA's US
Weather Research Program (USWRP) and Joint Polar Satellite System (JPSS)
Proving Ground and Risk Reduction Programs. Modeling system development
was supported by the NOAA's National Air Quality Forecast Capability
program. The authors are grateful to Nina Randazzo for data analysis and
two anonymous reviewers for their constructive comments. 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 view
of NOAA or the Department of Commerce.
NR 34
TC 0
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U1 6
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 SEP
PY 2016
VL 43
IS 17
BP 9280
EP 9288
DI 10.1002/2016GL069885
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200055
ER
PT J
AU Schobesberger, S
Lopez-Hilfiker, FD
Taipale, D
Millet, DB
D'Ambro, EL
Rantala, P
Mammarella, I
Zhou, PT
Wolfe, GM
Lee, BH
Boy, M
Thornton, JA
AF Schobesberger, Siegfried
Lopez-Hilfiker, Felipe D.
Taipale, Ditte
Millet, Dylan B.
D'Ambro, Emma L.
Rantala, Pekka
Mammarella, Ivan
Zhou, Putian
Wolfe, Glenn M.
Lee, Ben H.
Boy, Michael
Thornton, Joel A.
TI High upward fluxes of formic acid from a boreal forest canopy
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE formic acid; eddy covariance fluxes; chemical ionization mass
spectrometry; boreal forest; biogenic emissions
ID ORGANIC-COMPOUND EMISSIONS; GASEOUS DRY DEPOSITION; ACETIC-ACIDS; SCOTS
PINE; MASS-SPECTROMETER; EDDY COVARIANCE; PEROXY NITRATES;
SULFURIC-ACID; NEW-MODEL; GAS
AB Eddy covariance fluxes of formic acid, HCOOH, were measured over a boreal forest canopy in spring/summer 2014. The HCOOH fluxes were bidirectional but mostly upward during daytime, in contrast to studies elsewhere that reported mostly downward fluxes. Downward flux episodes were explained well by modeled dry deposition rates. The sum of net observed flux and modeled dry deposition yields an upward gross flux of HCOOH, which could not be quantitatively explained by literature estimates of direct vegetative/soil emissions nor by efficient chemical production from other volatile organic compounds, suggesting missing or greatly underestimated HCOOH sources in the boreal ecosystem. We implemented a vegetative HCOOH source into the GEOS-Chem chemical transport model to match our derived gross flux and evaluated the updated model against airborne and spaceborne observations. Model biases in the boundary layer were substantially reduced based on this revised treatment, but biases in the free troposphere remain unexplained.
C1 [Schobesberger, Siegfried; Lopez-Hilfiker, Felipe D.; Lee, Ben H.; Thornton, Joel A.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Schobesberger, Siegfried; Rantala, Pekka; Mammarella, Ivan; Zhou, Putian; Boy, Michael] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Taipale, Ditte] Estonian Univ Life Sci, Dept Plant Physiol, Tartu, Estonia.
[Taipale, Ditte] Univ Helsinki, Dept Forest Sci, Helsinki, Finland.
[Millet, Dylan B.] Univ Minnesota, Dept Soil Water & Climate, Minneapolis, MN USA.
[D'Ambro, Emma L.] Univ Washington, Dept Chem, Seattle, WA 98195 USA.
[Wolfe, Glenn M.] NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Schobesberger, S (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.; Schobesberger, S (reprint author), Univ Helsinki, Dept Phys, Helsinki, Finland.
EM sschobes@uw.edu
RI Millet, Dylan/G-5832-2012; Chem, GEOS/C-5595-2014; Thornton,
Joel/C-1142-2009; Wolfe, Glenn/D-5289-2011;
OI Thornton, Joel/0000-0002-5098-4867; Taipale, Ditte/0000-0002-2023-2461;
Boy, Michael/0000-0002-8107-4524; Mammarella, Ivan/0000-0002-8516-3356;
Zhou, Putian/0000-0003-0803-7337
FU U.S. Department of Energy [DE-SC0006867]; European Commission (OXFLUX)
[701958]; European Regional Development Fund (Centre of Excellence
EcolChange); NSF CAREER [1148951]; Minnesota Supercomputing Institute
FX We thank T. Vesala, P. Kolari, P. Keronen, E. Siivola, M. Kajos, and A.
Manninen at U. Helsinki for helpful discussions and model and
measurement data related to SMEAR II. We also thank J. de Gouw (NOAA
ESRL), and the SENEX and TES science teams for providing observations,
and P. Punttila (Ymparisto) and D.M. Sorger (NC State) for entomological
insights. The University of Washington participated in the BAECC
campaign with funds from the U.S. Department of Energy (DE-SC0006867).
S. Schobesberger acknowledges support from the European Commission
(OXFLUX, project 701958), D. Taipale from the European Regional
Development Fund (Centre of Excellence EcolChange), and D. B. M. from
NSF CAREER (1148951) and the Minnesota Supercomputing Institute. We
thank K. Cady-Pereira (AER), M. Shephard (Environment Canada), and M.
Luo (JPL) for developing TES HCOOH measurements, publicly available at
http://tes.jpl.nasa.gov/data/. GEOS-Chem model code is available at
www.geos-chem.org. SOSAA model output, the high-frequency HCOOH mixing
ratio measurements by CIMS, and anemometer wind measurements are
available at http://hdl.handle.net/1773/36867.
NR 68
TC 0
Z9 0
U1 11
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP
PY 2016
VL 43
IS 17
BP 9342
EP 9351
DI 10.1002/2016GL069599
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200062
ER
PT J
AU Zhou, DK
Liu, X
Larar, AM
Tian, JL
Smith, WL
Kizer, SH
Wu, W
Liu, QH
Goldberg, MD
AF Zhou, Daniel K.
Liu, Xu
Larar, Allen M.
Tian, Jialin
Smith, William L.
Kizer, Susan H.
Wu, Wan
Liu, Quanhua
Goldberg, Mitch D.
TI First Suomi NPP Cal/Val Campaign: Intercomparison of Satellite and
Aircraft Sounding Retrievals
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Atmospheric measurements; geophysical inverse problems; infrared
measurements; remote sensing
ID VALIDATION; EAQUATE; CLOUD
AB Satellite ultraspectral infrared sensors provide key data records essential for weather forecasting and climate change science. The Suomi National Polar-orbiting Partnership (NPP) satellite environmental data records (EDRs) are retrieved from calibrated ultraspectral radiance or sensor data records (SDRs). Understanding the accuracy of retrieved EDRs is critical. The first Suomi NPP Calibration/Validation Campaign was conducted during May 2013. The NASA high-altitude ER-2 aircraft carrying ultraspectral interferometer sounders such as the National Airborne Sounder Testbed-Interferometer (NAST-I) flew under the Suomi NPP satellite that carries the cross-track infrared sounder (CrIS) and the advanced technology microwave sounder (ATMS). Here, we intercompare the EDRs produced with different retrieval algorithms from SDRs measured from satellite and aircraft. The available dropsonde and radiosonde measurements together with the European Centre for Medium-Range Weather Forecasts (ECMWF) analysis are used to assess the results of this experiment. This study indicates that the CrIS/ATMS retrieval accuracy meets the Suomi NPP EDR requirement, except in the planetary boundary layer (PBL) where we have less confidence in meeting the requirement due to retrieval null-space error.
C1 [Zhou, Daniel K.; Liu, Xu; Larar, Allen M.; Tian, Jialin] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Smith, William L.; Kizer, Susan H.; Wu, Wan] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Liu, Quanhua; Goldberg, Mitch D.] NOAA, NESDIS, College Pk, MD 20740 USA.
RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM daniel.k.zhou@nasa.gov
FU NASA Headquarters; NASA Langley Research Center; NOAA NESDIS/JPSS
Program Office; NAST-I program
FX The authors greatly appreciate the contributions of NASA's Langley
Research Center and the U.K. Met Office. The authors would like to thank
NASA ER-2 aircraft pilots and crewmembers based at NASA's Armstrong
Flight Research Center for their dedication. The NAST-I program is
supported by NASA Headquarters, NASA Langley Research Center, and NOAA
NESDIS/JPSS Program Office. The authors would also like to thank Dr. A.
Gambacorta of NOAA NESDIS for useful discussion; and Dr. J. Kaye of
NASA's Science Mission Directorate for his continued, enabling support
of the NAST-I program.
NR 21
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U1 2
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD SEP
PY 2016
VL 9
IS 9
BP 4037
EP 4046
DI 10.1109/JSTARS.2016.2516765
PG 10
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DY6NW
UT WOS:000385245000005
ER
PT J
AU Selvakumaran, R
Veenadhari, B
Akiyama, S
Pandya, M
Gopalswamy, N
Yashiro, S
Kumar, S
Makela, P
Xie, H
AF Selvakumaran, R.
Veenadhari, B.
Akiyama, S.
Pandya, Megha
Gopalswamy, N.
Yashiro, S.
Kumar, Sandeep
Maekelae, P.
Xie, H.
TI On the reduced geoeffectiveness of solar cycle 24: A moderate storm
perspective
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE moderate storms; solar source identification; reduced geoeffectiveness
ID CORONAL MASS EJECTIONS; INTENSE GEOMAGNETIC STORMS; DST
LESS-THAN-OR-EQUAL-TO-50 NT; MAGNETIC STORMS; RING CURRENT;
INTERPLANETARY ORIGIN; INTERACTION REGIONS; SPACE WEATHER; TAIL CURRENT;
MAIN PHASE
AB The moderate and intense geomagnetic storms are identified for the first 77months of solar cycles 23 and 24. The solar sources responsible for the moderate geomagnetic storms are indentified during the same epoch for both the cycles. Solar cycle 24 has shown nearly 80% reduction in the occurrence of intense storms whereas it is only 40% in case of moderate storms when compared to previous cycle. The solar and interplanetary characteristics of the moderate storms driven by coronal mass ejection (CME) are compared for solar cycles 23 and 24 in order to see reduction in geoeffectiveness has anything to do with the occurrence of moderate storm. Though there is reduction in the occurrence of moderate storms, the Dst distribution does not show much difference. Similarly, the solar source parameters like CME speed, mass, and width did not show any significant variation in the average values as well as the distribution. The correlation between VBz and Dst is determined, and it is found to be moderate with value of 0.68 for cycle 23 and 0.61 for cycle 24. The magnetospheric energy flux parameter epsilon (epsilon) is estimated during the main phase of all moderate storms during solar cycles 23 and 24. The energy transfer decreased in solar cycle 24 when compared to cycle 23. These results are significantly different when all geomagnetic storms are taken into consideration for both the solar cycles.
C1 [Selvakumaran, R.; Veenadhari, B.; Pandya, Megha; Kumar, Sandeep] Indian Inst Geomagnetism, New Panvel, India.
[Akiyama, S.; Gopalswamy, N.; Yashiro, S.; Maekelae, P.; Xie, H.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD USA.
[Akiyama, S.; Yashiro, S.; Maekelae, P.; Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Selvakumaran, R (reprint author), Indian Inst Geomagnetism, New Panvel, India.
EM selva2986@gmail.com
FU NASA's LWS TRT program
FX R. Selvakumaran benefited from the SCOSTEP Visiting Scholar Program,
under which he visited NASA Goddard Space Flight Center, where this
research was performed. Authors from Indian Institute of Geomagnetism
(IIG) are grateful to Director, IIG, for support and encouragement to
carry out the work. We thank the ACE, Wind, and OMNIWeb teams for
providing the solar wind data. We acknowledge the use of solar imagery
from SDO, SOHO, and STEREO missions. This work greatly benefited from
the open data policy of NASA. The work of N.G., S.A., S.Y., P.M., and
H.X. was supported by NASA's LWS TR&T program.
NR 76
TC 0
Z9 0
U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8188
EP 8202
DI 10.1002/2016JA022885
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000003
ER
PT J
AU Neugebauer, M
Reisenfeld, D
Richardson, IG
AF Neugebauer, Marcia
Reisenfeld, Daniel
Richardson, Ian G.
TI Comparison of algorithms for determination of solar wind regimes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind
ID CORONAL MASS EJECTIONS; COROTATING INTERACTION REGIONS; STREAM
INTERFACES; QUASI-STATIONARY; EARTH; SPACECRAFT; MISSION; CLOUDS; MATTER
AB This study compares the designation of different solar wind flow regimes (transient, coronal hole, and streamer belt) according to two algorithms derived from observations by the Solar Wind Ion Composition Spectrometer, the Solar Wind Electron Proton Alpha Monitor, and the Magnetometer on the ACE spacecraft, with a similar regime determination performed on board the Genesis spacecraft. The comparison is made for the interval from late 2001 to early 2004 when Genesis was collecting solar wind ions for return to Earth. The agreement between hourly regime assignments from any pair of algorithms was less than two thirds, while the simultaneous agreement between all three algorithms was only 49%. When the results of the algorithms were compared to a catalog of interplanetary coronal mass ejection events, it was found that almost all the events in the catalog were confirmed by the spacecraft algorithms. On the other hand, many short transient events, lasting 1 to 13h, that were unanimously selected as transient like by the algorithms, were not included in the catalog.
C1 [Neugebauer, Marcia] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Reisenfeld, Daniel] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA.
[Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Neugebauer, M (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM mneugeb@lpl.arizona.edu
FU ACE mission; NSF; NASA Laboratory Analysis of Returned Samples (LARS)
program [NNX15AG19G]
FX The Genesis, SWICS, SWEPAM, and MAG parameters are all available at
http://cdaweb.gsfc.nasa.gov and other sites listed in the text. The
times of Genesis collector (regime) changes are available in the
supporting information of the paper by Reisenfeld et al. [2013]. I.G.R.
acknowledges support from the ACE mission. The Thule neutron monitor of
the Bartol Research Institute is supported by NSF. D.B.R. acknowledges
support from the NASA Laboratory Analysis of Returned Samples (LARS)
program, grant NNX15AG19G.
NR 35
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8215
EP 8227
DI 10.1002/2016JA023142
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000005
ER
PT J
AU Chamberlin, PC
Gong, Q
AF Chamberlin, Phillip C.
Gong, Qian
TI An integral field spectrograph utilizing mirrorlet arrays
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Heliophysics; instrumentation; EUV; solar; photons; solar eruptive
events
ID IMAGING SPECTROMETER; SOLAR; REGION; 3D
AB An integral field spectrograph (IFS) has been developed that utilizes a new and novel optical design to observe two spatial dimensions simultaneously with one spectral dimension. This design employs an optical 2-D array of reflecting and focusing mirrorlets. This mirrorlet array is placed at the imaging plane of the front-end telescope to generate a 2-D array of tiny spots replacing what would be the slit in a traditional slit spectrometer design. After the mirrorlet in the optical path, a grating on a concave mirror surface will image the spot array and provide high-resolution spectrum for each spatial element at the same time; therefore, the IFS simultaneously obtains the 3-D data cube of two spatial and one spectral dimensions. The new mirrorlet technology is currently in-house and undergoing laboratory testing at NASA Goddard Space Flight Center. Section 1 describes traditional classes of instruments that are used in Heliophysics missions and a quick introduction to the new IFS design. Section 2 discusses the details of the most generic mirrorlet IFS, while section 3 presents test results of a lab-based instrument. An example application to a Heliophysics mission to study solar eruptive events in extreme ultraviolet wavelengths is presented in section 4 that has high spatial resolution (0.5arcsecpixels) in the two spatial dimensions and high spectral resolution (66m angstrom) across a 15 angstrom spectral window. Section 4 also concludes with some other optical variations that could be employed on the more basic IFS for further capabilities of this type of instrument.
C1 [Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Gong, Qian] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD USA.
RP Chamberlin, PC (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM Phillip.C.Chamberlin@NASA.gov
RI Chamberlin, Phillip/C-9531-2012
OI Chamberlin, Phillip/0000-0003-4372-7405
FU NASA Goddard Space Flight Center's Internal Research and Development
(IRAD) program
FX This work was support under NASA Goddard Space Flight Center's Internal
Research and Development (IRAD) program. The authors would like to thank
RPC Photonics for producing the mirrorlet array. No data were used in
producing this manuscript.
NR 25
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8250
EP 8259
DI 10.1002/2016JA022487
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000008
ER
PT J
AU Poh, G
Slavin, JA
Jia, XZ
DiBraccio, GA
Raines, JM
Imber, SM
Gershman, DJ
Sun, WJ
Anderson, BJ
Korth, H
Zurbuchen, TH
McNutt, RL
Solomon, SC
AF Poh, Gangkai
Slavin, James A.
Jia, Xianzhe
DiBraccio, Gina A.
Raines, Jim M.
Imber, Suzanne M.
Gershman, Daniel J.
Sun, Wei-Jie
Anderson, Brian J.
Korth, Haje
Zurbuchen, Thomas H.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of cusp plasma filaments at Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE cusp filaments; Mercury; reconnection
ID FLUX-TRANSFER EVENTS; MAGNETIC-FIELD; SOLAR-WIND; MAGNETOPAUSE
RECONNECTION; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERE; INSTRUMENT; MODEL;
HOLES; SHEAR
AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft while in orbit about Mercury observed highly localized, similar to 3-s-long reductions in the dayside magnetospheric magnetic field, with amplitudes up to 90% of the ambient intensity. These magnetic field depressions are termed cusp filaments because they were observed from just poleward of the magnetospheric cusp to midlatitudes, i.e., similar to 55 degrees to 85 degrees N. We analyzed 345 high- and low-altitude cusp filaments identified from MESSENGER magnetic field data to determine their physical properties. Minimum variance analysis indicates that most filaments resemble cylindrical flux tubes within which the magnetic field intensity decreases toward its central axis. If the filaments move over the spacecraft at an estimated magnetospheric convection speed of similar to 35km/s, then they have a typical diameter of similar to 105km or similar to 7gyroradii for 1keVH(+) ions in a 300nT magnetic field. During these events, MESSENGER's Fast Imaging Plasma Spectrometer observed H+ ions with magnetosheath-like energies. MESSENGER observations during the spacecraft's final low-altitude campaign revealed that these cusp filaments likely extend down to Mercury's surface. We calculated an occurrence-rate-normalized integrated particle precipitation rate onto the surface from all filaments of (2.700.09)x10(25)s(-1). This precipitation rate is comparable to published estimates of the total precipitation rate in the larger-scale cusp. Overall, the MESSENGER observations analyzed here suggest that cusp filaments are the magnetospheric extensions of the flux transfer events that form at the magnetopause as a result of localized magnetic reconnection.
C1 [Poh, Gangkai; Slavin, James A.; Jia, Xianzhe; Raines, Jim M.; Imber, Suzanne M.; Gershman, Daniel J.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[DiBraccio, Gina A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
[Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England.
[Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Sun, Wei-Jie] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China.
[Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] 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 Poh, G (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM gangkai@umich.edu
RI Jia, Xianzhe/C-5171-2012; Slavin, James/H-3170-2012
OI Jia, Xianzhe/0000-0002-8685-1484; Slavin, James/0000-0002-9206-724X
FU NASA [NASW-00002, NAS5-97271, NNX15K88G, NNX15AL01G]; Living With a Star
Program [NNX16AJ67G]; Solar System Workings Program [NNX15AH28G]
FX Conversations with J. C. Kasper on the identification method used here
are appreciated. We also thank two anonymous reviewers for constructive
comments on an earlier draft. 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. All data analyzed in this paper are archived
with the NASA Planetary Data System. Further support was provided by
NASA Discovery Data Analysis Program grants NNX15K88G and NNX15AL01G,
Living With a Star Program grant NNX16AJ67G, and Solar System Workings
Program grant NNX15AH28G to the University of Michigan.
NR 58
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8260
EP 8285
DI 10.1002/2016JA022552
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000009
ER
PT J
AU Fennell, JF
Blake, JB
Claudepierre, S
Mazur, J
Kanekal, S
O'Brien, P
Baker, D
Crain, W
Mabry, D
Clemmons, J
AF Fennell, J. F.
Blake, J. B.
Claudepierre, S.
Mazur, J.
Kanekal, S.
O'Brien, P.
Baker, D.
Crain, W.
Mabry, D.
Clemmons, J.
TI Current energetic particle sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE energetic particles; sensors
ID ALLEN PROBES OBSERVATIONS; RELATIVISTIC ELECTRONS; IMPENETRABLE BARRIER;
MAGNETOSONIC WAVES; RADIATION BELTS; STORM; PRECIPITATION; ACCELERATION;
PLASMASPHERE; ZONE
AB Several energetic particle sensors designed to make measurements in the current decade are described and their technology and capabilities discussed and demonstrated. Most of these instruments are already on orbit or approaching launch. These include the Magnetic Electron Ion Spectrometers (MagEIS) and the Relativistic Electron Proton Telescope (REPT) that are flying on the Van Allen Probes, the Fly's Eye Electron Proton Spectrometers (FEEPS) flying on the Magnetospheric Multiscale (MMS) mission, and Dosimeters flying on the AC6 Cubesat mission. We focus mostly on the electron measurement capability of these sensors while providing summary comments of their ion measurement capabilities if they have any.
C1 [Fennell, J. F.; Blake, J. B.; Claudepierre, S.; Mazur, J.; O'Brien, P.; Crain, W.; Mabry, D.; Clemmons, J.] Aerosp Corp, El Segundo, CA 90245 USA.
[Kanekal, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Baker, D.] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Fennell, JF (reprint author), Aerosp Corp, El Segundo, CA 90245 USA.
EM joseph.fennell@aero.org
OI Claudepierre, Seth/0000-0001-5513-5947; Clemmons,
James/0000-0002-5298-5222
FU Van Allen Probes ECT - JHU/APL [967399]; Southwest Research Institute
[792084N/E99017JD]; JHU/APL under NASA's prime [967399, NAS5-01072];
Research Opportunities in Space and Earth Science (ROSES)
[NNH12ZDA001N-GEO]; US Air Force SMC/AD (Space and Missile Systems
Center Advanced Systems and Development Directorate)
FX The development of the MagEIS and FEEPS sensors and the analysis of
their data were supported in part by Van Allen Probes ECT funding
provided by JHU/APL contract 967399 and by Southwest Research Institute
contract 792084N/E99017JD, respectively. The REPT sensor development at
LASP, University of Colorado, was supported by JHU/APL contract 967399
under NASA's prime contract NAS5-01072. CeREs is funded under the
NNH12ZDA001N-GEO for Research Opportunities in Space and Earth
Science-2012 (ROSES-2012). The AC6 bus was developed under the Aerospace
Corporation Multi-Program Acquisition Capability Enhancement Program,
and the AC6 dosimeter payload was funded by US Air Force SMC/AD (Space
and Missile Systems Center Advanced Systems and Development
Directorate). The Van Allen Probes ECT data are available at
http://www.rbsp-ect.lanl.gov/science/DataDirectories.php or from the
authors. The MMS/FEEPS data are available at
https://lasp.colorado.edu/mms/sdc/about/browse-wrapper/ or from the
authors.
NR 45
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8840
EP 8858
DI 10.1002/2016JA022588
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000044
ER
PT J
AU Peterson, WK
Thiemann, EMB
Eparvier, FG
Andersson, L
Fowler, CM
Larson, D
Mitchell, D
Mazelle, C
Fontenla, J
Evans, JS
Xu, SS
Liemohn, M
Bougher, S
Sakai, S
Cravens, TE
Elrod, MK
Benna, M
Mahaffy, P
Jakosky, B
AF Peterson, W. K.
Thiemann, E. M. B.
Eparvier, Francis G.
Andersson, Laila
Fowler, C. M.
Larson, Davin
Mitchell, Dave
Mazelle, Christian
Fontenla, Juan
Evans, J. Scott
Xu, Shaosui
Liemohn, Mike
Bougher, Stephen
Sakai, Shotaro
Cravens, T. E.
Elrod, M. K.
Benna, M.
Mahaffy, P.
Jakosky, Bruce
TI Photoelectrons and solar ionizing radiation at Mars: Predictions versus
MAVEN observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE photoelectron; observation; model; Mars; thermosphere
ID ELECTRON; IRRADIANCE; MODEL; CODE; EUV
AB Understanding the evolution of the Martian atmosphere requires knowledge of processes transforming solar irradiance into thermal energy well enough to model them accurately. Here we compare Martian photoelectron energy spectra measured at periapsis by Mars Atmosphere and Volatile Evolution MissioN (MAVEN) with calculations made using three photoelectron production codes and three solar irradiance models as well as modeled and measured CO2 densities. We restricted our comparisons to regions where the contribution from solar wind electrons and ions were negligible. The two intervals examined on 19 October 2014 have different observed incident solar irradiance spectra. In spite of the differences in photoionization cross sections and irradiance spectra used, we find the agreement between models to be within the combined uncertainties associated with the observations from the MAVEN neutral density, electron flux, and solar irradiance instruments.
C1 [Peterson, W. K.; Thiemann, E. M. B.; Eparvier, Francis G.; Andersson, Laila; Fowler, C. M.; Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Larson, Davin; Mitchell, Dave; Xu, Shaosui] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
[Mazelle, Christian] Univ Toulouse, IRAP, UPS OMP, Toulouse, France.
[Mazelle, Christian] CNRS, IRAP, Toulouse, France.
[Fontenla, Juan] Northwest Res Associates, Boulder, CO USA.
[Evans, J. Scott] Computat Phys Inc, Springfield, VA USA.
[Xu, Shaosui; Liemohn, Mike; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Sakai, Shotaro; Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Elrod, M. K.; Benna, M.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Elrod, M. K.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
RP Peterson, WK (reprint author), Univ Colorado, LASP, Boulder, CO 80309 USA.
EM bill.peterson@lasp.colorado.edu
RI Peterson, WK/A-8706-2009;
OI Peterson, WK/0000-0002-1513-6096; EPARVIER, FRANCIS/0000-0001-7143-2730;
Sakai, Shotaro/0000-0001-9135-2076
FU CNES; NASA's Planetary Science Division
FX We thank the MAVEN team for providing spacecraft instruments capable of
returning the exceptionally good data used in this report. Input values
used for the models are available on request from the lead author. Work
related to observations with the SWEA instrument was partially supported
by CNES. This research was supported by NASA's Planetary Science
Division.
NR 30
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U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8859
EP 8870
DI 10.1002/2016JA022677
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000045
ER
PT J
AU Verkhoglyadova, OP
Tsurutani, BT
Mannucci, AJ
Mlynczak, MG
Hunt, LA
Paxton, LJ
Komjathy, A
AF Verkhoglyadova, O. P.
Tsurutani, B. T.
Mannucci, A. J.
Mlynczak, M. G.
Hunt, L. A.
Paxton, L. J.
Komjathy, A.
TI Solar wind driving of ionosphere-thermosphere responses in three storms
near St. Patrick's Day in 2012, 2013, and 2015
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ionosphere; thermosphere; coupling; solar wind; ICME; geomagnetic storm
ID ULTRAVIOLET IMAGER GUVI; GEOMAGNETIC STORMS; MAGNETIC STORMS; MASS
EJECTIONS; LOW-LATITUDE; CAWSES II; SUBSTORMS; SHOCKS; ELECTRODYNAMICS;
PROMINENCE
AB We identify interplanetary plasma regions associated with three intense interplanetary coronal mass ejections (ICMEs)-driven geomagnetic storm intervals which occurred around the same time of the year: day of year 74-79 (March) of 2012, 2013, and 2015. We show that differences in solar wind drivers lead to different dynamical ionosphere-thermosphere (IT) responses and to different preconditioning of the IT system. We introduce a new hourly based global metric for average low-latitude and northern middle-latitude vertical total electron content responses in the morning, afternoon, and evening local time ranges, derived from measurements from globally distributed Global Navigation Satellite System ground stations. Our novel technique of estimating nitric oxide (NO) cooling radiation in 11 degrees latitudinal zones is based on Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED)/Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) measurements. The thermospheric cooling throughout the storm phases is studied with this high latitudinal resolution for the first time. Additionally, TIMED/Global Ultraviolet Imager (GUVI) observations of the dynamical response of the thermospheric composition (O/N-2 ratio) are utilized to study negative ionospheric storm effects. Based on these data sets, we describe and quantify distinct IT responses to driving by ICME sheaths, magnetic clouds, coronal loop remnants, plasma discontinuities, and high-speed streams following ICMEs. Our analysis of coupling functions indicates strong connection between coupling with the solar wind and IT system response in ICME-type storms and also some differences. Knowledge of interplanetary features is crucial for understanding IT storm dynamics.
C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.; Komjathy, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Olga.Verkhoglyadova@jpl.nasa.gov
RI Paxton, Larry/D-1934-2015;
OI Paxton, Larry/0000-0002-2597-347X; Hunt, Linda/0000-0002-5330-541X
FU NASA TIMED project office
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. M.
Mlynczak and L. Paxton would like to acknowledge support from the NASA
TIMED project office. O. Verkhoglyadova would like to thank M. Butala
(now at University of Illinois at Urbana-Champaign) for help with TEC
data processing and E. Astafyeva for stimulating discussions. SABER data
are available at http://saber.gats-inc.com/. GUVI data are available at
http://timedguvi.jhuapl.edu. Solar wind parameters and activity indices
are taken from the OMNI database
(http://omniweb.gsfc.nasa.gov/form/omni_min.html). We acknowledge IGS
data service, Geoscience Australia
(ftp://ftp.ga.gov.au/geodesy-outgoing/gnss/pub/maps/argn_map.pdf) and
the Geospatial Information Authority of Japan for providing GEONET data
(http://www.gsi.go.jp/ENGLISH/page_e30233.html). ACE magnetometer data
were provided by the ACE Science Center through
http://www.srl.caltech.edu/ACE/ASC/level2/index.html.
NR 75
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U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8900
EP 8923
DI 10.1002/2016JA022883
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000048
ER
PT J
AU Zhou, YL
Luhr, H
Xiong, C
Pfaff, RF
AF Zhou, Yun-Liang
Luehr, Hermann
Xiong, Chao
Pfaff, Robert F.
TI Ionospheric storm effects and equatorial plasma irregularities during
the 17-18 March 2015 event
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ionospheric storms; equatorial plasma irregularities; prompt penetration
electric field; disturbance dynamo electric field
ID PATRICKS DAY STORM; GEOMAGNETIC STORMS; ELECTRIC-FIELDS; F-REGION;
THERMOSPHERIC DYNAMICS; TOPSIDE IONOSPHERE; CHAMP OBSERVATIONS; BUBBLE
OCCURRENCE; MAGNETIC STORM; LOW LATITUDES
AB The intense magnetic storm on 17-18 March 2015 caused large disturbances of the ionosphere. Based on the plasma density (Ni) observations performed by the Swarm fleet of satellites, the Gravity Recovery and Climate Experiment mission, and the Communications/Navigation Outage Forecasting System satellite, we characterize the storm-related perturbations at low latitudes. All these satellites sampled the ionosphere in morning and evening time sectors where large modifications occurred. Modifications of plasma density are closely related to changes of the solar wind merging electric field (E-m). We consider two mechanisms, prompt penetration electric field (PPEF) and disturbance dynamo electric field (DDEF), as the main cause for the Ni redistribution, but effects of meridional wind are also taken into account. At the start of the storm main phase, the PPEF is enhancing plasma density on the dayside and reducing it on the nightside. Later, DDEF takes over and causes the opposite reaction. Unexpectedly, there appears during the recovery phase a strong density enhancement in the morning/prenoon sector and a severe Ni reduction in the afternoon/evening sector, and we suggest a combined effect of vertical plasma drift, and meridional wind is responsible for these ionospheric storm effects. Different from earlier studies about this storm, we also investigate the influence of storm dynamics on the initiation of equatorial plasma irregularities (EPIs). Shortly after the start of the storm main phase, EPIs appear in the postsunset sector. As a response to a short-lived decline of E-m, EPI activity appears in the early morning sector. Following the second start of the main phase, EPIs are generated for a few hours in the late evening sector. However, for the rest of the storm main phase, no more EPIs are initiated for more than 12h. Only after the onset of recovery phase does EPI activity start again in the postmidnight sector, lasting more than 7h. This comprehensive view of ionospheric storm effects and plasma irregularities adds to our understanding of conditions that lead to ionospheric instabilities.
C1 [Zhou, Yun-Liang] Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan, Peoples R China.
[Zhou, Yun-Liang; Luehr, Hermann; Xiong, Chao] GFZ German Res Ctr Geosci, Potsdam, Germany.
[Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
RP Luhr, H (reprint author), GFZ German Res Ctr Geosci, Potsdam, Germany.
EM hluehr@gfz-potsdam.de
RI Barbosa, Flavio/G-3630-2013
FU Space Agency of the German Aerospace Center (DLR) through funds of the
Federal Ministry of Economics and Technology; National Nature Science
Foundation of China [41274194, 41431073]; China Scholarship Council
[201506275011]
FX The European Space Agency (ESA) is acknowledged for providing the Swarm
data. The electron density is obtained from http://earth.esa.int/swarm.
The GRACE mission is sponsored by the Space Agency of the German
Aerospace Center (DLR) through funds of the Federal Ministry of
Economics and Technology. The GRACE data are available at the
Information System and Data Center (ISDC) of GFZ German Research Centre
for Geosciences. Data set names are as follows: GA-OG-1B-NAVSOL,
GB-OG-1B-NAVSOL, and GX-OG-1B-KBRDAT. The solar wind and interplanetary
magnetic field data are derived from NASA's ACE mission, and they can be
found at http://www.srl.caltech.edu/ACE/ASC/level2/. The SYMH data are
provided by the World Data Center for Geomagnetism, Kyoto, and
downloaded from http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html. The
global ionospheric maps (GIM) are available from
ftp://cddis.gsfc.nasa.gov/gps/products/ionex/. The work of YunLiang Zhou
is supported by the National Nature Science Foundation of China
(41274194 and 41431073) and China Scholarship Council (201506275011).
NR 58
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U1 6
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 9146
EP 9163
DI 10.1002/2016JA023122
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000065
ER
PT J
AU Qiu, JX
Crow, WT
Nearing, GS
AF Qiu, Jianxiu
Crow, Wade T.
Nearing, Grey S.
TI The Impact of Vertical Measurement Depth on the Information Content of
Soil Moisture for Latent Heat Flux Estimation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID NEAR-SURFACE; ERS SCATTEROMETER; ASSIMILATION; VALIDATION; VEGETATION;
PRODUCTS; QUALITY
AB This study aims to identify the impact of vertical support on the information content of soil moisture (SM) for latent heat flux estimation. This objective is achieved via calculation of the mutual information (MI) content between multiple soil moisture variables (with different vertical supports) and current/future evaporative fraction (EF) using ground-based soil moisture and latent/sensible heat flux observations acquired from the AmeriFlux network within the contiguous United States. Through the intercomparison of MI results from different SM-EF pairs, the general value (for latent heat flux estimation) of superficial soil moisture observations theta(S), vertically integrated soil moisture observations theta(V), and vertically extrapolated soil moisture time series [soil wetness index (SWI) from a simple low-pass transformation of theta(S)] are examined. Results suggest that, contrary to expectations, 2-day averages of theta(S) and theta(V) have comparable mutual information with regards to EF. That is, there is no clear evidence that the information content for flux estimation is enhanced via deepening the vertical support of superficial soil moisture observations. In addition, the utility of SWI in monitoring and forecasting EF is partially dependent on the adopted parameterization of time-scale parameter T in the exponential filter. Similar results are obtained when analyses are conducted at the monthly time scale, only with larger error bars. The contrast between the results of this paper and past work focusing on utilizing soil moisture to predict vegetation condition demonstrates that the particular application should be considered when characterizing the information content of soil moisture time series measurements.
C1 [Qiu, Jianxiu] Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China.
[Crow, Wade T.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD USA.
[Nearing, Grey S.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA.
RP Qiu, JX (reprint author), Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China.
EM qiujianxiu@mail.sysu.edu.cn
FU National Natural Science Foundation of China [41501450]; Natural Science
Foundation of Guangdong Province, China [2016A030310154]; Fundamental
Research Funds for the Central Universities [16lgpy06]
FX This work was supported by National Natural Science Foundation of China
(Grant 41501450), Natural Science Foundation of Guangdong Province,
China (Grant 2016A030310154), and the Fundamental Research Funds for the
Central Universities (16lgpy06). We thank the anonymous reviewers for
their helpful comments.
NR 31
TC 1
Z9 1
U1 3
U2 3
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 SEP
PY 2016
VL 17
IS 9
BP 2419
EP 2430
DI 10.1175/JHM-D-16-0044.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY8YZ
UT WOS:000385419800005
ER
PT J
AU Tan, J
Petersen, WA
Tokay, A
AF Tan, Jackson
Petersen, Walter A.
Tokay, Ali
TI A Novel Approach to Identify Sources of Errors in IMERG for GPM Ground
Validation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID MULTISATELLITE PRECIPITATION ANALYSIS; UNCERTAINTY QUANTIFICATION;
PASSIVE MICROWAVE; UNITED-STATES; ANALYSIS TMPA; DAY-1 IMERG; REAL-TIME;
PRODUCTS; RESOLUTION; RAINFALL
AB The comparison of satellite and high-quality, ground-based estimates of precipitation is an important means to assess the confidence in satellite-based algorithms and to provide a benchmark for their continued development and future improvement. To these ends, it is beneficial to identify sources of estimation uncertainty, thereby facilitating a precise understanding of the origins of the problem. This is especially true for new datasets such as the Integrated Multisatellite Retrievals for GPM(IMERG) product, which provides global precipitation gridded at a high resolution using measurements from different sources and techniques. Here, IMERG is evaluated against a dense network of gauges in the mid-Atlantic region of the United States. A novel approach is presented, leveraging ancillary variables in IMERG to attribute the errors to the individual instruments or techniques within the algorithm. As a whole, IMERG exhibits some misses and false alarms for rain detection, while its rain-rate estimates tend to overestimate drizzle and underestimate heavy rain with considerable random error. Tracing the errors to their sources, the most reliable IMERG estimates come from passive microwave satellites, which in turn exhibit a hierarchy of performance. The morphing technique has comparable proficiency with the less skillful satellites, but infrared estimations perform poorly. The approach here demonstrated that, underlying the overall reasonable performance of IMERG, different sources have different reliability, thus enabling both IMERG users and developers to better recognize the uncertainty in the estimate. Future validation efforts are urged to adopt such a categorization to bridge between gridded rainfall and instantaneous satellite estimates.
C1 [Tan, Jackson] Univ Space Res Assoc, Greenbelt, MD USA.
[Tan, Jackson; Tokay, Ali] NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Petersen, Walter A.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Tan, J (reprint author), NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM jackson.tan@nasa.gov
RI Measurement, Global/C-4698-2015;
OI Tan, Jackson/0000-0001-7085-3074
FU GPM Mission; PMM Science Team
FX We thank George Huffman and David Bolvin for informative discussions on
IMERG and Yudong Tian for instructive consultation on the multiplicative
error model. The gauge data are maintained by the NASA Wallops GPM GV
Team, and we acknowledge David Wolff for his assistance with the data.
The MRMS data were processed for the GPM GV Program by Pierre-Emmanuel
Kirstetter, and we appreciate the further assistance provided by Jianxin
Wang. We also thank two anonymous reviewers for their comments and
suggestions. J.T. is supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by
Universities Space Research Association through a contract with NASA.
W.A.P. and A.T. acknowledge support from the GPM Mission (Project
Scientist, Gail S. Jackson, and GV Systems Manager, Mathew Schwaller)
and also PMM Science Team funding provided by Dr. Ramesh Kakar. The
IMERG data were provided by the NASA Goddard Space Flight Center's PMM
and PPS teams, which develop and compute the IMERG as a contribution to
GPM, and archived at the NASA GES DISC. All codes used in this analysis
are freely available at
https://github.com/JacksonTanBS/2016_Tan-et-al._JHM.
NR 52
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U1 10
U2 10
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 SEP
PY 2016
VL 17
IS 9
BP 2477
EP 2491
DI 10.1175/JHM-D-16-0079.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY8YZ
UT WOS:000385419800008
ER
PT J
AU Righter, K
Cosca, MA
Morgan, LE
AF Righter, K.
Cosca, M. A.
Morgan, L. E.
TI Preservation of ancient impact ages on the R chondrite parent body:
Ar-40/Ar-39 age of hornblende-bearing R chondrite LAP 04840
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID INNER SOLAR-SYSTEM; RUMURUTI CHONDRITE; EXPOSURE AGES; HISTORY;
MINERALOGY; METEORITE; AMPHIBOLE; SHOCK; ABUNDANCES; CHRONOLOGY
AB The hornblende- and biotite-bearing R chondrite LAP 04840 is a rare kind of meteorite possibly containing outer solar system water stored during metamorphism or postshock annealing deep within an asteroid. Because little is known regarding its age and origin, we determined Ar-40/Ar-39 ages on hornblende-rich separates of the meteorite, and obtained plateau ages of 4340(+/- 40) to 4380(+/- 30) Ma. These well-defined plateau ages, coupled with evidence for postshock annealing, indicate this meteorite records an ancient shock event and subsequent annealing. The age of 4340-4380Ma (or 4.34-4.38Ga) for this and other previously dated R chondrites is much older than most impact events recorded by ordinary chondrites and points to an ancient event or events that predated the late heavy bombardment that is recorded in so many meteorites and lunar samples.
C1 [Righter, K.] NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
[Cosca, M. A.; Morgan, L. E.] US Geol Survey, Denver Fed Ctr, MS 963, Denver, CO 80225 USA.
RP Righter, K (reprint author), NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP from NASA Cosmochemistry program; NSF; NASA
FX Funding for this study was provided by an RTOP to KR from the NASA
Cosmochemistry program. U.S. Antarctic meteorite samples are recovered
by the Antarctic Search for Meteorites (ANSMET) program which has been
funded by NSF and NASA, and characterized and curated by the Department
of Mineral Sciences of the Smithsonian Institution and Astromaterials
Curation Office at NASA Johnson Space Center. Any use of trade, product,
or firm names is for descriptive purposes only and does not imply
endorsement by the U.S. government. Reviews by J. Park, M. McCanta, and
comments of AE Yamaguchi helped to improve presentation of our results.
NR 47
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2016
VL 51
IS 9
BP 1678
EP 1684
DI 10.1111/maps.12692
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DW4QX
UT WOS:000383629200008
ER
PT J
AU Pugh, TAM
Muller, C
Elliott, J
Deryng, D
Folberth, C
Olin, S
Schmid, E
Arneth, A
AF Pugh, T. A. M.
Mueller, C.
Elliott, J.
Deryng, D.
Folberth, C.
Olin, S.
Schmid, E.
Arneth, A.
TI Climate analogues suggest limited potential for intensification of
production on current croplands under climate change
SO NATURE COMMUNICATIONS
LA English
DT Article
ID RISING CO2 CONCENTRATIONS; CROP YIELD; IMPACTS; FOOD; AGRICULTURE;
MANAGEMENT; MODEL
AB Climate change could pose a major challenge to efforts towards strongly increase food production over the coming decades. However, model simulations of future climate-impacts on crop yields differ substantially in the magnitude and even direction of the projected change. Combining observations of current maximum-attainable yield with climate analogues, we provide a complementary method of assessing the effect of climate change on crop yields. Strong reductions in attainable yields of major cereal crops are found across a large fraction of current cropland by 2050. These areas are vulnerable to climate change and have greatly reduced opportunity for agricultural intensification. However, the total land area, including regions not currently used for crops, climatically suitable for high attainable yields of maize, wheat and rice is similar by 2050 to the present-day. Large shifts in land-use patterns and crop choice will likely be necessary to sustain production growth rates and keep pace with demand.
C1 [Pugh, T. A. M.; Arneth, A.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany.
[Pugh, T. A. M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
[Pugh, T. A. M.] Univ Birmingham, Birmingham Inst Forest Res, Birmingham B15 2TT, W Midlands, England.
[Mueller, C.] Potsdam Inst Climate Impact Res, POB 60 12 03, D-14412 Potsdam, Germany.
[Elliott, J.; Deryng, D.] Univ Chicago, Chicago, IL 60637 USA.
[Elliott, J.; Deryng, D.] Argonne Natl Lab, Computat Inst, Chicago, IL 60637 USA.
[Deryng, D.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Deryng, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Folberth, C.] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program, A-2361 Laxenburg, Austria.
[Folberth, C.] Univ Munich, Dept Geog, D-80333 Munich, Germany.
[Olin, S.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Schmid, E.] Univ Nat Resources & Life Sci, Dept Econ & Social Sci, Feistmantelstr 4, A-1180 Vienna, Austria.
RP Pugh, TAM (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany.
EM t.a.m.pugh@bham.ac.uk
RI Deryng, Delphine/F-7417-2010; Pugh, Thomas/A-3790-2010;
OI Deryng, Delphine/0000-0001-6214-7241; Pugh, Thomas/0000-0002-6242-7371;
Schmid, Erwin/0000-0003-4783-9666; Muller, Christoph/0000-0002-9491-3550
FU European Commission [603542 (LUC4C)]; German Federal Ministry of
Education and Research (BMBF), through the Helmholtz Association; MACMIT
project - BMBF [01LN1317A]; Research Fellowship of Ludwig Maximilian
University Munich; Global Gridded Crop Model Intercomparison project
(GGCMI) of the Agricultural Model Intercomparison and Improvement
Project (AgMIP)
FX T.A.M.P. and A.A. were funded by the European Commission's 7th Framework
Programme, under Grant Agreement number 603542 (LUC4C). This work was
supported, in part, by the German Federal Ministry of Education and
Research (BMBF), through the Helmholtz Association and its research
program ATMO. C.M. acknowledges financial support from the MACMIT
project (01LN1317A) funded through the BMBF. C.F. was supported by a
Research Fellowship of Ludwig Maximilian University Munich. We
acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modelling groups for producing and making available their model
output. The Global Gridded Crop Model Intercomparison project (GGCMI) of
the Agricultural Model Intercomparison and Improvement Project (AgMIP)
is thanked for funding travel to workshops where the ideas in this
manuscript were developed. This is paper number 17 of the Birmingham
Institute of Forest Research.
NR 34
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U2 9
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD SEP
PY 2016
VL 7
AR 12608
DI 10.1038/ncomms12608
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY7BH
UT WOS:000385283700001
PM 27646707
ER
PT J
AU Wang, ZC
Monteiro, CD
Jagodnik, KM
Fernandez, NF
Gundersen, GW
Rouillard, AD
Jenkins, SL
Feldmann, AS
Hu, KS
McDermott, MG
Duan, QN
Clark, NR
Jones, MR
Kou, Y
Goff, T
Woodland, H
Amaral, FMR
Szeto, GL
Fuchs, O
Rose, SMSF
Sharma, S
Schwartz, U
Bausela, XB
Szymkiewicz, M
Maroulis, V
Salykin, A
Barra, CM
Kruth, CD
Bongio, NJ
Mathur, V
Todoric, RD
Rubin, UE
Malatras, A
Fulp, CT
Galindo, JA
Motiejunaite, R
Juschke, C
Dishuck, PC
Lahl, K
Jafari, M
Aibar, S
Zaravinos, A
Steenhuizen, LH
Allison, LR
Gamallo, P
Segura, FD
Devlin, TD
Perez-Garcia, V
Ma'ayan, A
AF Wang, Zichen
Monteiro, Caroline D.
Jagodnik, Kathleen M.
Fernandez, Nicolas F.
Gundersen, Gregory W.
Rouillard, Andrew D.
Jenkins, Sherry L.
Feldmann, Axel S.
Hu, Kevin S.
McDermott, Michael G.
Duan, Qiaonan
Clark, Neil R.
Jones, Matthew R.
Kou, Yan
Goff, Troy
Woodland, Holly
Amaral, Fabio M. R.
Szeto, Gregory L.
Fuchs, Oliver
Rose, Sophia M. Schussler-Fiorenza
Sharma, Shvetank
Schwartz, Uwe
Bengoetxea Bausela, Xabier
Szymkiewicz, Maciej
Maroulis, Vasileios
Salykin, Anton
Barra, Carolina M.
Kruth, Candice D.
Bongio, Nicholas J.
Mathur, Vaibhav
Todoric, Radmila D.
Rubin, Udi E.
Malatras, Apostolos
Fulp, Carl T.
Galindo, John A.
Motiejunaite, Ruta
Jueschke, Christoph
Dishuck, Philip C.
Lahl, Katharina
Jafari, Mohieddin
Aibar, Sara
Zaravinos, Apostolos
Steenhuizen, Linda H.
Allison, Lindsey R.
Gamallo, Pablo
de Andres Segura, Fernando
Devlin, Tyler Dae
Perez-Garcia, Vicente
Ma'ayan, Avi
TI Extraction and analysis of signatures from the Gene Expression Omnibus
by the crowd
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FACIOSCAPULOHUMERAL MUSCULAR-DYSTROPHY; ENDOMETRIAL CANCER-RISK;
ESTROGEN-RECEPTOR; HEPATOCELLULAR-CARCINOMA; DIFFERENTIAL EXPRESSION;
DATABASE; DISEASE; DISCOVERY; INSULIN; GROWTH
AB Gene expression data are accumulating exponentially in public repositories. Reanalysis and integration of themed collections from these studies may provide new insights, but requires further human curation. Here we report a crowdsourcing project to annotate and reanalyse a large number of gene expression profiles from Gene Expression Omnibus (GEO). Through a massive open online course on Coursera, over 70 participants from over 25 countries identify and annotate 2,460 single-gene perturbation signatures, 839 disease versus normal signatures, and 906 drug perturbation signatures. All these signatures are unique and are manually validated for quality. Global analysis of these signatures confirms known associations and identifies novel associations between genes, diseases and drugs. The manually curated signatures are used as a training set to develop classifiers for extracting similar signatures from the entire GEO repository. We develop a web portal to serve these signatures for query, download and visualization.
C1 [Wang, Zichen; Monteiro, Caroline D.; Jagodnik, Kathleen M.; Fernandez, Nicolas F.; Gundersen, Gregory W.; Rouillard, Andrew D.; Jenkins, Sherry L.; Feldmann, Axel S.; Hu, Kevin S.; McDermott, Michael G.; Duan, Qiaonan; Clark, Neil R.; Jones, Matthew R.; Kou, Yan; Goff, Troy; Ma'ayan, Avi] Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA.
[Jagodnik, Kathleen M.] NASA, Fluid Phys & Transport Processes Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Jagodnik, Kathleen M.] Baylor Coll Med, Ctr Space Med, 1 Baylor Plaza, Houston, TX 77030 USA.
[Woodland, Holly] Daylesford, Weybridge KT13 0RZ, Surrey, England.
[Amaral, Fabio M. R.] Univ Nottingham, Sch Biosci, Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England.
[Szeto, Gregory L.] MIT, Dept Biol Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, David H Koch Inst Integrat Canc Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, Dept Mat Sci & Engn, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, Ragon Inst MGH, 400 Technol Sq, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] Harvard, 400 Technol Sq, Cambridge, MA 02139 USA.
[Fuchs, Oliver] Univ Munich, German Ctr Lung Res DZL, Dr von Hauner Univ Childrens Hosp, Paediat Allergol & Pulmonol, Lindwurmstr 4, D-80337 Munich, Germany.
[Rose, Sophia M. Schussler-Fiorenza] Veteran Affairs Palo Alto Hlth Care Syst, Spinal Cord Injury Serv, Palo Alto, CA 94304 USA.
[Rose, Sophia M. Schussler-Fiorenza] Stanford Sch Med, Dept Neurosurg, Stanford, CA 94304 USA.
[Sharma, Shvetank] Inst Liver & Biliary Sci, Dept Res, D1 Vasant Kunj, New Delhi 110070, India.
[Schwartz, Uwe] Univ Regensburg, Dept Biochem 3, Univ Str 31, D-93053 Regensburg, Germany.
[Bengoetxea Bausela, Xabier] Univ Navarra, Dept Pharmacol & Toxicol, Irunlarrea 1, E-31008 Pamplona, Spain.
[Szymkiewicz, Maciej] Polish Acad Sci, Warsaw Sch Informat Technol Auspices, 6 Newelska St, PL-01447 Warsaw, Poland.
[Maroulis, Vasileios] Plomariou 1 St, Athens 15126, Greece.
[Salykin, Anton] Masaryk Univ, Fac Med, Dept Biol, Brno 62500, Czech Republic.
[Barra, Carolina M.] Hosp del Mar, IMIM, PRBB Barcelona, Dr Aiguader 88, Barcelona 08003, Spain.
[Kruth, Candice D.] 85 Hailey Ln,Apt C-11, Strasburg, VA 22657 USA.
[Bongio, Nicholas J.] Shenandoah Univ, Dept Biol, 1460 Univ Dr Winchester, Winchester, VA 22601 USA.
[Mathur, Vaibhav] IBM India Pvt Ltd, Bengaluru 560045, India.
[Todoric, Radmila D.] Dr Aleksandra Sijacica 20, Backa Topola 24300, Serbia.
[Rubin, Udi E.] Columbia Univ, Dept Biol Sci, 600 Fairchild Ctr,Mail Code 2402, New York, NY 10032 USA.
[Malatras, Apostolos] Univ Paris 04, Univ Paris 06, INSERM UMRS975, Ctr Res Myol,CNRS FRE3617, 47 Blvd Hop, F-75013 Paris, France.
[Fulp, Carl T.] 13-1,Higashi 4 Chome Shibuya Ku, Tokyo 1500011, Japan.
[Galindo, John A.] Univ Nacl Colombia, Dept Biol, Cr 30 45-08, Bogota, Colombia.
[Galindo, John A.] Univ Nacl Colombia, Inst Genet, Cr 30 45-08, Bogota, Colombia.
[Motiejunaite, Ruta] Brigham & Womens Hosp, Ctr Interdisciplinary Cardiovasc Sci, 3 Blackfan Circle, Boston, MA 02115 USA.
[Jueschke, Christoph] Carl von Ossietzky Univ Oldenburg, Fac Med & Hlth Sci, Dept Human Genet, Ammerlander Heerstr 114-118, D-26129 Oldenburg, Germany.
[Dishuck, Philip C.] 2312 40th ST NW 2, Washington, DC 20007 USA.
[Lahl, Katharina] Tech Univ Denmark, Natl Vet Inst, Bulowsvej 27 Bldg 2-3, DK-1870 Frederiksberg, Denmark.
[Jafari, Mohieddin] Pasteur Inst Iran, Biotechnol Res Ctr, Prot Chem & Prote Unit, 358,12th Farwardin Ave,Jomhhoori St, Tehran 13164, Iran.
[Jafari, Mohieddin] Inst Res Fundamental Sci, Sch Biol Sci, Niavaran Sq,POB, Tehran 193955746, Iran.
[Aibar, Sara] Univ Salamanca, Madrid 37008, Spain.
[Zaravinos, Apostolos] Karolinska Inst, Dept Lab Med, Div Clin Immunol, Alfred Nobels Alle 8,Level 7, SE-14186 Stockholm, Sweden.
[Zaravinos, Apostolos] European Univ Cyprus, Sch Sci, Dept Life Sci, 6 Diogenes Str Engomi,POB 22006, CY-1516 Nicosia, Cyprus.
[Steenhuizen, Linda H.] Anna Blamansingel 216, NL-102 SW Amsterdam, Netherlands.
[Allison, Lindsey R.] 7300 Brompton 6024, Houston, TX 77025 USA.
[Gamallo, Pablo] Aligustre 30 1-C, Madrid 28039, Spain.
[de Andres Segura, Fernando] Extremadura Univ Hosp, Clin Res Ctr, CICAB, Elvas Av,S-N 06006, Badajoz 06006, Spain.
[Devlin, Tyler Dae] 69 Brown St,Box 8278, Providence, RI 02912 USA.
[Perez-Garcia, Vicente] CSIC, Ctr Nacl Biotecnol, Dept Immunol & Oncol, C-Darwin 3, E-28049 Madrid, Spain.
RP Ma'ayan, A (reprint author), Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA.
EM avi.maayan@mssm.edu
OI Wang, Zichen/0000-0002-1415-1286; Szymkiewicz,
Maciej/0000-0003-1469-9396; Schussler-Fiorenza Rose, Sophia
Miryam/0000-0002-6311-6671; De Andres, Fernando/0000-0003-1076-0743
FU NIH [R01GM098316, U54HL127624, U54CA189201]
FX This work is supported by NIH grants: R01GM098316, U54HL127624 and
U54CA189201 to A.M.
NR 78
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U1 5
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 SEP
PY 2016
VL 7
AR 12846
DI 10.1038/ncomms12846
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY8FA
UT WOS:000385363000014
PM 27667448
ER
PT J
AU Kassemi, M
Thompson, D
AF Kassemi, Mohammad
Thompson, David
TI Prediction of renal crystalline size distributions in space using a PBE
analytic model. 1. Effect of microgravity-induced biochemical
alterations
SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY
LA English
DT Article
DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal
growth; agglomeration
ID URINARY STONE FORMATION; CALCIUM-OXALATE; RISK-FACTORS; GROWTH; DISEASE;
AGGLOMERATION; INHIBITION; ASTRONAUTS; KINETICS; KIDNEY
AB An analytical Population Balance Equation model is developed and used to assess the risk of critical renal stone formation for astronauts during future space missions. The model uses the renal biochemical profile of the subject as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating calcium oxalate crystals during their transit through the kidney. The model is verified through comparison with published results of several crystallization experiments. Numerical results indicate that the model is successful in clearly distinguishing between 1-G normal and 1-G recurrent stone-former subjects based solely on their published 24-h urine biochemical profiles. Numerical case studies further show that the predicted renal calculi size distribution for a microgravity astronaut is closer to that of a recurrent stone former on Earth rather than to a normal subject in 1 G. This interestingly implies that the increase in renal stone risk level in microgravity is relatively more significant for a normal person than a stone former. However, numerical predictions still underscore that the stone-former subject carries by far the highest absolute risk of critical stone formation during space travel.
C1 [Kassemi, Mohammad; Thompson, David] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA.
RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA.
EM Mohammad.Kassemi@nasa.gov
FU Exploration Medical Capabilities Element of NASA's Human Research
FX We gratefully acknowledge funding support from the Exploration Medical
Capabilities Element of NASA's Human Research.
NR 41
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U1 2
U2 2
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 1931-857X
EI 1522-1466
J9 AM J PHYSIOL-RENAL
JI Am. J. Physiol.-Renal Physiol.
PD SEP 1
PY 2016
VL 311
IS 3
BP F520
EP F530
DI 10.1152/ajprenal.00401.2015
PG 11
WC Physiology; Urology & Nephrology
SC Physiology; Urology & Nephrology
GA DY3FZ
UT WOS:000384977500004
PM 27279490
ER
PT J
AU Kassemi, M
Thompson, D
AF Kassemi, Mohammad
Thompson, David
TI Prediction of renal crystalline size distributions in space using a PBE
analytic model. 2. Effect of dietary countermeasures
SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY
LA English
DT Article
DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal
growth; agglomeration; inhibition; dietary countermeasures
ID OXALATE MONOHYDRATE CRYSTALLIZATION; POTASSIUM-MAGNESIUM CITRATE;
CALCIUM-OXALATE; STONE FORMATION; DIHYDRATE CRYSTALLIZATION; BED REST;
INHIBITION; GROWTH; URINE; FLIGHT
AB An analytic Population Balance Equation model is used to assess the efficacy of citrate, pyrophosphate, and augmented fluid intake as dietary countermeasures aimed at reducing the risk of renal stone formation for astronauts. The model uses the measured biochemical profile of the astronauts as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating renal calculi subject to biochemical changes brought about by administration of these dietary countermeasures. Numerical predictions indicate that an increase in citrate levels beyond its average normal ground-based urinary values is beneficial but only to a limited extent. Unfortunately, results also indicate that any decline in the citrate levels during space travel below its normal urinary values on Earth can easily move the astronaut into the stone-forming risk category. Pyrophosphate is found to be an effective inhibitor since numerical predictions indicate that even at quite small urinary concentrations, it has the potential of shifting the maximum crystal aggregate size to a much smaller and plausibly safer range. Finally, our numerical results predict a decline in urinary volume below 1.5 liters/day can act as a dangerous promoter of renal stone development in microgravity while urinary volume levels of 2.5-3 liters/day can serve as effective space countermeasures.
C1 [Kassemi, Mohammad; Thompson, David] NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
RP Kassemi, M (reprint author), NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
EM Mohammad.Kassemi@nasa.gov
FU Exploration Medical Capabilities Element of NASA's Human Research
Project
FX We gratefully acknowledge funding support from the Exploration Medical
Capabilities Element of NASA's Human Research Project.
NR 44
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U1 3
U2 3
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 1931-857X
EI 1522-1466
J9 AM J PHYSIOL-RENAL
JI Am. J. Physiol.-Renal Physiol.
PD SEP 1
PY 2016
VL 311
IS 3
BP F531
EP F538
DI 10.1152/ajprenal.00402.2015
PG 8
WC Physiology; Urology & Nephrology
SC Physiology; Urology & Nephrology
GA DY3FZ
UT WOS:000384977500005
PM 27279491
ER
PT J
AU Mukai, K
Luna, GJM
Cusumano, G
Segreto, A
Munari, U
Sokoloski, JL
Lucy, AB
Nelson, T
Nunez, NE
AF Mukai, K.
Luna, G. J. M.
Cusumano, G.
Segreto, A.
Munari, U.
Sokoloski, J. L.
Lucy, A. B.
Nelson, T.
Nunez, N. E.
TI SU Lyncis, a hard X-ray bright M giant: clues point to a large hidden
population of symbiotic stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: symbiotic; stars: individual: SU Lyn; X-rays: binaries
ID SWIFT-BAT; T CRB; HIPPARCOS; EVOLUTION; OUTBURST; CATALOG; BINARY; NOVAE
AB Symbiotic star surveys have traditionally relied almost exclusively on low resolution optical spectroscopy. However, we can obtain a more reliable estimate of their total Galactic population by using all available signatures of the symbiotic phenomenon. Here we report the discovery of a hard X-ray source, 4PBC J0642.9+5528, in the Swift hard X-ray all-sky survey, and identify it with a poorly studied red giant, SU Lyn, using pointed Swift observations and ground-based optical spectroscopy. The X-ray spectrum, the optical to UV spectrum, and the rapid UV variability of SU Lyn are all consistent with our interpretation that it is a symbiotic star containing an accreting white dwarf. The symbiotic nature of SU Lyn went unnoticed until now, because it does not exhibit emission lines strong enough to be obvious in low resolution spectra. We argue that symbiotic stars without shell-burning have weak emission lines, and that the current lists of symbiotic stars are biased in favour of shell-burning systems. We conclude that the true population of symbiotic stars has been underestimated, potentially by a large factor.
C1 [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Luna, G. J. M.] UBA, CONICET, IAFE, Ave Inte Guiraldes 2620,C1428ZAA, Buenos Aires, DF, Argentina.
[Cusumano, G.; Segreto, A.] INAF Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy.
[Munari, U.] INAF Astron Observ Padova, I-36012 Asiago, VI, Italy.
[Sokoloski, J. L.; Lucy, A. B.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Nelson, T.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Nunez, N. E.] UNSJ, ICATE, CONICET, Ave Espana S E-1512,J5402 DSP, San Juan, Argentina.
RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM Koji.Mukai@nasa.gov
FU NASA ADAP grant [NNX15AF19G]; [ANPCYT-PICT 0478/14]
FX We thank Neil Gehrels, the PI of the Swift mission, for a generous
allocation of TOO time. GJML and NEN are members of the 'Carrera del
Investigador Cientifico (CIC)' of CONICET and acknowledge support from
Argentina under grant ANPCYT-PICT 0478/14. JLS and ABL acknowledge
support from NASA ADAP grant NNX15AF19G. JLS thanks Scott Kenyon for
conversations (a decade ago) about shell burning and selection bias.
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U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
BP L1
EP L5
DI 10.1093/mnrasl/slw087
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9OE
UT WOS:000383269900001
ER
PT J
AU Fierce, L
Bond, TC
Bauer, SE
Mena, F
Riemer, N
AF Fierce, Laura
Bond, Tami C.
Bauer, Susanne E.
Mena, Francisco
Riemer, Nicole
TI Black carbon absorption at the global scale is affected by
particle-scale diversity in composition
SO NATURE COMMUNICATIONS
LA English
DT Article
ID MIXING STATE; SIZE DISTRIBUTIONS; OPTICAL-PROPERTIES; LIGHT-ABSORPTION;
BROWN CARBON; AEROSOL; SOOT; MODEL; CLIMATE; AMPLIFICATION
AB Atmospheric black carbon (BC) exerts a strong, but uncertain, warming effect on the climate. BC that is coated with non-absorbing material absorbs more strongly than the same amount of BC in an uncoated particle, but the magnitude of this absorption enhancement (E-abs) is not well constrained. Modelling studies and laboratory measurements have found stronger absorption enhancement than has been observed in the atmosphere. Here, using a particle-resolved aerosol model to simulate diverse BC populations, we show that absorption is overestimated by as much as a factor of two if diversity is neglected and population-averaged composition is assumed across all BC-containing particles. If, instead, composition diversity is resolved, we find E-abs=1-1.5 at low relative humidity, consistent with ambient observations. This study offers not only an explanation for the discrepancy between modelled and observed absorption enhancement, but also demonstrates how particle-scale simulations can be used to develop relationships for global-scale models.
C1 [Fierce, Laura] Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA.
[Fierce, Laura] Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA.
[Bond, Tami C.; Mena, Francisco] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
[Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bauer, Susanne E.] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Riemer, Nicole] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
RP Fierce, L (reprint author), Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA.; Fierce, L (reprint author), Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA.
EM lfierce@bnl.gov
FU US Environmental Protection Agency [R83504201]; NASA [NNX09AK66G];
Department of Energy [DE-FG02-08ER64533]; Fulbright-Chile CONICYT
fellowship; NOAA Climate & Global Change Postdoctoral Fellowship through
the University Corporation for Atmospheric Research Visiting Scientists
Program
FX This work was supported by the US Environmental Protection Agency
(R83504201) and by NASA (NNX09AK66G). F. Mena was funded by the
Department of Energy under DE-FG02-08ER64533 and by a Fulbright-Chile
CONICYT fellowship. L. Fierce is funded by a NOAA Climate & Global
Change Postdoctoral Fellowship through the University Corporation for
Atmospheric Research Visiting Scientists Program.
NR 49
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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 SEP
PY 2016
VL 7
AR 12361
DI 10.1038/ncomms12361
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY3CG
UT WOS:000384967800001
PM 27580627
ER
PT J
AU Thiery, W
Davin, EL
Seneviratne, SI
Bedka, K
Lhermitte, S
van Lipzig, NPM
AF Thiery, Wim
Davin, Edouard L.
Seneviratne, Sonia I.
Bedka, Kristopher
Lhermitte, Stef
van Lipzig, Nicole P. M.
TI Hazardous thunderstorm intensification over Lake Victoria
SO NATURE COMMUNICATIONS
LA English
DT Article
ID REGIONAL CLIMATE MODEL; AFRICAN GREAT-LAKES; EAST-AFRICA; PRECIPITATION
EXTREMES; RESOLUTION MODEL; TEMPERATURE; IMPACT; BASIN;
PARAMETERIZATION; SIMULATIONS
AB Weather extremes have harmful impacts on communities around Lake Victoria, where thousands of fishermen die every year because of intense night-time thunderstorms. Yet how these thunderstorms will evolve in a future warmer climate is still unknown. Here we show that Lake Victoria is projected to be a hotspot of future extreme precipitation intensification by using new satellite-based observations, a high-resolution climate projection for the African Great Lakes and coarser-scale ensemble projections. Land precipitation on the previous day exerts a control on night-time occurrence of extremes on the lake by enhancing atmospheric convergence (74%) and moisture availability (26%). The future increase in extremes over Lake Victoria is about twice as large relative to surrounding land under a high-emission scenario, as only over-lake moisture advection is high enough to sustain Clausius-Clapeyron scaling. Our results highlight a major hazard associated with climate change over East Africa and underline the need for high-resolution projections to assess local climate change.
C1 [Thiery, Wim; Lhermitte, Stef; van Lipzig, Nicole P. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium.
[Thiery, Wim; Davin, Edouard L.; Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
[Bedka, Kristopher] NASA, Langley Res Ctr, Sci Directorate, 21 Langley Blvd, Hampton, VA 23681 USA.
[Lhermitte, Stef] Delft Univ Technol, Dept Geosci & Remote Sensing, Stevinweg 1, NL-2600 GA Delft, Netherlands.
RP Thiery, W (reprint author), Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium.; Thiery, W (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM wim.thiery@env.ethz.ch
RI Davin, Edouard/L-7033-2016
OI Davin, Edouard/0000-0003-3322-9330
FU Research Foundation Flanders (FWO); ETH Zurich [Fel-45 15-1]; FWO;
Belgian Science Policy Office (BELSPO) [CD/AR/02A]; Hercules Foundation;
Flemish Government-department EWI
FX We acknowledge the CLM community (http://www.clm-community.eu) for
developing COSMO-CLM2 and making the model code available,
and Hans-Jurgen Panitz for providing the lateral boundary conditions. In
addition, we are grateful to the World Climate Research Programme (WRCP)
for initiating and coordinating the CORDEX-Africa initiative, to the
modelling centres for making their downscaling results publicly
available through ESGF, to ECMWF for providing access to ERA-Interim,
and to NASA and JAXA for developing the TRMM-3B42 data set. We
particularly thank Fabien Chatterjee, Matthias Demuzere, David Docquier,
Niels Souverijns and Kristof Van Tricht for their useful suggestions.
W.T. was supported by a PhD fellowship from the Research Foundation
Flanders (FWO) and an ETH Zurich postdoctoral fellowship (Fel-45 15-1).
S.L. was supported by an FWO postdoctoral fellowship. The Belgian
Science Policy Office (BELSPO) is acknowledged for the support through
the research project EAGLES (CD/AR/02A). Computational resources and
services used for the COSMO-CLM2 simulation were provided by
the VSC (Flemish Supercomputer Center), funded by the Hercules
Foundation and the Flemish Government-department EWI.
NR 52
TC 4
Z9 4
U1 8
U2 8
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD SEP
PY 2016
VL 7
AR 12786
DI 10.1038/ncomms12786
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY6RU
UT WOS:000385256500016
PM 27658848
ER
PT J
AU Donnelly, M
AF Donnelly, Michael
TI You can't sit in an office and issue edicts via email. You need to go
where the work is being performed
SO AEROSPACE AMERICA
LA English
DT Editorial Material
C1 [Donnelly, Michael] NASA, OSIRIS REx, Washington, DC 20546 USA.
RP Donnelly, M (reprint author), NASA, OSIRIS REx, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD SEP
PY 2016
VL 54
IS 8
BP 64
EP 64
PG 1
WC Engineering, Aerospace
SC Engineering
GA DX9TN
UT WOS:000384738200015
ER
PT J
AU Han, JW
Wong, HY
Moon, DI
Braga, N
Meyyappan, M
AF Han, Jin-Woo
Wong, Hiu Yung
Moon, Dong-Il
Braga, Nelson
Meyyappan, M.
TI Stringer Gate FinFET on Bulk Substrate
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE FinFET; low standby power; steep retrograde well; stringer gate; sub-fin
leakage
ID SUBTHRESHOLD LOGIC; DEVICE DESIGN; SOI MOSFETS; OPTIMIZATION;
TRANSISTORS; OPERATION; MOBILITY
AB A gate stringer normally considered parasitic is used as a subthreshold leakage suppressor in a bulk FinFET. The gate stringer remaining along the source/drain extension suppresses the formation of a sub-fin leakage path and improves the subthreshold slope. The stringer gate structure is implemented by simple process modification in the gate etch step while the other process steps are unchanged. The fabricated stringer gate FinFET shows 35% reduction in the OFF-state leakage current compared with a conventional FinFET without a retrograde well process at the expense of only 5% increase in parasitic capacitance. The power-delay product enhancement at reduced drive voltage characteristics exhibits that the stringer gate FinFET can be an attractive candidate for low standby power and subthreshold logic applications.
C1 [Han, Jin-Woo; Moon, Dong-Il; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wong, Hiu Yung; Braga, Nelson] Synopsys Inc, Mountain View, CA 94043 USA.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov; hywong@synopsys.com; dong-il.moon@nasa.gov;
nelson.braga@synopsys.com; m.meyyappan@nasa.gov
NR 27
TC 0
Z9 0
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
EI 1557-9646
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD SEP
PY 2016
VL 63
IS 9
BP 3432
EP 3438
DI 10.1109/TED.2016.2586607
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA DX7NK
UT WOS:000384574400009
ER
PT J
AU Singh, D
Swain, DL
Mankin, JS
Horton, DE
Thomas, LN
Rajaratnam, B
Diffenbaugh, NS
AF Singh, Deepti
Swain, Daniel L.
Mankin, Justin S.
Horton, Daniel E.
Thomas, Leif N.
Rajaratnam, Bala
Diffenbaugh, Noah S.
TI Recent amplification of the North American winter temperature dipole
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE climate change detection; climate change impacts; extreme event
attribution; atmospheric dynamics
ID ARCTIC SEA-ICE; ATMOSPHERIC CIRCULATION; INTERNAL VARIABILITY;
CALIFORNIA DROUGHT; CLIMATE; TRENDS; SNOW; PATTERNS; EXTREMES; WEATHER
AB During the winters of 2013-2014 and 2014-2015, anomalously warm temperatures in western North America and anomalously cool temperatures in eastern North America resulted in substantial human and environmental impacts. Motivated by the impacts of these concurrent temperature extremes and the intrinsic atmospheric linkage between weather conditions in the western and eastern United States, we investigate the occurrence of concurrent warm-West/cool-East surface temperature anomalies, which we call the North American winter temperature dipole. We find that, historically, warm-West/cool-East dipole conditions have been associated with anomalous mid-tropospheric ridging over western North America and downstream troughing over eastern North America. We also find that the occurrence and severity of warm-West/cool-East events have increased significantly between 1980 and 2015, driven largely by an increase in the frequency with which high-amplitude ridge-trough wave patterns result in simultaneous severe temperature conditions in both the West and East. Using a large single-model ensemble of climate simulations, we show that the observed positive trend in the warm-West/cool-East events is attributable to historical anthropogenic emissions including greenhouse gases, but that the co-occurrence of extreme western warmth and eastern cold will likely decrease in the future as winter temperatures warm dramatically across the continent, thereby reducing the occurrence of severely cold conditions in the East. Although our analysis is focused on one particular region, our analysis framework is generally transferable to the physical conditions shaping different types of extreme events around the globe.
C1 [Singh, Deepti; Swain, Daniel L.; Horton, Daniel E.; Thomas, Leif N.; Rajaratnam, Bala; Diffenbaugh, Noah S.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Singh, Deepti; Mankin, Justin S.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Horton, Daniel E.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
[Horton, Daniel E.; Diffenbaugh, Noah S.] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA.
[Rajaratnam, Bala] Stanford Univ, Dept Stat, Stanford, CA 94305 USA.
RP Singh, D (reprint author), Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.; Singh, D (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
EM dsingh@ldeo.columbia.edu
OI Swain, Daniel/0000-0003-4276-3092
FU Lamont Doherty Postdoctoral Fellowship; Switzer Foundation; ARCS
Foundation; Earth Institute Postdoctoral Fellowship; US National Science
Foundation [DMS-CMG 1025465, AGS-1003823, DMS-1106642,
DMS-CAREER-1352656]; U.S. Air Force Office of Scientific Research
[FA9550-13-1-0043]; NSF AGS CAREER [0955283]; DOE Integrated Assessment
Research Program [DE-SC005171]
FX We thank the National Oceanic and Atmospheric Administration's NCDC for
access to historical temperature and geopotential height data sets,
PRISM Climate Group and University of Idaho for access to historical
temperature data sets, and NCAR for access to the CESM LENS simulations.
We also thank Nathaniel Johnson for providing us the Self-Organizing
Maps algorithm. Our work is supported by the Lamont Doherty Postdoctoral
Fellowship to D.S.; graduate fellowships from the Switzer Foundation and
the ARCS Foundation to D.L.S.; Earth Institute Postdoctoral Fellowship
to J.S.M.; US National Science Foundation grants DMS-CMG 1025465,
AGS-1003823, DMS-1106642, and DMS-CAREER-1352656; and U.S. Air Force
Office of Scientific Research grant award FA9550-13-1-0043 to B.R.; and
NSF AGS CAREER grant 0955283 and DOE Integrated Assessment Research
Program grant DE-SC005171 to N.S.D. Gridded 2 m temperatures,
geopotential heights, meridional winds, and omega from the NCEP R1 and 2
m temperatures from the NCEP North American Regional Reanalysis (NARR)
are available at the NOAA ESRL website
(http://www.esrl.noaa.gov/psd/data/gridded/). Gridded temperatures from
PRISM Climate Group and University of Idaho Metdata data sets are
available at their respective websites
(http://www.prism.oregonstate.edu/ and
http://metdata.northwestknowledge.net/). All analysis scripts used in
this study can be obtained by contacting Deepti Singh
(dsingh@ldeo.columbia.edu).
NR 56
TC 3
Z9 3
U1 10
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP
PY 2016
VL 121
IS 17
BP 9911
EP 9928
DI 10.1002/2016JD025116
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000024
PM 27840780
ER
PT J
AU Payne, RC
Britt, AV
Chen, H
Kasting, JF
Catling, DC
AF Payne, Rebecca C.
Britt, Amber V.
Chen, Howard
Kasting, James F.
Catling, David C.
TI The response of Phanerozoic surface temperature to variations in
atmospheric oxygen concentration
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE atmospheric O-2 levels; surface temperature; Phanerozoic climate;
Cenomanian climate
ID MODEL; EVOLUTION; RECORD; EARTH; TIME; O-2; CO2
AB Recently, Poulsen et al. (2015) suggested that O-2 has played a major role in climate forcing during the Phanerozoic. Specifically, they argued that decreased O-2 levels during the Cenomanian stage of the middle Cretaceous (94-100Ma) could help explain the extremely warm climate during that time. The postulated warming mechanism involves decreased Rayleigh scattering by a thinner atmosphere, which reduces the planetary albedo and allows greater surface warming. This warming effect is then amplified by cloud feedbacks within their 3-D climate model. This increase in shortwave surface forcing, in their calculations, exceeds any decrease in the greenhouse effect caused by decreased O-2. Here we use a 1-D radiative-convective climate model (with no cloud feedback) to check their results. We also include a self-consistent calculation of the change in atmospheric ozone and its effect on climate. Our results are opposite to those of Poulsen et al.: we find that the climate warms by 1.4K at 35% O-2 concentrations as a result of increased pressure broadening of CO2 and H2O absorption lines and cools by 0.8K at 10% O-2 as a result of decreased pressure broadening. The surface temperature changes are only about 1K either way, though, for reasonable variations in Phanerozoic O-2 concentrations (10%-35% by volume). Hence, it seems unlikely that changes in atmospheric O-2 account for the warm climate of the Cenomanian. Other factors, such as a higher-than-expected sensitivity of climate to increased CO2 concentrations, may be required to obtain agreement with the paleoclimate data.
C1 [Payne, Rebecca C.; Britt, Amber V.; Kasting, James F.] Penn State Univ, Dept Geosci, State Coll, PA 16801 USA.
[Chen, Howard] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
[Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA USA.
[Kasting, James F.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Kasting, James F.; Catling, David C.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA.
[Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA USA.
RP Payne, RC (reprint author), Penn State Univ, Dept Geosci, State Coll, PA 16801 USA.
EM rvp5143@psu.edu
FU Undergraduate Research Opportunities Program (UROP) at Boston
University; NASA's Exobiology and Astrobiology programs
FX We are grateful to Jing-Jun Liu for his help with the photochemical
analysis. H. C. thanks the Undergraduate Research Opportunities Program
(UROP) at Boston University for primarily funding the research while in
residence at Penn State University in State College in the summer of
2015. J.F.K. acknowledge financial support from NASA's Exobiology and
Astrobiology programs. Data can be obtained from R.C. Payne
(rvp5143@psu.edu).
NR 18
TC 0
Z9 0
U1 5
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 SEP
PY 2016
VL 121
IS 17
BP 10089
EP 10096
DI 10.1002/2016JD025459
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000022
ER
PT J
AU Dong, XQ
Xi, BK
Qiu, SY
Minnis, P
Sun-Mack, S
Rose, F
AF Dong, Xiquan
Xi, Baike
Qiu, Shaoyue
Minnis, Patrick
Sun-Mack, Sunny
Rose, Fred
TI A radiation closure study of Arctic stratus cloud microphysical
properties using the collocated satellite-surface data and Fu-Liou
radiative transfer model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Arctic stratus cloud properties; radiation closure study; surface remote
sensing; satellite remote sensing
ID ANGULAR-DISTRIBUTION MODELS; GROUND-BASED MEASUREMENTS; ENERGY SYSTEM
INSTRUMENT; STRATIFORM CLOUDS; FLUX CALCULATION; TERRA SATELLITE; PART
I; CERES; BUDGET; RADAR
AB Retrievals of cloud microphysical properties based on passive satellite imagery are especially difficult over snow-covered surfaces because of the bright and cold surface. To help quantify their uncertainties, single-layered overcast liquid-phase Arctic stratus cloud microphysical properties retrieved by using the Clouds and the Earth's Radiant Energy System Edition 2 and Edition 4 (CERES Ed2 and Ed4) algorithms are compared with ground-based retrievals at the Atmospheric Radiation Measurement North Slope of Alaska (ARM NSA) site at Barrow, AK, during the period from March 2000 to December 2006. A total of 206 and 140 snow-free cases (R(sfc)0.3), and 108 and 106 snow cases (R-sfc>0.3), respectively, were selected from Terra and Aqua satellite passes over the ARM NSA site. The CERES Ed4 and Ed2 optical depth () and liquid water path (LWP) retrievals from both Terra and Aqua are almost identical and have excellent agreement with ARM retrievals under snow-free and snow conditions. In order to reach a radiation closure study for both the surface and top of atmosphere (TOA) radiation budgets, the ARM precision spectral pyranometer-measured surface albedos were adjusted (63.6% and 80% of the ARM surface albedos for snow-free and snow cases, respectively) to account for the water and land components of the domain of 30kmx30km. Most of the radiative transfer model calculated SWsfc and SWTOA fluxes by using ARM and CERES cloud retrievals and the domain mean albedos as input agree with the ARM and CERES flux observations within 10Wm(-2) for both snow-free and snow conditions. Sensitivity studies show that the ARM LWP and r(e) retrievals are less dependent on solar zenith angle (SZA), but all retrieved optical depths increase with SZA.
C1 [Dong, Xiquan; Xi, Baike; Qiu, Shaoyue] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Minnis, Patrick] NASA Langley Res Ctr, Hampton, VA USA.
[Sun-Mack, Sunny; Rose, Fred] SSAI Inc, Hampton, VA USA.
RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
FU U.S. Department of Energy (DOE) Office of Energy Research, Office of
Health and Environmental Research, Environmental Sciences Division; NASA
CERES project at the University of North Dakota [NNX14AP84G]; DOE ARM
Program at NASA Langley [DE-SC0013896]
FX The ground-based measurements were obtained from the Atmospheric
Radiation Measurement (ARM) Program sponsored by the U.S. Department of
Energy (DOE) Office of Energy Research, Office of Health and
Environmental Research, Environmental Sciences Division. The data can be
downloaded from http://www.archive.arm.gov/. The satellite data were
obtained from the NASA CERES cloud working group at NASA Langley
Research Center. Special thanks to Seiji Kato for the useful discussion
about NASA Langley Modified Fu-Liou radiative transfer model. This
research was supported by the NASA CERES project under grant NNX14AP84G
at the University of North Dakota and by the DOE ARM Program under
contract DE-SC0013896 at NASA Langley. Dates and times corresponding to
the sample numbers used in several figures are available from the lead
author on request (dong@aero.und.edu).
NR 46
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U1 6
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP
PY 2016
VL 121
IS 17
BP 10175
EP 10198
DI 10.1002/2016JD025255
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000018
ER
PT J
AU Saide, PE
Thompson, G
Eidhammer, T
da Silva, AM
Pierce, RB
Carmichael, GR
AF Saide, Pablo E.
Thompson, Gregory
Eidhammer, Trude
da Silva, Arlindo M.
Pierce, R. Bradley
Carmichael, Gregory R.
TI Assessment of biomass burning smoke influence on environmental
conditions for multiyear tornado outbreaks by combining aerosol-aware
microphysics and fire emission constraints
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE biomass burning; severe weather; tornadoes; fires;
aerosol-cloud-radiation interactions; WRF
ID MARINE STRATOCUMULUS; SPATIAL-DISTRIBUTION; WEATHER FORECASTS; OPTICAL
DEPTH; WRF-CHEM; MODEL; IMPACTS; CLIMATE; PARAMETERIZATION; ASSIMILATION
AB We use the Weather Research and Forecasting (WRF) system to study the impacts of biomass burning smoke from Central America on several tornado outbreaks occurring in the U.S. during spring. The model is configured with an aerosol-aware microphysics parameterization capable of resolving aerosol-cloud-radiation interactions in a cost-efficient way for numerical weather prediction (NWP) applications. Primary aerosol emissions are included, and smoke emissions are constrained using an inverse modeling technique and satellite-based aerosol optical depth observations. Simulations turning on and off fire emissions reveal smoke presence in all tornado outbreaks being studied and show an increase in aerosol number concentrations due to smoke. However, the likelihood of occurrence and intensification of tornadoes is higher due to smoke only in cases where cloud droplet number concentration in low-level clouds increases considerably in a way that modifies the environmental conditions where the tornadoes are formed (shallower cloud bases and higher low-level wind shear). Smoke absorption and vertical extent also play a role, with smoke absorption at cloud-level tending to burn-off clouds and smoke absorption above clouds resulting in an increased capping inversion. Comparing these and WRF-Chem simulations configured with a more complex representation of aerosol size and composition and different optical properties, microphysics, and activation schemes, we find similarities in terms of the simulated aerosol optical depths and aerosol impacts on near-storm environments. This provides reliability on the aerosol-aware microphysics scheme as a less computationally expensive alternative to WRF-Chem for its use in applications such as NWP and cloud-resolving simulations.
C1 [Saide, Pablo E.] Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA.
[Saide, Pablo E.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Thompson, Gregory; Eidhammer, Trude] Natl Ctr Atmospher Res, Res Applicat Lab, POB 3000, Boulder, CO 80307 USA.
[da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Data Assimilat Off, Greenbelt, MD USA.
[Pierce, R. Bradley] NOAA, Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res STAR, Madison, WI USA.
[Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA.
RP Saide, PE (reprint author), Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA.; Saide, PE (reprint author), Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
EM saide@ucar.edu
RI Pierce, Robert Bradley/F-5609-2010
OI Pierce, Robert Bradley/0000-0002-2767-1643
FU National Science Foundation
FX The National Center for Atmospheric Research is supported by the
National Science Foundation. Contact P.E. Saide (saide@ucar.edu) for
data and code requests. This work was carried out with the aid of NASA
grant NNXAF95G. A.M. da Silva is funded by NASA's Modeling and
Application Program. We acknowledge use of MOZART-4 global model output
available at http://www.acom.ucar.edu/wrf-chem/mozart.shtml. CALIPSO
data were obtained from the NASA Langley Research Center Atmospheric
Science Data Center (https://earthdata.nasa.gov/). The views, opinions,
and findings contained in this report are those of the author(s) and
should not be construed as an official National Oceanic and Atmospheric
Administration or U.S. Government position, policy, or decision.
NR 60
TC 0
Z9 0
U1 15
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP
PY 2016
VL 121
IS 17
BP 10294
EP 10311
DI 10.1002/2016JD025056
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000014
ER
PT J
AU Sullivan, JT
Mcgee, TJ
Langford, AO
Alvarez, RJ
Senff, CJ
Reddy, PJ
Thompson, AM
Twigg, LW
Sumnicht, GK
Lee, P
Weinheimer, A
Knote, C
Long, RW
Hoff, RM
AF Sullivan, John T.
McGee, Thomas J.
Langford, Andrew O.
Alvarez, Raul J., II
Senff, Christoph J.
Reddy, Patrick J.
Thompson, Anne M.
Twigg, Laurence W.
Sumnicht, Grant K.
Lee, Pius
Weinheimer, Andrew
Knote, Christoph
Long, Russell W.
Hoff, Raymond M.
TI Quantifying the contribution of thermally driven recirculation to a
high-ozone event along the Colorado Front Range using lidar
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone; air quality; remote sensing; lidar; air quality modeling; TOLNet
ID REGIONAL-SCALE FLOWS; MOUNTAINOUS TERRAIN; BOUNDARY-LAYER
AB A high-ozone (O-3) pollution episode was observed on 22 July 2014 during the concurrent Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ) and Front Range Air Pollution and Photochemistry Experiment (FRAPPE) campaigns in northern Colorado. Surface O-3 monitors at three regulatory sites exceeded the Environmental Protection Agency (EPA) 2008 National Ambient Air Quality Standard (NAAQS) daily maximum 8h average (MDA8) of 75ppbv. To further characterize the polluted air mass and assess transport throughout the event, measurements are presented from O-3 and wind profilers, O-3-sondes, aircraft, and surface-monitoring sites. Observations indicate that thermally driven upslope flow was established throughout the Colorado Front Range during the pollution episode. As the thermally driven flow persisted throughout the day, O-3 concentrations increased and affected high-elevation Rocky Mountain sites. These observations, coupled with modeling analyses, demonstrate a westerly return flow of polluted air aloft, indicating that the mountain-plains solenoid circulation was established and impacted surface conditions within the Front Range.
C1 [Sullivan, John T.; McGee, Thomas J.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Langford, Andrew O.; Alvarez, Raul J., II; Senff, Christoph J.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Senff, Christoph J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Reddy, Patrick J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD USA.
[Twigg, Laurence W.; Sumnicht, Grant K.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Lee, Pius] NOAA, Ctr Weather & Climate Predict, Air Resources Lab, College Pk, MD USA.
[Weinheimer, Andrew] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Knote, Christoph] Univ Munich, Meteorol Inst, Munich, Germany.
[Long, Russell W.] US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA.
[Hoff, Raymond M.] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Hoff, Raymond M.] Univ Maryland, Dept Atmospher Phys, Baltimore, MD 21201 USA.
RP Sullivan, JT (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
EM john.t.sullivan@nasa.gov
RI Langford, Andrew/D-2323-2009; Thompson, Anne /C-3649-2014; Manager, CSD
Publications/B-2789-2015
OI Langford, Andrew/0000-0002-2932-7061; Thompson, Anne
/0000-0002-7829-0920;
FU UMBC/JCET [374, 8306]; Maryland Department of the Environment (MDE)
[U00P4400079]; NOAA-CREST CCNY Foundation [49173B-02]; NASA/USRA
Postdoctoral Program at the Goddard Space Flight Center; NASA
DISCOVER-AQ [NNX10AR39G]; Pennsylvania State University; NASA
Tropospheric Chemistry Program; Tropospheric Ozone Lidar Network
(TOLNet)
FX Unless otherwise noted, all data used in this study can be found in the
DISCOVER-AQ data archive
(http://www-air.larc.nasa.gov/missions/discover-aq/), the FRAPPE data
archive (http://catalog.eol.ucar.edu/frappe), or the TOLNet data archive
(http://www-air.larc.nasa.gov/missions/TOLNet/). This work was supported
by UMBC/JCET (task 374, project 8306), the Maryland Department of the
Environment (MDE, contract U00P4400079), and NOAA-CREST CCNY Foundation
(subcontract 49173B-02). This research was supported by an appointment
to the NASA/USRA Postdoctoral Program at the Goddard Space Flight
Center. The Platteville Nittany Atmospheric Trailer and Integrated
Validation Experiment (NATIVE) operations were sponsored by NASA
DISCOVER-AQ grant NNX10AR39G and the Pennsylvania State University. The
authors gratefully acknowledge support provided by the NASA Tropospheric
Chemistry Program and the Tropospheric Ozone Lidar Network (TOLNet).
Thanks to the helpfulness and expertise of Ryan Stauffer, Hannah
Halliday, and Nikolai Balashov, who worked with the NATIVE trailer at
Platteville. Thanks to Debra Wicks Kollonige for providing her insight
and recommendations on this work. Thanks to Kenneth Pickering, Yonhua
Tang, Li Pan, and Barry Baker for their expertise in evaluating and
managing the CMAQ model output. Thanks to Timothy Coleman (NOAA ESRL
PSD) for providing the Greeley wind profiles. Thanks to the NOAA
Physical Science Division for their continued efforts in managing the
instrumentation and site coordination necessary for this work from the
300 m BAO Tower. Finally, thanks to the CDPHE for the continued efforts
to obtain observations at the many remote and urban sites throughout the
region used in this work. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 34
TC 0
Z9 0
U1 8
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP
PY 2016
VL 121
IS 17
BP 10377
EP 10390
DI 10.1002/2016JD025229
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000008
ER
PT J
AU Bokhorst, S
Pedersen, SH
Brucker, L
Anisimov, O
Bjerke, JW
Brown, RD
Ehrich, D
Essery, RLH
Heilig, A
Ingvander, S
Johansson, C
Johansson, M
Jonsdottir, IS
Inga, N
Luojus, K
Macelloni, G
Mariash, H
McLennan, D
Rosqvist, GN
Sato, A
Savela, H
Schneebeli, M
Sokolov, A
Sokratov, SA
Terzago, S
Vikhamar-Schuler, D
Williamson, S
Qiu, YB
Callaghan, TV
AF Bokhorst, Stef
Pedersen, Stine Hojlund
Brucker, Ludovic
Anisimov, Oleg
Bjerke, Jarle W.
Brown, Ross D.
Ehrich, Dorothee
Essery, Richard L. H.
Heilig, Achim
Ingvander, Susanne
Johansson, Cecilia
Johansson, Margareta
Jonsdottir, Ingibjorg Svala
Inga, Niila
Luojus, Kari
Macelloni, Giovanni
Mariash, Heather
McLennan, Donald
Rosqvist, Gunhild Ninis
Sato, Atsushi
Savela, Hannele
Schneebeli, Martin
Sokolov, Aleksandr
Sokratov, Sergey A.
Terzago, Silvia
Vikhamar-Schuler, Dagrun
Williamson, Scott
Qiu, Yubao
Callaghan, Terry V.
TI Changing Arctic snow cover: A review of recent developments and
assessment of future needs for observations, modelling, and impacts
SO AMBIO
LA English
DT Review
DE Climate change; Ecosystem services; Human health; Societal costs;
Indigenous; Snow
ID WINTER WARMING EVENTS; MICROWAVE BRIGHTNESS TEMPERATURE; LIGHT-ABSORBING
PARTICLES; GROUND-PENETRATING RADAR; LIQUID WATER-CONTENT; SEA-ICE;
SURFACE-AREA; ALBEDO FEEDBACK; CLIMATE MODELS; INFRARED REFLECTANCE
AB Snow is a critically important and rapidly changing feature of the Arctic. However, snow-cover and snowpack conditions change through time pose challenges for measuring and prediction of snow. Plausible scenarios of how Arctic snow cover will respond to changing Arctic climate are important for impact assessments and adaptation strategies. Although much progress has been made in understanding and predicting snow-cover changes and their multiple consequences, many uncertainties remain. In this paper, we review advances in snow monitoring and modelling, and the impact of snow changes on ecosystems and society in Arctic regions. Interdisciplinary activities are required to resolve the current limitations on measuring and modelling snow characteristics through the cold season and at different spatial scales to assure human well-being, economic stability, and improve the ability to predict manage and adapt to natural hazards in the Arctic region.
C1 [Bokhorst, Stef; Bjerke, Jarle W.] Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway.
[Bokhorst, Stef] Vrije Univ Amsterdam, Dept Ecol Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands.
[Pedersen, Stine Hojlund] Aarhus Univ, Dept Biosci, Arctic Res Ctr, Frederiksborgvej 399, DK-4000 Roskilde, Denmark.
[Brucker, Ludovic] NASA, GSFC, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA.
[Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA.
[Anisimov, Oleg] State Hydrol Inst Roshydromet, 23 Second Line VO, St Petersburg 199053, Russia.
[Anisimov, Oleg] North East Fed Univ, Int Ctr Sci & Educ Best, Yakutsk, Russia.
[Brown, Ross D.] Environm Canada Ouranos, Div Climate Res, 550 Sherbrooke St West,19th Floor, Montreal, PQ H3A 1B9, Canada.
[Ehrich, Dorothee] Univ Tromso, Dept Arctic & Marine Biol, N-9037 Tromso, Norway.
[Essery, Richard L. H.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland.
[Heilig, Achim] Heidelberg Univ, Inst Environm Phys, Neuenheimer Feld 229, D-69120 Heidelberg, Germany.
[Ingvander, Susanne; Rosqvist, Gunhild Ninis] Stockholm Univ, Dept Phys Geog, S-10691 Stockholm, Sweden.
[Johansson, Cecilia] Uppsala Univ, Dept Earth Sci, Villavagen 16, S-75236 Uppsala, Sweden.
[Johansson, Margareta; Callaghan, Terry V.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Johansson, Margareta] Royal Swedish Acad Sci, POB 50005, S-10405 Stockholm, Sweden.
[Jonsdottir, Ingibjorg Svala] Univ Ctr Svalbard, POB 156, N-9171 Longyearbyen, Norway.
[Jonsdottir, Ingibjorg Svala] Univ Iceland, Fac Life & Environm Sci, Sturlugata 7, IS-101 Reykjavik, Iceland.
[Inga, Niila] Leavas Sami Commun, Box 53, S-98121 Kiruna, Sweden.
[Luojus, Kari] Finnish Meteorol Inst, Arctic Res, POB 503, Helsinki 00101, Finland.
[Macelloni, Giovanni] CNR, IFAC CNR, Inst Appl Phys Nello Carrara, Via Madonna del Piano 10, I-50019 Sesto Fiorentino, FI, Italy.
[Mariash, Heather] Environm Canada, Natl Wildlife Res Ctr, 1125 Colonel By Dr, Ottawa, ON K1A 0H3, Canada.
[McLennan, Donald] CHARS, 360 Albert St,Suite 1710, Ottawa, ON K1R 7X7, Canada.
[Rosqvist, Gunhild Ninis] Univ Bergen, Dept Earth Sci, N-5020 Bergen, Norway.
[Sato, Atsushi] Natl Res Inst Earth Sci & Disaster Prevent, Snow & Ice Res Ctr, 187-16 Suyoshi, Nagaoka, Niigata 9400821, Japan.
[Savela, Hannele] Univ Oulu, Thule Insitute, POB 7300, Oulu 90014, Finland.
[Schneebeli, Martin] WSL Inst Snow & Avalanche Res SLF, Fluelastr 11, CH-7260 Davos, Switzerland.
[Sokolov, Aleksandr] Russian Acad Sci, Arctic Res Stn, Inst Plant & Anim Ecol, Ural Branch, Labytnangi 629400, Russia.
[Sokolov, Aleksandr] State Org Yamal Nenets Autonomous Dist, Sci Ctr Arctic Studies, Salekhard, Russia.
[Sokratov, Sergey A.] Moscow MV Lomonosov State Univ, Arctic Environm Lab, Fac Geog, Leninskie Gory 1, Moscow 119991, Russia.
[Terzago, Silvia] Natl Res Council ISAC CNR, Inst Atmospher Sci & Climate, Corso Fiume 4, I-10133 Turin, Italy.
[Vikhamar-Schuler, Dagrun] Norwegian Meteorol Inst, Div Model & Climate Anal, R&D Dept, Postboks 43, N-0313 Oslo, Norway.
[Williamson, Scott] Univ Alberta, Dept Biol Sci, CW 405,Biol Sci Bldg, Edmonton, AB T6G 2E9, Canada.
[Qiu, Yubao] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Beijing 100094, Peoples R China.
[Qiu, Yubao] Cold Reg Initiat, Grp Earth Observat, Geneva, Switzerland.
[Callaghan, Terry V.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Callaghan, Terry V.] Natl Res Tomsk Stated Univ, 36 Lenin Ave, Tomsk 634050, Russia.
RP Bokhorst, S (reprint author), Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway.
EM stefbokhorst@hotmail.com; shp@bios.au.dk; ludovic.brucker@nasa.gov;
oleg@oa7661.spb.edu; jarle.werner.bjerke@nina.no; ross.brown@ec.gc.ca;
dorothee.ehrich@uit.no; richard.essery@ed.ac.uk; achim.heilig@wsl.ch;
susanne.ingvander@natgeo.su.se; cecilia.johansson@met.uu.se;
margareta.johansson@nateko.lu.se; isj@hi.is; niila@laevas.se;
kari.luojus@fmi.fi; g.macelloni@ifac.cnr.it; heather.mariash@gmail.com;
donald.mclennan@polar.gc.ca; gunhild.rosqvist@natgeo.su.se;
asato@bosai.go.jp; hannele.savela@oulu.fi; martin.schneebeli@wsl.ch;
sokhol@yandex.ru; sokratov@geol.msu.ru; s.terzago@isac.cnr.it;
dagrun@met.no; snw@ualberta.ca; terry_callaghan@btinternet.com
RI Sokratov, Sergey/A-6602-2011; Ehrich, Dorothee/F-6492-2015; Schneebeli,
Martin/B-1063-2008; Brucker, Ludovic/A-8029-2010; Callaghan,
Terens/N-7640-2014;
OI Sokratov, Sergey/0000-0001-9265-2935; Ehrich,
Dorothee/0000-0002-3028-9488; Schneebeli, Martin/0000-0003-2872-4409;
Brucker, Ludovic/0000-0001-7102-8084; Essery,
Richard/0000-0003-1756-9095; Bjerke, Jarle/0000-0003-2721-1492
FU IASC ICARP III Activity grant
FX The writing of this paper was initiated by an IASC ICARP III Activity
grant to TVC enabling a workshop hosted by the European Environment
Agency. The authors acknowledge funding from their respective national
and international funding bodies, which has enabled the contribution of
all authors to this work.
NR 167
TC 5
Z9 5
U1 37
U2 37
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0044-7447
EI 1654-7209
J9 AMBIO
JI Ambio
PD SEP
PY 2016
VL 45
IS 5
BP 516
EP 537
DI 10.1007/s13280-016-0770-0
PG 22
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DT6GD
UT WOS:000381580800002
PM 26984258
ER
PT J
AU McIntire, J
Moyer, D
Brown, SW
Lykke, KR
Waluschka, E
Oudrari, H
Xiong, XX
AF McIntire, Jeff
Moyer, David
Brown, Steven W.
Lykke, Keith R.
Waluschka, Eugene
Oudrari, Hassan
Xiong, Xiaoxiong
TI Monochromatic measurements of the JPSS-1 VIIRS polarization sensitivity
SO APPLIED OPTICS
LA English
DT Article
ID PERFORMANCE; CALIBRATION; SATELLITE; MODIS
AB Polarization sensitivity is a critical property that must be characterized for spaceborne remote sensing instruments designed to measure reflected solar radiation. Broadband testing of the first Joint Polar-orbiting Satellite System (JPSS-1) Visible Infrared Imaging Radiometer Suite (VIIRS) showed unexpectedly large polarization sensitivities for the bluest bands on VIIRS (centered between 400 and 600 nm). Subsequent ray trace modeling indicated that large diattenuation on the edges of the bandpass for these spectral bands was the driver behind these large sensitivities. Additional testing using the National Institute of Standards and Technology's Traveling Spectral Irradiance and Radiance Responsivity Calibrations Using Uniform Sources was added to the test program to verify and enhance the model. The testing was limited in scope to two spectral bands at two scan angles; nonetheless, this additional testing provided valuable insight into the polarization sensitivity. Analysis has shown that the derived diattenuation agreed with the broadband measurements to within an absolute difference of about 0.4% and that the ray trace model reproduced the general features of the measured data. Additionally, by deriving the spectral responsivity, the linear diattenuation is shown to be explicitly dependent on the changes in bandwidth with polarization state. (C) 2016 Optical Society of America
C1 [McIntire, Jeff; Oudrari, Hassan] Sci Syst Applicat Int, Lanham, MD 20706 USA.
[Moyer, David] Aerosp Corp, El Segundo, CA 90245 USA.
[Brown, Steven W.; Lykke, Keith R.] NIST, Gaithersburg, MD 20899 USA.
[Waluschka, Eugene; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McIntire, J (reprint author), Sci Syst Applicat Int, Lanham, MD 20706 USA.
EM jeffrey.mcintire@ssaihq.com
NR 16
TC 0
Z9 0
U1 5
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD SEP
PY 2016
VL 55
IS 27
BP 7444
EP 7454
DI 10.1364/AO.55.007444
PG 11
WC Optics
SC Optics
GA DW9QO
UT WOS:000383996900001
PM 27661568
ER
PT J
AU Sun, JQ
Xiong, XX
Waluschka, E
Wang, MH
AF Sun, Junqiang
Xiong, Xiaoxiong
Waluschka, Eugene
Wang, Menghua
TI Suomi National Polar-Orbiting Partnership Visible Infrared Imaging
Radiometer Suite polarization sensitivity analysis
SO APPLIED OPTICS
LA English
DT Article
ID REFLECTIVE SOLAR BANDS; CALIBRATION; SPECTRORADIOMETER; PERFORMANCE;
DIFFUSER
AB The Visible Infrared Imaging Radiometer Suite (VIIRS) is one of five instruments onboard the Suomi National Polar-Orbiting Partnership (SNPP) satellite that launched from Vandenberg Air Force Base, California, on October 28, 2011. It is a whiskbroom radiometer that provides +/- 56.28 degrees scans of the Earth view. It has 22 bands, among which 14 are reflective solar bands (RSBs). The RSBs cover a wavelength range from 410 to 2250 nm. The RSBs of a remote sensor are usually sensitive to the polarization of incident light. For VIIRS, it is specified that the polarization factor should be smaller than 3% for 410 and 862 nm bands and 2.5% for other RSBs for the scan angle within +/- 45 degrees. Several polarization sensitivity tests were performed prelaunch for SNPP VIIRS. The first few tests either had large uncertainty or were less reliable, while the last one was believed to provide the more accurate information about the polarization property of the instrument. In this paper, the measured data in the last polarization sensitivity test are analyzed, and the polarization factors and phase angles are derived from the measurements for all the RSBs. The derived polarization factors and phase angles are band, detector, and scan angle dependent. For near-infrared bands, they also depend on the half-angle mirror side. Nevertheless, the derived polarization factors are all within the specification, although the strong detector dependence of the polarization parameters was not expected. Compared to the Moderate Resolution Imaging Spectroradiometer on both Aqua and Terra satellites, the polarization effect on VIIRS RSB is much smaller. (C) 2016 Optical Society of America
C1 [Sun, Junqiang; Wang, Menghua] NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA.
[Sun, Junqiang] Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA.
[Xiong, Xiaoxiong; Waluschka, Eugene] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA.
RP Sun, JQ (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA.; Sun, JQ (reprint author), Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA.
EM junqiang.sun@noaa.gov
RI Wang, Menghua/F-5631-2010
OI Wang, Menghua/0000-0001-7019-3125
FU National Oceanic and Atmospheric Administration (NOAA) National
Aeronautics and Space Administration (NASA) Joint Polar Satellite System
FX National Oceanic and Atmospheric Administration (NOAA) National
Aeronautics and Space Administration (NASA) Joint Polar Satellite
System.
NR 31
TC 0
Z9 0
U1 5
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD SEP
PY 2016
VL 55
IS 27
BP 7645
EP 7658
DI 10.1364/AO.55.007645
PG 14
WC Optics
SC Optics
GA DW9QO
UT WOS:000383996900027
PM 27661594
ER
PT J
AU Guerrero, G
Smolarkiewicz, PK
Dal Pino, EMD
Kosovichev, AG
Mansour, NN
AF Guerrero, G.
Smolarkiewicz, P. K.
de Gouveia Dal Pino, E. M.
Kosovichev, A. G.
Mansour, N. N.
TI UNDERSTANDING SOLAR TORSIONAL OSCILLATIONS FROM GLOBAL DYNAMO MODELS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: interior; Sun: magnetic fields; Sun: rotation
ID CONVECTION-ZONE; MERIDIONAL FLOW; CYCLE VARIATION; ROTATION; INTERIOR;
SURFACE; SUN
AB The phenomenon of solar "torsional oscillations" (TO) represents migratory zonal flows associated with the solar cycle. These flows are observed on the solar surface and, according to helioseismology, extend through the convection zone. We study the origin of the TO using results from a global MHD simulation of the solar interior that reproduces several of the observed characteristics of the mean-flows and magnetic fields. Our results indicate that the magnetic tension (MT) in the tachocline region is a key factor for the periodic changes in the angular momentum transport that causes the TO. The torque induced by the MT at the base of the convection zone is positive at the poles and negative at the equator. A rising MT torque at higher latitudes causes the poles to speed up, whereas a declining negative MT torque at the lower latitudes causes the equator to slow-down. These changes in the zonal flows propagate through the convection zone up to the surface. Additionally, our results suggest that it is the magnetic field at the tachocline that modulates the amplitude of the surface meridional flow rather than the opposite as assumed by flux-transport dynamo models of the solar cycle.
C1 [Guerrero, G.] Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.
[Smolarkiewicz, P. K.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[de Gouveia Dal Pino, E. M.] Univ Sao Paulo, Dept Astron, IAG USP, Rua Matao 1226, BR-05508090 Sao Paulo, SP, Brazil.
[Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07103 USA.
[Mansour, N. N.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
RP Guerrero, G (reprint author), Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.
EM guerrero@fisica.ufmg.br; smolar@ecmwf.int; dalpino@astro.iag.usp.br;
alexander.g.kosovichev@njit.edu; Nagi.N.Mansour@nasa.gov
FU FAPEMIG [APQ-01168/14]; FAPESP [2013/10559-5, 2009/54006-4]; CNPq
[306598/2009-4]; NASA [NNX09AJ85g, NNX14AB70G]; European Research
Council under the European Union's Seventh Framework Programme (FP7/ERC)
[320375]
FX We thank the anonymous referee for insightful comments that helped to
improve the paper. This work was partly funded by FAPEMIG grant
APQ-01168/14 (GG), FAPESP grant 2013/10559-5 (EMGDP), CNPq grant
306598/2009-4 (EMGDP), and NASA grants NNX09AJ85g and NNX14AB70G. P.K.S.
is supported by funding received from the European Research Council
under the European Union's Seventh Framework Programme (FP7/2012/ERC
grant agreement no. 320375). The simulations were performed in the NASA
cluster Pleiades and the computing facilities of the Laboratory of
Astroinformatics (IAG/USP, NAT/Unicsul) supported by a FAPESP (grant
2009/54006-4).
NR 25
TC 0
Z9 0
U1 4
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2016
VL 828
IS 1
AR L3
DI 10.3847/2041-8205/828/1/L3
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9MZ
UT WOS:000383985500003
ER
PT J
AU Sterling, AC
Moore, RL
AF Sterling, Alphonse C.
Moore, Ronald L.
TI A MICROFILAMENT-ERUPTION MECHANISM FOR SOLAR SPICULES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: chromosphere; Sun: filaments, prominences; Sun: flares; Sun:
magnetic fields; Supporting material: animations
ID X-RAY JETS; POLAR CORONAL HOLES; ACTIVE-REGION; II SPICULES; TELESCOPE;
EVOLUTION; HINODE; PARAMETERS; RESOLUTION; NETWORK
AB Recent investigations indicate that solar coronal jets result from eruptions of small-scale chromospheric filaments, called minifilaments; that is, the jets are produced by scaled-down versions of typical-sized filament eruptions. We consider whether solar spicules might in turn be scaled-down versions of coronal jets, being driven by eruptions of microfilaments. Assuming a microfilament' s size is about a spicule' s width (similar to 300 km), the estimated occurrence number plotted against the estimated size of erupting filaments, minifilaments, and microfilaments approximately follows a power-law distribution (based on counts of coronal mass ejections, coronal jets, and spicules), suggesting that many or most spicules could result from microfilament eruptions. Observed spicule-base Ca II brightenings plausibly result from such microfilament eruptions. By analogy with coronal jets, microfilament eruptions might produce spicules with many of their observed characteristics, including smooth rise profiles, twisting motions, and EUV counterparts. The postulated microfilament eruptions are presumably eruptions of twisted-core micro-magnetic bipoles that are similar to 1 ''.0 wide. These explosive bipoles might be built and destabilized by merging and cancelation of approximately a few to 100 G magnetic-flux elements of size less than or similar to 0 ''.5-1 ''.0. If, however, spicules are relatively more numerous than indicated by our extrapolated distribution, then only a fraction of spicules might result from this proposed mechanism.
C1 [Sterling, Alphonse C.; Moore, Ronald L.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA.
[Moore, Ronald L.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RP Sterling, AC (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA.
EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov
FU Heliophysics Division of NASA's Science Mission Directorate through the
Heliophysics Guest Investigator (HGI) Program; Hinode Project
FX The authors thank two referees for useful comments and interesting
discussions. This work was supported by funding from the Heliophysics
Division of NASA's Science Mission Directorate through the Heliophysics
Guest Investigator (HGI) Program, and the Hinode Project. We thank T.
Tarbell for assistance with SOT images. Hinode is a Japanese mission
developed and launched by ISAS/JAXA, with NAOJ as domestic partner and
NASA and STFC (UK) as international partners, and operated by these
agencies in co-operation with ESA and NSC (Norway). Figure 1 and Figures
3(g)-(i) and animations, adapted by permission from Macmillan Publishers
Ltd: Nature, Sterling et al. (2015), copyright 2015.
NR 37
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2016
VL 828
IS 1
AR L9
DI 10.3847/2041-8205/828/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9MZ
UT WOS:000383985500009
ER
PT J
AU Wernet, MP
AF Wernet, Mark P.
TI Application of Tomo-PIV in a large-scale supersonic jet flow facility
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
ID PARTICLE IMAGE VELOCIMETRY
AB Particle imaging velocimetry (PIV) has been used extensively at NASA GRC over the last 15 years to build a benchmark data set of hot and cold jet flow measurements in an effort to understand acoustic noise sources in high-speed jets. Identifying the noise sources in highspeed jets is critical for ultimately modifying the nozzle hardware design/operation and therefore reducing the jet noise. Tomographic PIV (Tomo-PIV) is an innovative approach for acquiring and extracting velocity information across extended volumes of a flow field, enabling the computation of additional fluid mechanical properties not typically available using traditional PIV techniques. The objective of this work was to develop and implement the Tomo-PIV measurement capability and apply it in a large-scale outdoor test facility, where seeding multiple flow streams and operating in the presence of daylight presents formidable challenges. The newly developed Tomo-PIV measurement capability was applied in both a subsonic M 0.9 flow and an under-expanded M 1.4 heated jet flow field. Measurements were also obtained using traditional two-component (2C) PIV and stereo PIV in the M 0.9 flow field for comparison and validation of the Tomo-PIV results. In the case of the M 1.4 flow, only the 2C PIV was applied to allow a comparison with the Tomo-PIV measurement. The Tomo-PIV fields-of-view covered 180 x 180 x 10 mm, and the reconstruction domains were 3500 x 3500 x 200 voxels. These Tomo-PIV measurements yielded all three components of vorticity across entire planes for the first time in heated supersonic jet flows and provided the first full 3D reconstruction of the Mach disk and oblique shock intersections inside of the barrel shocks. Measuring all three components of vorticity across multiple planes in the flow, potentially reduces the number of measurement configurations (streamwise and cross-stream PIV) required to fully characterize the mixing-enhanced nozzle flows routinely studied in aeroacoustics research.
C1 [Wernet, Mark P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Wernet, MP (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM mark.p.wernet@nasa.gov
FU NASA's Fundamental Aeronautics' Transformational Tools and Technologies
Program
FX The author would like to thank NASA's Fundamental Aeronautics'
Transformational Tools and Technologies Program for their support of
this effort. The author also thanks Dr. Randy Locke, Dr. Adam Wroblewski
and Garrett Clayo for their efforts in the setting up and implementation
of the 2C PIV, SPIV and Tomo-PIV systems. The author thanks Dr. James
Bridges for helpful discussions and for the use of the SHJAR facility.
Lastly, the author thanks the staff at the AAPL for their dedication and
support in making these tests possible.
NR 33
TC 0
Z9 0
U1 5
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
EI 1432-1114
J9 EXP FLUIDS
JI Exp. Fluids
PD SEP
PY 2016
VL 57
IS 9
AR 144
DI 10.1007/s00348-016-2228-3
PG 24
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA DX2QM
UT WOS:000384215700007
ER
PT J
AU Tang, A
Kim, Y
Xu, Y
Chang, MCF
AF Tang, Adrian
Kim, Yanghyo
Xu, Yinuo
Chang, Mau-Chung Frank
TI A 5.8 GHz 54 Mb/s Backscatter Modulator for WLAN With Symbol
Pre-Distortion and Transmit Pulse Shaping
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE CMOS backscatter link; pre-distortion; pulse shaping; reflector link
AB This letter discusses the implementation of microwave backscatter links in CMOS technology which are similar to existing systems at mid-UHF for RFID, but intended for use at the 5.8 GHz ISM band for supporting future low-power WLAN applications. In order for backscatter links to operate in highly channelized environments we introduce a pulse-shaping technique to reduce out-of-band emissions as well as a symbol pre-distortion technique to improve the constellation spacing. Both techniques are introduced into a 65 nm prototype backscatter modulator chip and are shown to operate with QPSK modulation at 54 Mb/s (typical of WLAN standards). The backscatter modulator chip was shown to consume 1.61 mW of power.
C1 [Tang, Adrian; Kim, Yanghyo; Xu, Yinuo; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA.
[Tang, Adrian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Tang, A (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA.
EM atang@seas.ucla.edu; yanghyokim@ucla.edu; yinuo@ucla.edu;
mfchang@ee.ucla.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD SEP
PY 2016
VL 26
IS 9
BP 729
EP 731
DI 10.1109/LMWC.2016.2597173
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA DX0PV
UT WOS:000384067100029
ER
PT J
AU Lall, P
Mirza, KM
Harsha, M
Goebel, K
AF Lall, Pradeep
Mirza, Kazi Mahmud
Harsha, Mahendra
Goebel, Kai
TI Microstructural Indicators for Assessment of Effect of Prolonged and
Intermittent Storage on Reliability of Lead-free Electronics
SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY
LA English
DT Article
DE Materials reliability; integrated circuit reliability; soldering;
integrated circuit interconnections
ID BOUNDARY-SCAN; TESTABILITY; DESIGN; BIST; BIT
AB Electronic systems may be subjected to prolonged and intermittent periods of storage prior to deployment or usage. Prior studies have shown that the lead-free solder interconnects show measurable degradation in the mechanical properties even after the brief exposures to high temperature. In this paper, a method has been developed for determining the equivalent storage time to produce identical damage at a different temperature. Electronics subjected to accelerated tests often have a well-defined thermal profile for a specified period of time. Quantification of the thermal profile in field-deployed electronics may be often difficult because of the variance in the environment conditions and usage profile. There is a need for tools and techniques to quantify the damage in deployed systems in the absence of macroindicators of damage without the knowledge of prior stress history. The approach for mapping damage in the lead-free second-level interconnects between different thermal conditions is new. High-reliability applications, such as avionics and missile systems, may be often exposed to long periods of storage prior to deployment. The effect of storage at different temperature conditions can be mapped using the presented approach. A framework has been developed to investigate the system state and estimate the remaining useful life of the solder ball subjected to a variety of isothermal aging conditions, including 60 degrees C, 75 degrees C, and 125 degrees C for periods of time between 1 and 4 weeks. Data on damage precursors, including the rate of change in the normalized phase growth and the normalized IMC thickness, has been collected and analyzed to derive physics-based damage mapping relationships for aging. Mathematical relationships have been derived for the damage mapping to various thermal storage environments to facilitate determining an appropriate time-temperature combination to reach a particular level of damage state. Activation energy for the leading indicators of failure is also computed. Specific damage proxies examined include the phase-growth indicator and the intermetallic thickness. The viability of the approach has been demonstrated for the lead-free test assemblies subjected to multiple thermal aging at 60 degrees C, 75 degrees C, and 125 degrees C. Damage mapping relationships are derived from the data based on the two separate leading indicators.
C1 [Lall, Pradeep; Mirza, Kazi Mahmud; Harsha, Mahendra] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Harsha, Mahendra] Skyworks Solut Inc, Woburn, MA 01801 USA.
[Goebel, Kai] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM lall@auburn.edu; kmm0039@tigermail.auburn.edu;
mahendra.harsha@skyworksinc.com; kai.f.goebel@nasa.gov
OI Lall, Pradeep/0000-0002-4074-937X
NR 27
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1530-4388
EI 1558-2574
J9 IEEE T DEVICE MAT RE
JI IEEE Trans. Device Mater. Reliab.
PD SEP
PY 2016
VL 16
IS 3
BP 304
EP 317
DI 10.1109/TDMR.2016.2597740
PG 14
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA DX0QP
UT WOS:000384069500005
ER
PT J
AU Thipphavong, DP
AF Thipphavong, David P.
TI Top-of-Climb Matching Method for Reducing Aircraft Trajectory Prediction
Errors
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control (GNC) Conference / AIAA Infotech
at Aerospace Conference
CY AUG 19-22, 2013
CL Boston, MA
SP AIAA
AB The inaccuracies of the aircraft performance models used by trajectory predictors with regard to takeoff weight, thrust, climb profile, and other parameters result in altitude errors during the climb phase that often exceed the vertical separation standard of 1000 ft. This study investigates the potential reduction in altitude trajectory prediction errors that could be achieved for climbing flights if just one additional parameter is made available: top-of-climb time. The top-of-climb matching method developed and evaluated in this paper is straightforward: A set of candidate trajectory predictions is generated using different aircraft weight parameters, and the one that most closely matches top of climb in terms of time is selected. This algorithm was tested using more than 1000 climbing flights in Fort Worth Center. Compared with the baseline trajectory predictions of a real-time research prototype (Center/Terminal Radar Approach Control Automation System), the top-of-climb matching method reduced the altitude root mean square error for a 5min prediction time by 38%. It also decreased the percentage of flights with absolute altitude error greater than the vertical separation standard of 1000ft for the same look-ahead time from 55 to 30%.
C1 [Thipphavong, David P.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.
[Thipphavong, David P.] AIAA, Reston, VA 20191 USA.
RP Thipphavong, DP (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.; Thipphavong, DP (reprint author), AIAA, Reston, VA 20191 USA.
NR 10
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD SEP-OCT
PY 2016
VL 53
IS 5
BP 1211
EP 1223
DI 10.2514/1.C032966
PG 13
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800003
ER
PT J
AU Brandon, JM
Morelli, EA
AF Brandon, Jay M.
Morelli, Eugene A.
TI Real-Time Onboard Global Nonlinear Aerodynamic Modeling from Flight Data
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference
CY JUN 16-20, 2014
CL Atlanta, GA
SP AIAA
ID IDENTIFICATION
AB Flight test and modeling techniques were developed to accurately identify global nonlinear aerodynamic models onboard an aircraft. The techniques were developed and demonstrated during piloted flight testing of an Aermacchi MB-326M Impala jet aircraft. Advanced piloting techniques and nonlinear modeling techniques based on fuzzy logic and multivariate orthogonal function methods were implemented with efficient onboard calculations and flight operations to achieve real-time maneuver monitoring, near-real-time global nonlinear aerodynamic modeling, and prediction validation testing in flight. Results demonstrated that global nonlinear aerodynamic models for a large portion of the flight envelope were identified rapidly and accurately using piloted flight test maneuvers during a single flight, with the final identified and validated models available before the aircraft landed.
C1 [Brandon, Jay M.] NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.
[Morelli, Eugene A.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA.
[Brandon, Jay M.; Morelli, Eugene A.] AIAA, Reston, VA 20191 USA.
RP Brandon, JM (reprint author), NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.; Brandon, JM (reprint author), AIAA, Reston, VA 20191 USA.
NR 15
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1261
EP 1297
DI 10.2514/1.C033133
PG 37
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800007
ER
PT J
AU Su, WH
Swei, SSM
Zhu, GMG
AF Su, Weihua
Swei, Sean Shan-Min
Zhu, Guoming G.
TI Optimum Wing Shape of Highly Flexible Morphing Aircraft for Improved
Flight Performance
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID NONLINEAR AEROELASTICITY; DESIGN OPTIMIZATION; BODY AIRCRAFT; DYNAMICS;
AIRFOIL
AB In this paper, optimum wing bending and torsion deformations are explored for a mission adaptive, highly flexible morphing aircraft. The complete highly flexible aircraft is modeled using a strain-based geometrically nonlinear beam formulation, coupled with unsteady aerodynamics and six-degree-of-freedom rigid-body motions. Since there are no conventional discrete control surfaces for trimming the flexible aircraft, the design space for searching the optimum wing geometries is enlarged. To achieve high-performance flight, the wing geometry is best tailored according to the specific flight mission needs. In this study, the steady level flight and the coordinated turn flight are considered, and the optimum wing deformations with the minimum drag at these flight conditions are searched by using a modal-based optimization procedure, subject to the trim and other constraints. The numerical study verifies the feasibility of the modal-based optimization approach, and it shows the resulting optimum wing configuration and its sensitivity under different flight profiles.
C1 [Su, Weihua] Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.
[Swei, Sean Shan-Min] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[Zhu, Guoming G.] Michigan State Univ, Dept Mech Engn, E Lansing, MI 48824 USA.
[Su, Weihua; Swei, Sean Shan-Min] AIAA, Reston, VA 20191 USA.
RP Su, WH (reprint author), Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.; Su, WH (reprint author), AIAA, Reston, VA 20191 USA.
EM suw@eng.ua.edu; sean.s.swei@nasa.gov; zhug@egr.msu.edu
RI Su, Weihua/F-1561-2011
OI Su, Weihua/0000-0002-4458-0524
FU NASA Ames Research Center's Summer Faculty Fellowship; NASA Aeronautics
Research Mission Directorate's Team Seedling Fund; Convergent
Aeronautics Solutions project
FX The first author acknowledges sponsorship from the NASA Ames Research
Center's Summer Faculty Fellowship. The work was partially supported by
the NASA Aeronautics Research Mission Directorate's Team Seedling Fund
and the Convergent Aeronautics Solutions project.
NR 29
TC 0
Z9 0
U1 11
U2 11
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD SEP-OCT
PY 2016
VL 53
IS 5
BP 1305
EP 1316
DI 10.2514/1.C033490
PG 12
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800009
ER
PT J
AU Perry, B
AF Perry, Boyd, III
TI Results of National Advisory Committee for Aeronautics Report Number
496: Revisited
SO JOURNAL OF AIRCRAFT
LA English
DT Article
C1 [Perry, Boyd, III] NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Perry, B (reprint author), NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
NR 7
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1561
EP +
DI 10.2514/1.C033663
PG 4
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800030
ER
PT J
AU Liao, L
Meneghini, R
Tokay, A
Bliven, LF
AF Liao, Liang
Meneghini, Robert
Tokay, Ali
Bliven, Larry F.
TI Retrieval of Snow Properties for Ku- and Ka-Band Dual-Frequency Radar
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SINGLE-SCATTERING PROPERTIES; ICE PARTICLES; FALL SPEED; SIZE;
HYDROMETEORS; PARAMETERS; APPROXIMATION; DISDROMETER; CRYSTALS; DATABASE
AB The focus of this study is on the estimation of snow microphysical properties and the associated bulk parameters such as snow water content and water equivalent snowfall rate for Ku- and Ka-band dual-frequency radar. This is done by exploring a suitable scattering model and the proper particle size distribution (PSD) assumption that accurately represent, in the electromagnetic domain, the micro-/macrophysical properties of snow. The scattering databases computed from simulated aggregates for small-to-moderate particle sizes are combined with a simple scattering model for large particle sizes to characterize snow-scattering properties over the full range of particle sizes. With use of the single-scattering results, the snow retrieval lookup tables can be formed in a way that directly links the Ku- and Ka-band radar reflectivities to snow water content and equivalent snowfall rate without use of the derived PSD parameters. A sensitivity study of the retrieval results to the PSD and scattering models is performed to better understand the dual-wavelength retrieval uncertainties. To aid in the development of the Ku- and Ka-band dual-wavelength radar technique and to further evaluate its performance, self-consistency tests are conducted using measurements of the snow PSD and fall velocity acquired from the Snow Video Imager/Particle Image Probe (SVI/PIP) during the winter of 2014 at the NASA Wallops Flight Facility site in Wallops Island, Virginia.
C1 [Liao, Liang] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA.
[Meneghini, Robert] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Tokay, Ali] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Bliven, Larry F.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM liang.liao-1@nasa.gov
FU Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement
Mission (PMM) [NNH12ZDA001N-PMM]
FX This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's
Precipitation Measurement Mission (PMM; Grant NNH12ZDA001N-PMM). The
authors also thank Mr. Jorel Torres of the South Dakota School of Mines
and Technology for providing and processing SVI/PIP data, and Dr.
Kwo-Sen Kuo of the University of Maryland for providing the scattering
database.
NR 40
TC 0
Z9 0
U1 3
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 1845
EP 1858
DI 10.1175/JAMC-D-15-0355.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100001
ER
PT J
AU Bedka, KM
Khlopenkov, K
AF Bedka, Kristopher M.
Khlopenkov, Konstantin
TI A Probabilistic Multispectral Pattern Recognition Method for Detection
of Overshooting Cloud Tops Using Passive Satellite Imager Observations
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PROFILING RADAR OBSERVATIONS; STRATOSPHERIC WATER-VAPOR; GOES-R;
PRECIPITATION SYSTEMS; GLOBAL DISTRIBUTION; SEVERE WEATHER;
CLIMATE-CHANGE; CONVECTION
AB Deep convective updrafts often penetrate through the surrounding cirrus anvil and into the lower stratosphere. Cross-tropopause transport of ice, water vapor, and chemicals occurs within these "overshooting tops'' (OTs) along with a variety of hazardous weather conditions. OTs are readily apparent in satellite imagery, and, given the importance of OTs for weather and climate, a number of automated satellite-based detection methods have been developed. Some of these methods have proven to be relatively reliable, and their products are used in diverse Earth science applications. Nevertheless, analysis of these methods and feedback from product users indicate that use of fixed infrared temperature-based detection criteria often induces biases that can limit their utility for weather and climate analysis. This paper describes a new multispectral OT detection approach that improves upon those previously developed by minimizing use of fixed criteria and incorporating pattern recognition analyses to arrive at an OT probability product. The product is developed and validated using OT and non-OT anvil regions identified by a human within MODIS imagery. The product offered high skill for discriminating between OTs and anvils and matched 69% of human OT identifications for a particular probability threshold with a false-detection rate of 18%, outperforming previously existing methods. The false-detection rate drops to 1% when OT-induced texture detected within visible imagery is used to constrain the IR-based OT probability product. The OT probability product is also shown to improve severe-storm detection over the United States by 20% relative to the best existing method.
C1 [Bedka, Kristopher M.] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
[Khlopenkov, Konstantin] Sci Syst & Applicat Inc, Hampton, VA USA.
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. We thank Patrick Minnis and Christopher Velden
for their advice and collaboration throughout the algorithm-development
process. We thank Cameron Homeyer for providing the WSR-88D data shown
in this paper. We also thank Jake Smith for manually identifying OT
locations in GOES-14 satellite imagery.
NR 41
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Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 1983
EP 2005
DI 10.1175/JAMC-D-15-0249.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100008
ER
PT J
AU Magi, BI
Winesett, T
Cecil, DJ
AF Magi, Brian I.
Winesett, Thomas
Cecil, Daniel. J.
TI Estimating Lightning from Microwave Remote Sensing Data
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID CLIMATE DATA RECORD; UNITED-STATES; SSM/I SENSORS; PART I; CLOUD;
THUNDERSTORMS; RATES; EARTH; FIRE; IMAGER/SOUNDER
AB This study evaluates a method for estimating the cloud-to-ground (CG) lightning flash rate from microwave remote sensing data. Defense Meteorological Satellite Program satellites have been in operation since 1987 and include global-viewing microwave sensors that capture thunderstorms as brightness temperature depressions. The National Lightning Detection Network (NLDN) has monitored CG lightning in the United States since 1997. This study investigates the relationship between CG lightning and microwave brightness temperature fields for the contiguous United States from April to September for the years 2005-12. The findings suggest that an exponential function, empirically fit to the NLDN and SSM/I data, provides lightning count measurements that agree to within 60%-70% with NLDN lightning, but with substantial misses and false alarms in the predictions. The discrepancies seem to be attributable to regional differences in thunderstorm characteristics that require a detailed study at smaller spatial scales to truly resolve, but snow at higher elevations also produces some anomalous microwave temperature depressions similar to those of thunderstorms. The results for the contiguous United States in this study are a step toward potentially using SSM/I data to estimate CG lightning around the world, although the sensitivity of the results to regional differences related to meteorological regimes would need further study.
C1 [Magi, Brian I.; Winesett, Thomas] Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA.
[Cecil, Daniel. J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
RP Magi, BI (reprint author), Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA.
EM brian.magi@uncc.edu
OI Magi, Brian/0000-0001-8131-0083
FU North Carolina Space Grant Consortium's New Investigator Program; UNC
Charlotte faculty research grant; Lightning Imaging Sensor (LIS) team
via the NASA Tropical Rainfall Measuring Mission
FX The authors thank the staff at the Precipitation Research Group at
Colorado State University for maintaining and managing the SSM/I data
distribution. BIM and TW were partially supported by the North Carolina
Space Grant Consortium's New Investigator Program. BIM was also
partially supported by a UNC Charlotte faculty research grant. DJC was
supported through the Lightning Imaging Sensor (LIS) team via the NASA
Tropical Rainfall Measuring Mission.
NR 46
TC 0
Z9 0
U1 4
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 2021
EP 2036
DI 10.1175/JAMC-D-15-0306.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100010
ER
PT J
AU Huang, XL
Chen, XH
Zhou, DK
Liu, X
AF Huang, Xianglei
Chen, Xiuhong
Zhou, Daniel K.
Liu, Xu
TI An Observationally Based Global Band-by-Band Surface Emissivity Dataset
for Climate and Weather Simulations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SEA-SURFACE; ALGORITHM; DATABASE; WINDOW; MODEL; SNOW; ICE
AB While current atmospheric general circulation models (GCMs) still treat the surface as a blackbody in their longwave radiation scheme, recent studies suggest the need for taking realistic surface spectral emissivity into account. There have been few measurements available for the surface emissivity in the far IR (<650 cm(-1)). Based on first-principle calculation, the authors compute the spectral emissivity over the entire longwave spectrum for a variety of surface types. MODIS-retrieved mid-IR surface emissivity at 0.05 degrees x 0.05 degrees spatial resolution is then regressed against the calculated spectral emissivity to determine the surface type for each grid. The derived spectral emissivity data are then spatially averaged onto 0.5 degrees x 0.5 degrees grids and spectrally integrated onto the bandwidths used by the RRTMG_LW-a longwave radiation scheme widely used in current climate and numerical weather models. The band-by-band surface emissivity dataset is then compared with retrieved surface spectral emissivities from Infrared Atmospheric Sounding Interferometer (IASI) measurements. The comparison shows favorable agreement between two datasets in all the bands covered by the IASI measurements. The authors further use the dataset in conjunction with ERA-Interim to evaluate its impact on the top-of-atmosphere radiation budget. Depending on the blackbody surface assumptions used in the original calculation, the globally averaged difference caused by the inclusion of realistic surface emissivity ranges from -1.2 to -1.5 W m(-2) for clear-sky OLR and from -0.67 to -0.94 W m(-2) for all-sky OLR. Moreover, the difference is not spatially uniform and has a distinct spatial pattern.
C1 [Huang, Xianglei; Chen, Xiuhong] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Zhou, Daniel K.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM xianglei@umich.edu
FU DOE Office of Biological and Environmental Research [DE-SC0012969]; NASA
[NNX15AC25G]
FX We wish to thank three anonymous reviewers for their thorough and
thoughtful comments, which improved the clarity of the presentation. The
ECMWF-Interim data were obtained from http://apps.ecmwf.int/datasets/.
The MODIS retrievals of surface emissivity were from
ftp://ftp.ssec.wisc.edu/pub/g_emis/. This research is supported by DOE
Office of Biological and Environmental Research under Grant DE-SC0012969
and by NASA under Grant NNX15AC25G awarded to the University of
Michigan.
NR 36
TC 0
Z9 0
U1 1
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3541
EP 3555
DI 10.1175/JAS-D-15-0355.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500011
ER
PT J
AU Guimond, SR
Heymsfield, GM
Reasor, PD
Didlake, AC
AF Guimond, Stephen R.
Heymsfield, Gerald M.
Reasor, Paul D.
Didlake, Anthony C., Jr.
TI The Rapid Intensification of Hurricane Karl (2010): New Remote Sensing
Observations of Convective Bursts from the Global Hawk Platform
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID TROPICAL CYCLONE INTENSIFICATION; HIGH-RESOLUTION SIMULATION;
INNER-CORE; PART I; 3-DIMENSIONAL PERTURBATIONS; DOPPLER RADAR; BONNIE
1998; EVOLUTION; EYEWALL; EYE
AB The evolution of rapidly intensifying Hurricane Karl (2010) is examined from a suite of remote sensing observations during the NASA Genesis and Rapid Intensification Processes (GRIP) field experiment. The novelties of this study are in the analysis of data from the airborne Doppler radar High-Altitude Imaging Wind and Rain Airborne Profiler (HI WRAP) and the new Global Hawk airborne platform that allows long endurance sampling of hurricanes. Supporting data from the High-Altitude Monolithic Microwave Integrated Circuit (MMIC) Sounding Radiometer (HAMSR) microwave sounder coincident with HIWRAP and coordinated flights with the NOAA WP-3D aircraft help to provide a comprehensive understanding of the storm. The focus of the analysis is on documenting and understanding the structure, evolution, and role of small-scale deep convective forcing in the storm intensification process. Deep convective bursts are sporadically initiated in the downshear quadrants of the storm and rotate into the upshear quadrants for a period of similar to 12 h during the rapid intensification. The aircraft data analysis indicates that the bursts are being formed and maintained through a combination of two main processes: 1) convergence generated from counterrotating mesovortex circulations and the larger vortex-scale flow and 2) the turbulent (scales of similar to 25 km) transport of anomalously warm, buoyant air from the eye to the eyewall at low levels. The turbulent mixing across the eyewall interface and forced convective descent adjacent to the bursts assists in carving out the eye of Karl, which leads to an asymmetric enhancement of the warm core. The mesovortices play a key role in the evolution of the features described above. The Global Hawk aircraft allowed an examination of the vortex response and axisymmetrization period in addition to the burst pulsing phase. A pronounced axisymmetric development of the vortex is observed following the pulsing phase that includes a sloped eyewall structure and formation of a clear, wide eye.
C1 [Guimond, Stephen R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Guimond, Stephen R.; Heymsfield, Gerald M.; Didlake, Anthony C., Jr.] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
[Reasor, Paul D.] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA.
[Didlake, Anthony C., Jr.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
RP Guimond, SR (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM stephen.guimond@nasa.gov
RI Reasor, Paul/B-2932-2014
OI Reasor, Paul/0000-0001-6407-017X
FU Heymsfield's NASA GRIP through NASA; Heymsfield's NASA HS3 through NASA;
NOAA; NASA; Institute of Geophysics and Planetary Physics (IGPP) at Los
Alamos National Laboratory
FX We thank Dr. Lihua Li, Matt McLinden, Martin Perrine, and Jaime
Cervantes for their engineering efforts on HIWRAP during GRIP. We also
thank the JPL HAMSR team for providing level 1B data used in this study,
which was obtained from NASA Global Hydrology Resource Center in
Huntsville, Alabama. Discussions with Dr. Scott Braun were useful and
helped to clarify the presentation of the data. Dr. Lin Tian helped with
early HIWRAP data processing. Author Guimond and coauthors Heymsfield
and Didlake were funded under Heymsfield's NASA GRIP and HS3 funding,
through NASA headquarters Program Manager Dr. Ramesh Kakar. Coauthor
Reasor was funded through NOAA base funds. The NASA weather program
under Dr. Ramesh Kakar supported GRIP. The first author was also
partially supported by the Institute of Geophysics and Planetary Physics
(IGPP) at Los Alamos National Laboratory. The first author thanks Robert
Kilgore for his work on the conceptual diagram. Finally, we thank Rob
Rogers and two anonymous reviewers for their very helpful comments.
NR 47
TC 1
Z9 1
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3617
EP 3639
DI 10.1175/JAS-D-16-0026.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500016
ER
PT J
AU Lin, Y
Wang, Y
Pan, BW
Hu, JX
Liu, YG
Zhang, RY
AF Lin, Yun
Wang, Yuan
Pan, Bowen
Hu, Jiaxi
Liu, Yangang
Zhang, Renyi
TI Distinct Impacts of Aerosols on an Evolving Continental Cloud Complex
during the RACORO Field Campaign
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID DEEP CONVECTIVE CLOUDS; FINE PARTICULATE MATTER; LONG-TERM IMPACTS;
ANTHROPOGENIC AEROSOLS; SHALLOW CUMULUS; MICROPHYSICS PARAMETERIZATION;
STRATOCUMULUS CLOUDS; ABSORBING AEROSOLS; RESOLVING MODEL; CLIMATE
MODELS
AB A continental cloud complex, consisting of shallow cumuli, a deep convective cloud (DCC), and stratus, is simulated by a cloud-resolving Weather Research and Forecasting Model to investigate the aerosol micro physical effect (AME) and aerosol radiative effect (ARE) on the various cloud regimes and their transitions during the Department of Energy Routine Atmospheric Radiation Measurement Aerial Facility Clouds with Low Optical Water Depths Optical Radiative Observations (RACORO) campaign. Under an elevated aerosol loading with AME only, a reduced cloudiness for the shallow cumuli and stratus resulted from more droplet evaporation competing with suppressed precipitation, but an enhanced cloudiness for the DCC is attributed to more condensation. With the inclusion of ARE, the shallow cumuli are suppressed owing to the thermodynamic effects of light-absorbing aerosols. The responses of DCC and stratus to aerosols are monotonic with AME only but nonmonotonic with both AME and ARE. The DCC is invigorated because of favorable convection and moisture conditions at night induced by daytime ARE, via the so-called aerosol-enhanced conditional instability mechanism. The results reveal that the overall aerosol effects on the cloud complex are distinct from the individual cloud types, highlighting that the aerosol cloud interactions for diverse cloud regimes and their transitions need to be evaluated to assess the regional and global climatic impacts.
C1 [Lin, Yun; Pan, Bowen; Hu, Jiaxi; Zhang, Renyi] Texas A&M Univ, College Stn, TX USA.
[Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, Oceanog & Meteorol Bldg,Room 1108,MS 3150, College Stn, TX 77843 USA.
EM renyi-zhang@tamu.edu
OI Lin, Yun/0000-0001-8222-0346
FU DOE's Earth System Modeling (ESM) Program via the FASTER project
[DOE-DE-AC02-98CH10886]; NASA [ROSES14-ACMAP, 105357-281945.02.31.03.24]
FX This research is supported by DOE's Earth System Modeling (ESM) Program
via the FASTER project (www.bnl.gov/faster), under Grant
DOE-DE-AC02-98CH10886. The RACORO field campaign was supported by DOE's
ARM program. We are grateful for discussions on RACORO with Dr. Andrew
Vogelmann at BNL and on aerosol microphysics effects on various clouds
with Dr. Jonathan H. Jiang at JPL. The data from the RACORO field
campaign, utilized only for education and research, are open to public
after registration and application. Supercomputing computational
facilities were provided by the Texas A&M University. Yuan Wang's
contribution to this work was sponsored by NASA ROSES14-ACMAP and was
carried at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA (Grant
105357-281945.02.31.03.24).
NR 93
TC 0
Z9 0
U1 9
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 SEP
PY 2016
VL 73
IS 9
BP 3681
EP 3700
DI 10.1175/JAS-D-15-0361.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500019
ER
PT J
AU Holt, LA
Alexander, MJ
Coy, L
Molod, A
Putman, W
Pawson, S
AF Holt, Laura A.
Alexander, M. Joan
Coy, Lawrence
Molod, Andrea
Putman, William
Pawson, Steven
TI Tropical Waves and the Quasi-Biennial Oscillation in a 7-km Global
Climate Simulation
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; COUPLED EQUATORIAL WAVES; QBO-LIKE
OSCILLATION; GRAVITY-WAVES; CONVECTION; TEMPERATURE; PARAMETERIZATION;
STRATOSPHERE; IMPROVEMENTS; VARIABILITY
AB This study investigates tropical waves and their role in driving a quasi-biennial oscillation (QBO)-like signal in stratospheric winds in a global 7-km-horizontal-resolution atmospheric general circulation model. The Nature Run (NR) is a 2-yr global mesoscale simulation of the Goddard Earth Observing System Model, version 5 (GEOS-5). In the tropics, there is evidence that the NR supports a broad range of convectively generated waves. The NR precipitation spectrum resembles the observed spectrum in many aspects, including the preference for westward-propagating waves. However, even with very high horizontal resolution and a healthy population of resolved waves, the zonal force provided by the resolved waves is still too low in the QBO region and parameterized gravity wave drag is the main driver of the NR-QBO-like oscillation (NR-QBO). The authors suggest that causes include coarse vertical resolution and excessive dissipation. Nevertheless, the very-high-resolution NR provides an opportunity to analyze the resolved wave forcing of the NR-QBO. In agreement with previous studies, large-scale Kelvin and small-scale waves contribute to the NR-QBO driving in eastward shear zones and small-scale waves dominate the NR-QBO driving in westward shear zones. Waves with zonal wavelength < 1000 km account for up to half of the small-scale (<3300 km) resolved wave forcing in eastward shear zones and up to 70% of the small-scale resolved wave forcing in westward shear zones of the NR-QBO.
C1 [Holt, Laura A.; Alexander, M. Joan] NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA.
[Coy, Lawrence; Putman, William; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Coy, Lawrence] Sci Syst & Applicat Inc, Lanham, MD USA.
[Molod, Andrea] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Holt, LA (reprint author), NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA.
EM laura@nwra.com
FU NASA Global Modeling and Assimilation Office [NNX14O76G]; NASA's
Modeling, Analysis and Prediction (MAP) program
FX We thank Dr. Ji-Eun Kim for providing the TRMM spectrum for Fig. 2, and
we thank three anonymous reviewers for their thoughtful and helpful
suggestions. This work is funded by the NASA Global Modeling and
Assimilation Office, Grant NNX14O76G. This work was also supported by
NASA's Modeling, Analysis and Prediction (MAP) program.
NR 51
TC 2
Z9 2
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3771
EP 3783
DI 10.1175/JAS-D-15-0350.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500024
ER
PT J
AU Thurman, D
Poinsatte, P
Ameri, A
Culley, D
Raghu, S
Shyam, V
AF Thurman, Douglas
Poinsatte, Philip
Ameri, Ali
Culley, Dennis
Raghu, Surya
Shyam, Vikram
TI Investigation of Spiral and Sweeping Holes
SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME
LA English
DT Article
AB Surface infrared thermography, hotwire anemometry, and thermocouple surveys were performed on two new film cooling hole geometries: spiral/rifled holes and fluidic sweeping holes. The spiral holes attempt to induce large-scale vorticity to the film cooling jet as it exits the hole to prevent the formation of the kidney-shaped vortices commonly associated with film cooling jets. The fluidic sweeping hole uses a passive in-hole geometry to induce jet sweeping at frequencies that scale with blowing ratios. The spiral hole performance is compared to that of round holes with and without compound angles. The fluidic hole is of the diffusion class of holes and is therefore compared to a 777 hole and square holes. A patent-pending spiral hole design showed the highest potential of the nondiffusion-type hole configurations. Velocity contours and flow temperature were acquired at discreet cross sections of the downstream flow field. The passive fluidic sweeping hole shows the most uniform cooling distribution but suffers from low span-averaged effectiveness levels due to enhanced mixing. The data were taken at a Reynolds number of 11,000 based on hole diameter and freestream velocity. Infrared thermography was taken for blowing ratios of 1.0, 1.5, 2.0, and 2.5 at a density ratio of 1.05. The flow inside the fluidic sweeping hole was studied using 3D unsteady Reynolds-average Navier-Stokes (RANS).
C1 [Thurman, Douglas] US Army Res Lab, Cleveland, OH 44135 USA.
[Poinsatte, Philip; Culley, Dennis; Shyam, Vikram] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Ameri, Ali] Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA.
[Raghu, Surya] Adv Fluid LLC, Columbia, MD 21045 USA.
RP Thurman, D (reprint author), US Army Res Lab, Cleveland, OH 44135 USA.
EM drthurman@nasa.gov; poinsatte@nasa.gov; ali.a.ameri@nasa.gov;
dennis.e.culley@nasa.gov; sraghu@advancedfluidics.com;
vikram.shyam-1@nasa.gov
FU NASA's Fundamental Aeronautics Program's Fixed Wing Project; NASA's
Center Innovation Fund
FX This work was funded by NASA's Fundamental Aeronautics Program's Fixed
Wing Project and NASA's Center Innovation Fund. The authors would also
like to thank Dr. Mark Wernet and Dr. Adam Wroblewski for the particle
image velocimetry results.
NR 15
TC 0
Z9 0
U1 0
U2 0
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0889-504X
EI 1528-8900
J9 J TURBOMACH
JI J. Turbomach.-Trans. ASME
PD SEP
PY 2016
VL 139
IS 9
AR 091007
DI 10.1115/1.4032839
PG 11
WC Engineering, Mechanical
SC Engineering
GA DX3BE
UT WOS:000384246800007
ER
PT J
AU Abarca, SF
Montgomery, MT
Braun, SA
Dunion, J
AF Abarca, Sergio F.
Montgomery, Michael T.
Braun, Scott A.
Dunion, Jason
TI On the Secondary Eyewall Formation of Hurricane Edouard (2014)
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID TROPICAL CYCLONES; RITA 2005; REPLACEMENT; INTENSITY; EVOLUTION;
DYNAMICS; VORTEX; CORE; CYCLE; FIELD
AB A first observationally based estimation of departures from gradient wind balance during secondary eyewall formation is presented. The study is based on the Atlantic Hurricane Edouard (2014). This storm was observed during the National Aeronautics and Space Administration's (NASA) Hurricane and Severe Storm Sentinel (HS3) experiment, a field campaign conducted in collaboration with the National Oceanic and Atmospheric Administration (NOAA). A total of 135 dropsondes are analyzed in two separate time periods: one named the secondary eyewall formation period and the other one referred to as the decaying double eyewalled storm period. During the secondary eyewall formation period, a time when the storm was observed to have only one eyewall, the diagnosed agradient force has a secondary maximum that coincides with the radial location of the secondary eyewall observed in the second period of study. The maximum spinup tendency of the radial influx of absolute vertical vorticity is within the boundary layer in the region of the eyewall of the storm and the spinup tendency structure elongates radially outward into the secondary region of supergradient wind, where the secondary wind maximum is observed in the second period of study. An analysis of the boundary layer averaged vertical structure of equivalent potential temperature reveals a conditionally unstable environment in the secondary eyewall formation region. These findings support the hypothesis that deep convective activity in this region contributed to spinup of the boundary layer tangential winds and the formation of a secondary eyewall that is observed during the decaying double eyewalled storm period.
C1 [Abarca, Sergio F.] Natl Ocean & Atmospher Adm, IM Syst Grp, Natl Ctr Environm Protect, Natl Weather Serv, College Pk, MD USA.
[Montgomery, Michael T.] Naval Postgrad Sch, Monterey, CA USA.
[Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Dunion, Jason] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA.
[Dunion, Jason] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA.
RP Abarca, SF (reprint author), NOAA, IM Syst Grp, NWS, NCEP, 5830 Univ Res Court, College Pk, MD 20740 USA.
EM sergio.abarca@noaa.gov
RI Dunion, Jason/B-1352-2014
OI Dunion, Jason/0000-0001-7489-0569
FU National Research Council (NRC) through Research Associateship Program;
Naval Postgraduate School (NPS) in Monterey, California; NSF
[AGS-1313948]; NOAA HFIP Grant [N0017315WR00048]; NASA HS3 Grant
[NNG11PK021]; U.S. Naval Postgraduate School
FX The first author gratefully acknowledges the support from the National
Research Council (NRC) through its Research Associateship Program; the
host institution, the Naval Postgraduate School (NPS) in Monterey,
California; and Scott Braun for the funding that made it possible for
him to participate in the H53 deployment during the 2014 hurricane
season. MTM acknowledges the support of NSF Grant AGS-1313948, NOAA HFIP
Grant N0017315WR00048, NASA HS3 Grant NNG11PK021, and the U.S. Naval
Postgraduate School.
NR 37
TC 0
Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD SEP
PY 2016
VL 144
IS 9
BP 3321
EP 3331
DI 10.1175/MWR-D-15-0421.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RN
UT WOS:000383923300014
ER
PT J
AU Lee, JH
Biging, GS
Fisher, JB
AF Lee, Jun-Hak
Biging, Gregory S.
Fisher, Joshua B.
TI An Individual Tree-Based Automated Registration of Aerial Images to
Lidar Data in a Forested Area
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID MULTISPECTRAL DATA FUSION; AIRBORNE LASER SCANNER; CROWN DETECTION;
LAND-COVER; DELINEATION; HEIGHT; CLASSIFICATION; RECONSTRUCTION;
SEGMENTATION; MOSAICKING
AB In this paper, we demonstrate an approach to align aerial images to airborne lidar data by using common object features (tree tops) from both data sets under the condition that conventional correlation-based approaches are challenging due to the fact that the spatial pattern of pixel gray-scale values in aerial images hardly exist in lidar data. We extracted tree tops by using an image processing technique called extended-maxima transformation from both aerial images and lidar data. Our approach was tested at the Angelo Coast Range Reserve on the South Fork Eel River forests in Mendocino County, California. Although the aerial images were acquired simultaneously with the lidar data, the images had only approximate exposure point locations and average flight elevation information, which mimicked the condition of limited information availability about the aerial images. Our results showed that this approach enabled us to align aerial images to airborne lidar data at the single-tree level with reasonable accuracy. With a local transformation model (piecewise linear model), the RMSE and the median absolute deviation (MAD) of the registration were 9.2 pixels (2.3 meters) and 6.8 pixels (1.41 meters), respectively. We expect our approach to be applicable to fine scale change detection for forest ecosystems and may serve to extract detailed forest biophysical parameters.
C1 [Lee, Jun-Hak] Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA.
[Biging, Gregory S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, JH (reprint author), Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA.
EM junhaklee@uoregon.edu
FU W.S. Rosecrans Fellowship, Environmental Science, Policy, and
Management, University of California, Berkeley; National Aeronautics and
Space Administration
FX We gratefully acknowledge the use of lidar data sets supplied by Dr.
William E. Dietrich and the National Center of Airborne Laser Mapping
(NCALM). The first author was partially funded by the W.S. Rosecrans
Fellowship, Environmental Science, Policy, and Management, University of
California, Berkeley. Dr. Joshua B. Fisher contributed to this paper
through work by the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 60
TC 0
Z9 0
U1 12
U2 12
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
EI 2374-8079
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD SEP
PY 2016
VL 82
IS 9
BP 699
EP 710
DI 10.14358/PERS.82.9.699
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA DX0NR
UT WOS:000384060300007
ER
PT J
AU Mendez-Villanueva, A
Suarez-Arrones, L
Rodas, G
Fernandez-Gonzalo, R
Tesch, P
Linnehan, R
Kreider, R
Di Salvo, V
AF Mendez-Villanueva, Alberto
Suarez-Arrones, Luis
Rodas, Gil
Fernandez-Gonzalo, Rodrigo
Tesch, Per
Linnehan, Richard
Kreider, Richard
Di Salvo, Valter
TI MRI-Based Regional Muscle Use during Hamstring Strengthening Exercises
in Elite Soccer Players
SO PLOS ONE
LA English
DT Article
ID MEDICAL-RESEARCH PROGRAM; PROFESSIONAL FOOTBALL; ECCENTRIC OVERLOAD;
NONUNIFORM CHANGES; INJURIES; PREVENTION; MECHANICS; STRAINS; SCIENCE;
RETURN
AB The present study examined site-specific hamstring muscles use with functional magnetic resonance imaging (MRI) in elite soccer players during strength training. Thirty-six players were randomized into four groups, each performing either Nordic hamstring, flywheel legcurl, Russian belt or the hip-extension conic-pulley exercise. The transverse relaxation time (T-2) shift from pre-to post-MRI were calculated for the biceps femoris long (BFI) and short (BFs) heads, semitendinosus (ST) and semimembranosus (SM) muscles at proximal, middle and distal areas of the muscle length. T-2 values increased substantially after flywheel leg-curl in all regions of the BFI (from 9 +/- 8 to 16 +/- 8%), BFs (41 +/- 6-71 +/- 11%), and ST (60 +/- 1-69 +/- 7%). Nordic hamstring induced a substantial T2 increase in all regions of the BFs (13 +/- 8-16 +/- 5%) and ST (15 +/- 7-17 +/- 5%). T-2 values after the Russian belt deadlift substantially increased in all regions of the BFI (6 +/- 4-7 +/- 5%), ST (8 +/- 3-11 +/- 2%), SM (6 +/- 4-10 +/- 4%), and proximal and distal regions of BFs (6 +/- 6-8 +/- 5%). T-2 values substantially increased after hip-extension conic-pulley only in proximal and middle regions of BFI (11 +/- 5-7 +/- 5%) and ST (7 +/- 3-12 +/- 4%). The relevance of such MRI-based inter-and intra-muscle use in designing more effective resistance training for improving hamstring function and preventing hamstring injuries in elite soccer players should be explored with more mechanistic studies.
C1 [Mendez-Villanueva, Alberto; Suarez-Arrones, Luis; Di Salvo, Valter] ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar.
[Suarez-Arrones, Luis] Pablo de Olavide Univ, Sports Dept, Seville, Spain.
[Rodas, Gil] Futbol Club Barcelona, Dept Med, Barcelona, Spain.
[Fernandez-Gonzalo, Rodrigo; Tesch, Per] Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden.
[Linnehan, Richard] Johnson Space Ctr, Natl Aeronaut & Space Adm, Houston, TX USA.
[Kreider, Richard] Texas A&M Univ, Dept Hlth & Kinesiol, College Stn, TX USA.
[Di Salvo, Valter] Univ Rome Foro Italico, Dept Movement Human & Hlth Sci, Rome, Italy.
RP Mendez-Villanueva, A (reprint author), ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar.
EM jose.villanueva@aspire.qa
FU NPRP grant from the Qatar National Research Fund [NPRP 6-1526-3-363]
FX This study was made possible by NPRP grant #NPRP 6-1526-3-363 from the
Qatar National Research Fund (a member of Qatar Foundation). The funder
provided support in the form of salaries for authors LSA, RFG and PT,
but did not have any additional role in the study design, data
collection and analysis, decision to publish, or preparation of the
manuscript. The specific roles of these authors are articulated in the
'author contributions' section.
NR 31
TC 0
Z9 0
U1 14
U2 14
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD SEP 1
PY 2016
VL 11
IS 9
AR e0161356
DI 10.1371/journal.pone.0161356
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV3WN
UT WOS:000382855600024
PM 27583444
ER
PT J
AU Ayers, A
Miller, K
Park, J
Schwartz, L
Antcliff, R
AF Ayers, Alan
Miller, Kimberly
Park, Jongwon
Schwartz, Lawrence
Antcliff, Rich
TI The Hollywood Model Leveraging the Capabilities of Freelance Talent to
Advance Innovation and Reduce Risk
SO RESEARCH-TECHNOLOGY MANAGEMENT
LA English
DT Article
DE Hollywood model; Talent management; Futures; IRI2038; IRI Research
ID ERA
AB In 2013, the Industrial Research Institute (IRI) commissioned the IRI2038 foresight project to research how developments in technology, business processes, regulation and other spheres will impact the art and science of research and technology management over the next 25 years. That study defined three scenarios likely to shape the innovation process in coming years. One of those scenarios was the Hollywood model, in which scientists, engineers, and innovators no longer work for a single firm but rather contract out their services to individual projects and then move on to other projects and companies. Over the course of six months, an IRI Research working group conducted four workshops with R&D leaders at IRI member companies to explore how talent management would be affected in this scenario. The workshops identified challenges and opportunities associated with the Hollywood model as a paradigm for industrial R&D, focused around eight critical aspects of current talent management practice. Although the Hollywood model faces significant infrastructure and legal impediments today, its employment of external R&D workers with diverse experiences and perspectives is likely to create a greater opportunity for significant innovation.
C1 [Ayers, Alan] UConn, Storrs, CT 06269 USA.
[Ayers, Alan] IDCC, Doha, Qatar.
[Ayers, Alan] Research on Res Comm, Arlington, VA 22203 USA.
[Ayers, Alan] ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA.
[Miller, Kimberly] Sutton House Consulting LLC, Florence, OR USA.
[Miller, Kimberly] Cargills Global R&D Team, Minneapolis, MN USA.
[Miller, Kimberly] Univ St Thomas, Org Dev, St Paul, MN USA.
[Park, Jongwon] Korea Innovat Ctr, Washington, DC USA.
[Park, Jongwon] Arizona State Univ, Consortium Sci Policy & Outcomes, Tempe, AZ 85287 USA.
[Schwartz, Lawrence] IP Business Tech Solut, Menlo Pk, CA USA.
[Antcliff, Rich] NASA, Langley Res Ctr, Off Strateg Anal Commun & Business Dev, Hampton, VA 23665 USA.
RP Ayers, A (reprint author), UConn, Storrs, CT 06269 USA.; Ayers, A (reprint author), IDCC, Doha, Qatar.; Ayers, A (reprint author), Research on Res Comm, Arlington, VA 22203 USA.; Ayers, A (reprint author), ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA.
EM adayers@buildinnovation.com; kim@suttonhouseconsulting.com;
jpglobalconsultingllc@gmail.com; larryschwartz333@aol.com;
Richard.R.Antcliff@nasa.gov
NR 18
TC 0
Z9 0
U1 15
U2 15
PU INDUSTRIAL RESEARCH INST, INC
PI ARLINGTON
PA 2300 CLARENDON BLVD, STE 400, ARLINGTON, VA 22201 USA
SN 0895-6308
EI 1930-0166
J9 RES TECHNOL MANAGE
JI Res.-Technol. Manage.
PD SEP-OCT
PY 2016
VL 59
IS 5
BP 27
EP 37
DI 10.1080/08956308.2016.1208041
PG 11
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA DX6ZQ
UT WOS:000384535600009
ER
PT J
AU Haarig, M
Engelmann, R
Ansmann, A
Veselovskii, I
Whiteman, DN
Althausen, D
AF Haarig, Moritz
Engelmann, Ronny
Ansmann, Albert
Veselovskii, Igor
Whiteman, David N.
Althausen, Dietrich
TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio
profiling: cirrus case study
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL
PLUME; MULTIWAVELENGTH LIDAR; SAHARAN DUST; WATER-VAPOR;
PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL
AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinction-to-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution.
C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia.
[Whiteman, David N.] NASA, GSFC, Greenbelt, MD USA.
RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany.
EM haarig@tropos.de
FU Russian Science Foundation [16-17-10241]
FX We thank Johannes Buhl for providing Doppler lidar observations of
vertical velocity and estimated ice crystal sizes. Modeling of the
rotational Raman filter parameters was supported by the Russian Science
Foundation (project no. 16-17-10241).
NR 63
TC 0
Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD SEP 1
PY 2016
VL 9
IS 9
BP 4269
EP 4278
DI 10.5194/amt-9-4269-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8FZ
UT WOS:000383891500002
ER
PT J
AU Diskin, B
Thomas, JL
Rumsey, CL
Schwoppe, A
AF Diskin, Boris
Thomas, James L.
Rumsey, Christopher L.
Schwoeppe, Axel
TI Grid-Convergence of Reynolds-Averaged Navier-Stokes Solutions for
Benchmark Flows in Two Dimensions
SO AIAA JOURNAL
LA English
DT Article
ID TURBULENCE MODEL; EULER EQUATIONS
AB A detailed grid-convergence study has been conducted to establish reference solutions corresponding to the one-equation linear eddy-viscosity Spalart-Allmaras turbulence model for two-dimensional turbulent flows around the NACA0012 airfoil and a flat plate. The study involved the three widely used codes CFL3D (NASA), FUN3D (NASA), and TAU (DLR, The German Aerospace Center), as well as families of uniformly refined structured grids that differed in the grid density patterns. Solutions computed by different codes on different grid families appeared to converge to the same continuous limit but exhibited strikingly different convergence characteristics. The grid resolution in the vicinity of geometric singularities, such as a sharp trailing edge, was found to be the major factor affecting accuracy and convergence of discrete solutions; the effects of this local grid resolution were more prominent than differences in discretization schemes and/or grid elements. The results reported for these relatively simple turbulent flows demonstrated that CFL3D, FUN3D, and TAU solutions were very similar on the finest grids used in the study, but even those grids were not sufficient to conclusively establish an asymptotic convergence order.
C1 [Diskin, Boris] Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA.
[Thomas, James L.; Rumsey, Christopher L.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Schwoeppe, Axel] German Aerosp Ctr, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
[Diskin, Boris] Univ Virginia, Charlottesville, VA 22904 USA.
RP Diskin, B (reprint author), Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA.
FU NASA [NNL09AA00A]
FX The first author acknowledges support from NASA Cooperative Agreement
NNL09AA00A.
NR 38
TC 0
Z9 0
U1 3
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 SEP
PY 2016
VL 54
IS 9
BP 2563
EP 2588
DI 10.2514/1.J054555
PG 26
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600002
ER
PT J
AU Pandya, MJ
Diskin, B
Thomas, JL
Frink, NT
AF Pandya, Mohagna J.
Diskin, Boris
Thomas, James L.
Frink, Neal T.
TI Improved Convergence and Robustness of USM3D Solutions on Mixed-Element
Grids
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 53rd AIAA Aerospace Sciences Meeting / AIAA Atmospheric Flight Mechanics
Conference / 17th AIAA Non-Deterministic Approaches Conference / AIAA
Science and Technology Forum and Exposition (SciTech) / AIAA Infotech at
Aerospace Conference
CY JAN 05-09, 2015
CL Kissimmee, FL
SP AIAA
ID EULER EQUATIONS; GENERATION; ALGORITHM; DYNAMICS; TETRUSS; FLOWS; CODES
AB Several improvements to the mixed-element USM3D discretization and defect-correction schemes have been made. A new methodology for nonlinear iterations, called the Hierarchical Adaptive Nonlinear Iteration Method, has been developed and implemented. The Hierarchical Adaptive Nonlinear Iteration Method provides two additional hierarchies around a simple and approximate preconditioner of USM3D. The hierarchies are a matrix-free linear solver for the exact linearization of Reynolds-averaged Navier-Stokes equations and a nonlinear control of the solution update. Two variants of the Hierarchical Adaptive Nonlinear Iteration Method are assessed on four benchmark cases, namely, a zero-pressure-gradient flat plate, a bump-in-channel configuration, the NACA 0012 airfoil, and a NASA Common Research Model configuration. The new methodology provides a convergence acceleration factor of 1.4 to 13 over the preconditioner-alone method representing the baseline solver technology.
C1 [Pandya, Mohagna J.] NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA.
[Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Thomas, James L.; Frink, Neal T.] NASA Langley Res Ctr, Computat Aerosci Branch, Mail Stop 499, Hampton, VA 23681 USA.
[Diskin, Boris] Univ Virginia, MAE Dept, Charlottesville, VA USA.
RP Pandya, MJ (reprint author), NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA.
NR 47
TC 0
Z9 0
U1 3
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 SEP
PY 2016
VL 54
IS 9
BP 2589
EP 2610
DI 10.2514/1.J054545
PG 22
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600003
ER
PT J
AU Ceze, MA
Fidkowski, KJ
AF Ceze, Marco A.
Fidkowski, Krzysztof J.
TI High-Order Output-Based Adaptive Simulations of Turbulent Flow in Two
Dimensions
SO AIAA JOURNAL
LA English
DT Article
ID NAVIER-STOKES EQUATIONS; DISCONTINUOUS GALERKIN DISCRETIZATIONS; MESH
ADAPTATION; FLUID-DYNAMICS; PREDICTION
AB Output-based high-order adaptive results are presented for several benchmark two-dimensional turbulent-flow simulations. The discretization is a high-order discontinuous Galerkin finite element method, and the equations solved are compressible Navier-Stokes, Reynolds-averaged with a modified version of the Spalart-Allmaras one-equation model. Mesh refinement requirements are studied through automated output-based adaptation in which a discrete adjoint solution associated with an output (e.g., the drag coefficient) weights a fine-space residual and automatically selects the elements that need more resolution. The roles of high-order and mesh anisotropy are also investigated. Finally, differences are investigated between two mesh refinement strategies: hanging-node refinement of structured meshes versus metric-based remeshing of unstructured triangles.
C1 [Ceze, Marco A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Fidkowski, Krzysztof J.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
[Ceze, Marco A.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
RP Ceze, MA (reprint author), NASA Ames Res Ctr, Moffett Field, CA USA.; Ceze, MA (reprint author), Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
EM marco.a.ceze@nasa.gov
FU U.S. Air Force Office of Scientific Research [FA9550-11-1-0081]
FX The authors acknowledge support from the U.S. Air Force Office of
Scientific Research under grant FA9550-11-1-0081.
NR 23
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD SEP
PY 2016
VL 54
IS 9
BP 2611
EP 2625
DI 10.2514/1.J054517
PG 15
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600004
ER
PT J
AU Eisfeld, B
Rumsey, C
Togiti, V
AF Eisfeld, Bernhard
Rumsey, Chris
Togiti, Vamshi
TI Verification and Validation of a Second-Moment Closure Model (vol 54, pg
1524, 2016)
SO AIAA JOURNAL
LA English
DT Correction
C1 [Eisfeld, Bernhard; Togiti, Vamshi] DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
[Rumsey, Chris] NASA Langley Res Ctr, MS 128, Hampton, VA USA.
RP Eisfeld, B (reprint author), DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
NR 1
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD SEP
PY 2016
VL 54
IS 9
BP 2925
EP 2925
DI 10.2514/1.J055336
PG 1
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600030
ER
PT J
AU Young, KE
Evans, CA
Hodges, KV
Bleacher, JE
Graff, TG
AF Young, Kelsey E.
Evans, Cynthia A.
Hodges, Kip V.
Bleacher, Jacob E.
Graff, Trevor G.
TI A review of the handheld X-ray fluorescence spectrometer as a tool for
field geologic investigations on Earth and in planetary surface
exploration
SO APPLIED GEOCHEMISTRY
LA English
DT Review
DE Handheld X-ray fluorescence spectrometer (hXRF); In situ geochemistry;
Planetary field geology; In situ field geologic instrument; Field
portable technology; Field spectroscopy
ID PORTABLE XRF; ROCKS; SAMPLES; DETECTOR; MARS; SOIL
AB X-ray fluorescence (XRF) spectroscopy is a well-established and commonly used technique in obtaining diagnostic compositional data on geological samples. Recently, developments in X-ray tube and detector technologies have resulted in miniaturized, field-portable instruments that enable new applications both in and out of standard laboratory settings. These applications, however, have not been extensively applied to geologic field campaigns. This study investigates the feasibility of using developing handheld XRF (hXRF) technology to enhance terrestrial field geology, with potential applications in planetary surface exploration missions. We demonstrate that the hXRF is quite stable, providing reliable and accurate data continuously over a several year period. Additionally, sample preparation is proved to have a marked effect on the strategy for collecting and assimilating hXRF data. While the hXRF is capable of obtaining data that are comparable to laboratory XRF analysis for several geologically-important elements (such as Si, Ca, Ti, and K), the instrument is unable to detect other elements (such as Mg and Na) reliably. While this limits the use of the hXRF, especially when compared to laboratory XRF techniques, the hXRF is still capable of providing the field user with significantly improved contextual awareness of a field site, and more work is needed to fully evaluate the potential of this instrument in more complex geologic environments. (C) 2016 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license.
C1 [Young, Kelsey E.; Hodges, Kip V.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Evans, Cynthia A.; Graff, Trevor G.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Graff, Trevor G.] Jacobs Engn Grp Inc, Houston, TX 77058 USA.
[Young, Kelsey E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Young, Kelsey E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Young, KE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.; Young, KE (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Young, KE (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM Kelsey.E.Young@nasa.gov
RI Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
FU GSRP (Graduate Student Researcher's Program) [NNX10AK72H]
FX The authors would like to thank Dr. Chris Condit for his thoughtful
review. The majority of this work was completed under the GSRP (Graduate
Student Researcher's Program) Grant Number NNX10AK72H as well as under
the RIS4E SSERVI team (Remote, In Situ and Synchrotron
Studies for Science and Exploration Solar System Exploration Research
Virtual Institute), led by Dr. Timothy Glotch at Stony Brook University.
The authors of this paper would also like to acknowledge Dr. Richard
Morris. Without his permission for access to the sample standards, this
work would not have been possible. In addition, we thank Dr. Stanley
Mertzman for his thoughtful discussions about calibrating against
laboratory data. We would also like to thank Dr. Carlton Allen and
Andrea Mosie for their assistance in both obtaining access to and
working with the lunar samples at NASA Johnson Space Center. Finally, we
thank Cameron Mercer for his figure organization insights. This is
SSERVI publication number SSERVI-2016-061.
NR 45
TC 1
Z9 1
U1 21
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0883-2927
J9 APPL GEOCHEM
JI Appl. Geochem.
PD SEP
PY 2016
VL 72
BP 77
EP 87
DI 10.1016/j.apgeochem.2016.07.003
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DW3DI
UT WOS:000383521900008
ER
PT J
AU Chirayath, V
Earle, SA
AF Chirayath, Ved
Earle, Sylvia A.
TI Drones that see through waves - preliminary results from airborne fluid
lensing for centimetre-scale aquatic conservation
SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS
LA English
DT Article; Proceedings Paper
CT 6th IUCN World Parks Congress
CY NOV, 2014
CL Sydney, AUSTRALIA
SP IUCN
DE fluid lensing; airborne remote sensing; coastal bathymetry; coral reef;
stromatolite; American Samoa; Shark Bay
AB 1. The use of fluid lensing technology on unmanned aerial vehicles (UAVs, or drones) is presented as a novel means for 3D imaging of aquatic ecosystems from above the water's surface at the centimetre scale. Preliminary results are presented from airborne fluid lensing campaigns conducted over the coral reefs of Ofu Island, American Samoa (2013) and the stromatolite reefs of Shark Bay, Western Australia (2014), covering a combined area of 15 km(2). These reef ecosystems were revealed with centimetre-scale 2D resolution, and an accompanying 3D bathymetry model was derived using fluid lensing, Structure from Motion and UAV position data. Data products were validated from in situ survey methods including underwater calibration targets, depth measurements and millimetre-scale high-dynamic-range gigapixel photogrammetry.
2. Fluid lensing is an experimental technology that uses water-transmitting wavelengths to passively image underwater objects at high-resolution by exploiting time-varying optical lensing events caused by surface waves. Fluid lensing data are captured from low-altitude, cost-effective electric UAVs to achieve multispectral imagery and bathymetry models at the centimetre scale over regional areas. As a passive system, fluid lensing is presently limited by signal-to-noise ratio and water column inherent optical properties to similar to 10 m depth over visible wavelengths in clear waters.
3. The datasets derived from fluid lensing present the first centimetre-scale images of a reef acquired from above the ocean surface, without wave distortion. The 3D multispectral data distinguish coral, fish and invertebrates in American Samoa, and reveal previously undocumented, morphologically distinct, stromatolite structures in Shark Bay. These findings suggest fluid lensing and multirotor electric drones represent a promising advance in the remote sensing of aquatic environments at the centimetre scale, or 'reef scale' relevant to the conservation of reef ecosystems. Pending further development and validation of fluid lensing methods, these technologies present a solution for large-scale 3D surveys of shallow aquatic habitats with centimetre-scale spatial resolution and hourly temporal sampling. Copyright (C) 2016 John Wiley & Sons, Ltd.
C1 [Chirayath, Ved] NASA, Ames Res Ctr, Lab Adv Sensing, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Chirayath, V (reprint author), NASA, Ames Res Ctr, Mailstop 232-22, Moffett Field, CA 94305 USA.
EM ved.chirayath@nasa.gov
NR 15
TC 1
Z9 1
U1 17
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1052-7613
EI 1099-0755
J9 AQUAT CONSERV
JI Aquat. Conserv.-Mar. Freshw. Ecosyst.
PD SEP
PY 2016
VL 26
SU 2
BP 237
EP 250
DI 10.1002/aqc.2654
PG 14
WC Environmental Sciences; Marine & Freshwater Biology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA DW5FL
UT WOS:000383668500017
ER
PT J
AU McCaig, HC
Stockton, A
Crilly, C
Chung, S
Kanik, I
Lin, Y
Zhong, F
AF McCaig, Heather C.
Stockton, Amanda
Crilly, Candice
Chung, Shirley
Kanik, Isik
Lin, Ying
Zhong, Fang
TI Supercritical Carbon Dioxide Extraction of Coronene in the Presence of
Perchlorate for In Situ Chemical Analysis of Martian Regolith
SO ASTROBIOLOGY
LA English
DT Article
DE Biomarkers; Carbon dioxide; In situ measurement; Mars; Search for Mars'
organics
ID POLYCYCLIC AROMATIC-HYDROCARBONS; MASS-SPECTROMETRY; ORGANIC-MATTER;
SUBCRITICAL WATER; METEORITE ALH84001; FLUID EXTRACTION; GALE CRATER;
MARS; MOLECULES; ORIGIN
AB The analysis of the organic compounds present in the martian regolith is essential for understanding the history and habitability of Mars, as well as studying the signs of possible extant or extinct life. To date, pyrolysis, the only technique that has been used to extract organic compounds from the martian regolith, has not enabled the detection of unaltered native martian organics. The elevated temperatures required for pyrolysis extraction can cause native martian organics to react with perchlorate salts in the regolith and possibly result in the chlorohydrocarbons that have been detected by in situ instruments. Supercritical carbon dioxide (SCCO2) extraction is an alternative to pyrolysis that may be capable of delivering unaltered native organic species to an in situ detector. In this study, we report the SCCO2 extraction of unaltered coronene, a representative polycyclic aromatic hydrocarbon (PAH), from martian regolith simulants, in the presence of 3 parts per thousand (ppth) sodium perchlorate. PAHs are a class of nonpolar molecules of astrobiological interest and are delivered to the martian surface by meteoritic infall. We also determined that the extraction efficiency of coronene was unaffected by the presence of perchlorate on the regolith simulant, and that no sodium perchlorate was extracted by SCCO2. This indicates that SCCO2 extraction can provide de-salted samples that could be directly delivered to a variety of in situ detectors. SCCO2 was also used to extract trace native fluorescent organic compounds from the martian regolith simulant JSC Mars-1, providing further evidence that SCCO2 extraction may provide an alternative to pyrolysis to enable the delivery of unaltered native organic compounds to an in situ detector on a future Mars rover.
C1 [McCaig, Heather C.; Crilly, Candice; Chung, Shirley; Kanik, Isik; Lin, Ying; Zhong, Fang] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Stockton, Amanda] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Crilly, Candice] Occidental Coll, Los Angeles, CA 90041 USA.
RP Zhong, F (reprint author), CALTECH, Jet Prop Lab, M-S 70-24,4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Lin, Y (reprint author), CALTECH, Jet Prop Lab, M-S 321-550,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ying.lin@jpl.nasa.gov; fang.zhong@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA Astrobiology
Science and Technology Instrument Development program
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA)
and was supported by the NASA Astrobiology Science and Technology
Instrument Development program. The JPL author's copyright for this
paper is held by the California Institute of Technology. Government
sponsorship is acknowledged.
NR 48
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PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2016
VL 16
IS 9
BP 703
EP 714
DI 10.1089/ast.2015.1443
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DW9IK
UT WOS:000383971100004
PM 27623199
ER
PT J
AU Misra, AK
Acosta-Maeda, TE
Sharma, SK
Mckay, CP
Gasda, PJ
Taylor, GJ
Lucey, PG
Flynn, L
Abedin, MN
Clegg, SM
Wiens, R
AF Misra, Anupam K.
Acosta-Maeda, Tayro E.
Sharma, Shiv K.
Mckay, Christopher P.
Gasda, Patrick J.
Taylor, G. Jeffrey
Lucey, Paul G.
Flynn, Luke
Abedin, M. Nurul
Clegg, Samuel M.
Wiens, Roger
TI "Standoff Biofinder" for Fast, Noncontact, Nondestructive, Large-Area
Detection of Biological Materials for Planetary Exploration
SO ASTROBIOLOGY
LA English
DT Article
DE Standoff Biofinder; Luminescence; Time-resolved fluorescence;
Biofluorescence; Planetary exploration; Planetary protection; Noncontact
nondestructive biodetection
ID LASER-INDUCED FLUORESCENCE; TIME-RESOLVED FLUORESCENCE; CHEMCAM
INSTRUMENT SUITE; REMOTE RAMAN; ULTRAVIOLET FLUORESCENCE; SPECTROSCOPIC
DETECTION; ROOM-TEMPERATURE; NUCLEIC-ACIDS; STEADY-STATE; EXCITATION
AB We developed a prototype instrument called the Standoff Biofinder, which can quickly locate biological material in a 500 cm(2) area from a 2 m standoff distance with a detection time of 0.1 s. All biogenic materials give strong fluorescence signals when excited with UV and visible lasers. In addition, the luminescence decay time of biogenic compounds is much shorter (<100 ns) than the micro-to millisecond decay time of transition metal ions and rare-earth ions in minerals and rocks. The Standoff Biofinder takes advantage of the short lifetime of biofluorescent materials to obtain real-time fluorescence images that show the locations of biological materials among luminescent minerals in a geological context. The Standoff Biofinder instrument will be useful for locating biological material during future NASA rover, lander, and crewed missions. Additionally, the instrument can be used for nondestructive detection of biological materials in unique samples, such as those obtained by sample return missions from the outer planets and asteroids. The Standoff Biofinder also has the capacity to detect microbes and bacteria on space instruments for planetary protection purposes.
C1 [Misra, Anupam K.; Acosta-Maeda, Tayro E.; Sharma, Shiv K.; Taylor, G. Jeffrey; Lucey, Paul G.; Flynn, Luke] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gasda, Patrick J.; Clegg, Samuel M.; Wiens, Roger] Los Alamos Natl Lab, Los Alamos, NM USA.
[Abedin, M. Nurul] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Misra, AK (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
EM anupam@hawaii.edu
OI Gasda, Patrick/0000-0003-0895-1153; Clegg, Sam/0000-0002-0338-0948
FU NASA EPSCoR grant [NNX13AM98A]
FX This work has been supported by NASA EPSCoR grant NNX13AM98A. The
authors would like to thank Nancy Hulbirt and May Izumi for their
valuable help with figures and editing. Authors would like to thank the
reviewers for their valuable time in providing critical review and
constructive comments, which greatly helped improve the manuscript.
NR 83
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PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2016
VL 16
IS 9
BP 715
EP 729
DI 10.1089/ast.2015.1400
PG 15
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DW9IK
UT WOS:000383971100005
PM 27623200
ER
PT J
AU Bannister, MT
Kavelaars, JJ
Petit, JM
Gladman, BJ
Gwyn, SDJ
Chen, YT
Volk, K
Alexandersen, M
Benecchi, SD
Delsanti, A
Fraser, WC
Granvik, M
Grundy, WM
Guilbert-Lepoutre, A
Hestroffer, D
Ip, WH
Jakubik, M
Jones, RL
Kaib, N
Kavelaars, CF
Lacerda, P
Lawler, S
Lehner, MJ
Lin, HW
Lister, T
Lykawka, PS
Monty, S
Marsset, M
Murray-Clay, R
Noll, KS
Parker, A
Pike, RE
Rousselot, P
Rusk, D
Schwamb, ME
Shankman, C
Sicardy, B
Vernazza, P
Wang, SY
AF Bannister, Michele T.
Kavelaars, J. J.
Petit, Jean-Marc
Gladman, Brett J.
Gwyn, Stephen D. J.
Chen, Ying-Tung
Volk, Kathryn
Alexandersen, Mike
Benecchi, Susan D.
Delsanti, Audrey
Fraser, Wesley C.
Granvik, Mikael
Grundy, Will M.
Guilbert-Lepoutre, Aurelie
Hestroffer, Daniel
Ip, Wing-Huen
Jakubik, Marian
Jones, R. Lynne
Kaib, Nathan
Kavelaars, Catherine F.
Lacerda, Pedro
Lawler, Samantha
Lehner, Matthew J.
Lin, Hsing Wen
Lister, Tim
Lykawka, Patryk Sofia
Monty, Stephanie
Marsset, Michael
Murray-Clay, Ruth
Noll, Keith S.
Parker, Alex
Pike, Rosemary E.
Rousselot, Philippe
Rusk, David
Schwamb, Megan E.
Shankman, Cory
Sicardy, Bruno
Vernazza, Pierre
Wang, Shiang-Yu
TI THE OUTER SOLAR SYSTEM ORIGINS SURVEY. I. DESIGN AND FIRST-QUARTER
DISCOVERIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Kuiper Belt: general; surveys
ID KUIPER-BELT OBJECTS; ABSOLUTE MAGNITUDE DISTRIBUTION; TRANS-NEPTUNIAN
POPULATIONS; SIZE DISTRIBUTION; DATA RELEASE; DYNAMICAL CLASSIFICATION;
ORBITAL STRUCTURE; SCATTERED DISK; PLANE; SEARCH
AB We report the discovery, tracking, and detection circumstances for 85 trans-Neptunian objects (TNOs) from the first 42 deg(2) of the Outer Solar System Origins Survey. This ongoing r-band solar system survey uses the 0.9 deg(2) field of view MegaPrime camera on the 3.6m Canada-France-Hawaii Telescope. Our orbital elements for these TNOs are precise to a fractional semimajor axis uncertainty <0.1%. We achieve this precision in just two oppositions, as compared to the normal three to five oppositions, via a dense observing cadence and innovative astrometric technique. These discoveries are free of ephemeris bias, a first for large trans-Neptunian surveys. We also provide the necessary information to enable models of TNO orbital distributions to be tested against our TNO sample. We confirm the existence of a cold "kernel" of objects within the main cold classical Kuiper Belt and infer the existence of an extension of the "stirred" cold classical Kuiper Belt to at least several au beyond the 2:1 mean motion resonance with Neptune. We find that the population model of Petit et al. remains a plausible representation of the Kuiper Belt. The full survey, to be completed in 2017, will provide an exquisitely characterized sample of important resonant TNO populations, ideal for testing models of giant planet migration during the early history of the solar system.
C1 [Bannister, Michele T.; Kavelaars, J. J.; Kavelaars, Catherine F.; Monty, Stephanie; Pike, Rosemary E.; Rusk, David; Shankman, Cory] Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
[Bannister, Michele T.; Kavelaars, J. J.; Gwyn, Stephen D. J.; Lawler, Samantha] Natl Res Council Canada, NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada.
[Petit, Jean-Marc; Rousselot, Philippe] Univ Bourgogne Franche Comte, CNRS, Inst UTINAM UMR6213, OSU Theta, F-25000 Besancon, France.
[Gladman, Brett J.; Alexandersen, Mike] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada.
[Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Acad Sinica, Inst Astron & Astrophys, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
[Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Natl Taiwan Univ, AS NTU11F, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
[Volk, Kathryn] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, 1629 Univ Blvd, Tucson, AZ 85721 USA.
[Benecchi, Susan D.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
[Delsanti, Audrey] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Fraser, Wesley C.; Lacerda, Pedro] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Granvik, Mikael] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland.
[Granvik, Mikael] Finnish Geospatial Res Inst, POB 15, FI-02430 Masala, Finland.
[Grundy, Will M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Hestroffer, Daniel] Univ Lille 1, Univ Paris 06, CNRS, IMCCE,Observ Paris,PSL Res Univ, F-75014 Paris, France.
[Ip, Wing-Huen; Lin, Hsing Wen] Natl Cent Univ, Inst Astron, Taoyuan, Taiwan.
[Ip, Wing-Huen] Macau Univ Sci & Technol, Space Sci Inst, Macau, Peoples R China.
[Jakubik, Marian] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia.
[Jones, R. Lynne] Univ Washington, Washington, DC USA.
[Kaib, Nathan] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA.
Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Lehner, Matthew J.; Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA.
[Lykawka, Patryk Sofia] Kinki Univ, Sch Interdisciplinary Social & Human Sci, Astron Grp, Higashiosaka, Osaka 577, Japan.
[Marsset, Michael] ESO, Alonso de Cordova 3107,1900 Casilla Vitacura, Santiago, Chile.
[Murray-Clay, Ruth] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Noll, Keith S.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
[Parker, Alex] Southwest Res Inst, Boulder, CO USA.
[Sicardy, Bruno] Univ Paris 06, Univ Paris Diderot, CNRS UMR 8109, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
RP Bannister, MT (reprint author), Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
EM micheleb@uvic.ca
OI Volk, Kathryn/0000-0001-8736-236X; Bannister,
Michele/0000-0003-3257-4490; Sofia Lykawka, Patryk/0000-0003-0926-2448
FU National Research Council of Canada; National Science and Engineering
Research Council of Canada; Academia Sinica Postdoctoral Fellowship
FX This research was supported by funding from the National Research
Council of Canada and the National Science and Engineering Research
Council of Canada. This project could not have been a success without
the dedicated staff of the Canada France Hawaii telescope. The authors
recognize and acknowledge the sacred nature of Maunakea, and appreciate
the opportunity to observe from the mountain. This research has made use
of NASA's Astrophysics Data System, GNU parallel (Tange 2011), and many
Python packages, particularly astropy (The Astropy Collaboration et al.
2013), matplotlib (Hunter 2007) and SciPy (Jones et al. 2001); we thank
their contributors for their open-source efforts. MES is supported in
part by an Academia Sinica Postdoctoral Fellowship. Based on
observations obtained with MegaPrime/MegaCam, a joint project of the
Canada France Hawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT which is
operated by the National Research Council (NRC) of Canada, the Institute
National des Sciences de l'universe of the Centre National de la
Recherche Scientifique (CNRS) of France, and the University of Hawaii.
This work is based in part on data produced and hosted at the Canadian
Astronomy Data Centre.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
VL 152
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PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300018
ER
PT J
AU McCandliss, SR
Feldman, PD
Weaver, H
Fleming, B
Redwine, K
Li, MJ
Kutyrev, A
Moseley, SH
AF McCandliss, Stephan R.
Feldman, Paul D.
Weaver, Harold
Fleming, Brian
Redwine, Keith
Li, Mary J.
Kutyrev, Alexander
Moseley, S. Harvey
TI FAR-ULTRAVIOLET OBSERVATIONS OF COMET C/2012 S1 (ISON) FROM FORTIS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE general; comets: individual (C/2012 S1 (ISON), C/2001 Q4 (NEAT), C/2004
Q2 (MACHHOLZ)); molecular processes; Oort Cloud
ID SPECTROSCOPY; EVOLUTION; HYDROGEN
AB We have used the unique far-UV imaging capability offered by a sounding-rocket-borne instrument to acquire observations of C/2012 S1 (ISON) when its angular separation with respect to the Sun was 26.degrees 3 on 2013 November 20.49. At the time of observation, the comet's heliocentric distance and velocity relative to the Sun were r(h) = 0.43 au and (r) over dot(h) = -62.7 km s(-1). Images dominated by C I lambda 1657 and H I lambda 1216 were acquired over a 10(6) x 10(6) km(2) region. The water production rate implied by the Ly alpha observations is constrained to be Q(H2O)approximate to 8 x 10(29) s(-1) while the neutral carbon production rate was Q(C) approximate to 4 x 10(28) s(-1). The radial profile of C I was consistent with it being a dissociation product of a parent molecule with a lifetime tau similar to 5 x 10(4) s, favoring a parent other than CO. We constrain the Q(CO) production rate to 5(-7.5)(+1.5) x 10(28) s(-1) with 1 sigma errors derived from photon statistics. The upper limit on the Q(CO)/Q(H2O) is less than or similar to 6%.
C1 [McCandliss, Stephan R.; Feldman, Paul D.; Redwine, Keith] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Weaver, Harold] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Fleming, Brian] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Li, Mary J.; Kutyrev, Alexander; Moseley, S. Harvey] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McCandliss, SR (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM stephan@pha.jhu.edu
OI Feldman, Paul/0000-0002-9318-259X
FU Johns Hopkins University through NASA [NNX11AG54G, NNX14A178G]
FX The authors would like to acknowledge the sacrifices made by the
personnel associated with the NASA Sounding Rocket Program Office, their
Contractors, the Navy Launcher Team, and the Army Range Control at White
Sands Missile Range, all of whom showed exemplary dedication in carrying
out this time critical mission. We would also like to acknowledge the
innumerable, essential, and critical contributions of our JHU project
engineer, Russell Pelton, in providing support to this mission. Funding
for this work was provided to the Johns Hopkins University through NASA
sounding rocket grants No. NNX11AG54G and NNX14A178G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
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AR 65
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PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300013
ER
PT J
AU Nugent, CR
Mainzer, A
Bauer, J
Cutri, RM
Kramer, EA
Grav, T
Masiero, J
Sonnett, S
Wright, EL
AF Nugent, C. R.
Mainzer, A.
Bauer, J.
Cutri, R. M.
Kramer, E. A.
Grav, T.
Masiero, J.
Sonnett, S.
Wright, E. L.
TI NEOWISE REACTIVATION MISSION YEAR TWO: ASTEROID DIAMETERS AND ALBEDOS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; surveys
ID MAIN-BELT ASTEROIDS; NEAR-EARTH OBJECTS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; WISE/NEOWISE OBSERVATIONS; ABSOLUTE
MAGNITUDES; POPULATION; PERFORMANCE; FAMILIES; IDENTIFICATION
AB The Near-Earth Object Wide-Field Infrared Survey Explorer (NEOWISE) mission continues to detect, track, and characterize minor planets. We present diameters and albedos calculated from observations taken during the second year since the spacecraft was reactivated in late 2013. These include 207 near-Earth asteroids (NEAs) and 8885 other asteroids. Of the NEAs, 84% NEAs did not have previously measured diameters and albedos by the NEOWISE mission. Comparison of sizes and albedos calculated from NEOWISE measurements with those measured by occultations, spacecraft, and radar-derived shapes shows accuracy consistent with previous NEOWISE publications. Diameters and albedos fall within +/-similar to 20% and +/-similar to 40%, 1-sigma, respectively, of those measured by these alternate techniques. NEOWISE continues to preferentially discover near-Earth objects which are large (>100 m), and have low albedos.
C1 [Nugent, C. R.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Mainzer, A.; Bauer, J.; Kramer, E. A.; Masiero, J.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Nugent, CR (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
EM cnugent@ipac.caltech.edu
OI Cutri, Roc/0000-0002-0077-2305
FU NASA; Planetary Science Division of NASA; JPL Office of the CIO; 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; Center for Cosmology
and Astro-Particle Physics at the Ohio State University; Mitchell
Institute for Fundamental Physics and Astronomy at Texas AM University;
Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia,
Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating
Institutions in the Dark Energy Survey; Ministerio da Ciencia,
Tecnologia e Inovacao (Brazil) [GS-2015A-LP-3, GS-2015B-LP-3]
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 JPL/California Institute of Technology,
funded by NASA. This publication also makes use of data products from
NEOWISE, which is a project of the JPL/California Institute of
Technology, funded by the Planetary Science Division of NASA. The JPL
High Performance Computing Facility used for our simulations is
supported by the JPL Office of the CIO.; This project used data obtained
with the Dark Energy Camera (DECam), which was constructed by the Dark
Energy Survey (DES) collaboration. 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, the Center for Cosmology and Astro-Particle
Physics at the Ohio State University, the Mitchell Institute for
Fundamental Physics and Astronomy at Texas A&M University, Financiadora
de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa
do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e
Inovacao, 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
University of Edinburgh, the Eidgenossische Technische Hochschule (ETH)
Zurich, Fermi National Accelerator Laboratory, 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 Munchen 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.; This
publication makes use of 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), Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina), and Ministerio da Ciencia, Tecnologia e Inovacao (Brazil).
Observing Program IDs: GS-2015A-LP-3, GS-2015B-LP-3.
NR 55
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300011
ER
PT J
AU Schneider, G
Grady, CA
Stark, CC
Gaspar, A
Carson, J
Debes, JH
Henning, T
Hines, DC
Jang-Condell, H
Kuchner, MJ
Perrin, M
Rodigas, TJ
Tamura, M
Wisniewski, JP
AF Schneider, Glenn
Grady, Carol A.
Stark, Christopher C.
Gaspar, Andras
Carson, Joseph
Debes, John H.
Henning, Thomas
Hines, Dean C.
Jang-Condell, Hannah
Kuchner, Marc J.
Perrin, Marshall
Rodigas, Timothy J.
Tamura, Motohide
Wisniewski, John P.
TI DEEP HST/STIS VISIBLE-LIGHT IMAGING OF DEBRIS SYSTEMS AROUND SOLAR
ANALOG HOSTS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: observational; planet-disk interactions; stars: individual (HD
207129, HD 202628, HD 202917); stars: solar-type
ID MAIN-SEQUENCE STARS; INTERSTELLAR-MEDIUM; HD 207129; SPACE-TELESCOPE;
MOVING GROUP; DISK; PLANETS; RING; DUST; AGE
AB We present new Hubble Space Telescope observations of three a priori known starlight-scattering circumstellar debris systems (CDSs) viewed at intermediate inclinations around nearby close-solar analog stars: HD 207129, HD 202628, and HD 202917. Each of these CDSs possesses ring-like components that are more massive analogs of our solar system's Edgeworth-Kuiper Belt. These systems were chosen for follow-up observations to provide imaging with higher fidelity and better sensitivity for the sparse sample of solar-analog CDSs that range over two decades in systemic ages, with HD 202628 and HD 207129 (both similar to 2.3 Gyr) currently the oldest CDSs imaged in visible or near-IR light. These deep (10-14 ks) observations, made with six-roll point-spread-function template visible-light coronagraphy. using the Space Telescope Imaging Spectrograph, were designed to better reveal their angularly large debris rings of diffuse/low surface brightness, and for all targets probe their exo-ring environments for starlight-scattering materials that present observational challenges for current ground-based facilities and instruments. Contemporaneously also observing with a narrower occulter position, these observations additionally probe the CDS endo-ring environments that are seen to be relatively devoid of scatterers. We discuss the morphological, geometrical, and photometric properties of these CDSs also in the context of other CDSs hosted by FGK stars that we have previously imaged as a homogeneously observed ensemble. From this combined sample we report a general decay in quiescent-disk F-disk/F-star optical brightness similar to t(-0.8), similar to what is seen at thermal IR wavelengths, and CDSs with a significant diversity in scattering phase asymmetries, and spatial distributions of their starlight-scattering grains.
C1 [Schneider, Glenn; Gaspar, Andras] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Schneider, Glenn; Gaspar, Andras] Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Stark, Christopher C.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, 66 George St, Charleston, SC 29424 USA.
[Debes, John H.; Hines, Dean C.; Perrin, Marshall] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Branch Rd NW, Washington, DC 20015 USA.
[Tamura, Motohide] Univ Tokyo, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA.
RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.; Schneider, G (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
EM gschneider@as.arizona.edu
OI Gaspar, Andras/0000-0001-8612-3236
FU Association of Universities for Research in Astronomy, Inc., under NASA
[NAS 5-26555]; NASA through STScI [13786]; South Carolina Space Grant
Consortium; [12228]
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute (STScI), which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated
with programs #13786 and 12228. Support for program #13786 was provided
by NASA through a grant from STScI. J. Carson acknowledges support from
the South Carolina Space Grant Consortium.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
VL 152
IS 3
AR 64
DI 10.3847/0004-6256/152/3/64
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300012
ER
PT J
AU Hinkel, NR
Young, PA
Pagano, MD
Desch, SJ
Anbar, AD
Adibekyan, V
Blanco-Cuaresma, S
Carlberg, JK
Mena, ED
Liu, F
Nordlander, T
Sousa, SG
Korn, A
Gruyters, P
Heiter, U
Jofre, P
Santos, NC
Soubiran, C
AF Hinkel, Natalie R.
Young, Patrick A.
Pagano, Michael D.
Desch, Steven J.
Anbar, Ariel D.
Adibekyan, Vardan
Blanco-Cuaresma, Sergi
Carlberg, Joleen K.
Mena, Elisa Delgado
Liu, Fan
Nordlander, Thomas
Sousa, Sergio G.
Korn, Andreas
Gruyters, Pieter
Heiter, Ulrike
Jofre, Paula
Santos, Nuno C.
Soubiran, Caroline
TI A COMPARISON OF STELLAR ELEMENTAL ABUNDANCE TECHNIQUES AND MEASUREMENTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars: abundances; stars: individual (HD 361, HD 10700, HD 121504, HD
202206); techniques: spectroscopic
ID METAL-POOR STARS; PLANET-HOST STARS; GENEVA-COPENHAGEN SURVEY; GALACTIC
CHEMICAL EVOLUTION; NEUTRAL HYDROGEN COLLISIONS; I OSCILLATOR-STRENGTHS;
SOLAR-TYPE STARS; WAY THICK DISK; DWARF STARS; OXYGEN ABUNDANCES
AB Stellar elemental abundances are important for understanding the fundamental properties of a star or stellar group, such as age and evolutionary history, as well as the composition of an orbiting planet. However, as abundance measurement techniques have progressed, there has been little standardization between individual methods and their comparisons. As a result, different stellar abundance procedures determine measurements that vary beyond the quoted error for the same elements within the same stars. The purpose of this paper is to better understand the systematic variations between methods and offer recommendations for producing more accurate results in the future. We invited a number of participants from around the world (Australia, Portugal, Sweden, Switzerland, and the United States) to calculate 10 element abundances (C, O, Na, Mg, Al, Si, Fe, Ni, Ba, and Eu) using the same stellar spectra for four stars (HD 361, HD 10700, HD 121504, and HD 202206). Each group produced measurements for each star using (1) their own autonomous techniques, (2) standardized stellar parameters, (3) a standardized line list, and (4) both standardized parameters and a line list. We present the resulting stellar parameters, absolute abundances, and a metric of data similarity that quantifies the homogeneity of the data. We conclude that standardization of some kind, particularly stellar parameters, improves the consistency between methods. However, because results did not converge as more free parameters were standardized, it is clear there are inherent issues within the techniques that need to be reconciled. Therefore, we encourage more conversation and transparency within the community such that stellar abundance determinations can be reproducible as well as accurate and precise.
C1 [Hinkel, Natalie R.; Young, Patrick A.; Pagano, Michael D.; Desch, Steven J.; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Adibekyan, Vardan; Mena, Elisa Delgado; Sousa, Sergio G.; Santos, Nuno C.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal.
[Blanco-Cuaresma, Sergi] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
[Carlberg, Joleen K.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Liu, Fan] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia.
[Nordlander, Thomas; Korn, Andreas; Gruyters, Pieter; Heiter, Ulrike] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Gruyters, Pieter] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden.
[Jofre, Paula] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Santos, Nuno C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal.
[Soubiran, Caroline] Univ Bordeaux, CNRS, LAB, UMR 5804, F-33270 Floirac, France.
RP Hinkel, NR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM natalie.hinkel@gmail.com
FU NASA's Science Mission Directorate; Fundacao para a Ciencia e Tecnologia
(FCT, Portugal) [SFRH/BPD/76606/2011, SFRH/BPD/70574/2010]; Swedish
National Space Board (SNSB); FCT [IF/00169/2012, IF/00028/2014,
PTDC/FIS-AST/7073/2014 (POCI-01-0145-FEDER-007672),
PTDC/FIS-AST/1526/2014]; POPH/FSE (EC) by FEDER funding through the
program "Programa Operacional de Factores de Competitividade"
FX The authors would like to thank Paul Butler for providing the original
stellar spectra in addition to Eric Mamajek for his help determining
accurate stellar types for our sample. They would also like to thank the
anonymous referee for support and guidance, which has greatly improved
the manuscript. NRH would like to thank CHW3. The ASU team (NRH, PAY,
MDP, SJD, and ADA) acknowledge that the results reported herein
benefited from collaborations and/or information exchange within NASA's
Nexus for Exoplanet System Science (NExSS) research coordination network
sponsored by NASA's Science Mission Directorate. EDM and VA acknowledge
the support from the Fundacao para a Ciencia e Tecnologia (FCT,
Portugal) in the form of the grants SFRH/BPD/76606/2011 and
SFRH/BPD/70574/2010, respectively. JKC acknowledges partial support from
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Universities Space Research Association
through a contract with NASA. TN, AK, and UH acknowledge support by the
Swedish National Space Board (SNSB). NCS and SGS acknowledge the support
from FCT through Investigador FCT contracts of reference IF/00169/2012
and IF/00028/2014, respectively, and POPH/FSE (EC) by FEDER funding
through the program "Programa Operacional de Factores de
Competitividade." The Porto group also acknowledges the support from FCT
in the form of grant reference PTDC/FIS-AST/7073/2014
(POCI-01-0145-FEDER-007672) and project PTDC/FIS-AST/1526/2014. This
research has made use of the SIMBAD database and VizieR catalog access
tools operated at CDS, Strasbourg, France, as well as the Exoplanet
Orbit Database at exoplanets.org.
NR 179
TC 1
Z9 1
U1 3
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 SEP
PY 2016
VL 226
IS 1
AR 4
DI 10.3847/0067-0049/226/1/4
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9XF
UT WOS:000384015400004
ER
PT J
AU Paganini, L
Mumma, MJ
AF Paganini, L.
Mumma, M. J.
TI A SOLAR-PUMPED FLUORESCENCE MODEL FOR LINE-BY-LINE EMISSION INTENSITIES
IN THE B-X, A-X, AND X-X BAND SYSTEMS OF (CN)-C-12-N-14
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astronomical databases: miscellaneous; comets: general; molecular data;
molecular processes; comets: individual; C/2014 Q2 (Lovejoy);
techniques: spectroscopic
ID OH PROMPT EMISSION; CHEMICAL-COMPOSITION; VIOLET SYSTEMS; COMETS; CN;
SPECTRUM; CYANOGEN; WATER; EXCITATION; MOLECULES
AB We present a new quantitative model for detailed solar-pumped fluorescent emission of the main isotopologue of CN. The derived fluorescence efficiencies permit estimation and interpretation of ro-vibrational infrared line intensities of CN in exospheres exposed to solar (or stellar) radiation. Our g-factors are applicable to astronomical observations of CN extending from infrared to optical wavelengths, and we compare them with previous calculations in the literature. The new model enables extraction of rotational temperature, column abundance, and production rate from astronomical observations of CN in the inner coma of comets. Our model accounts for excitation and de-excitation of rotational levels in the ground vibrational state by collisions, solar excitation to the A(2)Pi(i) and B-2 Sigma(+) electronically excited states followed by cascade to ro-vibrational levels of X-2 Sigma(+), and direct solar infrared pumping of ro-vibrational levels in the X-2 Sigma(+) state. The model uses advanced solar spectra acquired at high spectral resolution at the relevant infrared and optical wavelengths and considers the heliocentric radial velocity of the comet (the Swings effect) when assessing the exciting solar flux for a given transition. We present model predictions for the variation of fluorescence rates with rotational temperature and heliocentric radial velocity. Furthermore, we test our fluorescence model by comparing predicted and measured line-by-line intensities for X-2 Sigma(+) (1-0) in comet C/2014 Q2 (Lovejoy), thereby identifying multiple emission lines observed at IR wavelengths.
C1 [Paganini, L.; Mumma, M. J.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Paganini, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Paganini, L (reprint author), NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Paganini, L (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
FU NASA's Planetary Astronomy Program; Keck PI Data Award
FX The authors would like to thank David Schleicher and James S. A. Brooke
for interesting insights about this work. We also acknowledge support by
NASA's Planetary Astronomy Program (L.P., M.J.M.) and Keck PI Data Award
(L.P.), administered by the NASA Exoplanet Science Institute. Data were
obtained at the W. M. Keck Observatory from telescope time allocated to
the National Aeronautics and Space Administration through the agency's
scientific partnership with the California Institute of Technology and
the University of California. The 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.
NR 61
TC 0
Z9 0
U1 1
U2 1
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 SEP
PY 2016
VL 226
IS 1
AR 3
DI 10.3847/0067-0049/226/1/3
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9XF
UT WOS:000384015400003
ER
PT J
AU Haarig, M
Engelmann, R
Ansmann, A
Veselovskii, I
Whiteman, DN
Althausen, D
AF Haarig, Moritz
Engelmann, Ronny
Ansmann, Albert
Veselovskii, Igor
Whiteman, David N.
Althausen, Dietrich
TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio
profiling: cirrus case study
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL
PLUME; MULTIWAVELENGTH LIDAR; WATER-VAPOR; SAHARAN DUST;
PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL
AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinctiont-o-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution.
C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia.
[Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany.
EM haarig@tropos.de
FU Russian Science Foundation [16-17-10241]
FX We thank Johannes Buhl for providing Doppler lidar observations of
vertical velocity and estimated ice crystal sizes. Modeling of the
rotational Raman filter parameters was supported by the Russian Science
Foundation (project no. 16-17-10241).
NR 63
TC 0
Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD SEP 1
PY 2016
VL 9
IS 9
BP 4269
EP 4278
DI 10.5194/amt-9-4269-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8LC
UT WOS:000383906300001
ER
PT J
AU Colman, DR
Feyhl-Buska, J
Fecteau, KM
Xu, HF
Shock, EL
Boyd, ES
AF Colman, Daniel R.
Feyhl-Buska, Jayme
Fecteau, Kristopher M.
Xu, Huifang
Shock, Everett L.
Boyd, Eric S.
TI Ecological differentiation in planktonic and sediment-associated
chemotrophic microbial populations in Yellowstone hot springs
SO FEMS MICROBIOLOGY ECOLOGY
LA English
DT Article
DE Yellowstone hot springs; chemotroph; thermophiles; archaea; Aquificales;
ecological differentiation
ID STREAMER BIOFILM COMMUNITIES; NATIONAL-PARK; GEOTHERMAL SPRINGS;
RIBOSOMAL-RNA; SP-NOV; HIGH-TEMPERATURE; GLOBAL PATTERNS; GEN. NOV.;
DIVERSITY; SULFUR
AB Chemosynthetic sediment and planktonic community composition and sizes, aqueous geochemistry and sediment mineralogy were determined in 15 non-photosynthetic hot springs in Yellowstone National Park (YNP). These data were used to evaluate the hypothesis that differences in the availability of dissolved or mineral substrates in the bulk fluids or sediments within springs coincides with ecologically differentiated microbial communities and their populations. Planktonic and sediment-associated communities exhibited differing ecological characteristics including community sizes, evenness and richness. pH and temperature influenced microbial community composition among springs, but within-spring partitioning of taxa into sediment or planktonic communities was widespread, statistically supported (P < 0.05) and could be best explained by the inferred metabolic strategies of the partitioned taxa. Microaerophilic genera of the Aquificales predominated in many of the planktonic communities. In contrast, taxa capable of mineral-based metabolism such as S-o oxidation/reduction or Fe-oxide reduction predominated in sediment communities. These results indicate that ecological differentiation within thermal spring habitats is common across a range of spring geochemistry and is influenced by the availability of dissolved nutrients and minerals that can be used in metabolism.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs.
C1 [Colman, Daniel R.; Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA.
[Fecteau, Kristopher M.; Shock, Everett L.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
[Xu, Huifang] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Xu, Huifang; Shock, Everett L.; Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94035 USA.
[Shock, Everett L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA.
EM eboyd@montana.edu
FU National Aeronautics and Space Administration (NASA) Exobiology and
Evolutionary Biology [NNX13AI11G]; [EAR- 1529963]; [NNA15BB02A];
[NNA13AA94A]
FX This work was supported by a National Aeronautics and Space
Administration (NASA) Exobiology and Evolutionary Biology [grant number
NNX13AI11G] grant to ESB and a National Science Foundation grant [grant
number EAR- 1529963] to ELS. The NASA Astrobiology Institute is
supported by grant numbers NNA15BB02A (to ELS and ESB) and NNA13AA94A
(to HX and ESB).
NR 72
TC 1
Z9 1
U1 8
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0168-6496
EI 1574-6941
J9 FEMS MICROBIOL ECOL
JI FEMS Microbiol. Ecol.
PD SEP
PY 2016
VL 92
IS 9
AR fiw137
DI 10.1093/femsec/fiw137
PG 13
WC Microbiology
SC Microbiology
GA DW8IL
UT WOS:000383898400011
ER
PT J
AU van Vliet, MTH
van Beek, LPH
Eisner, S
Florke, M
Wada, Y
Bierkens, MFP
AF van Vliet, M. T. H.
van Beek, L. P. H.
Eisner, S.
Floerke, M.
Wada, Y.
Bierkens, M. F. P.
TI Multi-model assessment of global hydropower and cooling water discharge
potential under climate change
SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS
LA English
DT Article
DE Water resources; Water temperature; Hydropower; Cooling water; Climate
change; Global hydrological models
ID PACIFIC-NORTHWEST; POWER-GENERATION; CHANGE IMPACTS; MODEL; ELECTRICITY;
VALIDATION; TEMPERATURE; RESOURCES; HYDROLOGY; SCALE
AB Worldwide, 98% of total electricity is currently produced by thermoelectric power and hydropower. Climate change is expected to directly impact electricity supply, in terms of both water availability for hydropower generation and cooling water usage for thermoelectric power. Improved understanding of how climate change may impact the availability and temperature of water resources is therefore of major importance. Here we use a multi-model ensemble to show the potential impacts of climate change on global hydropower and cooling water discharge potential. For the first time, combined projections of streamflow and water temperature were produced with three global hydrological models (GHMs) to account for uncertainties in the structure and parametrization of these GHMs in both water availability and water temperature. The GHMs were forced with bias-corrected output of five general circulation models (GCMs) for both the lowest and highest representative concentration pathways (RCP2.6 and RCP8.5). The ensemble projections of streamflow and water temperature were then used to quantify impacts on gross hydropower potential and cooling water discharge capacity of rivers worldwide. We show that global gross hydropower potential is expected to increase between +2.4% (GCM-GHM ensemble mean for RCP 2.6) and +6.3% (RCP 8.5) for the 2080s compared to 1971-2000. The strongest increases in hydropower potential are expected for Central Africa, India, central Asia and the northern high-latitudes, with 18-33% of the world population living in these areas by the 2080s. Global mean cooling water discharge capacity is projected to decrease by 4.5-15% (2080s). The largest reductions are found for the United States, Europe, eastern Asia, and southern parts of South America, Africa and Australia, where strong water temperature increases are projected combined with reductions in mean annual streamflow. These regions are expected to affect 11-14% (for RCP2.6 and the shared socioeconomic pathway (SSP)1, SSP2, SSP4) and 41-51% (RCP8.5-SSP3, SSP5) of the world population by the 2080s. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [van Vliet, M. T. H.] Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
[van Vliet, M. T. H.; Wada, Y.] Int Inst Appl Syst Anal IIASA, Schlosspl 1, A-2361 Laxenburg, Austria.
[van Beek, L. P. H.; Wada, Y.; Bierkens, M. F. P.] Univ Utrecht, Dept Phys Geog, POB 80115, NL-3508 TC Utrecht, Netherlands.
[Eisner, S.; Floerke, M.] Univ Kassel, Ctr Environm Syst Res, Wilhelmshoher Allee 47, D-34109 Kassel, Germany.
[Wada, Y.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Wada, Y.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
[Bierkens, M. F. P.] Deltares, Soil & Groundwater Syst Unit, POB 80015, NL-3508 TA Utrecht, Netherlands.
RP van Vliet, MTH (reprint author), Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
EM michelle.vanvliet@wur.nl
RI van Beek, Rens/B-4904-2014
OI van Beek, Rens/0000-0002-4758-108X
FU Niels Stensen Fellowship; Veni-grant of NWO Earth and Life Sciences
(ALW) [863.14.008]
FX The Inter-Sectoral Impact Model Intercomparison Project (ISIMIP) is
kindly acknowledged for providing the bias-corrected general circulation
model output and gridded population projections for this study. Dr.
Michelle van Vliet was supported by a contribution from the Niels
Stensen Fellowship and a Veni-grant (project 863.14.008) of NWO Earth
and Life Sciences (ALW).
NR 58
TC 1
Z9 1
U1 8
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0959-3780
EI 1872-9495
J9 GLOBAL ENVIRON CHANG
JI Glob. Environ. Change-Human Policy Dimens.
PD SEP
PY 2016
VL 40
BP 156
EP 170
DI 10.1016/j.gloenvcha.2016.07.007
PG 15
WC Environmental Sciences; Environmental Studies; Geography
SC Environmental Sciences & Ecology; Geography
GA DV9YD
UT WOS:000383297200014
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Brace Yourself
SO IEEE SOFTWARE
LA English
DT Editorial Material
C1 [Holzmann, Gerard J.] Jet Prop Lab, Pasadena, CA 91125 USA.
RP Holzmann, GJ (reprint author), Jet Prop Lab, Pasadena, CA 91125 USA.
EM gholzmann@acm.org
NR 4
TC 0
Z9 0
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
EI 1937-4194
J9 IEEE SOFTWARE
JI IEEE Softw.
PD SEP-OCT
PY 2016
VL 33
IS 5
BP 34
EP 37
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA DV7DI
UT WOS:000383095900008
ER
PT J
AU Zhu, YY
Antao, DS
Chu, KH
Chen, SY
Hendricks, TJ
Zhang, TJ
Wang, EN
AF Zhu, Yangying
Antao, Dion S.
Chu, Kuang-Han
Chen, Siyu
Hendricks, Terry J.
Zhang, Tiejun
Wang, Evelyn N.
TI Surface Structure Enhanced Microchannel Flow Boiling
SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME
LA English
DT Article
DE microchannel flow boiling; surface microstructures; flow instabilities;
critical heat flux
ID CRITICAL HEAT-FLUX; PRESSURE-DROP; PIN FIN; MICROPILLAR ARRAYS; LIQUID;
PREDICTION; CHANNELS; REGIME; SINK
AB We investigated the role of surface microstructures in two-phase microchannels on suppressing flow instabilities and enhancing heat transfer. We designed and fabricated microchannels with well-defined silicon micropillar arrays on the bottom heated microchannel wall to promote capillary flow for thin film evaporation while facilitating nucleation only from the sidewalls. Our experimental results show significantly reduced temperature and pressure drop fluctuation especially at high heat fluxes. A critical heat flux (CHF) of 969 W/cm(2) was achieved with a structured surface, a 57% enhancement compared to a smooth surface. We explain the experimental trends for the CHF enhancement with a liquid wicking model. The results suggest that capillary flow can be maximized to enhance heat transfer via optimizing the microstructure geometry for the development of high performance two-phase microchannel heat sinks.
C1 [Zhu, Yangying; Antao, Dion S.; Chu, Kuang-Han; Chen, Siyu; Wang, Evelyn N.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
[Hendricks, Terry J.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, Tiejun] Masdar Inst Sci & Technol, Dept Mech & Mat Engn, Bldg 1A,POB 54224, Abu Dhabi, U Arab Emirates.
RP Wang, EN (reprint author), MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
EM yyzhu@mit.edu; dantao@mit.edu; flyjohn@gmail.com; chensiyu@mit.edu;
terry.j.hendricks@jpl.nasa.gov; tjzhang@masdar.ac.ae; enwang@mit.edu
FU Office of Naval Research (ONR) [N00014-15-1-2483]; Masdar Institute of
Science and Technology (Masdar Institute), Abu Dhabi, UAE
[02/MI/MI/CP/11/07633/GEN/G/00]; Massachusetts Institute of Technology
(MIT), Cambridge, MA [02/MI/MI/CP/11/07633/GEN/G/00]; Battelle Memorial
Institute; Air Force Office of Scientific Research (AFOSR);
Singapore-MIT Alliance for Research and Technology (SMART)
FX This work was partially funded by the Office of Naval Research (ONR)
with Dr. Mark Spector as program manager (N00014-15-1-2483), the
Cooperative Agreement between the Masdar Institute of Science and
Technology (Masdar Institute), Abu Dhabi, UAE and the Massachusetts
Institute of Technology (MIT), Cambridge, MA,-Reference
02/MI/MI/CP/11/07633/GEN/G/00, the Battelle Memorial Institute, the Air
Force Office of Scientific Research (AFOSR) and the Singapore-MIT
Alliance for Research and Technology (SMART). The research was
technically supported and encouraged by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The authors would also like to
acknowledge the MIT Microsystems Technology Lab for fabrication staff
support, help, and use of equipment.
NR 49
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U1 16
U2 16
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0022-1481
EI 1528-8943
J9 J HEAT TRANS-T ASME
JI J. Heat Transf.-Trans. ASME
PD SEP
PY 2016
VL 138
IS 9
AR 091501
DI 10.1115/1.4033497
PG 13
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DW6TS
UT WOS:000383784700014
ER
PT J
AU Otto, SE
Trefny, CJ
Slater, JW
AF Otto, Samuel E.
Trefny, Charles J.
Slater, John W.
TI Inward-Turning Streamline-Traced Inlet Design Method Low-Boom Low-Drag
Applications
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT AIAA Propulsion and Energy Forum
CY JUL 27-29, 2015
CL Orlando, FL
SP AIAA
ID BUSEMANN-INLET; SPEEDS
AB A new design method for inward-turning streamline-traced inlets is presented. Resulting designs are intended for low-supersonic low-drag low-boom applications such as that required for NASA's proposed low-boom flight demonstration aircraft. A critical feature of these designs is the internal cowl lip angle that allows for little or no flow turning on the outer nacelle. Present methods using conical-flow Busemann parent flowfields have simply truncated, or otherwise modified, the stream-traced contours to include this internal cowl angle. Such modifications disrupt the parent flowfield, reducing inlet performance and flow uniformity. The method presented herein merges a conical flowfield that includes a leading shock with a truncated Busemann flowfield in a manner that minimizes unwanted interactions. A leading internal cowl angle is now inherent in the parent flowfield, and inlet contours traced from this flowfield retain its high performance and good flow uniformity. Computational fluid dynamics analysis of a candidate inlet design is presented that verifies the design technique, and it reveals a starting issue with the basic geometry. A minor modification to the cowl lip region is shown to eliminate this phenomenon, thereby allowing starting and smooth transition to subcritical operation as backpressure is increased. An inlet critical-point total pressure recovery of 96% is achieved based on computational fluid dynamics results for a Mach 1.7 freestream design. Correction for boundary-layer displacement thickness and sizing for a given engine airflow requirement are also discussed.
C1 [Otto, Samuel E.] Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA.
[Trefny, Charles J.; Slater, John W.] NASA, John H Glenn Res Ctr, Inlets & Nozzles Branch, 21000 Brookpark Rd Mail Stop 5-11, Cleveland, OH 44135 USA.
RP Otto, SE (reprint author), Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA.
NR 12
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U1 4
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD SEP
PY 2016
VL 32
IS 5
BP 1178
EP 1189
DI 10.2514/1.B36028
PG 12
WC Engineering, Aerospace
SC Engineering
GA DW2MH
UT WOS:000383476000015
ER
PT J
AU Pokhrel, R
Gutermuth, R
Ali, B
Megeath, T
Pipher, J
Myers, P
Fischer, WJ
Henning, T
Wolk, SJ
Allen, L
Tobin, JJ
AF Pokhrel, R.
Gutermuth, R.
Ali, B.
Megeath, T.
Pipher, J.
Myers, P.
Fischer, W. J.
Henning, T.
Wolk, S. J.
Allen, L.
Tobin, J. J.
TI A Herschel-SPIRE survey of the Mon R2 giant molecular cloud: analysis of
the gas column density probability density function
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: clouds; ISM: individual objects: Mon R2; ISM: structure
ID YOUNG STELLAR CLUSTERS; GOULD BELT SURVEY; STAR-FORMATION; MONOCEROS R2;
INTERSTELLAR CLOUDS; REFLECTION NEBULAE; DUST TEMPERATURE; TURBULENCE;
ORION; RESOLUTION
AB We present a far-IR survey of the entire Mon R2 giant molecular cloud (GMC) with Herschel-Spectral and Photometric Imaging REceiver cross-calibrated with Planck-High Frequency Instrument data. We fit the spectral energy distributions of each pixel with a greybody function and an optimal beta value of 1.8. We find that mid-range column densities obtained from far-IR dust emission and near-IR extinction are consistent. For the entire GMC, we find that the column density histogram, or column density probability distribution function (N-PDF), is lognormal below similar to 10(21) cm(-2). Above this value, the distribution takes a power law form with an index of -2.15. We analyse the gas geometry, N-PDF shape, and young stellar object (YSO) content of a selection of subregions in the cloud. We find no regions with pure lognormal N-PDFs. The regions with a combination of lognormal and one power-law N-PDF have a YSO cluster and a corresponding centrally concentrated gas clump. The regions with a combination of lognormal and two power-law N-PDF have significant numbers of typically younger YSOs but no prominent YSO cluster. These regions are composed of an aggregate of closely spaced gas filaments with no concentrated dense gas clump. We find that for our fixed scale regions, the YSO count roughly correlates with the N-PDF power-law index. The correlation appears steeper for single power-law regions relative to two power-law regions with a high column density cut-off, as a greater dense gas mass fraction is achieved in the former. A stronger correlation is found between embedded YSO count and the dense gas mass among our regions.
C1 [Pokhrel, R.; Gutermuth, R.] Univ Massachusetts, Amherst, MA 01003 USA.
[Ali, B.] Space Sci Inst, Boulder, CO 80301 USA.
[Megeath, T.] Univ Toledo, 2801 W Bancroft St, Toledo, OH 43606 USA.
[Pipher, J.] Univ Rochester, 601 Elmwood Ave, Rochester, NY 14627 USA.
[Myers, P.; Wolk, S. J.] Harvard Univ, CFA, Cambridge, MA 02138 USA.
[Fischer, W. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Henning, T.] MPIA Heidelberg, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Tobin, J. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Gutermuth, R (reprint author), Univ Massachusetts, Amherst, MA 01003 USA.
EM rgutermu@astro.umass.edu
FU NASA through JPL/Caltech [1489384]; NASA [NAS8-03060]; CSA (Canada);
NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy);
MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); BMVIT (Austria);
ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); CICT/MCT (Spain)
FX This work is based on observations made with Herschel, a European Space
Agency cornerstone mission with science instruments provided by
European-led Principal Investigator consortia and with significant
participation by NASA. Support for this work was provided by NASA
through an award issued by JPL/Caltech (contract number 1489384). SJW
was supported by NASA contract NAS8-03060. We are thankful to Stella
Offner, Mark Heyer, Grant Wilson and Ronald Snell from the University of
Massachusetts (UMASS), Amherst for helpful conversations, suggestions,
and feedback. We also thank Amy Stutz of the Max-Planck Institute for
Astronomy, Germany for important suggestions on the paper. We also thank
Bernhard Schulz and David Shupe from NASA Herschel Science Center for
helping us with data reduction. We are grateful to Manikarajamuthaly Sri
Saravana for helping us with technical aspects. Finally, we would like
to thank the anonymous referee for valuable comments and suggestions.
SPIRE has been developed by a consortium of institutes led by Cardiff
University (UK) and including University of Lethbridge (Canada); NAOC
(China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC
(Spain); Stockholm Observatory (Sweden); Imperial College London, RAL,
UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC,
University of Colorado (USA). This development has been supported by
national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA
(USA). PACS has been developed by a consortium of institutes led by MPE
(Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA,
OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA
(Italy); IAC (Spain). This development has been supported by the funding
agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR
(Germany), ASI (Italy), and CICT/MCT (Spain).
NR 60
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U1 0
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
BP 22
EP 35
DI 10.1093/mnras/stw1303
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500003
ER
PT J
AU Archambault, S
Archer, A
Barnacka, A
Behera, B
Beilicke, M
Benbow, W
Berger, K
Bird, R
Bottcher, M
Buckley, JH
Bugaev, V
Cardenzana, JV
Cerruti, M
Chen, X
Christiansen, JL
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Furniss, A
Gillanders, GH
Godambe, S
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Hakansson, N
Hanna, D
Holder, J
Hughes, G
Johnson, CA
Kaaret, P
Kar, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Kumar, S
Lang, MJ
Madhavan, AS
Maier, G
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Nelson, T
Nieto, D
de Bhroithe, AO
Ong, RA
Otte, AN
Park, N
Perkins, JS
Pohl, M
Popkow, A
Prokoph, H
Pueschel, E
Quinn, J
Ragan, K
Rajotte, J
Reyes, LC
Reynolds, PT
Richards, GT
Roache, E
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Sweeney, K
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Welsing, R
Wilhelm, A
Williams, DA
Zitzer, B
AF Archambault, S.
Archer, A.
Barnacka, A.
Behera, B.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Bottcher, M.
Buckley, J. H.
Bugaev, V.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Christiansen, J. L.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Furniss, A.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hakansson, N.
Hanna, D.
Holder, J.
Hughes, G.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Kumar, S.
Lang, M. J.
Madhavan, A. S.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Nelson, T.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Park, N.
Perkins, J. S.
Pohl, M.
Popkow, A.
Prokoph, H.
Pueschel, E.
Quinn, J.
Ragan, K.
Rajotte, J.
Reyes, L. C.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Sweeney, K.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
TI Discovery of very high energy gamma rays from 1ES 1440+122
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE BL Lacertae objects: general; gamma-rays: general
ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND
LIGHT; INTERGALACTIC MAGNETIC-FIELD; ACTIVE GALACTIC NUCLEI; EINSTEIN
SLEW SURVEY; TEV BLAZARS; MULTIWAVELENGTH OBSERVATIONS; BRIGHT BLAZARS;
SOURCE CATALOG
AB The BL Lacertae object 1ES 1440+ 122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 h, resulted in the discovery of gamma-ray emission from the blazar, which has a redshift z = 0.163. 1ES 1440+ 122 is detected at a statistical significance of 5.5 standard deviations above the background with an integral flux of (2.8 +/- 0.7(stat) +/- 0.8sys) x 10(-12) cm(-2) s(-1) (1.2 per cent of the Crab Nebula's flux) above 200 GeV. The measured spectrum is described well by a power law from 0.2 to 1.3 TeV with a photon index of 3.1 +/- 0.4(stat) +/- 0.2(sys). Quasi-simultaneous multiwavelength data from the Fermi Large Area Telescope (0.3-300 GeV) and the Swift X-ray Telescope (0.2-10 keV) are additionally used to model the properties of the emission region. A synchrotron self-Compton model produces a good representation of the multiwavelength data. Adding an external-Compton or a hadronic component also adequately describes the data.
C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Benbow, W.; Cerruti, M.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Collins-Hughes, E.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Bottcher, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Madhavan, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany.
[Christiansen, J. L.; Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Nelson, T.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Errando, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Godambe, S.] Bhabha Atom Res Ctr, Astrophys Sci Div, Bombay 400085, Maharashtra, India.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, 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, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Dublin, Ireland.
[Nieto, D.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA.
[Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Sweeney, K.] Ohio Univ, Dept Phys & Astron, Clippinger Res Lab 251B, Athens, OH 45701 USA.
[Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
RP Dumm, J (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM dumm@physics.umn.edu
FU 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; South African Department
of Science and Technology through the National Research Foundation under
NRF SARChI Chair [64789]
FX This research is supported by 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. M. Bottcher acknowledges
support by the South African Department of Science and Technology
through the National Research Foundation under NRF SARChI Chair grant
no. 64789. The VERITAS Collaboration is grateful to Trevor Weekes for
his seminal contributions and leadership in the field of VHE gamma-ray
astrophysics, which made this study possible.
NR 59
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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 SEP 1
PY 2016
VL 461
IS 1
BP 202
EP 208
DI 10.1093/mnras/stw1319
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500017
ER
PT J
AU Sifon, C
Battaglia, N
Hasselfield, M
Menanteau, F
Barrientos, LF
Bond, JR
Crichton, D
Devlin, MJ
Dunner, R
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, JP
Infante, L
Kosowsky, A
Marsden, D
Marriage, TA
Moodley, K
Niemack, MD
Page, LA
Spergel, DN
Staggs, ST
Trac, H
Wollack, EJ
AF Sifon, Cristobal
Battaglia, Nick
Hasselfield, Matthew
Menanteau, Felipe
Felipe Barrientos, L.
Bond, J. Richard
Crichton, Devin
Devlin, Mark J.
Dunner, Rolando
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Hughes, John P.
Infante, Leopoldo
Kosowsky, Arthur
Marsden, Danica
Marriage, Tobias A.
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Spergel, David N.
Staggs, Suzanne T.
Hy Trac
Wollack, Edward J.
TI The Atacama Cosmology Telescope: dynamical masses for 44 SZ-selected
galaxy clusters over 755 square degrees
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; Galaxies: distances and redshifts;
cosmology: observations; large-scale structure of Universe
ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES;
ZELDOVICH-SELECTED CLUSTERS; ACT-CL J0102-4915; X-RAY-PROPERTIES;
SUNYAEV-ZELDOVICH; SCALING RELATIONS; VELOCITY DISPERSIONS; RICH
CLUSTERS
AB We present galaxy velocity dispersions and dynamical mass estimates for 44 galaxy clusters selected via the Sunyaev-Zel'dovich (SZ) effect by the Atacama Cosmology Telescope. Dynamical masses for 18 clusters are reported here for the first time. Using N-body simulations, we model the different observing strategies used to measure the velocity dispersions and account for systematic effects resulting from these strategies. We find that the galaxy velocity distributions may be treated as isotropic, and that an aperture correction of up to 7 per cent in the velocity dispersion is required if the spectroscopic galaxy sample is sufficiently concentrated towards the cluster centre. Accounting for the radial profile of the velocity dispersion in simulations enables consistent dynamical mass estimates regardless of the observing strategy. Cluster masses M200 are in the range (1-15) x 10(14)M(circle dot). Comparing with masses estimated from the SZ distortion assuming a gas pressure profile derived from X-ray observations gives a mean SZ-to-dynamical mass ratio of 1.10 +/- 0.13, but there is an additional 0.14 systematic uncertainty due to the unknown velocity bias; the statistical uncertainty is dominated by the scatter in the mass-velocity dispersion scaling relation. This ratio is consistent with previous determinations at these mass scales.
C1 [Sifon, Cristobal; Hughes, John P.] Gemini South Observ, Hilo, HI 96720 USA.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands.
[Battaglia, Nick; Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Hasselfield, Matthew] Penn State Univ, Dept Astron & Astrophys, Davey Lab, 525 Davey Lab, University Pk, PA 16802 USA.
[Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA.
[Menanteau, Felipe] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Felipe Barrientos, L.; Dunner, Rolando; Infante, Leopoldo] Pontificia Univ Catolica, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Bond, J. Richard] Canadian Inst Theoret Astrophys, 60 St George, Toronto, ON M5S 3H8, Canada.
[Crichton, Devin; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Devlin, Mark J.; Marsden, Danica] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
[Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Hincks, Adam D.] Pontificia Univ Gregoriana, Piazza Pilotta 4, I-00187 Rome, Italy.
[Huffenberger, Kevin M.] Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Hy Trac] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sifon, C (reprint author), Gemini South Observ, Hilo, HI 96720 USA.; Sifon, C (reprint author), Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands.
EM sifon@strw.leidenuniv.nl
RI Wollack, Edward/D-4467-2012; Trac, Hy/N-8838-2014;
OI Wollack, Edward/0000-0002-7567-4451; Trac, Hy/0000-0001-6778-3861;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352
FU European Research Council under FP7 grant [279396]; FONDECYT [1120676];
NSF [1312380]; US National Science Foundation [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT);
CFI under the auspices of 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; Spanish MultiDark Consolider Project [CSD2009-00064]
FX CS acknowledges support from the European Research Council under FP7
grant number 279396 awarded to H. Hoekstra. NB and RH acknowledge
support from the iii Fellowship. LFB's research is supported by FONDECYT
under project 1120676. AK acknowledges support from NSF grant 1312380.
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. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
Astronomico Atacama in northern Chile under the auspices of the Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT).
Computations were performed on the GPC supercomputer at the SciNet HPC
Consortium. SciNet is funded by the CFI under the auspices of Compute
Canada, the Government of Ontario, the Ontario Research Fund - Research
Excellence; and the University of Toronto. 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.sdss9.org/. The MultiDark Database used in this paper and the
web application providing online access to it were constructed as part
of the activities of the German Astrophysical Virtual Observatory as
result of a collaboration between the Leibniz-Institute for Astrophysics
Potsdam (AIP) and the Spanish MultiDark Consolider Project
CSD2009-00064. The Bolshoi and MultiDark simulations were run on the
NASA's Pleiades supercomputer at the NASA Ames Research Center. The MDPL
and the BigMD simulation suite have been performed in the Supermuc
supercomputer at LRZ using time granted by PRACE.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
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DI 10.1093/mnras/stw1284
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500022
ER
PT J
AU Clavel, M
Tomsick, JA
Bodaghee, A
Chiu, JL
Fornasini, FM
Hong, J
Krivonos, R
Ponti, G
Rahoui, F
Stern, D
AF Clavel, M.
Tomsick, J. A.
Bodaghee, A.
Chiu, J. -L.
Fornasini, F. M.
Hong, J.
Krivonos, R.
Ponti, G.
Rahoui, F.
Stern, D.
TI IGR J18293-1213 is an eclipsing cataclysmic variable
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: eclipsing; stars: individual: IGR J18293-1213-white dwarfs;
X-rays: stars
ID X-RAY BINARIES; INTERMEDIATE POLARS; MILKY-WAY; EMISSION; MISSION;
REFLECTION; TELESCOPE; EVOLUTION; STARS; SKY
AB Studying the population of faint hard X-ray sources along the plane of the Galaxy is challenging because of high extinction and crowding, which make the identification of individual sources more difficult. IGR J18293-1213 is part of the population of persistent sources which have been discovered by the INTEGRAL satellite. We report on NuSTAR and Swift/XRT observations of this source, performed on 2015 September 11. We detected three eclipsing intervals in the NuSTAR light curve, allowing us to constrain the duration of these eclipses, Delta t = 30.8(-0.0)(+6.3) min, and the orbital period of the system, T = 6.92 +/- 0.01 h. Even though we only report an upper limit on the amplitude of a putative spin modulation, the orbital period and the hard thermal bremsstrahlung spectrum of IGR J18293-1213 provide strong evidence that this source is a magnetic cataclysmic variable. Our NuSTAR and Swift/XRT joint spectral analysis places strong constraints on the white dwarf mass M-wd = 0.78(-0.09)(+0.10) M-circle dot. Assuming that the mass to radius ratio of the companion star M star /R star = 1 (solar units) and using T, Delta t, and M-wd, we derived the mass of the companion star M-star = 0.82 +/- 0.01 M-circle dot, the orbital separation of the binary system a = 2.14 +/- 0.04 R-circle dot, and its orbital inclination compared to the line of sight i = (72 degrees.2(-0.0)(+2.4)) +/- 1 degrees.0.
C1 [Clavel, M.; Tomsick, J. A.; Chiu, J. -L.; Fornasini, F. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Bodaghee, A.] Georgia Coll, 231 W Hancock St, Milledgeville, GA 31061 USA.
[Fornasini, F. M.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Hong, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Krivonos, R.] Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Ponti, G.] Max Planck Inst Extraterr Phys, Gissenbachstr, D-85748 Garching, Germany.
[Rahoui, F.] European Southern Observ, Karl Schwarzchild Str 2, D-85748 Garching, Germany.
[Rahoui, F.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Clavel, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM maica.clavel@ssl.berkeley.edu
OI Clavel, Maica/0000-0003-0724-2742
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Russian Science Foundation [14-22-00271]; Bundesministerium fur
Wirtschaft und Technologie/Deutsches Zentrum fur Luftund Raumfahrt
(BMWI/DLR) [FKZ 50 OR 1408]
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). RK acknowledges support from Russian
Science Foundation (grant 14-22-00271). GP acknowledges the
Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1408).
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
BP 304
EP 311
DI 10.1093/mnras/stw1330
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500026
ER
PT J
AU Joachimi, K
Gatuzz, E
Garcia, JA
Kallman, TR
AF Joachimi, Katerine
Gatuzz, Efrain
Garcia, Javier A.
Kallman, Timothy R.
TI On the detectability of CO molecules in the interstellar medium via
X-ray spectroscopy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; ISM: molecules; ISM: structure; X-rays: ISM
ID K-SHELL PHOTOABSORPTION; MILKY-WAY; ABSORPTION MODEL; XMM-NEWTON;
OXYGEN; BINARIES; CLOUDS; NEON; EDGE; PHOTOIONIZATION
AB We present a study of the detectability of CO molecules in the Galactic interstellar medium using high-resolution X-ray spectra obtained with the XMM-Newton Reflection Grating Spectrometer. We analysed 10 bright low mass X-ray binaries (LMXBs) to study the CO contribution in their line of sights. A total of 25 observations were fitted with the ISMabs X-ray absorption model which includes photoabsorption cross-sections for OI, OII, OIII and CO. We performed a Monte Carlo (MC) simulation analysis of the goodness of fit in order to estimate the significance of the CO detection. We determine that the statistical analysis prevents a significant detection of CO molecular X-ray absorption features, except for the lines of sight towards XTE J1718-330 and 4U 1636-53. In the case of XTE J1817-330, this is the first report of the presence of CO along its line of sight. Our results reinforce the conclusion that molecules have a minor contribution to the absorption features in the O K-edge spectral region. We estimate a CO column density lower limit to perform a significant detection with XMM-Newton of N(CO) > 6 x 10(16) cm(-2) for typical exposure times.
C1 [Joachimi, Katerine; Gatuzz, Efrain] Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.
[Gatuzz, Efrain] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Garcia, Javier A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gatuzz, E (reprint author), Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.; Gatuzz, E (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany.
EM efraingatuzz@gmail.com; jajgarcia@gmail.com
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
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EP 357
DI 10.1093/mnras/stw1371
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500030
ER
PT J
AU Davies, LJM
Driver, SP
Robotham, ASG
Grootes, MW
Popescu, CC
Tuffs, RJ
Hopkins, A
Alpaslan, M
Andrews, SK
Bland-Hawthorn, J
Bremer, MN
Brough, S
Brown, MJI
Cluver, ME
Croom, S
da Cunha, E
Dunne, L
Lara-Lopez, MA
Liske, J
Loveday, J
Moffett, AJ
Owers, M
Phillipps, S
Sansom, AE
Taylor, EN
Michalowski, MJ
Ibar, E
Smith, M
Bourne, N
AF Davies, L. J. M.
Driver, S. P.
Robotham, A. S. G.
Grootes, M. W.
Popescu, C. C.
Tuffs, R. J.
Hopkins, A.
Alpaslan, M.
Andrews, S. K.
Bland-Hawthorn, J.
Bremer, M. N.
Brough, S.
Brown, M. J. I.
Cluver, M. E.
Croom, S.
da Cunha, E.
Dunne, L.
Lara-Lopez, M. A.
Liske, J.
Loveday, J.
Moffett, A. J.
Owers, M.
Phillipps, S.
Sansom, A. E.
Taylor, E. N.
Michalowski, M. J.
Ibar, E.
Smith, M.
Bourne, N.
TI GAMA/H-ATLAS: a meta-analysis of SFR indicators - comprehensive measures
of the SFR-M* relation and cosmic star formation history at z < 0.4
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: star formation
ID MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTION;
HIGH-REDSHIFT GALAXIES; DEEP FIELD SOUTH; FORMING GALAXIES; SPIRAL
GALAXIES; STELLAR MASS; MAIN-SEQUENCE; FORMATION RATES
AB We present a meta-analysis of star formation rate (SFR) indicators in the Galaxy And Mass Assembly (GAMA) survey, producing 12 different SFR metrics and determining the SFRM* relation for each. We compare and contrast published methods to extract the SFR from each indicator, using a well-defined local sample of morphologically selected spiral galaxies, which excludes sources which potentially have large recent changes to their SFR. The different methods are found to yield SFR-M* relations with inconsistent slopes and normalizations, suggesting differences between calibration methods. The recovered SFR-M* relations also have a large range in scatter which, as SFRs of the targets may be considered constant over the different time-scales, suggests differences in the accuracy by which methods correct for attenuation in individual targets. We then recalibrate all SFR indicators to provide new, robust and consistent luminosity-to-SFR calibrations, finding that the most consistent slopes and normalizations of the SFR-M* relations are obtained when recalibrated using the radiation transfer method of Popescu et al. These new calibrations can be used to directly compare SFRs across different observations, epochs and galaxy populations. We then apply our calibrations to the GAMA II equatorial data set and explore the evolution of star formation in the local Universe. We determine the evolution of the normalization to the SFR-M* relation from 0 < z < 0.35 - finding consistent trends with previous estimates at 0.3 < z < 1.2. We then provide the definitive z < 0.35 cosmic star formation history, SFR-M* relation and its evolution over the last 3 billion years.
C1 [Davies, L. J. M.; Driver, S. P.; Robotham, A. S. G.; Andrews, S. K.; Moffett, A. J.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
[Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Grootes, M. W.] ESA ESTEC SCI S, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Popescu, C. C.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Popescu, C. C.] Romanian Acad, Astron Inst, Str Cutitul Argint 5, Bucharest 040557, Romania.
[Tuffs, R. J.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
[Hopkins, A.; Brough, S.; Owers, M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Alpaslan, M.] NASA, Ames Res Ctr, N232, Mountain View, CA 94034 USA.
[Bland-Hawthorn, J.; Croom, S.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Bremer, M. N.; Phillipps, S.] Univ Bristol, Sch Phys, Astrophys Grp, Tyndall Ave, Bristol BS8 1TL, Avon, England.
[Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.
[Cluver, M. E.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa.
[da Cunha, E.; Taylor, E. N.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
[Dunne, L.; Michalowski, M. J.; Bourne, N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dunne, L.; Smith, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Lara-Lopez, M. A.] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, DF, Mexico.
[Liske, J.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Owers, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso, Chile.
RP Davies, LJM (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
EM luke.j.davies@uwa.edu.au
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Alpaslan, Mehmet/0000-0003-0321-1033
FU STFC (UK); ARC (Australia); AAO; UNAM through the PAPIIT project
[IA101315]; European Research Council Advanced Investigator grant Cosmic
Dust
FX GAMA is a joint European-Australasian project based around a
spectroscopic campaign using the Anglo-Australian Telescope. The GAMA
input catalogue is based on data taken from the Sloan Digital Sky Survey
and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the
GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP providing UV-to-radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO and the
participating institutions. The GAMA website is
http://www.gama-survey.org/.; MALL acknowledges support from UNAM
through the PAPIIT project IA101315. LD acknowledges support from
European Research Council Advanced Investigator grant Cosmic Dust.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
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PY 2016
VL 461
IS 1
BP 458
EP 485
DI 10.1093/mnras/stw1342
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500037
ER
PT J
AU Pieres, A
Santiago, B
Balbinot, E
Luque, E
Queiroz, A
da Costa, LN
Maia, MAG
Drlica-Wagner, A
Roodman, A
Abbott, TMC
Allam, S
Benoit-Levy, A
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Cunha, CE
Desai, S
Diehl, HT
Eifler, TF
Finley, DA
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, DW
Gruen, D
Gruendl, RA
Gutierrez, G
Honscheid, K
James, DJ
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Marshall, L
Martini, P
Miller, CJ
Miquel, R
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Romer, AK
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Tucker, DL
Walker, AR
AF Pieres, A.
Santiago, B.
Balbinot, E.
Luque, E.
Queiroz, A.
da Costa, L. N.
Maia, M. A. G.
Drlica-Wagner, A.
Roodman, A.
Abbott, T. M. C.
Allam, S.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Rosell, A. Carnero
Kind, M. Carrasco
Carretero, J.
Cunha, C. E.
Desai, S.
Diehl, H. T.
Eifler, T. F.
Finley, D. A.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gerdes, D. W.
Gruen, D.
Gruendl, R. A.
Gutierrez, G.
Honscheid, K.
James, D. J.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Marshall, L.
Martini, P.
Miller, C. J.
Miquel, R.
Nichol, R. C.
Nord, B.
Ogando, R.
Plazas, A. A.
Romer, A. K.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D. L.
Walker, A. R.
TI Physical properties of star clusters in the outer LMC as observed by the
DES
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; Magellanic Cloud; galaxies: star clusters: general
ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; CHEMICAL ENRICHMENT
HISTORY; SIMPLE STELLAR POPULATIONS; STRUCTURAL PARAMETERS; METALLICITY
RELATION; PHOTOMETRIC SYSTEMS; SOURCE EXTRACTION; AGE DISTRIBUTION; RED
CLUMP
AB The Large Magellanic Cloud (LMC) harbours a rich and diverse system of star clusters, whose ages, chemical abundances and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey (DES) to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalogue. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10 per cent inside typical LMC cluster cores. We therefore reanalysed the DES co-add images around each candidate cluster and remeasured positions and magnitudes for their stars. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal rich than [Fe/H] similar or equal to -0.7 beyond 8 kpc from the LMC centre. The age distribution has two peaks at similar or equal to 1.2 and similar or equal to 2.7 Gyr.
C1 [Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.; da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England.
[da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Drlica-Wagner, A.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Roodman, A.; Burke, D. L.; Cunha, C. E.; Frieman, J.; Gruen, D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Roodman, A.; Burke, D. L.; Gruen, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.
[Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain.
[Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain.
[Desai, S.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Li, T. S.; Marshall, L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Li, T. S.; Marshall, L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain.
[Sobreira, F.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil.
[Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
RP Pieres, A (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.; Pieres, A (reprint author), Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
EM adriano.pieres@ufrgs.br; basilio.santiago@ufrgs.br;
e.balbinot@surrey.ac.uk
RI Ogando, Ricardo/A-1747-2010;
OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira,
Flavia/0000-0002-7822-0658
FU Brazilian Institution CNPq; European Research Council [ERC-StG-335936];
US Department of Energy; US National Science Foundation; Ministry of
Science and Education of Spain; Science and Technology Facilities
Council of the United Kingdom; Higher Education Funding Council for
England; National Center for Supercomputing Applications at the
University of Illinois at Urbana-Champaign; Kavli Institute of
Cosmological Physics at the University of Chicago; Center for Cosmology
and Astro-Particle Physics at the Ohio State University; Mitchell
Institute for Fundamental Physics and Astronomy at Texas AM University;
Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia,
Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating
Institutions in the Dark Energy Survey; National Science Foundation
[AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986];
Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research
Council under the European Union [240672, 291329, 306478]
FX AdP acknowledges financial support from the Brazilian Institution CNPq.
EdB acknowledges financial support from the European Research Council
(ERC-StG-335936, CLUSTERS).; Funding for the DES Projects has been
provided by the US Department of Energy, the US National Science
Foundation, the Ministry of Science and Education of Spain, the Science
and Technology Facilities Council of the United Kingdom, the Higher
Education Funding Council for England, the National Center for
Supercomputing Applications at the University of Illinois at
Urbana-Champaign, the Kavli Institute of Cosmological Physics at the
University of Chicago, the Center for Cosmology and Astro-Particle
Physics at the Ohio State University, the Mitchell Institute for
Fundamental Physics and Astronomy at Texas A&M University, Financiadora
de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa
do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e
Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating
Institutions in the Dark Energy Survey.; The DES data management system
is supported by the National Science Foundation under Grant Number
AST-1138766. The DES participants from Spanish institutions are
partially supported by MINECO under grants AYA2012-39559, ESP2013-48274,
FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234.
Research leading to these results has received funding from the European
Research Council under the European Union's Seventh Framework Programme
(FP7/2007-2013) including ERC grant agreements 240672, 291329 and
306478.
NR 67
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U1 5
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 SEP 1
PY 2016
VL 461
IS 1
BP 519
EP 541
DI 10.1093/mnras/stw1260
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500041
ER
PT J
AU LeGrande, AN
Tsigaridis, K
Bauer, SE
AF LeGrande, Allegra N.
Tsigaridis, Kostas
Bauer, Susanne E.
TI Role of atmospheric chemistry in the climate impacts of stratospheric
volcanic injections
SO NATURE GEOSCIENCE
LA English
DT Article
ID WATER-VAPOR; NORTHERN MIDLATITUDES; ERUPTIONS; OZONE; PINATUBO; WINTER;
RECONSTRUCTIONS; SPECTROMETER; SENSITIVITY; AEROSOLS
AB The climate impact of a volcanic eruption is known to be dependent on the size, location and timing of the eruption. However, the chemistry and composition of the volcanic plume also control its impact on climate. It is not just sulfur dioxide gas, but also the coincident emissions of water, halogens and ash that influence the radiative and climate forcing of an eruption. Improvements in the capability of models to capture aerosol microphysics, and the inclusion of chemistry and aerosol microphysics modules in Earth system models, allow us to evaluate the interaction of composition and chemistry within volcanic plumes in a new way. These modelling efforts also illustrate the role of water vapour in controlling the chemical evolution - and hence climate impacts - of the plume. A growing realization of the importance of the chemical composition of volcanic plumes is leading to a more sophisticated and realistic representation of volcanic forcing in climate simulations, which in turn aids in reconciling simulations and proxy reconstructions of the climate impacts of past volcanic eruptions. More sophisticated simulations are expected to help, eventually, with predictions of the impact on the Earth system of any future large volcanic eruptions.
C1 [LeGrande, Allegra N.; Tsigaridis, Kostas; Bauer, Susanne E.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Tsigaridis, Kostas; Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY USA.
RP LeGrande, AN (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM allegra.n.legrande@nasa.gov; kostas.tsigaridis@columbia.edu
FU NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center
FX We thank NASA GISS for institutional support. We also thank the NASA MAP
programme for continued support. Resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center.
NR 50
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U1 14
U2 14
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD SEP
PY 2016
VL 9
IS 9
BP 652
EP 655
DI 10.1038/NGEO2771
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA DV9TA
UT WOS:000383283700006
ER
PT J
AU Wooden, DH
Cook, AM
Colaprete, A
Glenar, DA
Stubbs, TJ
Shirley, M
AF Wooden, D. H.
Cook, A. M.
Colaprete, A.
Glenar, D. A.
Stubbs, T. J.
Shirley, M.
TI Evidence for a dynamic nanodust cloud enveloping the Moon
SO NATURE GEOSCIENCE
LA English
DT Article
ID GENERATED DUST CLOUDS; HYPERVELOCITY IMPACTS; PLANETARY SATELLITES;
COMET P/HALLEY; SURFACES; SPACE; FE
AB The exospheres that surround airless bodies such as the Moon are tenuous, atmosphere-like layers whose constituent particles rarely collide with one another. Some particles contained within such exospheres are the product of direct interactions between airless bodies and the space environment, and offer insights into space weathering processes. NASA's Lunar Atmosphere and Dust Environment Explorer (LADEE) mission studied the Moon's exospheric constituents in situ and detected a permanent dust exosphere(1) of particles with radii as small as 300 nm. Here we present evidence from LADEE spectral data for an additional fluctuating nanodust exosphere at the Moon containing a population of particles sufficiently dense to be detectable via scattered sunlight. We compare two anti-Sun spectral observations: one near the peak of the Quadrantid meteoroid stream, the other during a period of comparatively weak stream activity. The former shows a negative spectral slope consistent with backscattering of sunlight by nanodust grains with radii less than 20 to 30 nm; the latter has a flatter spectral slope. We hypothesize that a spatially and temporally variable nanodust exosphere may exist at the Moon, and that it is modulated by changes in meteoroid impact rates, such as during encounters with meteoroid streams. The findings suggest that similar nanodust exospheres-and the particle ejection and transport processes that form them-may occur at other airless bodies.
C1 [Wooden, D. H.; Cook, A. M.; Colaprete, A.; Shirley, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cook, A. M.] Millenium Engn & Integrat Co, 350 North Akron Rd Bldg 19,Suite 2080, Moffett Field, CA 94035 USA.
[Glenar, D. A.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Stubbs, T. J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Wooden, DH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM diane.wooden@nasa.gov
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
FU NASA Lunar Quest Program; LADEE Guest Observer Program; NASA's Science
Mission Directorate
FX LADEE UVS was supported through the NASA Lunar Quest Program. The
authors also acknowledge financial support from the LADEE Guest Observer
Program and NASA's Science Mission Directorate.
NR 29
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U1 5
U2 5
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD SEP
PY 2016
VL 9
IS 9
BP 665
EP +
DI 10.1038/NGEO2779
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DV9TA
UT WOS:000383283700008
ER
PT J
AU Dhakal, B
Nicholson, DE
Saleeb, AF
Padula, SA
Vaidyanathan, R
AF Dhakal, B.
Nicholson, D. E.
Saleeb, A. F.
Padula, S. A., II
Vaidyanathan, R.
TI Three-dimensional deformation response of a NiTi shape memory
helical-coil actuator during thermomechanical cycling: experimentally
validated numerical model
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE experimental validation; NiTi; multi-axial; shape memory alloy; thermal
cycling; helical-coil actuators; springs
ID PERFORMANCE-CHARACTERISTICS; CONSTITUTIVE MODEL; ALLOYS; TRANSFORMATION;
EVOLUTION; PHASE
AB Shape memory alloy (SMA) actuators often operate under a complex state of stress for an extended number of thermomechanical cycles in many aerospace and engineering applications. Hence, it becomes important to account for multi-axial stress states and deformation characteristics (which evolve with thermomechanical cycling) when calibrating any SMA model for implementation in large-scale simulation of actuators. To this end, the present work is focused on the experimental validation of an SMA model calibrated for the transient and cyclic evolutionary behavior of shape memory Ni49.9Ti50.1, for the actuation of axially loaded helical-coil springs. The approach requires both experimental and computational aspects to appropriately assess the thermomechanical response of these multi-dimensional structures. As such, an instrumented and controlled experimental setup was assembled to obtain temperature, torque, degree of twist and extension, while controlling end constraints during heating and cooling of an SMA spring under a constant externally applied axial load. The computational component assesses the capabilities of a general, multi-axial, SMA material-modeling framework, calibrated for Ni49.9Ti50.1 with regard to its usefulness in the simulation of SMA helical-coil spring actuators. Axial extension, being the primary response, was examined on an axially-loaded spring with multiple active coils. Two different conditions of end boundary constraint were investigated in both the numerical simulations as well as the validation experiments: Case (1) where the loading end is restrained against twist (and the resulting torque measured as the secondary response) and Case (2) where the loading end is free to twist (and the degree of twist measured as the secondary response). The present study focuses on the transient and evolutionary response associated with the initial isothermal loading and the subsequent thermal cycles under applied constant axial load. The experimental results for the helical-coil actuator under two different boundary conditions are found to be within error to their counterparts in the numerical simulations. The numerical simulation and the experimental validation demonstrate similar transient and evolutionary behavior in the deformation response under the complex, inhomogeneous, multi-axial stress-state and large deformations of the helical-coil actuator. This response, although substantially different in magnitude, exhibited similar evolutionary characteristics to the simple, uniaxial, homogeneous, stress-state of the isobaric tensile tests results used for the model calibration. There was no significant difference in the axial displacement (primary response) magnitudes observed between Cases (1) and (2) for the number of cycles investigated here. The simulated secondary responses of the two cases evolved in a similar manner when compared to the experimental validation of the respective cases.
C1 [Dhakal, B.; Saleeb, A. F.] Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA.
[Nicholson, D. E.; Vaidyanathan, R.] Univ Cent Florida, Dept Mat Sci & Engn, Dept Mech & Aerosp Engn, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
RP Dhakal, B (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA.
EM bd27@zips.uakron.edu
FU Fundamental Aeronautics Program, Fixed-Wing [NNH10ZEA001N-SFW1,
NNX11AI57A]; University of Central Florida
FX This work was supported by the Fundamental Aeronautics Program,
Fixed-Wing, Project No. NNH10ZEA001N-SFW1, Grant No: NNX11AI57A to the
University of Akron with the University of Central Florida as Sub
Contractor. The authors would like to acknowledge Dr S M Arnold for his
technical guidance and programmatic support during the different phases
of the project. The authors thank Dr O Benafan for helpful technical
discussions regarding the experiments.
NR 39
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U1 7
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2016
VL 25
IS 9
AR 095056
DI 10.1088/0964-1726/25/9/095056
PG 16
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA DW9SF
UT WOS:000384002200008
ER
PT J
AU Narapusetty, B
Murtugudde, R
Wang, H
Kumar, A
AF Narapusetty, Balachandrudu
Murtugudde, Raghu
Wang, Hui
Kumar, Arun
TI Ocean-atmosphere processes driving Indian summer monsoon biases in CFSv2
hindcasts
SO CLIMATE DYNAMICS
LA English
DT Article
DE CFSv2 forecast biases; Indian summer monsoon rainfall; Dry-land biases
ID WESTERN ARABIAN SEA; INTRASEASONAL OSCILLATIONS; RAINFALL VARIABILITY;
GLOBAL PRECIPITATION; ASIAN MONSOON; PREDICTION; CLIMATE; MODEL;
DYNAMICS
AB This paper analyzes the role of the Indian Ocean (IO) and the atmosphere biases in generating and sustaining large-scale precipitation biases over Central India (CI) during the Indian summer monsoon (ISM) in the climate forecast system version 2 (CFSv2) hindcasts that are produced by initializing the system each month from January 1982 to March 2011. The CFSv2 hindcasts are characterized by a systematic dry monsoon bias over CI that deteriorate with forecast lead-times and coexist with a wet bias in the tropical IO suggesting a large-scale interplay between coupled ocean-atmosphere and land biases. The biases evolving from spring-initialized forecasts are analyzed in detail to understand the evolution of summer biases. The northward migration of the Inter Tropical Convergence Zone (ITCZ) that typically crosses the equator in the IO sector during April in nature is delayed in the hindcasts when the forecast system is initialized in early spring. Our analyses show that the delay in the ITCZ coexists with wind and SST biases and the associated processes project onto the seasonal evolution of the coupled ocean-atmosphere features. This delay in conjunction with the SST and the wind biases during late spring and early summer contributes to excessive precipitation over the ocean and leading to a deficit in rainfall over CI throughout the summer. Attribution of bias to a specific component in a coupled forecast system is particularly challenging as seemingly independent biases from one component affect the other components or are affected by their feedbacks. In the spring-initialized forecasts, the buildup of deeper thermocline in association with warmer SSTs due to the enhanced Ekman pumping in the southwest IO inhibits the otherwise typical northward propagation of ITCZ in the month of April. Beyond this deficiency in the forecasts, two key ocean-atmosphere coupled mechanisms are identified; one in the Arabian Sea, where a positive windstress curl bias in conjunction with warmer SSTs lead to a weakening of Findlater jet and the other in the east equatorial IO where a remote forcing by the predominantly westerly bias in the western-central equatorial IO in the summer strengthen the seasonal downwelling Kelvin wave that in turn deepens the thermocline in the eastern IO. The equatorial Kelvin wave continues as a coastal Kelvin wave and disperses as Rossby waves off Sumatra and induces positive SST and precipitation biases in the eastern and southern Bay of Bengal. This study shows that the biases that first appear in winds lead to a cascade of coupled processes that exacerbate the subsequent biases by modulating the evolution of seasonal processes such as the annual Kelvin and Rossby waves and the cross-equatorial vertically integrated moisture transport. While this analysis does not offer any particular insights into improving the ISM forecasts, it is a foundational first step towards this goal.
C1 [Narapusetty, Balachandrudu; Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Narapusetty, Balachandrudu] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wang, Hui] INNOVIM, College Pk, MD USA.
[Wang, Hui] NOAA, NCEP, Climate Predict Ctr, College Pk, MD USA.
[Kumar, Arun] NOAA, NWS, NCEP, Climate Predict Ctr, College Pk, MD USA.
RP Narapusetty, B (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Narapusetty, B (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM bnarapus@umd.edu
FU Earth System Science Organization, Ministry of Earth Sciences,
Government of India [MM/SERP/Univ_Maryland_USA/2013/INT-16/002]
FX The authors gratefully acknowledge the financial support given by the
Earth System Science Organization, Ministry of Earth Sciences,
Government of India (MM/SERP/Univ_Maryland_USA/2013/INT-16/002) to
conduct this research under Monsoon Mission. The authors also
acknowledge Dr. Krishnan, Dr. Rajeevan, Dr. Shukla, and Dr. Kinter for
helpful comments and discussions.
NR 48
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U1 3
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2016
VL 47
IS 5-6
BP 1417
EP 1433
DI 10.1007/s00382-015-2910-9
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU3LK
UT WOS:000382112000005
ER
PT J
AU Stanfield, RE
Jiang, JH
Dong, XQ
Xi, BK
Su, H
Donner, L
Rotstayn, L
Wu, TW
Cole, J
Shindo, E
AF Stanfield, Ryan E.
Jiang, Jonathan H.
Dong, Xiquan
Xi, Baike
Su, Hui
Donner, Leo
Rotstayn, Leon
Wu, Tongwen
Cole, Jason
Shindo, Eiki
TI A quantitative assessment of precipitation associated with the ITCZ in
the CMIP5 GCM simulations
SO CLIMATE DYNAMICS
LA English
DT Article
DE GCM; Global climate models; GCM precipitation; Model precipitation;
AMIP; CMIP; CMIP5; Climate change; ITCZ; GCM bias
ID GENERAL-CIRCULATION MODEL; PACIFIC COLD-TONGUE; LARGE-SCALE MODELS;
INCLUDING MASS FLUXES; GLOBAL CLIMATE MODEL; EARTH SYSTEM MODEL; NASA
GISS CMIP5; PART I; CUMULUS CONVECTION; RAINFALL PRODUCTS
AB According to the Intergovernmental Panel on Climate Change 5th Assessment Report, the broad-scale features of precipitation as simulated by Phase 5 of the Coupled Model Intercomparison Project (CMIP5) are in modest agreement with observations, however, large systematic errors are found in the Tropics. In this study, a new algorithm has been developed to define the North Pacific Intertropical Convergence Zone (ITCZ) through several metrics, including: the centerline position of the ITCZ, the width of the ITCZ, and the magnitude of precipitation along the defined ITCZ. These metrics provide a quantitative analysis of precipitation associated with the ITCZ over the equatorial northern Pacific. Results from 29 CMIP5 Atmospheric Model Intercomparison Project (AMIP) Global Circulation Model (GCM) runs are compared with Global Precipitation Climatology Project (GPCP) and Tropical Rainfall Measuring Mission (TRMM) observations. Similarities and differences between the GCM simulations and observations are analyzed with the intent of quantifying magnitude-, location-, and width-based biases within the GCMs. Comparisons show that most of the GCMs tend to simulate a stronger, wider ITCZ shifted slightly northward compared to the ITCZ in GPCP and TRMM observations. Comparisons of CMIP and AMIP simulated precipitation using like-models were found to be nearly equally distributed, with roughly half of GCMs showing an increase (decrease) in precipitation when coupled (decoupled) from their respective ocean model. Further study is warranted to understand these differences.
C1 [Stanfield, Ryan E.; Dong, Xiquan; Xi, Baike] Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA.
[Jiang, Jonathan H.; Su, Hui] Jet Prop Lab, Pasadena, CA USA.
[Donner, Leo] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Rotstayn, Leon] CSIRO, Clayton, Vic, Australia.
[Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China.
[Cole, Jason] Environm Canada, Canadian Ctr Climate Modeling & Anal, Toronto, ON, Canada.
[Shindo, Eiki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
FU Jet Propulsion Laboratory (JPL), California Institute of Technology
under NASA; NASA CERES [NNX14AP84G]; EPSCoR projects; NASA [ROSES12-MAP,
ROSE13-NDOA]
FX We would like to acknowledge the contributions made by Trond Iversen,
for providing information and references on the NorESM model, and the
contributions made by Cyril Morcrette, for his comments and suggestions
related to HadGEM2-A model. The authors acknowledge the support by the
Jet Propulsion Laboratory (JPL), California Institute of Technology
under contract with NASA. The researchers at University of North Dakota
were supported by NASA CERES (NNX14AP84G) and EPSCoR projects, and the
researchers at JPL were supported by NASA ROSES12-MAP and ROSE13-NDOA
projects. Data were obtained from the CMIP5 ESGF PCMDI database at
http://pcmdi9.llnl.gov/esgf-web-fe/. GPCP and TRMM data are also
provided by the Obs4MIPS program and are available as well from the ESGF
PCMDI database at http://pcmdi9.llnl.gov/esgf-web-fe/. The GPCP SG
combined precipitation data were developed and computed at the
NASA/Goddard Space Flight Center's Mesoscale Atmospheric Processes
Laboratory - Atmospheres as a contribution to the GEWEX Global
Precipitation Climatology Project.
NR 64
TC 0
Z9 0
U1 7
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2016
VL 47
IS 5-6
BP 1863
EP 1880
DI 10.1007/s00382-015-2937-y
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU3LK
UT WOS:000382112000031
ER
PT J
AU Abdi, AM
Vrieling, A
Yengoh, GT
Anyamba, A
Seaquist, JW
Ummenhofer, CC
Ardo, J
AF Abdi, A. M.
Vrieling, A.
Yengoh, G. T.
Anyamba, A.
Seaquist, J. W.
Ummenhofer, C. C.
Ardo, J.
TI The El Nio - La Nia cycle and recent trends in supply and demand of net
primary productivity in African drylands
SO CLIMATIC CHANGE
LA English
DT Article
DE Sub-Saharan Africa; Drylands; El Nino-southern oscillation; Net primary
productivity; Climate variability
ID FOOD INSECURITY; CLIMATE; ECOSYSTEMS; PATTERNS; RAINFALL; ETHIOPIA;
CHARCOAL; ENSO
AB Inter-annual climatic variability over a large portion of sub-Saharan Africa is under the influence of the El Nio-Southern Oscillation (ENSO). Extreme variability in climate is a threat to rural livelihoods in sub-Saharan Africa, yet the role of ENSO in the balance between supply and demand of net primary productivity (NPP) over this region is unclear. Here, we analyze the impact of ENSO on this balance in a spatially explicit framework using gridded population data from the WorldPop project, satellite-derived data on NPP supply, and statistical data from the United Nations. Our analyses demonstrate that between 2000 and 2013 fluctuations in the supply of NPP associated with moderate ENSO events average +/- 2.8 g C m(-2) yr.(-1) across sub-Saharan drylands. The greatest sensitivity is in arid Southern Africa where a + 1 A degrees C change in the Nio-3.4 sea surface temperature index is associated with a mean change in NPP supply of -6.6 g C m(-2) yr.(-1). Concurrently, the population-driven trend in NPP demand averages 3.5 g C m(-2) yr.(-1) over the entire region with densely populated urban areas exhibiting the highest mean demand for NPP. Our findings highlight the importance of accounting for the role ENSO plays in modulating the balance between supply and demand of NPP in sub-Saharan drylands. An important implication of these findings is that increase in NPP demand for socio-economic metabolism must be taken into account within the context of climate-modulated supply.
C1 [Abdi, A. M.; Seaquist, J. W.; Ardo, J.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Vrieling, A.] Univ Twente, Fac Geoinformat Sci & Earth Observat, POB 217, NL-7500 AE Enschede, Netherlands.
[Yengoh, G. T.] Lund Univ, Ctr Sustainabil Studies, S-22362 Lund, Sweden.
[Anyamba, A.] Natl Aeronaut & Space Adm, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA.
[Ummenhofer, C. C.] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
RP Abdi, AM (reprint author), Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
EM hakim.abdi@gmail.com
RI Vrieling, Anton/B-2639-2012;
OI Vrieling, Anton/0000-0002-7979-1540; Abdi, PhD,
Abdulhakim/0000-0001-6486-8747
FU Swedish National Space Board [100/11]; Royal Physiographic Society in
Lund; Lund University Center for Studies of Carbon Cycle and Climate
Interactions (LUCCI); NSF [OCE-1203892]
FX We thank Dan Metcalfe, Lina Eklund, A.J. (Han) Dolman, and Katharina
Waha for their insight and comments during early stages of the
manuscript. We also thank the programming assistance provided by the
volunteers at the Stack Overflow and Cross Validated online communities.
Funding for this project was provided by the Swedish National Space
Board (contract no. 100/11 to J.A.). A.M.A. received support from the
Royal Physiographic Society in Lund and the Lund University Center for
Studies of Carbon Cycle and Climate Interactions (LUCCI). C.C.U. was
supported by NSF grant OCE-1203892.
NR 49
TC 0
Z9 0
U1 14
U2 14
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD SEP
PY 2016
VL 138
IS 1-2
BP 111
EP 125
DI 10.1007/s10584-016-1730-1
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU3UT
UT WOS:000382138400009
ER
PT J
AU Morgan, D
Subramanian, GP
Chung, SJ
Hadaegh, FY
AF Morgan, Daniel
Subramanian, Giri P.
Chung, Soon-Jo
Hadaegh, Fred Y.
TI Swarm assignment and trajectory optimization using variable-swarm,
distributed auction assignment and sequential convex programming
SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH
LA English
DT Article
ID FORMATION FLYING GUIDANCE; MODEL-PREDICTIVE CONTROL; SATELLITE CLUSTERS;
MULTIPLE ROBOTS; SPACECRAFT; ALGORITHM; STRATEGIES; OPTIMALITY; NETWORKS
AB This paper presents a distributed, guidance and control algorithm for reconfiguring swarms composed of hundreds to thousands of agents with limited communication and computation capabilities. This algorithm solves both the optimal assignment and collision-free trajectory generation for robotic swarms, in an integrated manner, when given the desired shape of the swarm ( without pre-assigned terminal positions). The optimal assignment problem is solved using a distributed auction assignment that can vary the number of target positions in the assignment, and the collision-free trajectories are generated using sequential convex programming. Finally, model predictive control is used to solve the assignment and trajectory generation in real time using a receding horizon. The model predictive control formulation uses current state measurements to resolve for the optimal assignment and trajectory. The implementation of the distributed auction algorithm and sequential convex programming using model predictive control produces the swarm assignment and trajectory optimization ( SATO) algorithm that transfers a swarm of robots or vehicles to a desired shape in a distributed fashion. Once the desired shape is uploaded to the swarm, the algorithm determines where each robot goes and how it should get there in a fuel-efficient, collision-free manner. Results of flight experiments using multiple quadcopters show the effectiveness of the proposed SATO algorithm.
C1 [Morgan, Daniel; Subramanian, Giri P.; Chung, Soon-Jo] Univ Illinois, Urbana, IL USA.
[Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Chung, SJ (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.; Chung, SJ (reprint author), Univ Illinois, Coordinated Sci Lab, Urbana, IL 61801 USA.
EM sjchung@illinois.edu
FU National Aeronautics and Space Administration; NASA Office of the Chief
Technologist Space Technology Research Fellowship; Air Force Office of
Scientific Research (AFOSR) [FA95501210193]
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. (C)2016 California Institute of
Technology. This work was supported by a NASA Office of the Chief
Technologist Space Technology Research Fellowship and an Air Force
Office of Scientific Research (AFOSR grant number FA95501210193).
Government sponsorship acknowledged.
NR 43
TC 1
Z9 1
U1 7
U2 7
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0278-3649
EI 1741-3176
J9 INT J ROBOT RES
JI Int. J. Robot. Res.
PD SEP
PY 2016
VL 35
IS 10
BP 1261
EP 1285
DI 10.1177/0278364916632065
PG 25
WC Robotics
SC Robotics
GA DV5PY
UT WOS:000382981300006
ER
PT J
AU Schonberg, WP
Hull, SM
AF Schonberg, William P.
Hull, Scott M.
TI Current Design Criteria for MMOD Impact of Metallic Pressurized Tanks
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
ID HYPERVELOCITY IMPACT; VESSELS
AB Most spacecraft have at least one pressurized vessel on board. For robotic spacecraft, it is usually a liquid propellant tank or battery. For human spacecraft, there are also pressurized living quarters and life-support systems. One of the design considerations of such spacecraft is the possible damage that might occur in the event of an on-orbit impact by a micrometeoroid or orbital debris (MMOD) particle. While considerable energy and effort has been expended in the study of the response of nonpressurized spacecraft components to these kinds of impacts, relatively few studies have been conducted on the pressurized elements of such spacecraft. In addition, the design criteria currently used by the National Aeronautics and Space Administration (NASA) for pressurized tanks operating in the MMOD environment have not been tested or scrutinized since they were first proposed nearly 45 years ago. This paper reviews current NASA design criteria for pressurized vessels and offers suggestions for next steps in their further development. (C) 2016 American Society of Civil Engineers.
C1 [Schonberg, William P.] Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA.
[Hull, Scott M.] NASA, Goddard Space Flight Ctr, Mission Engn & Syst Anal Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Schonberg, WP (reprint author), Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA.
EM wschon@mst.edu
FU NASA/Jet Propulsion Laboratory; NASA/Engineering Safety Center
FX The authors wish to extend their gratitude to the NASA/Jet Propulsion
Laboratory and the NASA/Engineering Safety Center for providing the
support that made this study possible.
NR 24
TC 0
Z9 0
U1 1
U2 1
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD SEP
PY 2016
VL 29
IS 5
DI 10.1061/(ASCE)AS.1943-5525.0000635
PG 4
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA DV7VJ
UT WOS:000383145800024
ER
PT J
AU Salinas, A
Altecor, A
Lizcano, M
Lozano, K
AF Salinas, A.
Altecor, A.
Lizcano, M.
Lozano, K.
TI Production of beta-Silicon Carbide Nanofibers using the Forcespinning
(R) Method
SO JOURNAL OF CERAMIC SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Silicon carbide; high-temperature materials; ceramic nanofibers;
Forcespinning (R)
ID FIBERS; NANOWIRES
AB Silicon carbide (SiC) nanofibers were produced on a large scale using the Forcespinning (R) method. Non-oxide ceramics such as SiC are known for their low density, oxidation resistance, thermal stability, and wear resistance. The nanofibers were prepared using a solution-based method with polystyrene and polycarbomethylsilane as the precursor materials. Fiber spinning was performed under different parameters to obtain high yield, fiber homogeneity, and small diameters. The fibers were spun under a controlled nitrogen environment to prevent fiber oxidation. The resultant nonwoven nanofiber mats were then subjected to different heat treatments to evaluate the effect of these on the crystalline structure. Characterization was conducted using scanning electron microscopy, x-ray diffraction, and thermogravimetric analysis. The results show high yield, semi-continuous bead-free nanofibers with diameters ranging from 280 nm to 2 micron depending on the selected processing parameters. The sintered precursors show formation of SiC nanofibers with a beta phase crystalline structure and oxygen content below 15 %.
C1 [Salinas, A.; Altecor, A.; Lozano, K.] Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA.
[Lizcano, M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Salinas, A (reprint author), Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA.
EM asalinasz73@broncs.utpa.edu
FU National Science Foundation under DMR grant [1523577]
FX The authors gratefully acknowledge financial support received from the
National Science Foundation under DMR grant No. 1523577 (PREM- UTRGV-UMN
Partnership for Fostering Innovation by Bridging Excellence in Research
and Student Success). We are also grateful to the Biology Department at
the University of Texas Rio Grande Valley for allowing use of the EDS
instrument.
NR 26
TC 0
Z9 0
U1 5
U2 5
PU GOLLER VERLAG GMBH
PI BADEN BADEN
PA ASCHMATTSTRASSE 8, D-76532 BADEN BADEN, GERMANY
SN 2190-9385
J9 J CERAM SCI TECHNOL
JI J. Ceram. Sci. Technol.
PD SEP
PY 2016
VL 7
IS 3
BP 229
EP 234
DI 10.4416/JCST2016-00026
PG 6
WC Materials Science, Ceramics
SC Materials Science
GA DW0FO
UT WOS:000383316500002
ER
PT J
AU Li, T
Calvo, N
Yue, J
Russell, JM
Smith, AK
Mlynczak, MG
Chandran, A
Dou, XK
Liu, AZ
AF Li, Tao
Calvo, Natalia
Yue, Jia
Russell, James M., III
Smith, Anne K.
Mlynczak, Martin G.
Chandran, Amal
Dou, Xiankang
Liu, Alan Z.
TI Southern Hemisphere Summer Mesopause Responses to El Nino-Southern
Oscillation
SO JOURNAL OF CLIMATE
LA English
DT Article
ID STRATOSPHERE; ATMOSPHERE; MIDDLE; MODEL; TEMPERATURES; CIRCULATION; ENSO
AB In the Southern Hemisphere (SH) polar region, satellite observations reveal a significant upper-mesosphere cooling and a lower-thermosphere warming during warm ENSO events in December. An opposite pattern is observed in the tropical mesopause region. The observed upper-mesosphere cooling agrees with a climate model simulation. Analysis of the simulation suggests that enhanced planetary wave (PW) dissipation in the Northern Hemisphere (NH) high-latitude stratosphere during El Nino strengthens the Brewer-Dobson circulation and cools the equatorial stratosphere. This increases the magnitude of the SH stratosphere meridional temperature gradient and thus causes the anomalous stratospheric easterly zonal wind and early breakdown of the SH stratospheric polar vortex. The resulting perturbation to gravity wave (GW) filtering causes anomalous SH mesospheric eastward GW forcing and polar upwelling and cooling. In addition, constructive inference of ENSO and quasi-biennial oscillation (QBO) could lead to stronger stratospheric easterly zonal wind anomalies at the SH high latitudes in November and December and early breakdown of the SH stratospheric polar vortex during warm ENSO events in the easterly QBO phase (defined by the equatorial zonal wind at similar to 25 hPa). This would in turn cause much more SH mesospheric eastward GW forcing and much colder polar temperatures, and hence it would induce an early onset time of SH summer polar mesospheric clouds (PMCs). The opposite mechanism occurs during cold ENSO events in the westerly QBO phase. This implies that ENSO together with QBO could significantly modulate the breakdown time of SH stratospheric polar vortex and the onset time of SH PMC.
C1 [Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Geospace Environm, Hefei 230026, Anhui, Peoples R China.
[Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, Mengcheng Natl Geophys Observ, Hefei 230026, Anhui, Peoples R China.
[Calvo, Natalia] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain.
[Yue, Jia; Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Smith, Anne K.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Chandran, Amal] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Liu, Alan Z.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA.
RP Li, T (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, 96 Jinzhai Rd, Hefei 230026, Anhui, Peoples R China.
EM litao@ustc.edu.cn
RI Dou, xiankang/M-9106-2013; Yue, Jia/D-8177-2011; Li, Tao/J-8950-2014
OI Li, Tao/0000-0002-5100-4429
FU National Natural Science Foundation of China [41225017, 41421063];
National Basic Research Program of China [2012CB825605]; NSF
[AGS-1115249, AGS-1110199]; Spanish Ministry of Economy and
Competitiveness through the PALEOSTRAT project [CGL2015-69699-R];
European Project under program [603557-STRATOCLIM, FP7-ENV.2013.6.1-2];
NASA AIM satellite mission; NASA TIMED satellite mission; NASA SABER
Grant [NNX15AD22G]; NASA TIMED satellite project; National Science
Foundation [AGS-1115249, AGS-1110199]
FX TL would like to thank Han-Li Liu and Chengyun Yang for helpful
discussion. TL and XD are supported by the National Natural Science
Foundation of China Grants 41225017 and 41421063 and the National Basic
Research Program of China Grant 2012CB825605. TL's visit to ERAU is
partially supported by the NSF Grants AGS-1115249 and AGS-1110199. NC
acknowledges partial support from the Spanish Ministry of Economy and
Competitiveness through the PALEOSTRAT project (Paleomodelization desde
una perspective estratoferica; Ref. CGL2015-69699-R) and the European
Project 603557-STRATOCLIM under program FP7-ENV.2013.6.1-2. JY is
supported by the NASA AIM and TIMED satellite missions. JMR is supported
under NASA SABER Grant NNX15AD22G. MGM is supported by the NASA TIMED
satellite project. AZL is supported by National Science Foundation
Grants AGS-1115249 and AGS-1110199. The WACCM 3.5 results were obtained
from the Atmospheric Chemistry Division at the National Center for
Atmospheric Research. The radiosonde dataset is downloaded from
http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/index.html. We
want to thank Bodil Karlsson and two other anonymous reviewers for their
constructive comments on this paper.
NR 28
TC 1
Z9 1
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP 1
PY 2016
VL 29
IS 17
BP 6319
EP 6328
DI 10.1175/JCLI-D-15-0816.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3DO
UT WOS:000382801400016
ER
PT J
AU Russell, RP
Lantukh, D
Broschart, SB
AF Russell, Ryan P.
Lantukh, Demyan
Broschart, Stephen B.
TI Heliotropic Orbits with Zonal Gravity and Shadow Perturbations:
Application at Bennu
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID SOLAR-RADIATION PRESSURE; ASTEROID 101955 BENNU; PLANETARY OBLATENESS;
EVEN HARMONICS; DUST DYNAMICS; SATELLITE; DENSITY; MOTION
AB Heliotropic orbits provide long-lifetime low-altitude orbits in the presence of large J2 and solar radiation pressure perturbations. Formal inclusion of high-degree zonal gravity harmonics and simple shadowing provides a more realistic model to initiate the search for heliotropic orbits at irregular primitive bodies like Bennu, which is the target of the OSIRIS-Rex mission. The constrained, doubly averaged potential and the Lagrange planetary equations yield a single equation to enforce the heliotropic constraint. The equation is solved for inclinations across a range of semimajor axes and eccentricities, providing a surface of potential solutions. The fast process allows for MonteCarlo simulations to assess the likelihood of a heliotropic orbit existing in the presence of parameter uncertainty. The existence of heliotropic orbits is shown to be reasonably robust to uncertainty in the solar radiation pressure acceleration and reference gravity parameters for Bennu.
C1 [Russell, Ryan P.; Lantukh, Demyan] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Broschart, Stephen B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Russell, RP (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
EM ryan.russell@utexas.edu; demyan@utexas.edu;
Stephen.B.Broschart@jpl.nasa.gov
FU NASA Office of the Chief Technologist via a NASA Space Technology
Research Fellowship [NNX12AI77H]; W. M. Keck Foundation; NASA
FX This work was supported in part by the NASA Office of the Chief
Technologist via a NASA Space Technology Research Fellowship grant
(NNX12AI77H). In particular, the authors thank Claudia Meyer for
continued interest and support of the project. The authors also thank
the W. M. Keck Foundation for supporting, in part, the presented work
through the W. M. Keck Foundation Endowed Graduate Fellowship in
Engineering. Part of the work described here was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 22
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP
PY 2016
VL 39
IS 9
BP 1925
EP 1933
DI 10.2514/1.G001279
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DV9LH
UT WOS:000383261500001
ER
PT J
AU Swei, SSM
Fusco, JC
Nakamura, RH
AF Swei, Sean S. M.
Fusco, Jesse C.
Nakamura, Robert H.
TI Design of Sun-Safe Controllers for Lunar Atmosphere and Dust Environment
Explorer
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
AB This paper presents the development of sun-safe controllers, which are designed to keep the spacecraft power positive and thermally balanced in the event an anomaly is detected. Employed by NASA's Lunar Atmosphere and Dust Environment Explorer, the controllers use the measured sun vector and the spacecraft body rates for feedback control. To improve the accuracy of sun vector estimation, the least-square minimization approach is applied to process the sensor data. A rotation with respect to the sun vector, which is proven to be effective in mitigating the momentum buildup due to the lunar gravity gradient, hence significantly extending the sun-safe duration, is commanded. To validate the controllers, the Lunar Atmosphere and Dust Environment Explorer spacecraft model engaging the sun-safe mode is first simulated and then compared with the actual Lunar Atmosphere and Dust Environment Explorer orbital flight data. The results demonstrate the applicability of the proposed sun-safe controllers.
C1 [Swei, Sean S. M.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[Fusco, Jesse C.; Nakamura, Robert H.] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA.
RP Swei, SSM (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
NR 9
TC 1
Z9 1
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP
PY 2016
VL 39
IS 9
BP 2022
EP 2033
DI 10.2514/1.G000270
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DV9LH
UT WOS:000383261500008
ER
PT J
AU Sung, K
Yu, SS
Pearson, J
Pirali, O
Tchana, FK
Manceron, L
AF Sung, Keeyoon
Yu, Shanshan
Pearson, John
Pirali, Olivier
Tchana, Fridolin Kwabia
Manceron, Laurent
TI Far-infrared (NH3)-N-14 line positions and intensities measured with a
FT-IR and AILES beamline, Synchrotron SOLEIL
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Ammonia spectroscopy; Ammonia line intensity; NH3 far-infrared
transitions; Inversion-rotation; FT-IR measurements; AILES beamline
ID SELF-BROADENING COEFFICIENTS; LASER STARK SPECTROSCOPY;
MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; ENERGY-LEVELS; NH3; AMMONIA;
BANDS; MICROWAVE; STATE
AB Extensive measurements of line positions and intensities are reported for the inversion-rotation and rovibrational transitions of (NH3)-N-14 in the 50-660 cm(-1) region. This study analyzes high-resolution (0.00167 cm(-1), unapodized) Fourier-transform spectra of high purity (99.5%) normal ammonia sample obtained using the AILES beamline of Synchrotron SOLEIL. The experimental conditions are designed to study transitions with intensities weaker than 1 x 10(-22) cm(-1)/(molecule cm(-2)) at room temperature. Line positions and intensities of more than 2830 transitions of (NH3)-N-14 are measured and compiled after proper quality control; the features from minor isotopologues ((NH3)-N-15 and NH2D) and H2O are identified and excluded. Based on the predictions of recent work from the empirical Hamiltonian modeling, systematic quantum assignments are made for 2047 transitions from eight bands including four inversion rotation (gs, v(2), 2v(2), and v(4)) and four ro-vibrational bands (v(2)-gs, 2v(2)-v(2), v(4)-v(2), and 2v(2)-v(4)), as well as covering their Delta K = 3 forbidden transitions. The measured line positions for the assigned transitions are in an excellent agreement (typically better than 0.001 cm(-1)) with the predictions in a wide range of J and K for all the eight bands. The comparison with the HITRAN 2012 database is also satisfactory, although systematic offsets are seen for transitions with high J and K and those from weak bands. Also we note that out of the eight bands, the 2v(2)-v(4) has not been listed in the HITRAN 2012 database. Differences of 20% are seen between our measured and calculated intensities depending on the bands. For line positions, greater differences are found for some NH3 bands in HITRAN 2012 than recent predictions. Measurements of the individual line positions and intensities are presented for the eight bands, and the final spectroscopic line positions and intensities are compiled as an electronic supplement. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Sung, Keeyoon; Yu, Shanshan; Pearson, John] CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Pirali, Olivier; Manceron, Laurent] LOrme Merisiers St Aubin, Synchrotron SOLEIL, AILES Beamline, F-91192 Gif Sur Yvette, France.
[Pirali, Olivier] Univ Paris Saclay, Univ Paris 11, CNRS, ISMO, F-91405 Orsay, France.
[Tchana, Fridolin Kwabia] UPEC, CNRS, UMR 7583, LISA, 61 Ave Gen Gaulle, F-94010 Creteil, France.
[Tchana, Fridolin Kwabia] UPD, 61 Ave Gen Gaulle, F-94010 Creteil, France.
[Manceron, Laurent] Univ Paris 06, CNRS, UMR 8233, MONARIS, Paris, France.
RP Sung, K (reprint author), CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ksung@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015
FU Synchrotron SOLEIL [2013080]; Astrophysics Research and Analysis (APRA)
Program under the National Aeronautics and Space Administration; SOLEIL;
LISA
FX K. Sung and S. Yu are grateful to Linda R. Brown for useful discussion
on the NH3 spectroscopy and designing the experimental study.
The JPL authors also acknowledge the Synchrotron SOLEIL for granting us
with the AILES beamline time (project #2013080). Research described in
this work was performed at Jet Propulsion Laboratory, California
Institute of Technology, and was supported by the Astrophysics Research
and Analysis (APRA) Program under the National Aeronautics and Space
Administration. F.K.T. and L.M. acknowledge SOLEIL and LISA support.
NR 64
TC 0
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U1 4
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2016
VL 327
SI SI
BP 1
EP 20
DI 10.1016/j.jms.2016.06.011
PG 20
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA DV8WY
UT WOS:000383218600001
ER
PT J
AU Orphal, J
Staehelin, J
Tamminen, J
Braathen, G
De Backer, MR
Bais, A
Balis, D
Barbe, A
Bhartia, PK
Birk, M
Burkholder, JB
Chance, K
von Clarmann, T
Cox, A
Degenstein, D
Evans, R
Flaud, JM
Flittner, D
Godin-Beekmann, S
Gorshelev, V
Gratien, A
Hare, E
Janssen, C
Kyrola, E
McElroy, T
McPeters, R
Pastel, M
Petersen, M
Petropavlovskikh, I
Picquet-Varrault, B
Pitts, M
Labow, G
Rotger-Languereau, M
Leblanc, T
Lerot, C
Liu, X
Moussay, P
Redondas, A
Van Roozendael, M
Sander, SP
Schneider, M
Serdyuchenko, A
Veefkind, P
Viallon, J
Viatte, C
Wagner, G
Weber, M
Wielgosz, RI
Zehner, C
AF Orphal, Johannes
Staehelin, Johannes
Tamminen, Johanna
Braathen, Geir
De Backer, Marie -Renee
Bais, Alkiviadis
Balis, Dimitris
Barbe, Alain
Bhartia, Pawan K.
Birk, Manfred
Burkholder, James B.
Chance, Kelly
von Clarmann, Thomas
Cox, Anthony
Degenstein, Doug
Evans, Robert
Flaud, Jean-Marie
Flittner, David
Godin-Beekmann, Sophie
Gorshelev, Viktor
Gratien, Aline
Hare, Edward
Janssen, Christof
Kyrola, Erkki
McElroy, Thomas
McPeters, Richard
Pastel, Maud
Petersen, Michael
Petropavlovskikh, Irina
Picquet-Varrault, Benedicte
Pitts, Michael
Labow, Gordon
Rotger-Languereau, Maud
Leblanc, Thierry
Lerot, Christophe
Liu, Xiong
Moussay, Philippe
Redondas, Alberto
Van Roozendael, Michel
Sander, Stanley P.
Schneider, Matthias
Serdyuchenko, Anna
Veefkind, Pepijn
Viallon, Joele
Viatte, Camille
Wagner, Georg
Weber, Mark
Wielgosz, Robert I.
Zehner, Claus
TI Absorption cross-sections of ozone in the ultraviolet and visible
spectral regions: Status report 2015
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Ozone; Absorption; Cross sections; Atmosphere; Remote sensing; Reference
data
ID 10 MU-M; TEMPERATURE-DEPENDENCE; PROFILE RETRIEVALS; MONITORING
INSTRUMENT; UV SPECTROSCOPY; TOTAL COLUMN; STRAY LIGHT; NM REGION;
BREWER; O-3
AB The activity "Absorption Cross-Sections of Ozone" (ACSO) started in 2008 as a joint initiative of the International Ozone Commission (IO3C), the World Meteorological Organization (WMO) and the IGACO ("Integrated Global Atmospheric Chemistry Observations") O-3/UV subgroup to study, evaluate, and recommend the most suitable ozone absorption cross-section laboratory data to be used in atmospheric ozone measurements. The evaluation was basically restricted to ozone absorption cross-sections in the UV range with particular focus on the Huggins band. Up until now, the data of Bass and Paur published in 1985 (BP, 1985) are still officially recommended for such measurements. During the last decade it became obvious that BP (1985) cross-section data have deficits for use in advanced space-borne ozone measurements. At the same time, it was recognized that the origin of systematic differences in ground-based measurements of ozone required further investigation, in particular whether the BP (1985) cross-section data might contribute to these differences.
In ACSO, different sets of laboratory ozone absorption cross-section data (including their dependence on temperature) of the group of Reims (France) (Brion et al., 1993, 1998, 1992, 1995, abbreviated as BDM, 1995) and those of Serdyuchenko et al. (2014), and Gorshelev et al. (2014), (abbreviated as SER, 2014) were examined for use in atmospheric ozone measurements in the Huggins band.
In conclusion, ACSO recommends:
The spectroscopic data of BP (1985) should no longer be used for retrieval of atmospheric ozone measurements
For retrieval of ground-based instruments of total ozone and ozone profile measurements by the Umkehr method performed by Brewer and Dobson instruments data of SER (2014) are recommended to be used. When SER (2014) is used, the difference between total ozone measurements of Brewer and Dobson instruments are very small and the difference between Dobson measurements at AD and CD wavelength pairs are diminished.
For ground-based Light Detection and Ranging (LIDAR) measurements the use of BDM (1995) or SER (2014) is recommended.
For satellite retrieval the presently widely used data of BDM (1995) should be used because SER (2014) seems less suitable for retrievals that use wavelengths close to 300 nm due to a deficiency in the signal-to-noise ratio in the SER (2014) dataset.
The work of ACSO also showed:
The need to continue laboratory cross-section measurements of ozone of highest quality. The importance of careful characterization of the uncertainties of the laboratory measurements.
The need to extend the scope of such studies to other wavelength ranges (particularly to cover not only the Huggins band but also the comparison with the mid-infrared region).
The need for regular cooperation of experts in spectral laboratory measurements and specialists in atmospheric (ozone) measurements. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Orphal, Johannes; von Clarmann, Thomas; Schneider, Matthias] KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany.
[Staehelin, Johannes] Swiss Fed Inst Technol, Zurich, Switzerland.
[Tamminen, Johanna; Kyrola, Erkki] FMI, Helsinki, Finland.
[Braathen, Geir] WMO, Geneva, Switzerland.
[De Backer, Marie -Renee; Barbe, Alain; Rotger-Languereau, Maud] CNRS, GSMA, Reims, France.
[De Backer, Marie -Renee; Barbe, Alain] Univ Reims, Reims, France.
[Bais, Alkiviadis; Balis, Dimitris] Aristotele Univ Thessaloniki, Thessaloniki, Greece.
[Bhartia, Pawan K.; McPeters, Richard; Labow, Gordon] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Birk, Manfred; Wagner, Georg] German Aerosp Ctr DLR, Oberpfaffenhofen, Germany.
[Evans, Robert; Petropavlovskikh, Irina] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Chance, Kelly; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Cox, Anthony] Univ Cambridge, Cambridge, England.
[Degenstein, Doug] Univ Saskatchewan, Saskatoon, SK, Canada.
[Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] CNRS, LISA, Creteil, France.
[Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] Univ Paris Est, Creteil, France.
[Flittner, David; Pitts, Michael] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Godin-Beekmann, Sophie; Pastel, Maud] CNRS, LATMOS, Paris, France.
[Godin-Beekmann, Sophie; Pastel, Maud] UVSQ, Paris, France.
[Gorshelev, Viktor; Serdyuchenko, Anna; Weber, Mark] Univ Bremen, Bremen, Germany.
[Hare, Edward] Environm Canada, Toronto, ON, Canada.
[Janssen, Christof] Univ Paris 06, Sorbonne Univ, LERMA, IPSL, Paris, France.
[Janssen, Christof] PSL Res Univ, Observ Paris, Paris, France.
[Janssen, Christof] CNRS, Paris, France.
[McElroy, Thomas] Univ Toronto, Toronto, ON, Canada.
[Petersen, Michael; Moussay, Philippe; Viallon, Joele; Wielgosz, Robert I.] BIPM, Sevres, France.
[Leblanc, Thierry; Sander, Stanley P.] NASA, JPL, Pasadena, CA USA.
[Lerot, Christophe; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Redondas, Alberto] State Meteorol Agcy AEMET, Izana, Spain.
[Veefkind, Pepijn] KNMI, De Bilt, Netherlands.
[Viatte, Camille] CALTECH, Pasadena, CA 91125 USA.
[Zehner, Claus] ESA, ESRIN, Frascati, Italy.
[Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA.
[Petropavlovskikh, Irina] NOAA, Global Monitoring Div, Boulder, CO USA.
[Petersen, Michael] Univ Neuchatel, CH-2000 Neuchatel, Switzerland.
RP Orphal, J (reprint author), KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany.
EM orphal@kit.edu
RI Schneider, Matthias/B-1441-2013; Liu, Xiong/P-7186-2014; Bais,
Alkiviadis/D-2230-2009; Tamminen, Johanna/D-7959-2014; Manager, CSD
Publications/B-2789-2015;
OI Liu, Xiong/0000-0003-2939-574X; Bais, Alkiviadis/0000-0003-3899-2001;
Tamminen, Johanna/0000-0003-3095-0069; Kyrola, Erkki/0000-0001-9197-9549
FU EU FP7 programme [284421]; NASA [NNX09AJ24G]
FX The work of Maud Pastel was performed in the frame of the NORS project
(Demonstration Network Of ground-based Remote Sensing Observations in
support of the Copernicus Atmospheric Service), funded by the EU FP7
programme under grant agreement no 284421. The work of Irina
Petropavlovskikh was supported by NASA Grant No. NNX09AJ24G (Enhancement
of ozone products from established Brewer ground-based networks for
validation of satellite-derived stratospheric ozone change). Johanna
Tamminen would like to thank the Finnish Academy INQUIRE project.
NR 76
TC 4
Z9 4
U1 12
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2016
VL 327
SI SI
BP 105
EP 121
DI 10.1016/j.jms.2016.07.007
PG 17
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA DV8WY
UT WOS:000383218600006
ER
PT J
AU Dreessen, J
Sullivan, J
Delgado, R
AF Dreessen, Joel
Sullivan, John
Delgado, Ruben
TI Observations and impacts of transported Canadian wildfire smoke on ozone
and aerosol air quality in the Maryland region on June 9-12, 2015
SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION
LA English
DT Article; Proceedings Paper
CT 7th International Workshop on Air Quality Forecasting Research (IWAQFR)
CY SEP 01-03, 2015
CL College Park, MD
ID VOLATILE ORGANIC-COMPOUNDS; SOUTHERN CALIFORNIA WILDFIRES; FOREST-FIRE
EMISSIONS; UNITED-STATES; PARTICULATE MATTER; NITROGEN-OXIDES;
CLIMATE-CHANGE; URBAN AREA; BOREAL; POLLUTION
AB Canadian wildfire smoke impacted air quality across the northern Mid-Atlantic (MA) of the United States during June 9-12, 2015. A multiday exceedance of the new 2015 70-ppb National Ambient Air Quality Standard (NAAQS) for ozone (O-3) followed, resulting in Maryland being incompliant with the Environmental Protection Agency's (EPA) revised 2015 O-3 NAAQS. Surface in situ, balloon-borne, and remote sensing observations monitored the impact of the wildfire smoke at Maryland air quality monitoring sites. At peak smoke concentrations in Maryland, wildfire-attributable volatile organic compounds (VOCs) more than doubled, while non-NOx oxides of nitrogen (NOz) tripled, suggesting long range transport of NOx within the smoke plume. Peak daily average PM2.5 was 32.5 mu g m(-3) with large fractions coming from black carbon (BC) and organic carbon (OC), with a synonymous increase in carbon monoxide (CO) concentrations. Measurements indicate that smoke tracers at the surface were spatially and temporally correlated with maximum 8-hr O-3 concentrations in the MA, all which peaked on June 11. Despite initial smoke arrival late on June 9, 2015, O-3 production was inhibited due to ultraviolet (UV) light attenuation, lower temperatures, and nonoptimal surface layer composition. Comparison of Community Multiscale Air Quality (CMAQ) model surface O-3 forecasts to observations suggests 14 ppb additional O-3 due to smoke influences in northern Maryland. Despite polluted conditions, observations of a nocturnal low-level jet (NLLJ) and Chesapeake Bay Breeze (BB) were associated with decreases in O-3 in this case. While infrequent in the MA, wildfire smoke may be an increasing fractional contribution to high-O-3 days, particularly in light of increased wildfire frequency in a changing climate, lower regional emissions, and tighter air quality standards.Implications: The presented event demonstrates how a single wildfire event associated with an ozone exceedance of the NAAQS can prevent the Baltimore region from complying with lower ozone standards. This relatively new problem in Maryland is due to regional reductions in NOx emissions that led to record low numbers of ozone NAAQS violations in the last 3 years. This case demonstrates the need for adequate means to quantify and justify ozone impacts from wildfires, which can only be done through the use of observationally based models. The data presented may also improve future air quality forecast models.
C1 [Dreessen, Joel] Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA.
[Sullivan, John] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Delgado, Ruben] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Dreessen, J (reprint author), Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA.
EM joel.dreessen@maryland.gov
NR 64
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U1 19
U2 19
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1096-2247
EI 2162-2906
J9 J AIR WASTE MANAGE
JI J. Air Waste Manage. Assoc.
PD SEP
PY 2016
VL 66
IS 9
SI SI
BP 842
EP 862
DI 10.1080/10962247.2016.1161674
PG 21
WC Engineering, Environmental; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA DV5IE
UT WOS:000382959700003
PM 26963934
ER
PT J
AU Albers, M
Zhu, S
Ayangeakaa, AD
Janssens, RVF
Gellanki, J
Ragnarsson, I
Alcorta, M
Baugher, T
Bertone, PF
Carpenter, MP
Chiara, CJ
Chowdhury, P
David, HM
Deacon, AN
DiGiovine, B
Gade, A
Hoffman, CR
Kondev, FG
Lauritsen, T
Lister, CJ
McCutchan, EA
Nair, C
Rogers, AM
Seweryniak, D
AF Albers, M.
Zhu, S.
Ayangeakaa, A. D.
Janssens, R. V. F.
Gellanki, J.
Ragnarsson, I.
Alcorta, M.
Baugher, T.
Bertone, P. F.
Carpenter, M. P.
Chiara, C. J.
Chowdhury, P.
David, H. M.
Deacon, A. N.
DiGiovine, B.
Gade, A.
Hoffman, C. R.
Kondev, F. G.
Lauritsen, T.
Lister, C. J.
McCutchan, E. A.
Nair, C.
Rogers, A. M.
Seweryniak, D.
TI Single-particle and collective excitations in Ni-62
SO PHYSICAL REVIEW C
LA English
DT Article
ID ROTATIONAL BANDS; TERMINATION; ISOTOPES; NUCLEUS; DECAY
AB Background: Level sequences of rotational character have been observed in several nuclei in the A = 60 mass region. The importance of the deformation-driving pi f(7/2) and nu g(9/2) orbitals on the onset of nuclear deformation is stressed.
Purpose: A measurement was performed in order to identify collective rotational structures in the relatively neutron-rich Ni-62 isotope.
Method: The Mg-26(Ca-48,2 alpha 4n gamma)Ni-62 complex reaction at beam energies between 275 and 320 MeV was utilized. Reaction products were identified in mass (A) and charge (Z) with the fragment mass analyzer (FMA) and gamma rays were detected with the Gammasphere array.
Results: Two collective bands, built upon states of single-particle character, were identified and sizable deformation was assigned to both sequences based on the measured transitional quadrupole moments, herewith quantifying the deformation at high spin.
Conclusions: Based on cranked Nilsson-Strutinsky calculations and comparisons with deformed bands in the A = 60 mass region, the two rotational bands are understood as being associated with configurations involving multiple f(7/2) protons and g(9/2) neutrons, driving the nucleus to sizable prolate deformation.
C1 [Albers, M.; Zhu, S.; Ayangeakaa, A. D.; Janssens, R. V. F.; Alcorta, M.; Bertone, P. F.; Carpenter, M. P.; Chiara, C. J.; David, H. M.; DiGiovine, B.; Hoffman, C. R.; Lauritsen, T.; Lister, C. J.; McCutchan, E. A.; Nair, C.; Rogers, A. M.; Seweryniak, D.] Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA.
[Gellanki, J.] Univ Groningen, KVI CART, NL-9747 AA Groningen, Netherlands.
[Ragnarsson, I.] Lund Univ, LTH, Div Math Phys, S-22100 Lund, Sweden.
[Baugher, T.; Gade, A.] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA.
[Baugher, T.; Gade, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Chiara, C. J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
[Chowdhury, P.; Lister, C. J.; Rogers, A. M.] Univ Massachusetts Lowell, Dept Phys, Lowell, MA 01854 USA.
[Deacon, A. N.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Kondev, F. G.] Argonne Natl Lab, Nucl Engn Div, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Alcorta, M.] TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada.
[Bertone, P. F.] Marshall Space Flight Ctr, Bldg 4600 Rideout Rd, Huntsville, AL 35812 USA.
[Chiara, C. J.] US Army Res Lab, Adelphi, MD 20783 USA.
[David, H. M.] GSI Helmholtzzentrum Schwerionenforsch GmbH, D-64291 Darmstadt, Germany.
[McCutchan, E. A.] Brookhaven Natl Lab, Natl Nucl Data Ctr, Upton, NY 11973 USA.
RP Albers, M (reprint author), Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA.
RI Gade, Alexandra/A-6850-2008
OI Gade, Alexandra/0000-0001-8825-0976
FU US Department of Energy, Office of Science, Office of Nuclear Physics
[DE-AC02-06CH11357, DE-FG02-94ER40834, DE-FG02-94ER40848,
DE-FG02-08ER41556]; National Science Foundation [PHY-1102511]; Swedish
Research Council; United Kingdom Science and Technology Facilities
Council (STFC)
FX The authors thank J. P. Greene (ANL) for target preparation and the
ATLAS operations staff for the efficient running of the accelerator
during the experiment. This work was supported in part by the US
Department of Energy, Office of Science, Office of Nuclear Physics,
under Contract No. DE-AC02-06CH11357 and Grant Nos. DE-FG02-94ER40834,
DE-FG02-94ER40848, and DE-FG02-08ER41556, by the National Science
Foundation under Contract No. PHY-1102511, by the Swedish Research
Council, and by the United Kingdom Science and Technology Facilities
Council (STFC). This research used resources of ANL's ATLAS facility,
which is a DOE Office of Science User Facility.
NR 53
TC 0
Z9 0
U1 2
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9985
EI 2469-9993
J9 PHYS REV C
JI Phys. Rev. C
PD SEP 1
PY 2016
VL 94
IS 3
AR 034301
DI 10.1103/PhysRevC.94.034301
PG 10
WC Physics, Nuclear
SC Physics
GA DV6KZ
UT WOS:000383045700001
ER
PT J
AU Sherwood, B
AF Sherwood, Brent
TI Strategic map for exploring the ocean-world Enceladus
SO ACTA ASTRONAUTICA
LA English
DT Article
ID PLUME; FUTURE; LIFE
AB Among the many "ocean worlds" of our solar system, Enceladus appears unique in its combination of astrobiologically relevant and exploration-worthy attributes: extensive liquid-water ocean with active hydrothermal activity, containing salts and organics expressed predictably into space. The Enceladus south polar plume allows direct access to telltale molecules, ions, isotopes, and potential cytofragments in space. Plume mass spectroscopy and sample return, in situ investigation of surface fallback deposits, direct vent exploration, and eventually oceanographic exploration can all be envisioned. However, building consensus to fund such ambitious exploration hinges on acquiring key new data. A roadmap is essential. It could start with cost-capped onramps such as flythrough analysis of the plume, following up on Cassini measurements with modern instruments; and sample return of plume material for analysis on Earth. A methodical mission sequence in which each step depends on emergent results from prior missions would push in situ oceanographic exploration into the second half of this century. Even for this scenario, prioritization by the next planetary Decadal Survey would be pivotal. (C) 2016 IAA Published by Elsevier Ltd. All rights reserved.
C1 [Sherwood, Brent] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Sherwood, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM brent.sherwood@jpl.nasa.gov
FU NASA
FX The author is grateful to several colleagues who shared insights that
were key to formulating the strategic analysis presented here: Linda
Spilker, Christophe Sotin, Jonathan Lunine, Kevin Hand, Hunter Waite,
Hajime Yano, Peter Tsou, and Carolyn Porco.
NR 21
TC 1
Z9 1
U1 9
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 52
EP 58
DI 10.1016/j.actaastro.2016.04.013
PG 7
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200008
ER
PT J
AU Nag, S
Gatebe, CK
Miller, DW
de Weck, OL
AF Nag, Sreeja
Gatebe, Charles K.
Miller, David W.
de Weck, Olivier L.
TI Effect of satellite formations and imaging modes on global albedo
estimation
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Small satellite; Formation flight; Cubesat; BRDF; Multi-angular; Remote
sensing; Constellation
ID AIRBORNE SPECTRAL MEASUREMENTS; MISSION; SURFACE; SPACE; CONSTELLATION;
ATMOSPHERE; OCEAN
AB We confirm the applicability of using small satellite formation flight for multi-angular earth observation to retrieve global, narrow band, narrow field-of-view albedo. The value of formation flight is assessed using a coupled systems engineering and science evaluation model, driven by Model Based Systems Engineering and Observing System Simulation Experiments. Albedo errors are calculated against bi-directional reflectance data obtained from NASA airborne campaigns made by the Cloud Absorption Radiometer for the seven major surface types, binned using MODIS' land cover map water, forest, cropland, grassland, snow, desert and cities. A full tradespace of architectures with three to eight satellites, maintainable orbits and imaging modes (collective payload pointing strategies) are assessed. For an arbitrary 4-sat formation, changing the reference, nadir-pointing satellite dynamically reduces the average albedo error to 0.003, from 0.006 found in the static reference case. Tracking pre-selected waypoints with all the satellites reduces the average error further to 0.001, allows better polar imaging and continued operations even with a broken formation. An albedo error of 0.001 translates to 136 W/m(2) or 0.4% in Earth's outgoing radiation error. Estimation errors are found to be independent of the satellites' altitude and inclination, if the nadir-looking is changed dynamically. The formation satellites are restricted to differ in only right ascension of planes and mean anomalies within slotted bounds. Three satellites in some specific formations show average albedo errors of less than 2% with respect to airborne, ground data and seven satellites in any slotted formation outperform the monolithic error of 3.6%. In fact, the maximum possible albedo error, purely based on angular sampling, of 12% for monoliths is outperformed by a five-satellite formation in any slotted arrangement and an eight satellite formation can bring that error down four fold to 3%. More than 70% ground spot overlap between the satellites is possible with 0.5 of pointing accuracy, 2 Km of GPS accuracy and commands uplinked once a day. The formations can be maintained at less than 1 m/s of monthly Delta V per satellite. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Nag, Sreeja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nag, Sreeja] Bay Area Environm Res Inst, Petaluma, CA USA.
[Gatebe, Charles K.] Univ Space Res Org, NASA, Goddard Space Flight Ctr, Columbia, MD USA.
[Miller, David W.] MIT, NASA Headquarters, Cambridge, MA 02139 USA.
[de Weck, Olivier L.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Nag, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Nag, S (reprint author), Bay Area Environm Res Inst, Petaluma, CA USA.
EM sreejanag@alum.mit.edu; Charles.K.Gatebe@nasa.gov; millerd@mit.edu;
deweck@mit.edu
FU Schlumberger Faculty for the Future Fellowship (FFTF); NASA Earth and
Space Science Fellowship (NESSF)
FX The authors acknowledge the following people, without whose help this
paper in its present quality would not have been possible: Rajesh
Poudyal (GSFC) for extracting and post processing the BRDF data for the
CAR instrument, Warren Wiscombe (GSFC) for his contribution and
consistent drive toward Leonardo-BRDF which first proposed the concept
of formation flight for BRDF, Jacqueline LeMoigne (GSFC), Ralph Kahn
(GSFC), Kerri Cahoy (MIT), Daniel Selva (Cornell), Alexei Lyapustin
(GSFC) for their invaluable ideas toward making this study better and
three anonymous reviewers for their comments to improve its readability.
The primary author was funded by the Schlumberger Faculty for the Future
Fellowship (FFTF) and the NASA Earth and Space Science Fellowship
(NESSF).
NR 59
TC 1
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U1 8
U2 8
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 77
EP 97
DI 10.1016/j.actaastro.2016.04.004
PG 21
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200011
ER
PT J
AU Yang, FY
Nelson, B
Aziz, J
Carlino, R
Perez, AD
Faber, N
Foster, C
Frost, C
Henze, C
Karacalioglu, AG
Levit, C
Marshall, W
Mason, J
O'Toole, C
Swenson, J
Worden, SP
Stupl, J
AF Yang, Fan Yang
Nelson, Bron
Aziz, Jonathan
Carlino, Roberto
Perez, Andres Dono
Faber, Nicolas
Foster, Cyrus
Frost, Chad
Henze, Chris
Karacalioglu, Arif Goktug
Levit, Creon
Marshall, William
Mason, James
O'Toole, Conor
Swenson, Jason
Worden, Simon P.
Stupl, Jan
TI LightForce photon-pressure collision avoidance: Efficiency analysis in
the current debris environment and long-term simulation perspective
SO ACTA ASTRONAUTICA
LA English
DT Article
ID MODEL; NASA
AB This work provides an efficiency analysis of the LightForce space debris collision avoidance scheme in the current debris environment and describes a simulation approach to assess its impact on the long-term evolution of the space debris environment LightForce aims to provide just-in-time collision avoidance by utilizing photon pressure from ground-based industrial lasers. These ground stations impart minimal accelerations to increase the miss distance for a predicted conjunction between two objects. In the first part of this paper we will present research that investigates the short-term effect of a few systems consisting of 20 kW class lasers directed by 1.5 m diameter telescopes using adaptive optics. The results found such a network of ground stations to mitigate more than 85 percent of conjunctions and could lower the expected number of collisions in Low Earth Orbit (LEO) by an order of magnitude. While these are impressive numbers that indicate LightForce's utility in the short-term, the remaining 15 % of possible collisions contain (among others) conjunctions between two massive objects that would add large amount of debris if they collide. Still, conjunctions between massive objects and smaller objects can be mitigated. Hence, we choose to expand the capabilities of the simulation software to investigate the overall effect of a network of LightForce stations on the long-term debris evolution. In the second part of this paper, we will present the planned simulation approach for that effort. For the efficiency analysis of collision avoidance in the current debris environment, we utilize a simulation approach that uses the entire Two Line Element (TLE) catalog in LEO for a given day as initial input These objects are propagated for one year and an all-on-all conjunction analysis is performed. For conjunctions that fall below a range threshold, we calculate the probability of collision and record those values. To assess efficiency, we compare a baseline (without collision avoidance) conjunction analysis with an analysis where LightForce is active. Using that approach, we take into account that collision avoidance maneuvers could have effects on third objects. Performing all-on-all conjunction analyses for extended period of time requires significant computer resources; hence we implemented this simulation utilizing a highly parallel approach on the NASA Pleiades supercomputer. (C) 2016 Published by Elsevier Ltd. on behalf of IAA.
C1 [Yang, Fan Yang; Perez, Andres Dono] NASA, Ames Res Ctr, MEI, Washington, DC USA.
[Nelson, Bron] NASA, Ames Res Ctr, Comp Sci Corp, Washington, DC USA.
[Aziz, Jonathan] Univ Colorado, Boulder, CO 80309 USA.
[Carlino, Roberto] NASA, Ames Res Ctr, STC, Washington, DC USA.
[Faber, Nicolas; Stupl, Jan] NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA.
[Foster, Cyrus; Levit, Creon; Marshall, William; Mason, James] Planet Labs, San Francisco, CA USA.
[Frost, Chad; Henze, Chris] NASA, Ames Res Ctr, Washington, DC USA.
[O'Toole, Conor] Univ Coll Dublin, NASA, Ames Res Ctr, Dublin, Ireland.
[Swenson, Jason] NASA, Ames Res Ctr, LMCO Space OPNS, Washington, DC USA.
[Worden, Simon P.] Breakthrough Prize Fdn, Stanford, CA USA.
RP Stupl, J (reprint author), NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA.
EM jan.stupl@nasa.gov
FU center management at NASA Ames Research Center
FX We would like to thank our colleagues and the center management at NASA
Ames Research Center for continuing support. We also would like to thank
the NAIF SPICE team at JPL, especially Nat Bachman for providing a long
term version of their Earth orientation file. Special thanks go to Wang
Ting (Princeton) for sharing his area-to-mass ratio database and for
providing insight in a past implementation of the EVOLVE breakup model.
For useful discussions we would like to thank Gene Stansbery, Paula
Krisko, Carsten Wiedemann, Jonas Radtke and Holger Krag. We thank Andrew
Shacker for providing useful input for future versions of the software.
We thank Jonas Jonsson for useful discussions and his help editing this
paper.
NR 32
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U1 2
U2 2
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 411
EP 423
DI 10.1016/j.actaastro.2016.04.032
PG 13
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200042
ER
PT J
AU Guzzetti, D
Bosanac, N
Haapala, A
Howell, KC
Folta, DC
AF Guzzetti, Davide
Bosanac, Natasha
Haapala, Amanda
Howell, Kathleen C.
Folta, David C.
TI Rapid trajectory design in the Earth Moon ephemeris system via an
interactive catalog of periodic and quasi-periodic orbits
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT IAF 66th International Astronautical Congress (IAC)
CY OCT, 2015
CL Jerusalem, ISRAEL
SP IAF
DE Multi-body systems; Three-body problem; Libration points; Quasi-periodic
solutions; Periodic solutions
ID LIBRATION POINTS
AB Upcoming missions and prospective design concepts in the Earth-Moon system extensively leverage multi-body dynamics that may facilitate access to strategic locations or reduce propellant usage. To incorporate these dynamical structures into the mission design process, Purdue University and the NASA Goddard Flight Space Center have initiated the construction of a trajectory design framework to rapidly access and compare solutions from the circular restricted three-body problem. This framework, based upon a 'dynamic' catalog of periodic and quasi-periodic orbits within the Earth-Moon system, can guide an end-to-end trajectory design in an ephemeris model. In particular, the inclusion of quasi-periodic orbits further expands the design space, potentially enabling the detection of additional orbit options. To demonstrate the concept of a 'dynamic' catalog, a prototype graphical interface is developed. Strategies to characterize and represent periodic and quasi-periodic information for interactive trajectory comparison and selection are discussed. Two sample applications for formation flying near the Earth-Moon 1,2 point and lunar space infrastructures are explored to demonstrate the efficacy of a 'dynamic' catalog for rapid trajectory design and validity in higher-fidelity models. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Guzzetti, Davide; Bosanac, Natasha; Haapala, Amanda; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Haapala, Amanda] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
RP Guzzetti, D (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
EM dguzzett@purdue.edu; nbosanac@purdue.edu; amanda.haapala@jhuapl.edu;
howell@purdue.edu; david.c.folta@nasa.gov
NR 31
TC 0
Z9 0
U1 2
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 439
EP 455
DI 10.1016/j.actaastro.2016.06.029
PG 17
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200044
ER
PT J
AU Rai, A
Robinson, JA
Tate-Brown, J
Buckley, N
Zell, M
Tasaki, K
Karabadzhak, G
Sorokin, IV
Pignataro, S
AF Rai, Amelia
Robinson, Julie A.
Tate-Brown, Judy
Buckley, Nicole
Zell, Martin
Tasaki, Kazuyuki
Karabadzhak, Georgy
Sorokin, Igor V.
Pignataro, Salvatore
TI Expanded benefits for humanity from the International Space Station
SO ACTA ASTRONAUTICA
LA English
DT Article
ID MICROGRAVITY; EXPERIENCE; RESOLUTION
AB In 2012, the International Space Station (ISS) (Fig. 1) partnership published the updated International Space Station Benefits for Humanity [1], a compilation of stories about the many benefits being realized in the areas of human health, Earth observations and disaster response, and global education. This compilation has recently been revised to include updated statistics on the impacts of the benefits, and new benefits that have developed since the first publication. Two new sections have also been added to the book, economic development of space and innovative technology. This paper will summarize the updates on behalf of the ISS Program Science Forum, made up of senior science representatives across the international partnership.
The new section on "Economic Development of Space" highlights case studies from public-private partnerships that are leading to a new economy in low earth orbit (LEO). Businesses provide both transportation to the ISS as well as some research facilities and services. These relationships promote a paradigm shift of government-funded, contractor-provided goods and services to commercially-provided goods purchased by government agencies. Other examples include commercial firms spending research and development dollars to conduct investigations on ISS and commercial service providers selling services directly to ISS users. This section provides examples of ISS as a test bed for new business relationships, and illustrates successful partnerships.
The second new section, "Innovative Technology," merges technology demonstration and physical science findings that promise to return Earth benefits through continued research. Robotic refueling concepts for life extensions of costly satellites in geo-synchronous orbit have applications to robotics in industry on Earth. Flame behavior experiments reveal insight into how fuel burns in microgravity leading to the possibility of improving engine efficiency on Earth. Nanostructures and smart fluids are examples of materials improvements that are being developed using data from ISS.
The publication also expands the benefits of research results in human health, environmental change and disaster response and in education activities developed to capture student imaginations in support of science, technology, engineering and mathematics, or STEM, education internationally. Applications to human health of the knowledge gained on ISS continue to grow and improve healthcare technologies and our understanding of human physiology. Distinct benefits return to Earth from the only orbiting multi-disciplinary laboratory of its kind. The ISS is a stepping stone for future space exploration by providing findings that develop LEO and improve life on our planet. (C) 2016 Published by Elsevier Ltd. on behalf of IAA.
C1 [Rai, Amelia; Robinson, Julie A.] NASA, Johnson Space Ctr, Washington, DC 20546 USA.
[Tate-Brown, Judy] Barrios Technol, Houston, TX 77058 USA.
[Buckley, Nicole] Canadian Space Agcy, Longueuil, PQ, Canada.
[Zell, Martin] European Space Agcy, Noordwijk, Netherlands.
[Tasaki, Kazuyuki] Japan Aerosp Explorat Agcy JAXA, Chofu, Tokyo, Japan.
[Karabadzhak, Georgy] TSNIIMASH, Kaliningrad, Russia.
[Sorokin, Igor V.] SP Korolev Rocket & Space Corp Energia, Korolev, Russia.
[Pignataro, Salvatore] Italian Space Agcy ASI, Rome, Italy.
RP Rai, A (reprint author), NASA, Johnson Space Ctr, Washington, DC 20546 USA.
EM amelia.e.rai@nasa.gov; julie.a.robinson@nasa.gov;
judy.tate-brown-1@nasa.gov; nicole.buckley@asc-csa.gc.ca;
martin.zell@esa.int; tasaki.kazuyuki@jaxa.jp; gfk@tsniimash.ru;
igor.v.sorokin@rsce.ru; salvatore.pignataro@asi.it
OI Robinson, Julie/0000-0002-6832-6459
NR 43
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U2 12
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 463
EP 474
DI 10.1016/j.actaastro.2016.06.030
PG 12
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200046
ER
PT J
AU Arvani, B
Pierce, RB
Lyapustin, AI
Wang, YJ
Ghermandi, G
Teggi, S
AF Arvani, Barbara
Pierce, R. Bradley
Lyapustin, Alexei I.
Wang, Yujie
Ghermandi, Grazia
Teggi, Sergio
TI Seasonal monitoring and estimation of regional aerosol distribution over
Po valley, northern Italy, using a high-resolution MAIAC product
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol optical depth (AOD); High resolution aerosol retrieval;
Seasonality AOD-PM10 correlation; MAIAC; MODIS; PM10; Planetary boundary
layer (PBL)
ID AIR-QUALITY ASSESSMENT; MODIS 3 KM; PARTICULATE MATTER PREDICTIONS;
SOUTHEASTERN UNITED-STATES; OPTICAL DEPTH RETRIEVALS; PM2.5
CONCENTRATIONS; EPIDEMIOLOGIC EVIDENCE; AOD RETRIEVALS; BOUNDARY-LAYER;
SATELLITE DATA
AB In this work, the new 1 km-resolved Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm is employed to characterize seasonal PM10 - AOD correlations over northern Italy. The accuracy of the new dataset is assessed compared to the widely used Moderate Resolution Imaging Spectroradiometer (MODIS) Collection 5.1 Aerosol Optical Depth (AOD) data, retrieved at 0.55 gm with spatial resolution of 10 km (MYD04_12). We focused on evaluating the ability of these two products to characterize both temporal and spatial distributions of aerosols within urban and suburban areas. Ground PM10 measurements were obtained from 73 of the Italian Regional Agency for Environmental Protection (ARPA) monitoring stations, spread across northern Italy, during a three-year period from 2010 to 2012. The Po Valley area (northern Italy) was chosen as the study domain because of its severe urban. air pollution, resulting from it having the highest population and industrial manufacturing density in the country, being located in a valley where two surrounding mountain chains favor the stagnation of pollutants. We found that the global correlations between the bin-averaged PM-to and AOD are R-2 = 0.83 and R-2 = 0.44 for MYD04_L2 and for MAIAC, respectively, suggesting a greater sensitivity of the high resolution product to small-scale deviations. However, the introduction of Relative Humidity (RH) and Planetary Boundary Layer (PBL) depth corrections allowed for a significant improvement to the bin averaged PM AOD correlation, which led to a similar performance: R-2 = 0.96 for MODIS and R-2 = 0.95 for MAIAC. Furthermore, the introduction of the PBL information in the corrected AOD values was found to be crucial in order to capture the clear seasonal cycle shown by measured PM10 values. The study allowed us to define four seasonal linear correlations that estimate PM10 concentrations satisfactorily from the remotely sensed MAIAC AOD retrieval. Overall, the results show that the high resolution provided by MAIAC retrieval data is much more relevant than the 10 km MODIS data to characterize PM10 in this region of Italy which has a pretty limited geographical domain but a broad variety of land usages and consequent particulate concentrations. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Arvani, Barbara; Ghermandi, Grazia; Teggi, Sergio] Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy.
[Pierce, R. Bradley] NOAA NESDIS Adv Satellite Prod Branch, 1225 W Dayton St, Madison, WI 53706 USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
[Wang, Yujie] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21228 USA.
RP Arvani, B (reprint author), Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy.
EM barbara.arvani@unimore.it
RI Pierce, Robert Bradley/F-5609-2010;
OI Pierce, Robert Bradley/0000-0002-2767-1643; Teggi,
Sergio/0000-0001-7375-0599
FU Italian Ministero dell'Istruzione, dell' Universita e della Ricerca
(Project PRIN) [2010WLNFY2]
FX This research has been funded by the Italian Ministero dell'Istruzione,
dell' Universita e della Ricerca (Project PRIN2010-11, 2010WLNFY2). The
authors are thankful for Italian agencies ARPA Emilia-Romagna, ARPA
Lombardia, ARPA Piemonte, and ARPA Veneto for providing ground
PM10 data. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 61
TC 1
Z9 1
U1 10
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 141
BP 106
EP 121
DI 10.1016/j.atmosenv.2016.06.037
PG 16
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900010
ER
PT J
AU Dolan, W
Payne, VH
Kualwik, SS
Bowman, KW
AF Dolan, Wayana
Payne, Vivienne H.
Kualwik, Susan S.
Bowman, Kevin W.
TI Satellite observations of ethylene (C2H4) from the Aura Tropospheric
Emission Spectrometer: A scoping study
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ethylene; Tropospheric Emission Spectrometer; Satellite remote sensing
ID ARCTAS; OZONE; AIRCRAFT; ISOPRENE; ATLANTIC; MISSION; IMPACT; FIRES;
TES; PAN
AB We present a study focusing on detection and initial quantitative estimates of ethylene (C2H4) in observations from the Tropospheric Emission Spectrometer (TES), a Fourier transform spectrometer aboard the Aura satellite that measures thermal infrared radiances with high spectral resolution (0.1 cm(-1)). We analyze observations taken in support of the 2008 Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) mission and demonstrate the feasibility of future development of C2H4 into a TES standard product. In the Northern Hemisphere, C2H4 is commonly associated with boreal fire plumes, motor vehicle exhaust and petrochemical emissions. It has a short lifetime (similar to 14-32 h) in the troposphere due to its reaction with OH and O-3. Chemical destruction of C2H4 in the atmosphere leads to the production of ozone and other species such as carbon monoxide (CO) and formaldehyde. Results indicate a correlation between C2H4 and CO in boreal fire plumes. Quantitative C2H4 estimates are sensitive to assumptions about the plume height and width. We find that C2H4 greater than 2-3 ppbv can be detected in a single TES observation (for a fire plume at 3 km altitude and 1.5 km width). Spatial averaging will be needed for surface-peaking profiles where TES sensitivity is lower. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Dolan, Wayana; Payne, Vivienne H.; Bowman, Kevin W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dolan, Wayana] Occidental Coll, Eagle Rock, CA USA.
[Kualwik, Susan S.] Bay Area Environm Res Inst Moffett Field, Moffett Field, CA USA.
RP Payne, VH (reprint author), Jet Prop Lab, M-S 233-200,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vivienne.h.payne@jpl.nasa.gov
NR 31
TC 0
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U1 3
U2 3
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 141
BP 388
EP 393
DI 10.1016/j.atmosenv.2016.07.009
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900035
ER
PT J
AU Titos, G
Cazorla, A
Zieger, P
Andrews, E
Lyamani, H
Granados-Munoz, MJ
Olmo, FJ
Alados-Arboledas, L
AF Titos, G.
Cazorla, A.
Zieger, P.
Andrews, E.
Lyamani, H.
Granados-Munoz, M. J.
Olmo, F. J.
Alados-Arboledas, L.
TI Effect of hygroscopic growth on the aerosol light-scattering
coefficient: A review of measurements, techniques and error sources
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Review
DE Scattering enhancement; Water uptake; Hygroscopicity; Aerosol light
scattering
ID ALPINE SITE JUNGFRAUJOCH; OPTICAL-PROPERTIES; RELATIVE-HUMIDITY;
RADIATIVE PROPERTIES; IN-SITU; HUMIDIFICATION FACTORS; AMMONIUM-SULFATE;
WATER-UPTAKE; ACE-ASIA; ATMOSPHERIC AEROSOLS
AB Knowledge of the scattering enhancement factor,.f(RH), is important for an accurate description of direct aerosol radiative forcing. This factor is defined as the ratio between the scattering coefficient at enhanced relative humidity, RH, to a reference (dry) scattering coefficient. Here, we review the different experimental designs used to measure the scattering coefficient at dry and humidified conditions as well as the procedures followed to analyze the measurements. Several empirical parameterizations for the relationship between f(RH) and RH have been proposed in the literature. These parameterizations have been reviewed and tested using experimental data representative of different hygroscopic growth behavior and a new parameterization is presented. The potential sources of error in f(RH) are discussed. A Monte Carlo method is used to investigate the overall measurement uncertainty, which is found to be around 20-40% for moderately hygroscopic aerosols. The main factors contributing to this uncertainty are the uncertainty in RH measurement, the dry reference state and the nephelometer uncertainty. A literature survey of nephelometry-based f(RH) measurements is presented as a function of aerosol type. In general, the highest f(RH) values were measured in clean marine environments, with pollution having a major influence on f(RH). Dust aerosol tended to have the lowest reported hygroscopicity of any of the aerosol types studied. Major open questions and suggestions for future research priorities are outlined. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain.
[Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Dept Appl Phys, Granada 18071, Spain.
[Zieger, P.] Stockholm Univ, Bolin Ctr Climate Res, Dept Environm Sci & Analyt Chem, S-11418 Stockholm, Sweden.
[Andrews, E.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA.
[Titos, G.] IDAEA CSIC, Inst Environm Assessment & Water Res, Barcelona, Spain.
[Granados-Munoz, M. J.] CALTECH, NASA, Jet Prop Lab, Table Mt Facil, Wrightwood, CA USA.
RP Titos, G (reprint author), Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain.
EM gtitos@ugr.es
RI Granados-Munoz, Maria Jose/G-9308-2014;
OI Granados-Munoz, Maria Jose/0000-0001-8718-5914; Titos Vela,
Gloria/0000-0003-3630-5079
FU Andalusia Regional Government [P10-RNM-6299, P12-RNM-2409]; FEDER
[CGL2013_45410-R]; Spanish Ministry of Economy and Competitiveness;
European Union [654109, ACTRIS-2]; Programa del Plan Propio de
Investigacion "Contrato Puente" of the University of Granada
FX This work was supported by the Andalusia Regional Government through
projects P10-RNM-6299 and P12-RNM-2409; by the Spanish Ministry of
Economy and Competitiveness and FEDER through project CGL2013_45410-R;
and by European Union's Horizon 2020 research and innovation programme
under grant agreement No 654109, ACTRIS-2. G. Titos was partially funded
by Programa del Plan Propio de Investigacion "Contrato Puente" of the
University of Granada. We thank the Stockholm International
Meteorological Institute (IMI) for travel support of G. Titos.
NR 90
TC 1
Z9 1
U1 20
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 141
BP 494
EP 507
DI 10.1016/j.atmosenv.2016.07.021
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900046
ER
PT J
AU Duval, S
Santini, JM
Lemaire, D
Chaspoul, F
Russell, MJ
Grimaldi, S
Nitschke, W
Schoepp-Cothenet, B
AF Duval, Simon
Santini, Joanne M.
Lemaire, David
Chaspoul, Florence
Russell, Michael J.
Grimaldi, Stephane
Nitschke, Wolfgang
Schoepp-Cothenet, Barbara
TI The H-bond network surrounding the pyranopterins modulates redox
cooperativity in the molybdenum-bisPGD cofactor in arsenite oxidase
SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS
LA English
DT Article
DE Arsenite oxidase; Molybdenum enzyme; Optical spectroscopy; EPR
spectroscopy; Redox titrations
ID COLI NITRATE REDUCTASE; IRON-SULFUR CENTERS; PARAMAGNETIC-RESONANCE
SPECTROSCOPY; ESCHERICHIA-COLI; DIMETHYLSULFOXIDE REDUCTASE;
ALCALIGENES-FAECALIS; BINDING-SITE; SEMIQUINONE; OXIDATION; SUBUNIT
AB While the molybdenum cofactor in the majority of bisPGD enzymes goes through two consecutive 1-electron redox transitions, previous protein-film voltammetric results indicated the possibility of cooperative (n = 2) redox behavior in the bioenergetic enzyme arsenite oxidase (Aio). Combining equilibrium redox titrations, optical and EPR spectroscopies on concentrated samples obtained via heterologous expression, we unambiguously confirm this claim and quantify Aio's redox cooperativity. The stability constant, K-s of the Mo-v semi-reduced intermediate is found to be lower than 10(-3). Site-directed mutagenesis of residues in the vicinity of the Mo-cofactor demonstrates that the degree of redox cooperativity is sensitive to H-bonding interactions between the pyranopterin moieties and amino acid residues. Remarkably, in particular replacing the Gln-726 residue by Gly results in stabilization of (low-temperature) EPR-observable Mo-v with K-s = 4. As evidenced by comparison of room temperature optical and low temperature EPR titrations, the degree of stabilization is temperature dependent. This highlights the importance of room-temperature redox characterizations for correctly interpreting catalytic properties in this group of enzymes.
Geochemical and phylogenetic data strongly indicate that molybdenum played an essential biocatalytic roles in early life. Molybdenum's redox versatility and in particular the ability to show cooperative (n = 2) redox behavior provide a rationale for its paramount catalytic importance throughout the evolutionary history of life. Implications of the H-bonding network modulating Molybdenum's redox properties on details of a putative inorganic metabolism at life's origin are discussed. (C) 2016 Published by Elsevier B.V.
C1 [Duval, Simon; Grimaldi, Stephane; Nitschke, Wolfgang; Schoepp-Cothenet, Barbara] Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France.
[Santini, Joanne M.] UCL, Inst Struct & Mol Biol, London WC1E 6BT, England.
[Lemaire, David] CEA Cadarache, Inst Biol Environm & Biotechnol, F-13108 St Paul Les Durance, France.
[Chaspoul, Florence] Aix Marseille Univ, IMBE, IRD CNRS UAPV, Fac Pharm, F-13005 Marseille, France.
[Russell, Michael J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Schoepp-Cothenet, B (reprint author), Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France.
EM schoepp@imm.cnrs.fr
OI Grimaldi, Stephane/0000-0002-9559-6112
FU CNRS; CEA; Aix-Marseille University; ANR [11-BSV5-005-01]; NASA
Astrobiology Institute (Icy Worlds); French EPR network (RENARD)
[IR3443]
FX We thank Axel Magalon and Frederic Biaso for helpful discussions and
Pierre Ceccaldi for Nar preparation. Our work is funded by the CNRS,
CEA, Aix-Marseille University, ANR (Project MC2, 11-BSV5-005-01). MJR's
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration and with support by the NASA Astrobiology
Institute (Icy Worlds). The authors are grateful to the EPR facilities
available at the Aix-Marseille University EPR center, and to financial
support from the French EPR network (RENARD, IR3443).
NR 54
TC 0
Z9 0
U1 10
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0005-2728
EI 0006-3002
J9 BBA-BIOENERGETICS
JI Biochim. Biophys. Acta-Bioenerg.
PD SEP
PY 2016
VL 1857
IS 9
BP 1353
EP 1362
DI 10.1016/j.bbabio.2016.05.003
PG 10
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA DV0EI
UT WOS:000382590400001
PM 27207587
ER
PT J
AU Gilman, E
Chaloupka, M
Swimmer, Y
Piovano, S
AF Gilman, Eric
Chaloupka, Milani
Swimmer, Yonat
Piovano, Susanna
TI A cross-taxa assessment of pelagic longline by-catch mitigation
measures: conflicts and mutual benefits to elasmobranchs
SO FISH AND FISHERIES
LA English
DT Article
DE At-vessel mortality; by-catch; circle hook; ray; shark; wire leader
ID SHARK ALOPIAS-SUPERCILIOSUS; EASTERN PACIFIC-OCEAN; TUNA THUNNUS-OBESUS;
SEA-TURTLE BYCATCH; CIRCLE HOOKS; POSTRELEASE SURVIVAL; RELATIVE
ABUNDANCE; DISCARD MORTALITY; ATLANTIC-OCEAN; NORTH-ATLANTIC
AB Elasmobranch mortality in pelagic longline fisheries poses a risk to some populations, alters the distribution of abundance between sympatric competitors, changing ecosystem structure, processes and stability. Individual and synergistic effects on elasmobranch catch and survival from pelagic longline gear factors, including methods prescribed to mitigate bycatch of other vulnerable taxa, were determined. Overall relative risk of higher circle vs. J-shaped hook shark catch rates conditioned on potentially informative moderators, from 30 studies, was estimated using an inverse-precision weighted mixed-effects meta-regression modelling approach. Sharks had a 1.20 times (95% CI: 1.03-1.39) significantly higher pooled relative risk of capture on circle hooks, with two significant moderators. The pooled relative risk estimate of ray circle hook catch from 15 studies was not significant (RR=1.22, 95% CI: 0.89-1.66) with no significant moderators. From a literature review, wire leaders had higher shark catch and haulback mortality than monofilament. Interacting effects of hook, bait and leader affect shark catch rates: hook shape and width and bait type determine hooking position and ability to sever monofilament leaders. Circle hooks increased elasmobranch catch, but reduced haulback mortality and deep hooking relative to J-shaped hooks of the same or narrower width. Using fish vs. squid for bait increased shark catch and deep hooking. Pelagic stingray (Pteroplatytrygon violacea) catch and mortality were lower on wider hooks. Using circle instead of J-shaped hooks and fish instead of squid for bait, while benefitting sea turtles, odontocetes and possibly seabirds, exacerbates elasmobranch catch and injury, therefore warranting fishery-specific assessments to determine relative risks.
C1 [Gilman, Eric] Nature Conservancy, Honolulu, HI USA.
[Gilman, Eric] Pelag Fisheries Res Serv, Honolulu, HI USA.
[Chaloupka, Milani] Univ Queensland, Ecol Modeling Serv, St Lucia, Qld 4067, Australia.
[Chaloupka, Milani] Univ Queensland, POB 6150, St Lucia, Qld 4067, Australia.
[Swimmer, Yonat] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 501 W Ocean Blvd, Long Beach, CA 90802 USA.
[Piovano, Susanna] Univ South Pacific, Laucala Campus,Private Mail Bag, Suva, Fiji.
RP Gilman, E (reprint author), 3661 Loulu St, Honolulu, HI 96822 USA.
EM EGilman@FisheriesResearchGroup.org
FU Sustainable Fisheries Fund Program of the Resources Legacy Fund; Nature
Conservancy
FX We are grateful for assistance provided by Victoria Jeffers, University
of Exeter, with compiling literature. We acknowledge the assistance
provided by Andre Afonso to correct copyediting errors in a table in
Afonso et al. (2012). We are grateful for clarifications provided by
John Watson and Daniel Foster on leader materials used in an experiment
from which findings were published in Watson et al. (2005), Epperly et
al. (2012), and Foster et al. (2012). Peer reviewer and journal editor
comments greatly improved the manuscript. The Sustainable Fisheries Fund
Program of the Resources Legacy Fund and The Nature Conservancy
contributed financial support for this study.
NR 160
TC 4
Z9 4
U1 16
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1467-2960
EI 1467-2979
J9 FISH FISH
JI Fish. Fish.
PD SEP
PY 2016
VL 17
IS 3
BP 748
EP 784
DI 10.1111/faf.12143
PG 37
WC Fisheries
SC Fisheries
GA DU8VW
UT WOS:000382494600012
ER
PT J
AU Cavosie, AJ
Timms, NE
Erickson, TM
Hagerty, JJ
Horz, F
AF Cavosie, Aaron J.
Timms, Nicholas E.
Erickson, Timmons M.
Hagerty, Justin J.
Horz, Friedrich
TI Transformations to granular zircon revealed: Twinning, reidite, and ZrO2
in shocked zircon from Meteor Crater (Arizona, USA)
SO GEOLOGY
LA English
DT Article
ID U-PB; VREDEFORT IMPACT; SOUTH-AFRICA; METAMORPHISM; MICROSTRUCTURES;
DECOMPOSITION; DEFORMATION; BADDELEYITE; MINERALS; EVENTS
AB Granular zircon in impact environments has long been recognized but remains poorly understood due to lack of experimental data to identify mechanisms involved in its genesis. Meteor Crater in Arizona (USA) contains abundant evidence of shock metamorphism, including shocked quartz, the high-pressure polymorphs coesite and stishovite, diaplectic SiO2 glass, and lechatelierite (fused SiO2). Here we report the presence of granular zircon, a new shocked-mineral discovery at Meteor Crater, that preserve critical orientation evidence of specific transformations that occurred during formation at extreme impact conditions. The zircon grains occur as aggregates of sub-micrometer neoblasts in highly shocked Coconino Sandstone (CS) comprised of lechatelierite. Electron backscatter diffraction shows that each grain consists of multiple domains, some with boundaries disoriented by 65 degrees around < 110 >, a known {112} shock-twin orientation. Other domains have {001} in alignment with {110} of neighboring domains, consistent with the former presence of the high-pressure ZrSiO4 polymorph reidite. Additionally, nearly all zircon preserve ZrO2 + SiO2, providing evidence of partial dissociation. The genesis of CS granular zircon started with detrital zircon that experienced shock twinning and reidite formation at pressures from 20 to 30 GPa, ultimately yielding a phase that retained crystallographic memory; this phase subsequently recrystallized to systematically oriented zircon neoblasts, and in some areas partially dissociated to ZrO2. The lechatelierite matrix, experimentally constrained to form at >2000 degrees C, provided the ultrahigh-temperature environment for zircon dissociation (similar to 1670 degrees C) and neoblast formation. The capacity of granular zircon to preserve a cumulative pressure-temperature record has not been recognized previously, and provides a new method for investigating histories of impact-related mineral transformations in the crust at conditions far beyond those at which most rocks melt.
C1 [Cavosie, Aaron J.; Timms, Nicholas E.; Erickson, Timmons M.] Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia.
[Cavosie, Aaron J.] Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA.
[Cavosie, Aaron J.] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA.
[Hagerty, Justin J.] USGS, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Horz, Friedrich] NASA, Johnson Space Ctr, Dept Sci, Jets,HX5,ARES, Houston, TX 77058 USA.
RP Cavosie, AJ (reprint author), Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia.; Cavosie, AJ (reprint author), Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA.; Cavosie, AJ (reprint author), Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA.
OI Erickson, Timmons/0000-0003-4520-7294
FU National Science Foundation [EAR-1145118]; USGS Meteor Crater Sample
Collection; NASA Astrobiology program; Curtin Research Fellowship;
Microscopy and Microanalysis Facility at Curtin University
FX B. Hess prepared the sample. Editor J.B. Murphy, S. Kamo, W. Cordua, and
an anonymous reviewer provided helpful comments. Support was provided by
the National Science Foundation (grant EAR-1145118), the USGS Meteor
Crater Sample Collection, the NASA Astrobiology program, a Curtin
Research Fellowship, and the Microscopy and Microanalysis Facility at
Curtin University.
NR 32
TC 3
Z9 3
U1 5
U2 5
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
EI 1943-2682
J9 GEOLOGY
JI Geology
PD SEP
PY 2016
VL 44
IS 9
BP 703
EP 706
DI 10.1130/G38043.1
PG 4
WC Geology
SC Geology
GA DU9FV
UT WOS:000382522700004
ER
PT J
AU Wang, YS
Hyyppa, J
Liang, XL
Kaartinen, H
Yu, XW
Lindberg, E
Holmgren, J
Qin, YC
Mallet, C
Ferraz, A
Torabzadeh, H
Morsdorf, F
Zhu, LL
Liu, JB
Alho, P
AF Wang, Yunsheng
Hyyppa, Juha
Liang, Xinlian
Kaartinen, Harri
Yu, Xiaowei
Lindberg, Eva
Holmgren, Johan
Qin, Yuchu
Mallet, Clement
Ferraz, Antonio
Torabzadeh, Hossein
Morsdorf, Felix
Zhu, Lingli
Liu, Jingbin
Alho, Petteri
TI International Benchmarking of the Individual Tree Detection Methods for
Modeling 3-D Canopy Structure for Silviculture and Forest Ecology Using
Airborne Laser Scanning
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne laser scanning (ALS); benchmark; canopy structure; crown class;
individual tree detection (ITD); LiDAR; point cloud; subordinate tree
ID LIDAR POINT CLOUD; SEGMENTATION; CROWNS; STANDS
AB Canopy structure plays an essential role in biophysical activities in forest environments. However, quantitative descriptions of a 3-D canopy structure are extremely difficult because of the complexity and heterogeneity of forest systems. Airborne laser scanning (ALS) provides an opportunity to automatically measure a 3-D canopy structure in large areas. Compared with other point cloud technologies such as the image-based Structure from Motion, the power of ALS lies in its ability to penetrate canopies and depict subordinate trees. However, such capabilities have been poorly explored so far. In this paper, the potential of ALS-based approaches in depicting a 3-D canopy structure is explored in detail through an international benchmarking of five recently developed ALS-based individual tree detection (ITD) methods. For the first time, the results of the ITD methods are evaluated for each of four crown classes, i.e., dominant, codominant, intermediate, and suppressed trees, which provides insight toward understanding the current status of depicting a 3-D canopy structure using ITD methods, particularly with respect to their performances, potential, and challenges. This benchmarking study revealed that the canopy structure plays a considerable role in the detection accuracy of ITD methods, and its influence is even greater than that of the tree species as well as the species composition in a stand. The study also reveals the importance of utilizing the point cloud data for the detection of intermediate and suppressed trees. Different from what has been reported in previous studies, point density was found to be a highly influential factor in the performance of the methods that use point cloud data. Greater efforts should be invested in the point-based or hybrid ITD approaches to model the 3-D canopy structure and to further explore the potential of high-density and multiwavelengths ALS data.
C1 [Wang, Yunsheng; Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin; Alho, Petteri] FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland.
[Wang, Yunsheng; Alho, Petteri] Univ Turku, Geog Sect, Dept Geog & Geol, Turku 20014, Finland.
[Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin] Acad Finland, Ctr Excellence Laser Scanning Res, Helsinki 00531, Finland.
[Lindberg, Eva; Holmgren, Johan] Swedish Univ Agr Sci, Dept Forest Resource Management, S-90183 Umea, Sweden.
[Qin, Yuchu; Mallet, Clement; Ferraz, Antonio] Univ Paris Est, IGN, MATIS, F-94160 Paris, France.
[Ferraz, Antonio] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Torabzadeh, Hossein; Morsdorf, Felix] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland.
[Torabzadeh, Hossein] Bu Ali Sina Univ, Dept Civil Engn, Hamadan 651784161, Iran.
RP Liang, XL (reprint author), FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland.
EM xinlian.liang@fgi.fi
RI Alho, Petteri/B-7989-2013; Ferraz, Antonio/D-9662-2017;
OI Alho, Petteri/0000-0001-5252-9609; Ferraz, Antonio/0000-0002-5328-5471;
Mallet, Clement/0000-0002-2675-165X
FU Finnish Academy through project "Centre of Excellence in Laser Scanning
Research (CoE-LaSR)" [272195]; Finnish Academy through project
"Interaction of Lidar/Radar Beams with Forests Using Mini-UAV and Mobile
Forest Tomography" [259348]; Finnish Academy through project "Competence
Based Growth Through Integrated Disruptive Technologies of 3-D
Digitalization, Robotics, Geospatial Information and Image
Processing/Computing Point Cloud Ecosystem" [293389]; European Community
[606971]; French National Research Agency through the FORESEE Project
[ANR-2010-BIOE-008]; Jet Propulsion Laboratory through the NASA
Postdoctoral Program; Oak Ridge Associated Universities through a
contract with NASA
FX This work was supported in part by the Finnish Academy through projects
"Centre of Excellence in Laser Scanning Research (CoE-LaSR)" under Grant
272195, "Interaction of Lidar/Radar Beams with Forests Using Mini-UAV
and Mobile Forest Tomography" under Grant 259348, and "Competence Based
Growth Through Integrated Disruptive Technologies of 3-D Digitalization,
Robotics, Geospatial Information and Image Processing/Computing Point
Cloud Ecosystem" under Grant 293389 and in part by the European
Community's Seventh Framework Program (FP7/2007-2013) under Grant
Agreement 606971. The work of Y. Qin, C. Mallet, and A. Ferraz was
supported by the French National Research Agency through the FORESEE
Project under Grant ANR-2010-BIOE-008. The work of A. Ferraz was
supported by the Jet Propulsion Laboratory through the NASA Postdoctoral
Program, which was administrated by the Oak Ridge Associated
Universities through a contract with NASA. Y. Wang, J. Hyyppa, and X.
Liang contributed equally to this work.
NR 24
TC 1
Z9 1
U1 22
U2 22
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2016
VL 54
IS 9
BP 5011
EP 5027
DI 10.1109/TGRS.2016.2543225
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300001
ER
PT J
AU Smith, GL
Thomas, S
Priestley, KJ
Walikainen, D
AF Smith, G. Louis
Thomas, Susan
Priestley, Kory J.
Walikainen, Dale
TI Tropical Mean Fluxes: A Tool for Calibration and Validation of CERES
Radiometers
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Clouds and the earth's radiant energy system (CERES); in-flight
calibration; radiation budget; radiometry; remote sensing; validation
ID RADIANT ENERGY SYSTEM; DATA RECORD VALIDATION; ABOARD EOS TERRA; FLIGHT
MODEL 5; INSTRUMENTS ABOARD; OCEAN MEASUREMENTS; CLOUDS; PERFORMANCE;
SENSORS
AB The Clouds and the Earth's Radiant Energy System (CERES) instrument requires in-flight calibration and validation to maintain its accuracy during orbit operations over an extended period. An internal calibration system provides calibration for the three channels; however, there is no device for calibration of the shortwave response of the total channel. A three-channel comparison technique has been developed to calibrate the shortwave response of the total channel using the tropical oceans as a vicarious calibration target. The difference between day and night outgoing longwave radiances (OLR) averaged over the tropical oceans is used to validate the day OLR. This paper evaluates the efficacy of the technique. A relation is computed at night between the window channel radiance and the OLR retrieved from the total channel for each month for each instrument. The relation has a standard deviation of 0.28 W.m(-2).sr(-1). Given 120 months of data, the precision of the curved line faired through these data is better than 0.05 W.m(-2).sr(-1). A bias is found between FM-1 and FM-3 of 0.3 W.m(-2).sr(-1), which is taken to be the accuracy with which the total channels can be calibrated with the internal blackbodies. This result includes the differences of longwave spectral responses of the instruments. The tropical mean OLR is between 87.4 and 90.2 W.m(-2).sr(-1) at night, with a standard deviation of 0.44 for FM-1 and 0.47 W.m(-2).sr(-1) for FM-3. The average difference between day and night tropical mean from the four instruments is 0.6 +/- 0.09 W.m(-2).sr(-1) over their data periods.
C1 [Smith, G. Louis; Thomas, Susan; Walikainen, Dale] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Priestley, Kory J.] Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
RP Smith, GL (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM g.l.smith@nasa.gov
FU Earth Science Directorate of the National Aeronautics and Space
Administration through the Science Directorate of the Langley Research
Center (LaRC); LaRC through Space Sciences Applications, Inc
FX This work was supported by the Earth Science Directorate of the National
Aeronautics and Space Administration through the Science Directorate of
the Langley Research Center (LaRC). The work of G. L. Smith, S. Thomas
and D. Walikainen was supported by LaRC through a contract with Space
Sciences Applications, Inc.
NR 25
TC 0
Z9 0
U1 4
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2016
VL 54
IS 9
BP 5135
EP 5142
DI 10.1109/TGRS.2016.2556581
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300010
ER
PT J
AU Polivka, TN
Wang, J
Ellison, LT
Hyer, EJ
Ichoku, CM
AF Polivka, Thomas N.
Wang, Jun
Ellison, Luke T.
Hyer, Edward J.
Ichoku, Charles M.
TI Improving Nocturnal Fire Detection With the VIIRS Day-Night Band
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Day-night band (DNB); fire detection; fires; gas flares; Visible
Infrared Imaging Radiometer Suite (VIIRS); visible light at night;
wildfires
ID PIXEL-BASED CALCULATION; RADIATIVE POWER; SENSITIVITY-ANALYSIS;
SATELLITE DETECTION; INITIAL ASSESSMENT; SOUTH-AMERICA; INFRARED DATA;
GAS FLARES; SCAR-B; MODIS
AB Building on existing techniques for satellite remote sensing of fires, this paper takes advantage of the day-night band (DNB) aboard the Visible Infrared Imaging Radiometer Suite (VIIRS) to develop the Firelight Detection Algorithm (FILDA), which characterizes fire pixels based on both visible-light and infrared (IR) signatures at night. By adjusting fire pixel selection criteria to include visible-light signatures, FILDA allows for significantly improved detection of pixels with smaller and/or cooler subpixel hotspots than the operational Interface Data Processing System (IDPS) algorithm. VIIRS scenes with near-coincident Advanced Spaceborne Thermal Emission and Reflection (ASTER) overpasses are examined after applying the operational VIIRS fire product algorithm and including a modified "candidate fire pixel selection" approach from FILDA that lowers the 4-mu m brightness temperature (BT) threshold but includes a minimum DNB radiance. FILDA is shown to be effective in detecting gas flares and characterizing fire lines during large forest fires (such as the Rim Fire in California and High Park fire in Colorado). Compared with the operational VIIRS fire algorithm for the study period, FILDA shows a large increase (up to 90%) in the number of detected fire pixels that can be verified with the finer resolution ASTER data (90 m). Part (30%) of this increase is likely due to a combined use of DNB and lower 4-mu m BT thresholds for fire detection in FILDA. Although further studies are needed, quantitative use of the DNB to improve fire detection could lead to reduced response times to wildfires and better estimate of fire characteristics (smoldering and flaming) at night.
C1 [Polivka, Thomas N.; Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
[Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Ellison, Luke T.; Ichoku, Charles M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hyer, Edward J.] Naval Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA.
RP Polivka, TN (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
EM thomas.polivka@huskers.unl.edu; jwangjun@gmail.com;
luke.ellison@nasa.gov; edward.hyer@nrlmry.navy.mil;
charles.ichoku@nasa.gov
RI Hyer, Edward/E-7734-2011; Wang, Jun/A-2977-2008
OI Hyer, Edward/0000-0001-8636-2026; Wang, Jun/0000-0002-7334-0490
FU NASA
FX This work was supported in part by the NASA Suomi NPP Program and
Applied Science Program managed by John A. Haynes and Lawrence A. Friedl
and in part by the Interdisciplinary Studies (IDS) Program directed by
J. Kaye and administered through the Radiation Sciences Program managed
by Hal B. Maring. The work of T. Polivka was also supported by the NASA
Nebraska Space Grant.
NR 75
TC 0
Z9 0
U1 10
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2016
VL 54
IS 9
BP 5503
EP 5519
DI 10.1109/TGRS.2016.2566665
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300038
ER
PT J
AU Khan, A
van Driel, M
Bose, M
Giardini, D
Ceylan, S
Yan, J
Clinton, J
Euchner, F
Lognonne, P
Murdoch, N
Mimoun, D
Panning, M
Knapmeyer, M
Banerdt, WB
AF Khan, A.
van Driel, M.
Bose, M.
Giardini, D.
Ceylan, S.
Yan, J.
Clinton, J.
Euchner, F.
Lognonne, P.
Murdoch, N.
Mimoun, D.
Panning, M.
Knapmeyer, M.
Banerdt, W. B.
TI Single-station and single-event marsquake location and inversion for
structure using synthetic Martian waveforms
SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS
LA English
DT Article
DE Mars; Waveforms; Marsquakes; Interior structure; Surface waves;
Body-waves; Travel times; Surface-wave overtones; Inversion
ID LUNAR MANTLE; GEOPHYSICAL CONSTRAINTS; INTERIOR STRUCTURE; TIDAL
DISSIPATION; SEISMIC DETECTION; MARS; MODEL; EARTH; CORE; MOON
AB In anticipation of the upcoming InSight mission, which is expected to deploy a single seismic station on the Martian surface in November 2018, we describe a methodology that enables locating marsquakes and obtaining information on the interior structure of Mars. The method works sequentially and is illustrated using single representative 3 -component seismograms from two separate events: a relatively large teleseismic event (Mw5.1) and a small-to-moderate-sized regional event (M(w)3.8). Location and origin time of the event is determined probabilistically from observations of Rayleigh waves and body-wave arrivals. From the recording of surface waves, averaged fundamental-mode group velocity dispersion data can be extracted and, in combination with body-wave arrival picks, inverted for crust and mantle structure. In the absence of Martian seismic data, we performed full waveform computations using a spectral element method (AxiSEM) to compute seismograms down to a period of 1 s. The model (radial profiles of density, P- and S-wave-speed, and attenuation) used for this purpose is constructed on the basis of an average Martian mantle composition and model areotherm using thermodynamic principles, mineral physics data, and viscoelastic modeling. Noise was added to the synthetic seismic data using an up-todate noise model that considers a whole series of possible noise sources generated in instrument and Iander, including wind-, thermal-, and pressure-induced effects and electromagnetic noise. The examples studied here, which are based on the assumption of spherical symmetry, show that we are able to determine epicentral distance and origin time to accuracies of similar to 0.5-1 degrees and +/- 3-6 s, respectively. For the events and the particular noise level chosen, information on Rayleigh-wave group velocity dispersion in the period range similar to 14-48 s (M(w)5.1) and similar to 14-34 s (M(w)3.8) could be determined. Stochastic inversion of dispersion data in combination with body-wave travel time information for interior structure, allows us to constrain mantle velocity structure to an uncertainty of 5%. Employing the travel times obtained with the initially inverted models, we are able to locate additional body-wave arrivals including depth phases, surface and Moho (multiple) reflections that may otherwise elude visual identification. This expanded data set is reinverted to refine interior structure models and source parameters (epicentral distance and origin time). (C) 2016 Elsevier B.V. All rights reserved.
C1 [Khan, A.; van Driel, M.; Bose, M.; Giardini, D.; Ceylan, S.; Yan, J.; Euchner, F.] Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland.
[Bose, M.; Clinton, J.] Swiss Fed Inst Technol, Swiss Seismol Serv, Zurich, Switzerland.
[Lognonne, P.] Inst Phys Globe Paris, Paris, France.
[Murdoch, N.; Mimoun, D.] Univ Toulouse, ISAE SUPAERO, DEOS Syst Spatiaux, Toulouse, France.
[Panning, M.] Univ Florida, Dept Geol Sci, Gainesville, FL USA.
[Knapmeyer, M.] DLR, Inst Planetary Res, Berlin, Germany.
[Banerdt, W. B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Khan, A (reprint author), Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland.
EM amir.khan@erdw.ethz.ch
RI Lognonne, Philippe/F-8846-2010; Panning, Mark/B-3805-2011
OI Panning, Mark/0000-0002-2041-3190
FU Swiss National Science Foundation (SNF-ANR project) [157133]; Swiss
National Supercomputing Centre (CSCS) [s528]
FX We would like to thank Lapo Boschi and an anonymous reviewer for
comments on the manuscript. We would also like to acknowledge Francis
Nimmo for sharing his visco-elastic attenuation code. This work was
supported by grants from the Swiss National Science Foundation (SNF-ANR
project 157133 "Seismology on Mars") and from the Swiss National
Supercomputing Centre (CSCS) under project ID s528. Numerical
computations have also been performed on the ETH cluster Brutus.
NR 89
TC 1
Z9 1
U1 9
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-9201
EI 1872-7395
J9 PHYS EARTH PLANET IN
JI Phys. Earth Planet. Inter.
PD SEP
PY 2016
VL 258
BP 28
EP 42
DI 10.1016/j.pepi.2016.05.017
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DU7SK
UT WOS:000382414700003
ER
PT J
AU McClelland, M
Campbell, M
Estlin, T
AF McClelland, Mark
Campbell, Mark
Estlin, Tara
TI Qualitative relational mapping and navigation for planetary rovers
SO ROBOTICS AND AUTONOMOUS SYSTEMS
LA English
DT Article
DE Navigation; Qualitative spatial reasoning; Qualitative methods; Mapping;
Landmark navigation
ID MOBILE ROBOTS; MAP; CONSISTENCY; INFORMATION; SPACE; SLAM
AB This paper presents a novel method for qualitative mapping of large scale spaces which decouples the mapping problem from that of position estimation. The proposed framework makes use of a graphical representation of the world in order to build a map consisting of qualitative constraints on the geometric relationships between landmark triplets. This process allows a mobile robot to extract information about landmark positions using a set of minimal sensors in the absence of GPS. A novel measurement method based on camera imagery is presented which extends previous work from the field of Qualitative Spatial Reasoning. A Branch-and-Bound approach is taken to solve a set of non-convex feasibility problems required for generating off-line operator lookup tables and on-line measurements, which are fused into the map using an iterative graph update. A navigation approach for travel between distant landmarks is developed, using estimates of the Relative Neighborhood Graph extracted from the qualitative map in order to generate a sequence of landmark objectives based on proximity. Average and asymptotic performance of the mapping algorithm is evaluated using Monte Carlo tests on randomly generated maps, and a data-driven simulation is presented for a robot traversing the Jet Propulsion Laboratory Mars Yard while building a relational map. These results demonstrate that the system can be effectively used to build a map sufficiently complete and accurate for long-distance navigation as well as other applications. (C) 2016 Elsevier B.V. All rights reserved.
C1 [McClelland, Mark; Campbell, Mark] Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Estlin, Tara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McClelland, Mark] Cornell Univ, Mech Engn, Ithaca, NY 14853 USA.
[Campbell, Mark] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Estlin, Tara] Mission Syst & Operat Div, Pasadena, CA USA.
RP McClelland, M (reprint author), Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.; McClelland, M (reprint author), Cornell Univ, Mech Engn, Ithaca, NY 14853 USA.
EM mjm496@cornell.edu; mc288@cornell.edu; Tara.Estlin@jpl.nasa.gov
RI Campbell, Mark/F-8312-2013
OI Campbell, Mark/0000-0003-0775-4297
FU National Science Foundation [IIS-1320490]; NASA Graduate Student
Research Program
FX The research presented in this paper has been supported by National
Science Foundation grant IIS-1320490 and a fellowship from the NASA
Graduate Student Research Program. This work was performed by Cornell
University and by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 31
TC 0
Z9 0
U1 7
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0921-8890
EI 1872-793X
J9 ROBOT AUTON SYST
JI Robot. Auton. Syst.
PD SEP
PY 2016
VL 83
BP 73
EP 86
DI 10.1016/j.robot.2016.05.017
PG 14
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Robotics
SC Automation & Control Systems; Computer Science; Robotics
GA DU6SB
UT WOS:000382343800006
ER
PT J
AU Patarasuk, R
Gurney, KR
O'Keeffe, D
Song, Y
Huang, JH
Rao, P
Buchert, M
Lin, JC
Mendoza, D
Ehleringer, JR
AF Patarasuk, Risa
Gurney, Kevin Robert
O'Keeffe, Darragh
Song, Yang
Huang, Jianhua
Rao, Preeti
Buchert, Martin
Lin, John C.
Mendoza, Daniel
Ehleringer, James R.
TI Urban high-resolution fossil fuel CO2 emissions quantification and
exploration of emission drivers for potential policy applications
SO URBAN ECOSYSTEMS
LA English
DT Article
DE Residential; Onroad; STIRPAT; Urban carbon; Hestia; Bottom-up approach
ID HOUSEHOLD ENERGY-CONSUMPTION; GREENHOUSE-GAS EMISSIONS; CARBON-DIOXIDE
SOURCES; SEA-LEVEL RISE; CLIMATE-CHANGE; INTEGRATED APPROACH; IMPACT;
SECTOR; MODEL; LIFE
AB Fossil fuel carbon dioxide (FFCO2) emissions are the largest driver of anthropogenic climate change. Approximately three-quarters of the world's fossil fuels carbon dioxide emissions are generated in urban areas. We used the Hestia high resolution approach to quantify FFCO2 for Salt Lake County, Utah, USA and demonstrate the importance of high resolution quantification to urban emissions mitigation policymaking. We focus on the residential and onroad sectors across both urbanized and urbanizing parts of the valley. Stochastic Impact by Regression on Population, Affluence, and Technology (STIRPAT) regression models using sociodemographic data at the census block group level shows that population, per capita income, and building age exhibit positive relationships while household size shows a negative relationship with FFCO2 emissions. Compact development shows little effect on FFCO2 emissions in this domain. FFCO2 emissions in high income block groups is twice as sensitive to income than low income block groups. Emissions are four times as sensitive to household size in low-income versus high-income block groups. These results suggest that policy options targeting personal responsibility or knowledge feedback loops may be the most effective strategies. Examples include utility bill performance comparison or publicly available energy maps identifying high-emitting areas. Within the onroad sector, high emissions density (FFCO2/km) is associated with primary roads, while high emissions intensity (FFCO2/VMT) is associated with secondary roads. Opportunities exist for alignment of public transportation extension with remaining high emission road segments, offering a prioritization of new onroad transportation policy in Salt Lake County.
C1 [Patarasuk, Risa; Gurney, Kevin Robert; O'Keeffe, Darragh; Song, Yang; Huang, Jianhua] Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA.
[Gurney, Kevin Robert; O'Keeffe, Darragh] Arizona State Univ, Global Inst Sustainabil, POB 875502, Tempe, AZ 85287 USA.
[Rao, Preeti] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Buchert, Martin] Univ Utah, Global Change & Sustainabil Ctr, 155 South 1452 East, Salt Lake City, UT USA.
[Lin, John C.; Mendoza, Daniel] Univ Utah, Dept Atmospher Sci, 135 South 1460 East, Salt Lake City, UT 84112 USA.
[Ehleringer, James R.] Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA.
RP Patarasuk, R (reprint author), Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA.
EM risa.patarasuk@asu.edu
OI Buchert, Martin/0000-0001-5974-001X; Rao, Preeti/0000-0002-5549-0583
FU Department of Energy [DE-SC-001-0624]; National Science Foundation
[EF-01241286]; National Institute of Standards and Technology
[70NANB14H321]; National Oceanic and Atmospheric Administration Climate
Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate
Program [NA14OAR4310178]
FX This research was supported by grants from the Department of Energy
DE-SC-001-0624, the National Science Foundation grant EF-01241286,
National Institute of Standards and Technology grant 70NANB14H321, and
National Oceanic and Atmospheric Administration Climate Program Office's
Atmospheric Chemistry, Carbon Cycle, and Climate Program grant
NA14OAR4310178. We also would like to thank Jerome Zenger, Kevin Bell,
and Semih Yildiz for assisting with the data collection and inquiry.
NR 109
TC 1
Z9 1
U1 19
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1083-8155
EI 1573-1642
J9 URBAN ECOSYST
JI Urban Ecosyst.
PD SEP
PY 2016
VL 19
IS 3
BP 1013
EP 1039
DI 10.1007/s11252-016-0553-1
PG 27
WC Biodiversity Conservation; Ecology; Environmental Sciences; Urban
Studies
SC Biodiversity & Conservation; Environmental Sciences & Ecology; Urban
Studies
GA DV1HB
UT WOS:000382670600001
ER
PT J
AU Liu, YC
Xu, YH
Hicks, MC
Avedisian, CT
AF Liu, Yu Cheng
Xu, Yuhao
Hicks, Michael C.
Avedisian, C. Thomas
TI Comprehensive study of initial diameter effects and other observations
on convection-free droplet combustion in the standard atmosphere for
n-heptane, n-octane, and n-decane
SO COMBUSTION AND FLAME
LA English
DT Article
DE Droplet combustion; Microgravity; Extinction; Radiation; Low temperature
combustion; Soot formation
ID MICROGRAVITY CONDITIONS; SOOT FORMATION; FUEL DROPLETS; BURNING RATE;
COOL-FLAMES; LOW-GRAVITY; EXTINCTION; MIXTURES; VAPORIZATION; RADIATION
AB This paper reports the results of a comprehensive experimental study on the effect of initial droplet diameter (Do) over a very wide range (0.5 mm < D-0 < 5 mm) on the spherically symmetric droplet burning characteristics in the standard atmosphere of three alkanes - n-heptane, n-octane and n-decane - that are representative of components found in petroleum-based transportation fuels and their surrogates. Spherical symmetry in the burning process was promoted by carrying out the experiments in a reduced convection (stagnant ambience) and buoyancy (low gravity) environment using the facilities of a ground based drop tower for D-0 < 0.8 mm and a spaced-based platform (the International Space Station) for D-0 > 1.0 mm.
The results show that for Do greater than about 2 mm, K decreases with increasing Do in an early period of burning and with the data being correlated in the form K similar to D-0(-n) based on a scale analysis of an energy balance on the flame. For Do larger than approximately 2 mm the droplet flames often disappeared indicating an extinction mechanism that was speculated to be due to radiative losses from the flame. Concurrently, measurements of wideband radiation dropped significantly and the burning rate gradually approached pure evaporation.
In some instances for n-heptane and n-octane radiative extinction was accompanied by droplet evaporation rates that were significantly higher than evaporation in a hot ambience which persisted for a significant fraction of the burning history before decreasing to evaporation in a cold ambience. An energy balance on the drop related the flame temperature to droplet diameter from which it was predicted that flame temperatures after ignition were greater than 1200 K before dropping to under approximately 800 K and remaining constant thereafter until eventually reaching near ambient conditions. This intermediate regime of burning was conjectured to be associated with a low temperature combustion process. The transition to this intermediate regime upon radiative extinction was occasionally accompanied by flame oscillations, the origin of which was uncertain but could have been initiated by motion of the droplet owing to the deployment process. (C) 2016 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Liu, Yu Cheng] Univ Michigan Flint, Dept Comp Sci Engn & Phys, Flint, MI 48502 USA.
[Xu, Yuhao; Avedisian, C. Thomas] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Hicks, Michael C.] NASA, Glenn Res Ctr, Combust & Reacting Syst Branch, Cleveland, OH 44135 USA.
[Liu, Yu Cheng] Tsinghua Univ, Ctr Combust Energy, Beijing 100084, Peoples R China.
RP Avedisian, CT (reprint author), Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
EM cta2@cornell.edu
OI Liu, Yu Cheng/0000-0001-7954-717X
FU National Administration of Space and Aeronautics (NASA) [NNX08AI51G]
FX This work was supported by the National Administration of Space and
Aeronautics (NASA) under Grants NNX08AI51G to Cornell University (where
the ground-based experiments were carried out). The authors are pleased
to acknowledge Drs. Vedha Nayagam and Daniel Dietrich of NASA-Glenn who
offered insights regarding data analysis and combustion physics of some
of the observed trends and assistance with some of the reported
experiments. Messrs Jeff Rah, Koffi Trenou, Wei-Chih Kuo and Anthony
Savas of Cornell provided assistance with the experiments reported here
and analyses of the data. The interest of F.A. Williams (UC-San Diego),
F.L. Dryer (Princeton), T. Farouk (U. South Carolina), and B.D. Shaw
(UC-Davis)) is also greatly appreciated.
NR 60
TC 4
Z9 4
U1 10
U2 12
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 SEP
PY 2016
VL 171
BP 27
EP 41
DI 10.1016/j.combustfiame.2016.05.013
PG 15
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA DU9CE
UT WOS:000382513000003
ER
PT J
AU de Wit, J
Wakeford, HR
Gillon, M
Lewis, NK
Valenti, JA
Demory, BO
Burgasser, AJ
Burdanov, A
Delrez, L
Jehin, E
Lederer, SM
Queloz, D
Triaud, AHMJ
Van Grootel, V
AF de Wit, Julien
Wakeford, Hannah R.
Gillon, Michael
Lewis, Nikole K.
Valenti, Jeff A.
Demory, Brice-Olivier
Burgasser, Adam J.
Burdanov, Artem
Delrez, Laetitia
Jehin, Emmanuel
Lederer, Susan M.
Queloz, Didier
Triaud, Amaury H. M. J.
Van Grootel, Valerie
TI A combined transmission spectrum of the Earth-sized exoplanets
TRAPPIST-1 b and c
SO NATURE
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; HABITABLE-ZONE; LIGHT CURVES; SUPER-EARTHS; GJ
1214B; SPECTROSCOPY; ATMOSPHERES; PLANETS; KEPLER; EVAPORATION
AB Three Earth-sized exoplanets were recently discovered close to the habitable zone(1,2) of the nearby ultracool dwarf star TRAPPIST-1 (ref. 3). The nature of these planets has yet to be determined, as their masses remain unmeasured and no observational constraint is available for the planetary population surrounding ultracool dwarfs, of which the TRAPPIST-1 planets are the first transiting example. Theoretical predictions span the entire atmospheric range, from depleted to extended hydrogen-dominated atmospheres(4-8). Here we report observations of the combined transmission spectrum of the two inner planets during their simultaneous transits on 4 May 2016. The lack of features in the combined spectrum rules out doud-free hydrogen-dominated atmospheres for each planet at >= 10 sigma levels; TRAPPIST-1 b and c are therefore unlikely to have an extended gas envelope as they occupy a region of parameter space in which high-altitude cloud/haze formation is not expected to be significant for hydrogen-dominated atmospheres(9). Many denser atmospheres remain consistent with the featureless transmission spectrum from a cloud-free water-vapour atmosphere to a Venus-like one.
C1 [de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Wakeford, Hannah R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gillon, Michael; Burdanov, Artem; Delrez, Laetitia; Jehin, Emmanuel; Van Grootel, Valerie] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 19C, B-4000 Liege, Belgium.
[Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Demory, Brice-Olivier; Queloz, Didier] Cavendish Lab, Astrophys Grp, 19 JJ Thomson Ave, Cambridge CB3 0HE, England.
[Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Lederer, Susan M.] NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Triaud, Amaury H. M. J.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RP de Wit, J (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM jdewit@mit.edu
OI Wakeford, Hannah/0000-0003-4328-3867
FU NASA through Space Telescope Science Institute [HST-GO-14500]; European
Research Council (ERC) [336480]; Action de Recherche Concertee (ARC) by
Wallonia-Brussels Federation; NASA; Fund for Research Training in
Industry and Agriculture of the FRS-FNRS
FX 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. These observations are associated with program
HST-GO-14500 (principal investigator J.d.W.), support for which was
provided by NASA through a grant from the Space Telescope Science
Institute. The research leading to our results was funded in part by the
European Research Council (ERC) under the FP/2007-2013 ERC grant 336480,
and through an Action de Recherche Concertee (ARC) grant financed by the
Wallonia-Brussels Federation. H.R.W. acknowledges support through an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by the Universities Space Research Association
through a contract with NASA. M.G. is Research Associate at the Belgian
Fonds (National) de la Recherche Scientifique (FRS-FNRS). L.D.
acknowledges support of the Fund for Research Training in Industry and
Agriculture of the FRS-FNRS. We thank D. Taylor, S. Deustua, P.
McCullough, and N. Reid for their assistance in planning and executing
our observations. We are also grateful for discussions with Z.
Berta-Thompson and Pierre Magain about this study and manuscript. We
thank the ATLAS and PHOENIX teams for providing stellar models.
NR 26
TC 6
Z9 6
U1 12
U2 15
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD SEP 1
PY 2016
VL 537
IS 7618
BP 69
EP 72
DI 10.1038/nature18641
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DU7XC
UT WOS:000382426900039
PM 27437572
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI The CO chondrites: Major recent Antarctic finds, their thermal and
radiation history, and describing the metamorphic history of members of
the class
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE CO chondrites; Metamorphism; Thermoluminescence; Antarctic meteorites
ID UNEQUILIBRATED ORDINARY CHONDRITES; NATURAL THERMOLUMINESCENCE;
CARBONACEOUS CHONDRITES; TERRESTRIAL AGES; TYPE-3 CHONDRITES;
OXYGEN-ISOTOPE; PARENT-BODY; METEORITES; LUMINESCENCE; ORBITS
AB Thermoluminescence (TL) properties of 29 CO chondrites from the Miller Range (MIL) and five chondrites from the Dominion Range (DOM) have been measured. MIL has a relatively strong natural TL signal (19.6 +/- 14.7 krad), while some of the DOM samples have a very weak natural TL signal (<1 krad) whereas others resemble the MIL meteorites. I argue that MIL and some of the DOM samples had a normal perihelion (similar to 1.0 AU) and terrestrial age of similar to 450-700 ka, while some of the DOM samples have a terrestrial age of similar to 100 ka but a perihelion of similar to 0.8 AU. The DOM meteorites also show considerable heterogeneity in their induced TL properties, also suggesting that the DOM fragments represent more than one fall. The induced TL data for the MIL samples studied here are consistent with them all being from a single fragmented meteorite. Small (50 mg) chips have TL properties similar to 500 mg chips, so that the smaller chips are representative, although samples taken from original masses less than similar to 2 g have low natural TL suggesting that they were heated during atmospheric fall. The properties of CO chondrites are reviewed in terms of their petrologic types. Correlations between TL sensitivity, the most quantitative technique for evaluating metamorphic alteration in CO chondrites, and data for olivine composition and heterogeneity, matrix composition, inert gas content, metal composition (Ni, Co, and Cr in the kamacite), bulk carbon, C and O isotopes, graphite ordering, spectral reflectance at 0.8 mu m, and textural characteristics of the ameboid olivine and Ca-rich inclusions are examined. The petrographic types appear to be largely metamorphic in origin with perhaps a minor role for metasomatism. Contrary to recent proposals it is here argued that petrologic type definitions should (1) be specific enough to be meaningful, but broad enough to be simple in application and robust to new developments, (2) be descriptive and not interpretative, (3) should not oversimplify and obscure important class-to-class differences, and (4) take account of all the available information, while avoiding reliance on any one technique or single observation whose application is based on interpretation. With these considerations in mind the petrographic type definitions for CO chondrites are restated and the petrologic type of 3.2 assigned to both the MIL and DOM CO chondrites. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Sears, Derek W. G.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA.
FU NASA's Solar System Exploration and Research Virtual Institute
FX I am grateful to Tim Lee and Chris McKay for providing facilities and an
exciting research environment at NASA Ames Research Center and I am
grateful to Mark Sittloh and his colleagues at the Bay Area
Environmental Research Institute for management support. I am also
grateful to the Antarctic Meteorite Working Group for providing the
samples and the Meteorite Processing Laboratory at Johnson Space Center
for so capably handling the sampling. I am also grateful to Hazel Sears
for reviewing and proofing this paper, David Sears for help with the
statistical analysis, four anonymous journal reviewers who provided much
appreciated reviews (which included the suggestion to include Fig. 7),
and Chris Herd for organizing these reviews. Finally, I am pleased to
acknowledge the Field Investigations to Enable Solar System Science and
Exploration team of NASA's Solar System Exploration and Research Virtual
Institute (PI: Jennifer Heldmann) for financial support.
NR 54
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2016
VL 188
BP 106
EP 124
DI 10.1016/j.gca.2016.05.033
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700007
ER
PT J
AU Robinson, KL
Barnes, JJ
Nagashima, K
Thomen, A
Franchi, IA
Huss, GR
Anand, M
Taylor, GJ
AF Robinson, Katharine L.
Barnes, Jessica J.
Nagashima, Kazuhide
Thomen, Aurelien
Franchi, Ian A.
Huss, Gary R.
Anand, Mahesh
Taylor, G. Jeffrey
TI Water in evolved lunar rocks: Evidence for multiple reservoirs
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Moon; Lunar volatiles; Apatite; Water; H isotopes
ID SILICATE-LIQUID-IMMISCIBILITY; HOSTED MELT INCLUSIONS; TERRESTRIAL
PLANETS; VOLCANIC GLASSES; MG-SUITE; VOLATILE ABUNDANCES; QUARTZ
MONZODIORITE; CRYSTAL-CHEMISTRY; COOLING HISTORY; OXYGEN FUGACITY
AB We have measured the abundance and isotopic composition of water in apatites from several lunar rocks representing Potassium (K), Rare Earth Elements (REE), and Phosphorus (P) - KREEP - rich lithologies, including felsites, quartz monzodiorites (QMDs), a troctolite, and an alkali anorthosite. The H-isotope data from apatite provide evidence for multiple reservoirs in the lunar interior. Apatite measurements from some KREEP-rich intrusive rocks display moderately elevated delta D signatures, while other samples show delta D signatures similar to the range known for the terrestrial upper mantle. Apatite grains in Apollo 15 quartz monzodiorites have the lowest delta D values measured from the Moon so far (as low as -749 parts per thousand), and could potentially represent a D-depleted reservoir in the lunar interior that had not been identified until now. Apatite in all of these intrusive rocks contains <267 ppm H2O, which is relatively low compared to apatites from the majority of studied mare basalts (200 to >6500 ppm H2O). Complexities in partitioning of volatiles into apatite make this comparison uncertain, but measurements of residual glass in KREEP basalt fragments in breccia 15358 independently show that the KREEP basaltic magmas were low in water. The source of 15358 contained similar to 10 ppm H2O, about an order of magnitude lower than the source of the Apollo 17 pyroclastic glass beads, suggesting potential variations in the distribution of water in the lunar interior. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Robinson, Katharine L.; Nagashima, Kazuhide; Thomen, Aurelien; Huss, Gary R.; Taylor, G. Jeffrey] Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
[Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii Manoa, Geol & Geophys, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
[Barnes, Jessica J.; Franchi, Ian A.; Anand, Mahesh] Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England.
RP Robinson, KL (reprint author), Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
EM katie.robinson@open.ac.uk
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute through the Office of Space Science [NNA09DA77A];
NASA Lunar Advanced Science and Exploration Research [NNX11AE85G]; Solar
System Exploration Research Virtual Institute (through the Center for
Lunar Science and Exploration) [NNA14AB07A]; Bullard Foundation; STFC
[ST/I001298/1, ST/L000776/1]
FX The authors thank Romain Tartese for his assistance in collecting data
and for highly useful discussions. This research was supported by the
National Aeronautics and Space Administration through the NASA
Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued
through the Office of Space Science, by NASA Lunar Advanced Science and
Exploration Research Grant NNX11AE85G, the Solar System Exploration
Research Virtual Institute (through the Center for Lunar Science and
Exploration cooperative agreement NNA14AB07A, David Kring, PI), and by
The Bullard Foundation. STFC are also thanked for a PhD studentship to
JJB and research grants to MA (Grant no. ST/I001298/1 and ST/L000776/1).
We thank three anonymous reviewers and associate editor Alexander
Nemchin for insightful and critical comments that helped improve the
quality of the manuscript.
NR 115
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2016
VL 188
BP 244
EP 260
DI 10.1016/j.gca.2016.05.030
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700014
ER
PT J
AU Peretyazhko, TS
Fox, A
Sutter, B
Niles, PB
Adams, M
Morris, RV
Ming, DW
AF Peretyazhko, T. S.
Fox, A.
Sutter, B.
Niles, P. B.
Adams, M.
Morris, R. V.
Ming, D. W.
TI Synthesis of akaganeite in the presence of sulfate: Implications for
akaganeite formation in Yellowknife Bay, Gale Crater, Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Mars; Gale crater; Yellowknife Bay; Fe oxides; Akaganeite
ID ACID-MINE DRAINAGE; BETA-FEOOH; AQUEOUS-SOLUTIONS; REFLECTANCE
SPECTROSCOPY; SPECTRAL PROPERTIES; FORCED HYDROLYSIS; MERIDIANI-PLANUM;
X-RAY; IRON; JAROSITE
AB Akaganeite, a Cl-bearing Fe(III) (hydr)oxide, has been recently discovered in Yellowknife Bay in Gale crater on Mars by the Mars Science Laboratory (MSL) Curiosity Rover. Akaganeite was associated with sulfate and sulfide minerals at Yellowknife Bay indicating that sulfate ions could be present in solution during akaganeite formation. The mechanism and conditions of akaganeite formation in the Yellowknife Bay mudstone are unknown. We investigated formation of akaganeite through hydrolysis of ferric chloride solution in the presence of 0, 0.01, 0.05, 0.1 and 0.2 M sulfate and at initial pH of 1.5, 2 and 4 at 90 degrees C. Mineralogy of the precipitated Fe(III) phases was characterized by X-ray diffraction and infrared spectroscopy. The precipitates were also acid digested to determine total sulfate and chloride contents. Akaganeite and natrojarosite formed at initial solution pH of 1.5; akaganeite, goethite and natrojarosite precipitated in initial pH 2 solutions and goethite, hematite and 2-line ferrihydrite precipitated at initial solution pH of 4. Sulfate addition did not inhibit akaganeite formation. Increasing initial solution sulfate concentrations resulted in increasing sulfate to chloride ratio in the precipitated akaganeite. Infrared spectroscopy revealed akaganeite bands at similar to 2 mu m (H2O combination band) and at similar to 2.46 mu m (OH combination band). The H2O combination band position linearly correlated with total chloride content in akaganeite. Overall, laboratory studies demonstrated formation of akaganeite at initial sulfate concentration <= 0.2 M (sulfate to chloride molar ratio <= 0.3) and pH <= 2, implying that those conditions might prevail (perhaps as micro-environments) during akaganeite formation in Yellowknife Bay mudstone. The occurrence of Fe(II) sulfides (pyrite and pyrrhotite) in Yellowknife Bay mudstone is a potential acidity source. Dissolution of sulfide minerals might occur under localized oxidizing waterlimiting Cl-rich conditions creating favorable environments for akaganeite formation. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Peretyazhko, T. S.; Sutter, B.] NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA.
[Fox, A.] Indiana Univ, Bloomington, IN 47406 USA.
[Niles, P. B.; Morris, R. V.; Ming, D. W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Adams, M.] Univ Hawaii, Hilo, HI 96720 USA.
RP Peretyazhko, TS (reprint author), NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA.
EM tanya.peretyazhko@nasa.gov
FU Summer Intern Scholarship of Lunar and Planetary Institute; NASA Mars
Science Laboratory Mission grants; NASA Solar System Workings grant
[15-SSW15_2-0074]
FX We are grateful to Z. Peng for performing ICP-MS analysis and K. Pando
and D. Locke for help with ion chromatography. We thank Dr. Bishop and
two anonymous reviewers for valuable suggestions and comments that help
to improve the quality of the manuscript. We thank the Associate Editor
Dr. Catalano for handling the manuscript. A. Fox acknowledges a Summer
Intern Scholarship of Lunar and Planetary Institute. This work was
supported by NASA Mars Science Laboratory Mission grants and by NASA
Solar System Workings grant #15-SSW15_2-0074. The data presented in
figures could be provided upon request.
NR 76
TC 0
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U1 18
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2016
VL 188
BP 284
EP 296
DI 10.1016/j.gca.2016.06.002
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700016
ER
PT J
AU Ting, DZ
Soibel, A
Hoglund, L
Hill, CJ
Keo, SA
Fisher, A
Gunapala, SD
AF Ting, David Z.
Soibel, Alexander
Hoeglund, Linda
Hill, Cory J.
Keo, Sam A.
Fisher, Anita
Gunapala, Sarath D.
TI High-Temperature Characteristics of an InAsSb/AlAsSb n(+)Bn Detector
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE Infrared detector; unipolar barrier; nBn; mid-wavelength infrared
AB The high-temperature characteristics of a mid-wavelength infrared (MWIR) detector based on the Maimon-Wicks InAsSb/AlAsSb nBn architecture was analyzed. The dark current characteristics are examined in reference to recent minority carrier lifetime results. The difference between the responsivity and absorption quantum efficiency (QE) at shorter wavelengths is clarified in terms of preferential absorption of higher-energy photons in the top contact layer, which cannot provide reverse-bias photo-response due to the AlAsSb electron blocking layer and strong recombination. Although the QE does not degrade when the operating temperature increases to 325 K, the turn-on bias becomes larger at higher temperatures. This behavior was originally attributed to the change in the valence band alignment between the absorber and top contact layers caused by the shift in Fermi level with temperature. In this work, we demonstrated the inadequacy of the original description, and offer a more likely explanation based on temperature-dependent band-bending effects.
C1 [Ting, David Z.; Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] CALTECH, Pasadena, CA 91109 USA.
RP Ting, DZ (reprint author), NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
NR 8
TC 2
Z9 2
U1 11
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD SEP
PY 2016
VL 45
IS 9
BP 4680
EP 4685
DI 10.1007/s11664-016-4633-z
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA DS9CM
UT WOS:000381080000027
ER
PT J
AU Suhir, E
Ghaffarian, R
AF Suhir, E.
Ghaffarian, R.
TI Board level drop test: exact solution to the problem of the nonlinear
dynamic response of a PCB to the drop impact
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
AB An analytical predictive model has been developed for the evaluation of the nonlinear dynamic response of a printed-circuit-board (PCB) to the drop impact during board-level testing. The hypothesis of "heavy-and-flexible" PCB is used in the analysis: the surface-mounted-devices (SMDs) are assumed to be small enough not to affect the PCB's flexural rigidity, but their masses have been considered and accounted for by "spreading out" the SMD total mass over the PCB surface. The analysis is restricted to the fundamental mode of vibrations, and the method of principal coordinates is used to evaluate the response. The exact solution to the nonlinear differential equation for the principal coordinate has been obtained. Another important finding is that the nonlinear amplitudes were determined even without solving the nonlinear differential equation of motion. The main objective of the analysis is to provide design guidelines for constructing a feasible experimental setup. A simply supported board is suggested as the most appropriate structure for an adequate test vehicle: the experimental data for such a board, as far as the behavior of the solder material in the second level of interconnections is concerned, can be easily and reliably interpreted and extrapolated for the practical use. The developed model enables one to predict the induced bending moments and the in-plane (membrane) forces that could be applied in the subsequent analyses to the PCB areas in the proximity of the package and its solder joint interconnections.
C1 [Suhir, E.] Portland State Univ, Portland, OR 97207 USA.
[Suhir, E.] ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
[Ghaffarian, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.; Suhir, E (reprint author), ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
EM suhire@aol.com
NR 21
TC 1
Z9 1
U1 10
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD SEP
PY 2016
VL 27
IS 9
BP 9423
EP 9430
DI 10.1007/s10854-016-4988-1
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA DT0FY
UT WOS:000381159800074
ER
PT J
AU Xie, YS
Fan, X
Chen, YP
Wilson, JD
Simons, RN
Xiao, JQ
AF Xie, Yunsong
Fan, Xin
Chen, Yunpeng
Wilson, Jeffrey D.
Simons, Rainee N.
Xiao, John Q.
TI THE IN-PHASE REFLECTION BANDWIDTH THEORETICAL LIMIT OF ARTIFICIAL
MAGNETIC CONDUCTORS BASED ON TRANSMISSION LINE MODEL
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE artificial magnetic conductors (AMCs); transmission line model;
bandwidth limitation
ID HIGH-IMPEDANCE SURFACES; FREQUENCY; ANTENNAS; ABSORBERS; DESIGN
AB Based on the transmission line model, the in-phase reflection (IPR) bandwidth theoretical limit using a function of permeability (l) and thickness (h) of the substrate as well as center frequency of IPR (f) was expressed. An experimental design strategy was further derived from this function for creating novel artificial magnetic conductors (AMCs). To date, they have successfully designed, simulated, and experimentally verified this proposed strategy with various AMCs, where the bandwidth ratio to the theoretical limit can be achieved by as high as 98.5%. This newly proposed theoretical limit function was further evaluated in two-ways, (1) our theoretical limit was compared with previously reported literature values, and (2) literature values were recalculated using our function. Herein, it was concluded that their IPR bandwidth theoretical limit function provided most restrictive and accurate value, and their AMC design strategy has showed evident advantages over literature. (C) 2016 Wiley Periodicals, Inc.
C1 [Xie, Yunsong; Chen, Yunpeng] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Fan, Xin] Univ Denver, Dept Phys & Astron, Newark, DE 19716 USA.
[Wilson, Jeffrey D.; Simons, Rainee N.; Xiao, John Q.] Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA.
RP Xiao, JQ (reprint author), Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA.
EM jqx@udel.edu
FU National Aeronautics and Space Administration (NASA) [NNX11AQ29A]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) under Grant No. NNX11AQ29A.
NR 22
TC 0
Z9 0
U1 6
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0895-2477
EI 1098-2760
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD SEP
PY 2016
VL 58
IS 9
BP 2257
EP 2261
DI 10.1002/mop.30024
PG 6
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA DS7DW
UT WOS:000380944000052
ER
PT J
AU Bianco, WT
Landis, R
AF Bianco, William T.
Landis, Robert
TI Engineering cooperation: How Americans and Russians manage joint
operation of the International Space Station
SO INTERNATIONAL AREA STUDIES REVIEW
LA English
DT Article
DE Cooperation; prisoners' dilemma; new economics of organization;
International Space Station; NASA
AB The 1990s agreements that created the International Space Station (ISS) described the effort as a partnership of equals, a joint venture between organizations that remained independent in terms of many procedures, norms, goals, and the assumptions underlying these factors. As a result, successful joint ISS operations required the participants, most notably the American and Russian space programs, to reconcile different procedures, norms, and training regimes, as well as the beliefs that underlie these practices. Drawing on a combination of operational experience, first-hand observation, and interviews, this paper focuses on how the two programs reduced conflict and engendered cooperation. It also uses the ISS experience to consider how future joint efforts can be designed to minimize conflict between international partners.
C1 [Bianco, William T.] Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA.
[Landis, Robert] NASA Headquarters, Washington, DC USA.
RP Bianco, WT (reprint author), Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA.
EM wbianco@indiana.edu
NR 12
TC 0
Z9 0
U1 4
U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 2233-8659
EI 2049-1123
J9 INT AREA STUD REV
JI Int. Area Stud. Rev.
PD SEP
PY 2016
VL 19
IS 3
BP 197
EP 209
DI 10.1177/2233865916636834
PG 13
WC International Relations
SC International Relations
GA DT6WT
UT WOS:000381626100001
ER
PT J
AU Ghods, M
Johnson, L
Lauer, M
Grugel, RN
Tewari, SN
Poirier, DR
AF Ghods, M.
Johnson, L.
Lauer, M.
Grugel, R. N.
Tewari, S. N.
Poirier, D. R.
TI Macrosegregation in Al-7Si alloy caused by abrupt cross-section change
during directional solidification
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Directional solidification; Cross-section change; Computer simulation;
Fluid flows; Segregation; Aluminum alloys
ID PB-SN ALLOYS; DENDRITIC SOLIDIFICATION; NATURAL-CONVECTION; METALLIC
ALLOYS; SUPERALLOY CASTINGS; GRAIN STRUCTURES; RAYLEIGH NUMBER;
CRYSTAL-GROWTH; TURBINE-BLADES; BINARY-ALLOYS
AB Hypoeutectic Al-7 wt.% Si alloys were directionally solidified vertically downward in cylindrical molds that incorporated an abrupt cross-section decrease (9.5 mm to 3.2 mm diameter) which, after 5 cm, reverted back to 9.5 mm diameter in a Bridgman furnace; two constant growth speeds and thermal gradients were investigated. Thermosolutal convection and cross-section-change-induced shrinkage flow effects on macrosegregation were investigated. Dendrite clustering and extensive radial macro segregation was seen, particularly in the larger cross-sections, before contraction and after expansion, this more evident at the lower growth speed. This alloy shows positive longitudinal macrosegregation near cross-section decrease followed by negative macrosegregation right after it; the extent of macro segregation, however, decreases with increasing growth speed. Primary dendrite steepling intensified as solidification proceeded into the narrower section and negative longitudinal macrosegregation was seen on the re-entrant shelves at expansion. A two-dimensional model accounting for both shrinkage and thermo-solutal convection was used to simulate solidification and the resulting mushy-zone steepling and macrosegregation. The experimentally observed longitudinal and radial macrosegregation associated with the cross-section changes during directional solidification of an Al-75i alloy is well captured by the numerical simulations. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Ghods, M.; Johnson, L.; Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA.
[Lauer, M.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA.
[Grugel, R. N.] NASA, Marshall Space Flight Space Ctr, Huntsville, AL 35811 USA.
[Johnson, L.] Avery Dennison Corp, Painesville, OH 44077 USA.
[Lauer, M.] ME Elecmetal Inc, Duluth, MN 55808 USA.
RP Ghods, M (reprint author), Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA.
EM ghods.masoud@gmail.com
FU NASA [NX10AV40G, NNX14AM18G]; Sandia National Laboratories Campus
Executive Fellowship program
FX This work was supported by NASA Grant NX10AV40G and NNX14AM18G. The
Al-7% Si alloys for our current research were kindly provided by Dr. Men
G. Chu at ALCOA Technical Center. M. Lauer would like to acknowledge
support from the Sandia National Laboratories Campus Executive
Fellowship program.
NR 54
TC 1
Z9 1
U1 6
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
EI 1873-5002
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD SEP 1
PY 2016
VL 449
BP 134
EP 147
DI 10.1016/j.jcrysgro.2016.06.010
PG 14
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA DS5RT
UT WOS:000380840700022
ER
PT J
AU Ryoo, MS
Matthies, L
AF Ryoo, M. S.
Matthies, Larry
TI First-Person Activity Recognition: Feature, Temporal Structure, and
Prediction
SO INTERNATIONAL JOURNAL OF COMPUTER VISION
LA English
DT Article
ID CLASSIFICATION
AB This paper discusses the problem of recognizing interaction-level human activities from a first-person viewpoint. The goal is to enable an observer (e.g., a robot or a wearable camera) to understand 'what activity others are performing to it' from continuous video inputs. These include friendly interactions such as 'a person hugging the observer' as well as hostile interactions like 'punching the observer' or 'throwing objects at the observer', whose videos involve a large amount of camera ego-motion caused by physical interactions. The paper investigates multi-channel kernels to integrate global and local motion information, and presents a new activity learning/recognition methodology that explicitly considers temporal structures displayed in first-person activity videos. Furthermore, we present a novel algorithm for early recognition (i.e., prediction) of activities from first-person videos, which allows us to infer ongoing activities at their early stage. In our experiments, we not only show classification results with segmented videos, but also confirm that our new approach is able to detect activities from continuous videos and perform early recognition reliably.
C1 [Ryoo, M. S.; Matthies, Larry] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Ryoo, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM mryoo@jpl.nasa.gov
FU National Aeronautics and Space Administration; Army Research Laboratory
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
research was sponsored by the Army Research Laboratory and was
accomplished under Cooperative Agreement Number W911NF-10-2-0016.
NR 33
TC 0
Z9 0
U1 7
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0920-5691
EI 1573-1405
J9 INT J COMPUT VISION
JI Int. J. Comput. Vis.
PD SEP
PY 2016
VL 119
IS 3
SI SI
BP 307
EP 328
DI 10.1007/s11263-015-0847-4
PG 22
WC Computer Science, Artificial Intelligence
SC Computer Science
GA DS0FE
UT WOS:000380270000007
ER
PT J
AU Barre, J
Edwards, D
Worden, H
Arellano, A
Gaubert, B
Da Silva, A
Lahoz, W
Anderson, J
AF Barre, Jerome
Edwards, David
Worden, Helen
Arellano, Avelino
Gaubert, Benjamin
Da Silva, Arlindo
Lahoz, William
Anderson, Jeffrey
TI On the feasibility of monitoring carbon monoxide in the lower
troposphere from a constellation of northern hemisphere geostationary
satellites: Global scale assimilation experiments (Part II)
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Atmospheric composition; Global scale; Geostationary constellation;
Remote sensing; OSSE; Carbon monoxide; CO lifetime; Long-range transport
of pollution; Data assimilation
ID EARTH SYSTEM MODEL; CHEMISTRY; OZONE; AEROSOLS; CO; EMISSIONS; GASES;
BIAS
AB This paper describes the second phase of an Observing System Simulation Experiment (OSSE) that utilizes the synthetic measurements from a constellation of satellites measuring atmospheric composition from geostationary (GEO) Earth orbit presented in part I of the study. Our OSSE is focused on carbon monoxide observations over North America, East Asia and Europe where most of the anthropogenic sources are located. Here we assess the impact of a potential GEO constellation on constraining northern hemisphere (NH) carbon monoxide (CO) using data assimilation. We show how cloud cover affects the GEO constellation data density with the largest cloud cover (i.e., lowest data density) occurring during Asian summer. We compare the modeled state of the atmosphere (Control Run), before CO data assimilation, with the known "true" state of the atmosphere (Nature Run) and show that our setup provides realistic atmospheric CO fields and emission budgets. Overall, the Control Run underestimates CO concentrations in the northern hemisphere, especially in areas close to CO sources. Assimilation experiments show that constraining CO close to the main anthropogenic sources significantly reduces errors in NH CO compared to the Control Run. We assess the changes in error reduction when only single satellite instruments are available as compared to the full constellation. We find large differences in how measurements for each continental scale observation system affect the hemispherical improvement in long-range transport patterns, especially due to seasonal cloud cover. A GEO constellation will provide the most efficient constraint on NH CO during winter when CO lifetime is longer and increments from data assimilation associated with source regions are advected further around the globe. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Barre, Jerome; Edwards, David; Worden, Helen; Gaubert, Benjamin; Anderson, Jeffrey] NCAR, Boulder, CO USA.
[Arellano, Avelino] Univ Arizona, Tucson, AZ USA.
[Da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lahoz, William] NILU, Kjeller, Norway.
RP Barre, J (reprint author), NCAR, Boulder, CO USA.
EM barre@ucar.edu
OI Arellano, Avelino/0000-0002-2615-5831
FU NASA [NNX09AH03G S02, NNX11AI10G, NNX11AG63G]; National Science
Foundation
FX This work was partly supported by NASA grants NNX09AH03G S02, NNX11AI10G
and NNX11AG63G. The National Center for Atmospheric Research is
sponsored by the National Science Foundation. The Climate Simulation
Laboratory at NCAR's Computational and Information Systems Laboratory
(CISL) provided computing resources. We would like to acknowledge
high-performance computing support from Yellowstone
(ark:/85065/d7wd3xhc) provided by NCAR's CISL. We also thank the
reviewers for their constructive comments.
NR 29
TC 0
Z9 0
U1 6
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 140
BP 188
EP 201
DI 10.1016/j.atmosenv.2016.06.001
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200018
ER
PT J
AU Hamill, P
Giordano, M
Ward, C
Giles, D
Holben, B
AF Hamill, Patrick
Giordano, Marco
Ward, Carolyne
Giles, David
Holben, Brent
TI An AERONET-based aerosol classification using the Mahalanobis distance
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Atmospheric aerosols; Aerosol typing; AERONET; Mahalanobis distance;
Seasonal aerosol variation; High AOD events
ID OPTICAL-PROPERTIES; ABSORPTION; MODELS; TRANSPORT; POLLUTION; MIXTURES;
NETWORK; CHINA; DUST; SIZE
AB We present an aerosol classification based on AERONET aerosol data from 1993 to 2012. We used the AERONET Level 2.0 almucantar aerosol retrieval products to define several reference aerosol clusters which are characteristic of the following general aerosol types: Urban-Industrial, Biomass Burning, Mixed Aerosol, Dust, and Maritime. The classification of a particular aerosol observation as one of these aerosol types is determined by its five-dimensional Mahalanobis distance to each reference cluster. We have calculated the fractional aerosol type distribution at 190 AERONET sites, as well as the monthly variation in aerosol type at those locations. The results are presented on a global map and individually in the supplementary material. Our aerosol typing is based on recognizing that different geographic regions exhibit characteristic aerosol types. To generate reference clusters we only keep data points that lie within a Mahalanobis distance of 2 from the centroid. Our aerosol characterization is based on the AERONET retrieved quantities, therefore it does not include low optical depth values. The analysis is based on "point sources" (the AERONET sites) rather than globally distributed values. The classifications obtained will be useful in interpreting aerosol retrievals from satellite borne instruments. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Hamill, Patrick] San Jose State Univ, San Jose, CA 95192 USA.
[Hamill, Patrick] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Giordano, Marco] Univ Nevada, Reno, NV 89557 USA.
[Giordano, Marco] Desert Res Inst, Reno, NV USA.
[Ward, Carolyne] Calif State Univ Long Beach, Long Beach, CA 90840 USA.
[Giles, David; Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Hamill, P (reprint author), San Jose State Univ, San Jose, CA 95192 USA.; Hamill, P (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM patrick.hamill@sjsu.edu
NR 60
TC 0
Z9 0
U1 8
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 140
BP 213
EP 233
DI 10.1016/j.atmosenv.2016.06.002
PG 21
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200020
ER
PT J
AU Creamean, JM
White, AB
Minnis, P
Palikonda, R
Spangenberg, DA
Prather, KA
AF Creamean, Jessie M.
White, Allen B.
Minnis, Patrick
Palikonda, Rabindra
Spangenberg, Douglas A.
Prather, Kimberly A.
TI The relationships between insoluble precipitation residues, clouds, and
precipitation over California's southern Sierra Nevada during winter
storms
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol-cloud-precipitation interactions; Ice nucleation; Cloud
glaciation; Sierra nevada
ID SEEDER-FEEDER MECHANISM; MINERAL DUST PARTICLES; MIXED-PHASE CLOUDS;
ICE-NUCLEATION; NORTHERN CALIFORNIA; ATMOSPHERIC RIVERS; OROGRAPHIC
PRECIPITATION; AQUEOUS SAMPLES; ASIAN AEROSOLS; BARRIER JETS
AB Ice formation in orographic mixed -phase clouds can enhance precipitation and depends on the type of aerosols that serve as ice nucleating particles (INPs). The resulting precipitation from these clouds is a viable source of water, especially for regions such as the California Sierra Nevada. Thus, a better understanding of the sources of INPs that impact orographic clouds is important for assessing water availability in California. This study presents a multi -site, multi -year analysis of single -particle insoluble residues in precipitation samples that likely influenced cloud ice and precipitation formation above Yosemite National Park. Dust and biological particles represented the dominant fraction of the residues (64% on average). Cloud glaciation, determined using satellite observations, not only depended on high cloud tops (>5.9 km) and low temperatures (<-23 degrees C), but also on the presence of what were likely dust and biological INPs. The greatest prevalence of ice -phase clouds occurred in conjunction with biologically -rich residues and mineral dust rich in calcium, followed by iron and aluminosilicates. Dust and biological particles are known to be efficient INPs, thus these residues likely influenced ice formation in clouds above the sites and subsequent precipitation quantities reaching the surface during events with similar meteorology. The goal of this study is to use precipitation chemistry information to gain a better understanding of the potential sources of INPs in the south-central Sierra Nevada, where cloud -aerosol precipitation interactions are poorly understood and where mixed -phase orographic clouds represent a key element in the generation of precipitation and thus the water supply in California. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Creamean, Jessie M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Creamean, Jessie M.; White, Allen B.] NOAA, Earth Syst Res Lab, Div Phys Sci, Boulder, CO USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Palikonda, Rabindra; Spangenberg, Douglas A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Prather, Kimberly A.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Prather, Kimberly A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Creamean, JM (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway,R-PSD2, Boulder, CO 80305 USA.
EM jessie.creamean@noaa.gov
RI Prather, Kimberly/A-3892-2008;
OI Prather, Kimberly/0000-0003-3048-9890; Creamean,
Jessie/0000-0003-3819-5600
FU National Research Council Research Associate Program
[EA133F-10-CN-0187]; NASA Modeling, Analysis, and Prediction Program;
DOE ARM Program
FX The authors would like to acknowledge the staff at the National Park
Service at Yosemite National Park for sample collection, including Katy
Warner, who organized the collection protocols, Rebecca Rising, and Rob
and Laura Pilewski. Ryan Spackman (NOAH/Science and Technology
Corporation) and Daniel Murphy (NOAH) provided insightful feedback. We
would also like to acknowledge the California Nevada River Forecast
Center (CNRFC) and DWR for providing the HADS data and CASTNET for
providing the meteorological measurements at YOS. The GPS WCR site data
was courtesy of the Plate Boundary Observatory (PBO) network operated by
UNAVCO. Thanks to Chris Yost for providing the satellite validation
results. Jessie Creamean was partially supported by the National
Research Council Research Associate Program (contract number
EA133F-10-CN-0187). Patrick Minnis, Rabindra Palikonda, and Doug
Spangenberg were supported by the NASA Modeling, Analysis, and
Prediction Program and DOE ARM Program. Data presented in the manuscript
tables and figures are available by email request to the corresponding
author.
NR 91
TC 1
Z9 1
U1 14
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 140
BP 298
EP 310
DI 10.1016/j.atmosenv.2016.06.016
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200026
ER
PT J
AU Nyhan, M
Sobolevsky, S
Kang, CG
Robinson, P
Corti, A
Szell, M
Streets, D
Lu, ZF
Britter, R
Barrett, SRH
Ratti, C
AF Nyhan, Marguerite
Sobolevsky, Stanislav
Kang, Chaogui
Robinson, Prudence
Corti, Andrea
Szell, Michael
Streets, David
Lu, Zifeng
Britter, Rex
Barrett, Steven R. H.
Ratti, Carlo
TI Predicting vehicular emissions in high spatial resolution using
pervasively measured transportation data and microscopic emission's
model
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; Transportation; Emissions; Microscopic emissions model;
Microscopic vehicle movement
ID AIR-POLLUTION; LOS-ANGELES; VEHICLE; MORTALITY; CITIES; VARIABILITY;
REDUCTION; EVOLUTION; NETWORKS; QUALITY
AB Air pollution related to traffic emissions pose an especially significant problem in cities; this is due to its adverse impact on human health and well-being. Previous studies which have aimed to quantify emissions from the transportation sector have been limited by either simulated or coarsely resolved traffic volume data. Emissions inventories form the basis of urban pollution models, therefore in this study, Global Positioning System (GPS) trajectory data from a taxi fleet of over 15,000 vehicles were analyzed with the aim of predicting air pollution emissions for Singapore. This novel approach enabled the quantification of instantaneous drive cycle parameters in high spatio-temporal resolution, which provided the basis for a microscopic emissions model. Carbon dioxide (CO2), nitrogen oxides (NOx), volatile organic compounds (VOCs) and particulate matter (PM) emissions were thus estimated. Highly localized areas of elevated emissions levels were identified, with a spatio-temporal precision not possible with previously used methods for estimating emissions. Relatively higher emissions areas were mainly concentrated in a few districts that were the Singapore Downtown Core area, to the north of the central urban region and to the east of it. Daily emissions quantified for the total motor vehicle population of Singapore were found to be comparable to another emissions dataset Results demonstrated that high resolution spatio-temporal vehicle traces detected using GPS in large taxi fleets could be used to infer highly localized areas of elevated acceleration and air pollution emissions in cities, and may become a complement to traditional emission estimates, especially in emerging cities and countries where reliable fine-grained urban air quality data is not easily available. This is the first study of its kind to investigate measured microscopic vehicle movement in tandem with microscopic emissions modeling for a substantial study domain. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Nyhan, Marguerite; Robinson, Prudence; Britter, Rex; Ratti, Carlo] MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Sobolevsky, Stanislav] NYU, Ctr Urban Sci & Progress, New York, NY USA.
[Kang, Chaogui] Wuhan Univ, Wuhan, Hubei, Peoples R China.
[Corti, Andrea] Politecn Milan, 32 Piazza Leonardo da Vinci, Milan, Italy.
[Szell, Michael] Northeastern Univ, Dept Phys, Ctr Complex Network Res, Boston, MA 02115 USA.
[Streets, David; Lu, Zifeng] NASA, Argonne Natl Lab, Lemont, IL USA.
[Barrett, Steven R. H.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
RP Nyhan, M (reprint author), MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mnyhan@mit.edu
OI Kang, Chaogui/0000-0002-0122-9419
FU MIT SENSEable City Lab Consortium; Singapore-MIT Alliance for Research &
Technology program
FX All the authors wish to thank the MIT SENSEable City Lab Consortium and
the Singapore-MIT Alliance for Research & Technology program for
supporting the research. M. Nyhan would like to thank Fulbright and the
Irish Environmental Protection Agency. The authors would also like to
acknowledge Dr. Luc Int. Panis for providing advice on some modeling
aspects of the study.
NR 68
TC 1
Z9 1
U1 30
U2 43
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2016
VL 140
BP 352
EP 363
DI 10.1016/j.atmosenv.2016.06.018
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200031
ER
PT J
AU Villac, BF
Anderson, RL
Pini, AJ
AF Villac, Benjamin F.
Anderson, Rodney L.
Pini, Alex J.
TI Computer Aided Ballistic Orbit Classification Around Small Bodies
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Article
DE Trajectory design; Periodic orbits; Clustering; Data mining; Asteroid
missions
ID INVARIANT-MANIFOLDS; TRAJECTORY DESIGN; RESONANCE; TRANSFERS; VESTA
AB Orbital dynamics around small bodies are as varied as the shapes and dynamical states of these bodies. While various classes of orbits have been analyzed in detail, the global overview of relevant ballistic orbits at particular bodies is not easily computed or organized. Yet, correctly categorizing these orbits will ease their future use in the overall trajectory design process. This paper overviews methods that have been used to organize orbits, focusing on periodic orbits in particular, and introduces new methods based on clustering approaches.
C1 [Villac, Benjamin F.] Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA.
[Anderson, Rodney L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA.
[Pini, Alex J.] NASA, GSFC, Ai Solut Inc, B28 N278, Greenbelt, MD 20771 USA.
RP Villac, BF (reprint author), Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA.
EM benjamin.villac@ai-solutions.com
FU AMMOS technology development task
FX This research has been sponsored by the AMMOS technology development
task. A portion of the research presented in this paper has been carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 60
TC 0
Z9 0
U1 23
U2 23
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0021-9142
EI 2195-0571
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD SEP
PY 2016
VL 63
IS 3
BP 175
EP 205
DI 10.1007/s40295-016-0089-x
PG 31
WC Engineering, Aerospace
SC Engineering
GA DR7SW
UT WOS:000380101000001
ER
PT J
AU Stickle, WB
Lindeberg, M
Rice, SD
Munley, K
Reed, V
AF Stickle, William B.
Lindeberg, Mandy
Rice, Stanley D.
Munley, Kathleen
Reed, Victoria
TI Seasonal changes in the thermal regime and gastropod tolerance to
temperature and desiccation stress in the rocky intertidal zone in
Southeast Alaska
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Thermal regime; Temperature probes; Vertical gastropod zonation;
Desiccation tolerance; Temperature tolerance
ID HEAT-SHOCK RESPONSE; CLIMATE-CHANGE; PHYSIOLOGICAL ECOLOGY; GENUS
PETROLISTHES; VERTICAL ZONATION; PORCELAIN CRABS; LIMITS; ACCLIMATION;
PATTERNS; TEGULA
AB Low tide emersion of intertidal fauna in the inside passage from Puget Sound, WA to Skagway, AK produces more extreme emersion temperatures than on the outer continental coastline because the timing of low tides increases the potential for summer high temperatures and winter low temperatures. This study documents seasonal changes in water/aerial temperatures at different tidal heights in 2007-2008 and the summer of 2015 and reports the high emersion temperature (5 h) and desiccation tolerance of three species of rocky shore gastropods. Vertical transects of probes were deployed at Bridget Cove at +5.0 m (above the tidal range), +3.5, +2.5 m, +1.5 m and 0 m. Two additional probes were partially buried at +1.5 m; burial ameliorated freezing temperatures. Duration of emersion increased with intertidal height and was of longer duration at +3.5 m during Neap tides and at +1.5 and 0 m during Spring tides. Monthly measures of temperature were: average temperature, monthly maximum, average daily monthly maximum, average daily monthly minimum, and monthly minimum. Monthly maximum air temperature increased with tidal height. Winter average daily monthly minimum fell below 0 degrees C at the +3.5, +2.5, and +1.5 m tidal heights for the aerially exposed probes. The number of days when emersion temperature fell below 0 degrees C increased with intertidal height as did the number of hours per day. High temperature emersion tolerance of Nucella lamellosa, Nucella lima and Littorina sitkana varied directly with their intertidal range but their desiccation tolerance did not suggesting that desiccation is not an abiotic stressor in this temperate rain forest intertidal zone. The LT50 temperature (5 h) was considerably above recorded monthly maximum temperatures in the vertical range of N. lamellosa and L. sitkana but the LT50 of N. lima was very near the maximum monthly temperature at +2.5 m. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Stickle, William B.; Munley, Kathleen] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Lindeberg, Mandy; Rice, Stanley D.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA.
[Reed, Victoria] Louisiana State Univ, Div Comp Sci & Engn, Baton Rouge, LA 70803 USA.
RP Stickle, WB (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
EM zostic@lsu.edu
NR 39
TC 1
Z9 1
U1 30
U2 58
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD SEP
PY 2016
VL 482
BP 56
EP 63
DI 10.1016/j.jembe.2016.04.011
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA DQ7EW
UT WOS:000379370700006
ER
PT J
AU Babcock, C
Finley, AO
Cook, BD
Weiskittel, A
Woodall, CW
AF Babcock, Chad
Finley, Andrew O.
Cook, Bruce D.
Weiskittel, Aaron
Woodall, Christopher W.
TI Modeling forest biomass and growth: Coupling long-term inventory and
LiDAR data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE LiDAR; Forest biomass; Biomass growth; Temporal misalignment; Long-term
forest inventory; Bayesian hierarchical models; Markov Chain Monte
Carlo; Gaussian process; Geospatial
ID ABOVEGROUND BIOMASS; CANOPY HEIGHT; CARBON; AIRBORNE; REGRESSION;
VARIABLES; COMPLEX; MISSION; PLOTS
AB Combining spatially-explicit long-term forest inventory and remotely sensed information from Light Detection and Ranging (LiDAR) datasets through statistical models can be a powerful tool for predicting and mapping above-ground biomass (AGB) at a range of geographic scales. We present and examine a novel modeling approach to improve prediction of AGB and estimate AGB growth using LiDAR data. The proposed model accommodates temporal misalignment between field measurements and remotely sensed data a problem pervasive in such settings by including multiple time-indexed measurements at plot locations to estimate AGB growth. We pursue a Bayesian modeling framework that allows for appropriately complex parameter associations and uncertainty propagation through to prediction. Specifically, we identify a space-varying coefficients model to predict and map AGB and its associated growth simultaneously. The proposed model is assessed using LiDAR data acquired from NASA Goddard's LiDAR, Hyper-spectral & Thermal imager and field inventory data from the Penobscot Experimental Forest in Bradley, Maine. The proposed model outperformed the time-invariant counterpart models in predictive performance as indicated by a substantial reduction in root mean squared error. The proposed model adequately accounts for temporal misalignment through the estimation of forest AGB growth and accommodates residual spatial dependence. Results from this analysis suggest that future AGB models informed using remotely sensed data, such as LiDAR, may be improved by adapting traditional modeling frameworks to account for temporal misalignment and spatial dependence using random effects. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Babcock, Chad] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
[Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA.
[Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20742 USA.
[Weiskittel, Aaron] Univ Maine, Sch Forest Resources, Orono, ME 04469 USA.
[Woodall, Christopher W.] US Forest Serv, USDA, No Res Stn, Forest Inventory & Anal Program, 1992 Folwell Ave, St Paul, MN 55114 USA.
RP Babcock, C (reprint author), Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
OI Babcock, Chad/0000-0001-9597-4462
FU U.S. Forest Service [USFS 15-JV-11242307-116]; National Science
Foundation (NSF) [DMS-1513481, EF-1137309, EF-1241874, EF-1253225]; NASA
Carbon Monitoring System grants
FX Data for this study were provided by a unit of the Northern Research
Station, U.S. Forest Service, located at the Penobscot Experimental
Forest in Maine. Significant funding for collection of these data was
provided by the U.S. Forest Service (USFS 15-JV-11242307-116). Andrew
Finley was supported by National Science Foundation (NSF) DMS-1513481,
EF-1137309, EF-1241874, and EF-1253225, as well as NASA Carbon
Monitoring System grants.
NR 52
TC 0
Z9 0
U1 29
U2 84
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 1
PY 2016
VL 182
BP 1
EP 12
DI 10.1016/j.rse.2016.04.014
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700001
ER
PT J
AU Huesca, M
Garcia, M
Roth, KL
Casas, A
Ustin, SL
AF Huesca, Margarita
Garcia, Mariano
Roth, Keely L.
Casas, Angeles
Ustin, Susan L.
TI Canopy structural attributes derived from AVIRIS imaging spectroscopy
data in a mixed broadleaf/conifer forest
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Canopy structure; AVIRIS; LiDAR; Random forest; Structural types
ID SPECTRAL MIXTURE ANALYSIS; REMOTE-SENSING DATA; VEGETATION INDEXES;
HYPERSPECTRAL DATA; AIRBORNE LIDAR; WATER-CONTENT; NITROGEN-CONTENT;
ABOVEGROUND BIOMASS; SPATIAL-PATTERNS; LANDSAT IMAGERY
AB There is a well-established need within the remote sensing community for improved estimation and understanding of canopy structure and its influence on the retrieval of leaf biochemical properties. The main goal of this research was to assess the potential of optical spectral information from NASA's Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) to discriminate different canopy structural types. In the first phase, we assessed the relationships between optical metrics and canopy structural parameters obtained from LiDAR in terms of different canopy structural attributes (biomass (i.e., area under Vegetation Vertical Profile, VVPint), canopy height and vegetation complexity). Secondly, we identified and classified different "canopy structural types" by integrating several structural traits using Random Forests (RF). The study area is a heterogeneous forest in Sierra National Forest in California (USA). AVIRIS optical properties were analyzed by means of several sets of variables, including single narrow band reflectance and 1st derivative, sub-pixel cover fractions, narrow-band indices, spectral absorption features, optimized normalized difference indices and Principal Component Analysis (PCA) components. Our results demonstrate that optical data contain structural information that can be retrieved. The first principal component, used as a proxy for albedo, was the most strongly correlated optical metric with vegetation complexity, and it also correlated well with biomass (VVPint) and height. In conifer forests, the shade fraction was especially correlated to vegetation complexity, while water-sensitive optical metrics had high correlations with biomass (VVPint). Single spectral band analysis results showed that correlations differ in magnitude and in direction, across the spectrum and by vegetation type and structural variable. This research illustrates the potential of AVIRIS to analyze canopy structure and to distinguish several structural types in a heterogeneous forest. Furthermore, RF using optical metrics derived from AVIRIS proved to be a powerful technique to generate maps of structural attributes. The results emphasize the importance of using the whole optical spectrum, since all spectral regions contributed to canopy structure assessment (C) 2016 Elsevier Inc. All rights reserved.
C1 [Huesca, Margarita; Roth, Keely L.; Casas, Angeles; Ustin, Susan L.] Univ Calif Davis, CSTARS, Land Air & Water Resources Dept, Davis, CA 95616 USA.
[Garcia, Mariano] Univ Leicester, Ctr Landscape & Climate Res, Leicester LE1 7RH, Leics, England.
[Garcia, Mariano] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Huesca, M (reprint author), Univ Calif Davis, CSTARS, Davis, CA 95616 USA.
EM mhuescamartinez@ucdavis.edu
FU HyspIRI Planning Mission (NASA Grant) [NNX12AP87G]; Marie Curie IOF
(ForeStMap - 3D Forest Structure Monitoring and Mapping) [629376]
FX This research was conducted within the framework of the HyspIRI Planning
Mission (NASA Grant # NNX12AP87G). Mariano Garcia is supported by the
Marie Curie IOF (ForeStMap - 3D Forest Structure Monitoring and Mapping,
Project Reference: 629376). The contents on this paper reflect only the
authors' views and not the views of the European Commission. I would
like to thank NEON for providing the LiDAR data and the NASA JPL AVIRIS
team for collecting and preprocessing the hyperspectral data. I would
also thank the anonymous reviewers for their help in improving the
manuscript.
NR 129
TC 3
Z9 3
U1 21
U2 40
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 1
PY 2016
VL 182
BP 208
EP 226
DI 10.1016/j.rse.2016.04.020
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700016
ER
PT J
AU Malakar, NK
Hulley, GC
AF Malakar, Nabin K.
Hulley, Glynn C.
TI A water vapor scaling model for improved land surface temperature and
emissivity separation of MODIS thermal infrared data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS; Land surface temperature; Atmospheric correction; Thermal
infrared; Emissivity; Validation; Infrared image sensors; Remote sensing
ID ATMOSPHERIC CORRECTION; SOIL RESPIRATION; ENERGY-BALANCE; AVHRR DATA;
ASTER; ALGORITHM; PRODUCTS; VALIDATION; RADIOMETER; SATELLITE
AB We present an improved water vapor scaling (WVS) model for atmospherically correcting MODIS thermal infrared (TIR) bands in the temperature emissivity separation (TES) algorithm. TES is used to retrieve the land surface temperature and emissivity (LST&E) from MODIS TIR bands 29, 31, and 32. The WVS model improves the accuracy of the atmospheric correction parameters in TES on a band-by-band and pixel-by-pixel basis. We used global atmospheric radiosondes profiles to generate view angle and day-night-dependent WVS coefficients that are valid for all MODIS scan angles up to 65. We demonstrate the effects of applying the improved WVS model on the retrieval accuracy of MODIS-TES (MODTES) LST&E using a case study for a granule over the southwest USA during very warm and moist monsoonal atmospheric conditions. Furthermore, a comprehensive validation of the MODTES LST&E retrieval was performed over two sites at the quartz-rich Algodones Dunes in California and a grassland site in Texas, USA using three full years of MODIS Aqua data. Results from the case study showed that absolute errors in the emissivity retrieval for the three MODIS TIR bands were reduced on average from 1.4% to 0.4% when applying the WVS method. A Radiance-based method was used to validate the MODTES LST retrievals for and the results showed that application of the WVS method with the MODTES algorithm led to significant reduction in both bias and root mean square error (RMSE) of the LST retrievals at both sites. When the WVS model was applied, LST RMSE's were reduced on average from 1.3 K to 1.0 K at the Algodones Dunes site, and from 1.2 K to 0.7 K at the Texas Grassland site. This study demonstrated that the WVS atmospheric correction model is critical for retrieving MODTES LST with <1 K accuracy and emissivity with <1% consistently for a wide range of challenging atmospheric conditions and land surface types. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Malakar, Nabin K.; Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Malakar, NK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Nabin.K.Malakar@jpl.nasa.gov
OI Malakar, Nabin/0000-0002-4816-6304
FU NASA ROSES grant [NRA NNH13ZDA001N]
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
study is supported by the NASA ROSES 2013 grant (NRA NNH13ZDA001N).
NR 53
TC 1
Z9 1
U1 16
U2 29
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 1
PY 2016
VL 182
BP 252
EP 264
DI 10.1016/j.rse.2016.04.023
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700018
ER
PT J
AU Cho, Y
Sugita, S
Miura, YN
Okazaki, R
Iwata, N
Morota, T
Kameda, S
AF Cho, Yuichiro
Sugita, Seiji
Miura, Yayoi N.
Okazaki, Ryuji
Iwata, Naoyoshi
Morota, Tomokatsu
Kameda, Shingo
TI An in-situ K-Ar isochron dating method for planetary landers using a
spot-by-spot laser-ablation technique
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE In-situ geochronology; K-Ar dating; Planetary missions; Laser-induced
breakdown spectroscopy; Noble gas mass spectrometry
ID INNER SOLAR-SYSTEM; LUNAR CATACLYSM; GALE CRATER; MARS; CHRONOLOGY;
ORIGIN; AGES; MASS; GEOCHRONOLOGY; STRATIGRAPHY
AB Age is essential information for interpreting the geologic record on planetary surfaces. Although crater counting has been widely used to estimate the planetary surface ages, crater chronology in the inner solar system is largely built on radiometric age data from limited sites on the Moon. This has resulted in major uncertainty in planetary chronology. Because opportunities for sample-return missions are limited, in-situ geochronology measurements from one-way lander/rover missions are extremely valuable. Here we developed an in-situ isochron-based dating method using the K-Ar system, with K and Ar in a single rock sample extracted locally by laser ablation and measured using laser-induced breakdown spectroscopy (LIBS) and a quadrupole mass spectrometer (QMS), respectively. We built an experimental system combining flight equivalent instruments and measured K-Ar ages for mineral samples with known ages (similar to 1.8 Ga) and K contents (1-8 wt%); we achieved precision of 20% except for a mineral with low mechanical strength. Furthermore, validation measurements with two natural rocks (gneiss slabs) obtained K-Ar isochron ages and initial Ar-40 consistent with known values for both cases. This result supports that our LIBS-MS approach can derive both isochron ages and contributions of non-in situ radiogenic Ar-40 from natural rocks. Error assessments suggest that the absolute ages of key geologic events including the Noachian/Hesperian- and the Hesperian/Amazonian-transition can be dated with 10-20% errors for a rock containing similar to 1 wt% K2O, greatly reducing the uncertainty of current crater chronology models on Mars. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Cho, Yuichiro; Sugita, Seiji] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Cho, Yuichiro; Kameda, Shingo] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
[Miura, Yayoi N.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, 1-1-1 Yayoi, Tokyo 1130032, Japan.
[Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan.
[Iwata, Naoyoshi] Yamagata Univ, Dept Earth & Environm Sci, 1-4-12 Kojirakawa, Yamagata 9908560, Japan.
[Morota, Tomokatsu] Nagoya Univ, Dept Earth & Planetary Sci, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Cho, Yuichiro] NASA, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
RP Cho, Y (reprint author), Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
EM cho@rikkyo.ac.jp
RI Iwata, Naoyoshi/B-7554-2008
OI Iwata, Naoyoshi/0000-0002-0017-9130
FU Institute of Space and Aeronautical Science (ISAS)/Japan Aerospace
Exploration Agency (JAXA); Japan Society for the Promotion of Science
(JSPS) [26247092]; JSPS [15K17796]
FX The authors are grateful to two anonymous reviewers whose careful
reading of this paper led to a number of significant improvements. This
study was supported by funds from the Institute of Space and
Aeronautical Science (ISAS)/Japan Aerospace Exploration Agency (JAXA)
and by Japan Society for the Promotion of Science (JSPS) Grant-in-Aid in
Scientific Research Grant Number 26247092. Y. Cho was supported by JSPS
Grant-in-Aid for Young Scientists (B.) Grant Number 15K17796. The
authors thank Keisuke Nagao of the University of Tokyo for providing the
mineral samples. We would like to thank Takahiko Yagi, Ehime University,
and Hirotada Goto, the University of Tokyo for assistance in making the
pellet samples with a cubic press at the Institute of Solid State
Physics, the University of Tokyo. The authors thank Naoto Ishikawa of
Kyoto University and the 41st and 42nd Japanese Antarctic Research
Expedition Program for acquiring the gneiss samples. Asako Takamasa in
Japan Agency for Marine-Earth Science and Technology (JAMSTEC) is
acknowledged for separating biotites from the gneiss rocks. We are
thankful to Kenji Mibe at Earthquake Research Institute, the University
of Tokyo, for preparing a basaltic glass sample used for Ar
measurements. All data and programs used for producing the results in
this paper are available from the lead author on request
(cho@rikkyo.ac.jp).
NR 59
TC 1
Z9 1
U1 10
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2016
VL 128
BP 14
EP 29
DI 10.1016/j.pss.2016.05.004
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DQ1LA
UT WOS:000378961300002
ER
PT J
AU Guo, JP
Liu, H
Wang, F
Huang, JF
Xia, F
Lou, MY
Wu, YR
Jiang, JH
Xie, T
Zhaxi, YZ
Yung, YL
AF Guo, Jianping
Liu, Huan
Wang, Fu
Huang, Jingfeng
Xia, Feng
Lou, Mengyun
Wu, Yerong
Jiang, Jonathan H.
Xie, Tao
Zhaxi, Yangzong
Yung, Yuk L.
TI Three-dimensional structure of aerosol in China: A perspective from
multi-satellite observations
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE CALIOP; Dust; Smoke; Frequency of occurrence; China
ID AIR-POLLUTION; INDUCED VARIABILITY; EASTERN CHINA; NORTH-AMERICA; WARM
CLOUDS; TRANSPORT; PRECIPITATION; DUST; ATMOSPHERE; ATLANTIC
AB Using eight years (2006-2014) of passive (MODIS/Aqua and OMI/Aura) and active (CALIOP/CALIPSO) satellite measurements of aerosols, we yield a three-dimensional (3D) distribution of the frequency of occurrence (FoO) of aerosols over China. As an indicator of the vertical heterogeneity of aerosol layers detected by CALIOP, two types of Most Probable Height (MPH), including MPH_FoO and MPH_AOD, are deduced. The FoO of "Total Aerosol" reveals significant geographical dependence. Eastern China showed much stronger aerosol FoD than northwestern China. The FoO vertical structures of aerosol layer are strongly dependent on altitudes. Among the eight typical ROls analyzed, aerosol layers over the Gobi Desert have the largest occurrence probability located at an altitude as high as 2.83 km, as compared to 126 km over Beijing-Tianjin-Hebei. The diurnal variation (nighttime-daytime) in MPH_AOD varies from an altitude as low as 0.07 km over the Sichuan basin to 0.27 km over the Gobi Desert, whereas the magnitude of the diurnal variation in terms of MPH_AOD is six times as large as the MPH_FoO, mostly attributable to the day/night lidar SNR difference. Also, the 3D distribution of dust and smoke aerosols was presented. The multi-sensor synergized 3D observations of dust aerosols, frequently observed in the zonal belt of 38 degrees N-45 degrees N, is markedly different from that of smoke aerosols that are predominantly located in the eastern and southern parts. The 3D FoO distribution of dust indicates a west-to-east passageway of dust originating from the westernmost Taklimakan Desert all the way to North China Plain (NCP). The findings from the multi-sensor synergetic observations greatly improved our understanding on the long-range aerosol dispersion, transport and passageway over China. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Guo, Jianping; Liu, Huan; Xia, Feng; Lou, Mengyun] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
[Wang, Fu] China Meteorol Adm, Natl Satellite Meteorol Ctr, Beijing 100081, Peoples R China.
[Huang, Jingfeng] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Wu, Yerong] Delft Univ Technol, Geosci & Remote Sensing Fac Civil Engn & Geosci, NL-2628 CN Delft, Netherlands.
[Jiang, Jonathan H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Xie, Tao] Guangzhou MapUniverse Technol Co Ltd, Guangzhou 510070, Guangdong, Peoples R China.
[Guo, Jianping; Zhaxi, Yangzong] Tibetan Inst Atmospher Environm & Sci, Lhasa 850000, Peoples R China.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Guo, JP (reprint author), Chinese Acad Meteorol Sci, 46 Zhong Guan Cun South Ave, Beijing 100081, Peoples R China.
EM jpguo@camscma.cn
RI Huang, Jingfeng/D-7336-2012
OI Huang, Jingfeng/0000-0002-8779-2922
FU Ministry of Science and Technology of the People's Republic of China
[2014BAC16B01]; Natural Science Foundation of China [91544217, 41471301,
41171294]; Chinese Academy of Meteorological Sciences [2014R18];
Guangdong Provincial Science and Technology Plan Projects
[2014A010101151]; NASA; California Institute of Technology
FX This work was carried out under the auspices of the Ministry of Science
and Technology of the People's Republic of China (Grant no.
2014BAC16B01), the Natural Science Foundation of China (Grant nos.
91544217, 41471301 and 41171294), the Chinese Academy of Meteorological
Sciences (Grant no. 2014R18), and Guangdong Provincial Science and
Technology Plan Projects (Grant no. 2014A010101151). The MODIS AOD data
used in this study were also, acquired as part of the NASA's Earth-Sun
System Division and archived and distributed by the Goddard Earth
Sciences (GES) Data and Information Services Center (DISC) Distributed
Active Archive Center (DAAC). Authors JHJ and YY thank the support by
the NASA sponsored Jet Propulsion Laboratory and by the California
Institute of Technology.
NR 52
TC 3
Z9 3
U1 13
U2 26
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD SEP 1
PY 2016
VL 178
BP 580
EP 589
DI 10.1016/j.atmosres.2016.05.010
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2YY
UT WOS:000378360700049
ER
PT J
AU Langseth, BJ
Schueller, AM
Shertzer, KW
Craig, JK
Smith, JW
AF Langseth, Brian J.
Schueller, Amy M.
Shertzer, Kyle W.
Craig, J. Kevin
Smith, Joseph W.
TI Management implications of temporally and spatially varying catchability
for the Gulf of Mexico menhaden fishery
SO FISHERIES RESEARCH
LA English
DT Article
DE Catchability; Hypoxia; Spatio-temporal variation; Stock assessment; Gulf
menhaden
ID STOCK ASSESSMENT MODELS; BROWN SHRIMP; HYPOXIA; PERFORMANCE; ABUNDANCE;
YIELD; AREA
AB Catchability relates fishing effort to fishing mortality, and is an important component in fishery stock assessment models. Mis-specifying catchability can lead to inaccurate estimation of model parameters and bias in the determination of stock status. The Gulf of Mexico has one of the largest seasonal occurrences of hypoxia in the world and it overlaps in time and space with the Gulf menhaden Brevoortia patronus fishery, potentially leading to temporal and spatial patterns in stock distribution and thus catchability. These patterns are not currently modeled in the Gulf menhaden stock assessment. To better understand the implications of spatial and temporal patterns in catchability due to hypoxia, we constructed an operating model of Gulf menhaden fishery dynamics under various assumptions of spatial coverages and temporal patterns, and used the output from the operating model as input into estimation models with alternative approaches on modeling catchability. Under the most extreme assumptions about the spatial coverage and magnitude of variation in catchability, median absolute error in estimates of fishing mortality and spawning stock reference points (F-30% and S-30%) was 73% and 29%, respectively, and median absolute error in estimates of fishing mortality and spawning stock based stock status was 23% and 79%, supporting the notion that errors in catchability are important. Under more reasonable assumptions, median absolute error declined to 20% and 2.9% for F-30% and S-30%, respectively, and to 3.8% and 2.4% for fishing mortality and spawning stock-based stock status, respectively. Modeling catchability as a random walk further reduced median absolute error to 5.0% for F-30% and 1.4% for S-30%, but slightly increased median absolute error for stock status indicators to 4.0% and 3.3%. Our results show generally that the spatial coverage, temporal pattern, and estimation approach of catchability affects the influence of mis-specifying catchability; and show specifically that the Gulf menhaden stock assessment is robust to the effects of hypoxia on catchability if assuming random-walk catchability. Published by Elsevier B.V.
C1 [Langseth, Brian J.; Schueller, Amy M.; Shertzer, Kyle W.; Craig, J. Kevin; Smith, Joseph W.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 101 Pivers Isl Rd, Beaufort, NC 28516 USA.
[Langseth, Brian J.] NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
RP Langseth, BJ (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM brian.langseth@noaa.gov
FU Fisheries and the Environment (FATE) Program of the National Oceanic and
Atmospheric Administration (NOAA)
FX We thank A. Yau and K. Siegfried, J. Thorson, and an anonymous reviewer
for contributions to previous drafts of the manuscript. This research
was supported by a grant from the Fisheries and the Environment (FATE)
Program of the National Oceanic and Atmospheric Administration (NOAA).
The views expressed herein are those of the authors and do not
necessarily reflect the view of NOAA or any of its subagencies.
NR 42
TC 0
Z9 0
U1 21
U2 25
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 SEP
PY 2016
VL 181
BP 186
EP 197
DI 10.1016/j.fishres.2016.04.013
PG 12
WC Fisheries
SC Fisheries
GA DP0LS
UT WOS:000378181900019
ER
PT J
AU Pajola, M
Rossato, S
Carter, J
Baratti, E
Pozzobon, R
Erculiani, MS
Coradini, M
McBride, K
AF Pajola, Maurizio
Rossato, Sandro
Carter, John
Baratti, Emanuele
Pozzobon, Riccardo
Erculiani, Marco Sergio
Coradini, Marcello
McBride, Karen
TI Eridania Basin: An ancient paleolake floor as the next landing site for
the Mars 2020 rover
SO ICARUS
LA English
DT Article
DE Mars, surface; Geological processes; Spectroscopy; Image processing;
Exobiology
ID ORBITER LASER ALTIMETER; EMISSION SPECTROMETER EXPERIMENT; LACUSTRINE
ENVIRONMENTS; PHYSICAL-PROPERTIES; THERMAL INERTIA; MARTIAN SURFACE;
GLOBAL SURVEYOR; MAADIM-VALLIS; CRATER LAKES; ORIGIN
AB The search for traces of past Martian life is directly connected to ancient paleolakes, where ponding water or low-energy water fluxes were present for long time intervals. The Eridania paleolakes system, located along the 180 meridian, is one of the largest lacustrine environments that were once present on Mars. Morphological features suggest that it was constituted by connected depressions filled by water to maximum depths of similar to 2400 m and a volume of at least 562,000 km(3). We focused our attention on the northern side of the Eridania Basin, where high-albedo, uneven patches of material characterized by the absence of dust are present. Based on OMEGA and CRISM orbital imaging spectroscopy data, a large clay-bearing unit has been identified there. In particular, a set of aqueous minerals in present in the stratigraphy, being visible through erosional windows in the first several tens of meters of the sedimentary sequence. Below this capping unit, a thin Al-rich clay stratum attributable to Al-smectite and/or kaolins is present. This overlies a Fe-rich clay stratum, attributable to the nontronite smectite. At the base of the mineralogic sequence a stratum that could be either a zeolite or more likely a hydrated sulfate is present. In addition, small deposits of alunite (a rare phase on Mars), and jarosite are here found at several locations. Such stratigraphy is interpreted as originating from a surface weathering process similar to terrestrial abiotic pedogenesis; nonetheless, possible exobiologic processes can be also invoked to explain it. NASA's Spirit rover landed on Gusev crater in 2004, near the mouth of the Ma'adim Vallis, which connects this crater with the considered paleolakes system. The Eridania site provides the unique opportunity to complete the measurements obtained in Gusev crater, while investigating the exposed mineralogical sequence in its depositionary setting. In addition, the extremely favorable landing parameters, such as elevation, slope, roughness, rock distribution, thermal inertia and dust coverage, support this location as a possible landing site for the NASA Mars 2020 rover. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pajola, Maurizio; Erculiani, Marco Sergio] Univ Padua, Ctr Studies & Act Space G Colombo, Via Venezia 15, I-35131 Padua, Italy.
[Rossato, Sandro; Pozzobon, Riccardo] Univ Padua, Geosci Dept, I-3513 Padua, Italy.
[Carter, John] Univ Paris 11, IAS, F-91405 Orsay, France.
[Baratti, Emanuele] Univ Bologna, Dept DICAM, Sch Civil Engn, I-40136 Bologna, Italy.
[Coradini, Marcello] European Space Agcy, F-75015 Paris, France.
[Coradini, Marcello] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[McBride, Karen] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
RP Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM maurizio.pajola@nasa.gov
OI Pajola, Maurizio/0000-0002-3144-1277; Coradini,
Marcello/0000-0002-1711-3197
NR 142
TC 0
Z9 0
U1 13
U2 24
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2016
VL 275
BP 163
EP 182
DI 10.1016/j.icarus.2016.03.029
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900012
ER
PT J
AU Meriggiola, R
Iess, L
Stiles, BW
Lunine, JI
Mitri, G
AF Meriggiola, Rachele
Iess, Luciano
Stiles, Bryan. W.
Lunine, Jonathan. I.
Mitri, Giuseppe
TI The rotational dynamics of Titan from Cassini RADAR images
SO ICARUS
LA English
DT Article
DE Titan, interior; Satellites, dynamics; Geophysics
ID INTERNAL STRUCTURE; GRAVITY-FIELD; OCEAN; TOPOGRAPHY; OBLIQUITY; STATE;
SHAPE; ICE
AB Between 2004 and 2009 the RADAR instrument of the Cassini mission provided 31 SAR images of Titan. We tracked the position of 160 surface landmarks as a function of time in order to monitor the rotational dynamics of Titan. We generated and processed RADAR observables using a least squares fit to determine the updated values of the rotational parameters. We provide a new rotational model of Titan, which includes updated values for spin pole location, spin rate, precession and nutation terms. The estimated pole location is compatible with the occupancy of a Cassini state 1. We found a synchronous value of the spin rate (22.57693 deg/day), compatible at a 3-sigma level with IAU predictions. The estimated obliquity is equal to 0.31, incompatible with the assumption of a rigid body with fully-damped pole and a moment of inertia factor of 0.34, as determined by gravity measurements. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Meriggiola, Rachele; Iess, Luciano] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy.
[Stiles, Bryan. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lunine, Jonathan. I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Mitri, Giuseppe] Univ Nantes, Lab Planetol & Geodynam Nantes, Nantes, France.
RP Meriggiola, R (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy.
EM rachele.meriggiola@uniromal.it
RI IESS, Luciano/F-4902-2011
OI IESS, Luciano/0000-0002-6230-5825
FU Cassini Project
FX We thank W. Jacobson and the Cassini Navigation Team (JPL) for the
provided support on the error source analysis. Support by the Cassini
Project is gratefully acknowledged. JIL is grateful for support from the
Cassini Project. A portion 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 33
TC 3
Z9 3
U1 2
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2016
VL 275
BP 183
EP 192
DI 10.1016/j.icarus.2016.01.019
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900013
ER
PT J
AU Gautier, T
Schmitz-Afonso, I
Touboul, D
Szopa, C
Buch, A
Carrasco, N
AF Gautier, Thomas
Schmitz-Afonso, Isabelle
Touboul, David
Szopa, Cyril
Buch, Arnaud
Carrasco, Nathalie
TI Development of HPLC-Orbitrap method for identification of N-bearing
molecules in complex organic material relevant to planetary environments
SO ICARUS
LA English
DT Article
DE Titan, atmosphere; Atmospheres, chemistry; Organic chemistry; Prebiotic
chemistry
ID TITANS THOLINS PRODUCTION; COMETARY ICE ANALOGS; MASS-SPECTROMETRY;
HEXAMETHYLENETETRAMINE HMT; PREBIOTIC CHEMISTRY; INTERSTELLAR ICE;
SOLID-STATE; PRODUCTS; MELAMINE; SPECTROSCOPY
AB Although the cassini Spacecraft and the Huygens Lander provided vast information about Titan atmospheric chemistry and the formation of its aerosols, the exact composition of these aerosols still remains unknown. A fruitful proxy to investigate these aerosols is the use of laboratory experiments that allow producing and studying analogs of Titan aerosol, the so-called tholins. Even when produced in the laboratory, unveiling the exact composition of the aerosol remains problematic due to the high complexity of the material. Numerous advances have been recently made using high-resolution mass spectrometry (HRMS) (Pernot et al. [2010] Anal. Chem. 82, 1371; Somogyi et al. [2012] Int. J. Mass Spectrom. 316-318, 157-163; Gautier et al. [2014] Earth Planet. Sci. Lett. 404, 33-42) that allowed the separation of isobaric compounds and a robust identification of chemical species composing tholins regarding their molecular formulae. Nevertheless isomeric species cannot be resolved by a simple mass measurement. We propose here an analysis of tholins by high performance liquid chromatography (HPLC) coupled to HRMS to unveil this isomeric ambiguity for some of the major tholins compounds. By comparing chromatograms obtained when analyzing tholins and chemical standards, we strictly identified seven molecules in our tholins samples: melamine, cyanoguanidine, 6-methyl-1,3,5-triazine-2,4-diamine, 2,4,6-triaminopyrimidine, 3-amino-1,2,4-triazole, 3,5-Dimethyl-1,2,4-triazole and 2,4-diamino-1,3,5-triazine. Several molecules, including hexamethylenetriamine (HMT) were not present at detectable levels in our sample. The use for the first time of a coupled HPLC-HRMS technique applied to tholins study demonstrated the interest of such a technique compared to single high-resolution mass spectrometry for the study of tholins composition. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Gautier, Thomas] NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Gautier, Thomas; Szopa, Cyril; Carrasco, Nathalie] Univ Paris 06, UVSQ Univ Paris Saclay, LATMOS IPSL, F-78280 Guyancourt, France.
[Schmitz-Afonso, Isabelle; Touboul, David] Univ Paris 11, ICSN, CNRS UPR 2301, 1 Ave Terrasse, F-91198 Gif Sur Yvette, France.
[Schmitz-Afonso, Isabelle] Normandie Univ, COBRA, UMR 6014, 1 Rue Tesniere, F-76821 Mont St Aignan, France.
[Schmitz-Afonso, Isabelle] Univ Rouen, INSA Rouen, CNRS, FR3038,IRCOF, 1 Rue Tesniere, F-76821 Mont St Aignan, France.
[Szopa, Cyril; Carrasco, Nathalie] Inst Univ France, 103 Bvd St Michel, F-75005 Paris, France.
[Buch, Arnaud] Ecole Cent Paris, LGPM, F-92295 Chatenay Malabry, France.
RP Gautier, T (reprint author), NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM thomas.j.gautier@nasa.gov
RI Carrasco, Nathalie/D-2365-2012; szopa, cyril/C-6865-2015
OI Carrasco, Nathalie/0000-0002-0596-6336; szopa, cyril/0000-0002-0090-4056
FU French Program National de Planetologie (PNP); European Research Council
(ERC Starting Grant PRIMCHEM) [636829]
FX The research presented in this paper was partially funded through the
French Program National de Planetologie (PNP). NC acknowledges the
European Research Council for their financial support (ERC Starting
Grant PRIMCHEM, Grant agreement no. 636829). TG acknowledges the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities.
NR 33
TC 0
Z9 0
U1 12
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 SEP 1
PY 2016
VL 275
BP 259
EP 266
DI 10.1016/j.icarus.2016.03.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900021
ER
PT J
AU Leon, JJD
Fryauf, DM
Cormia, RD
Zhang, MXM
Samuels, K
Williams, RS
Kobayashi, NP
AF Leon, Juan J. Diaz
Fryauf, David M.
Cormia, Robert D.
Zhang, Min-Xian Max
Samuels, Kathryn
Williams, R. Stanley
Kobayashi, Nobuhiko P.
TI Reflectometry-Ellipsometry Reveals Thickness, Growth Rate, and Phase
Composition in Oxidation of Copper
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE copper oxide; reflectometry; ellipsometry; memristor; volatile
conductive bridge
ID THIN-FILMS; NATIVE OXIDATION; SINGLE-CRYSTAL; OXIDE; SURFACES; KINETICS;
BULK; XPS
AB The oxidation of copper is a complicated process. Copper oxide develops two stable phases at room temperature and standard pressure (RTSP): cuprous oxide (Cu2O) and cupric oxide (CuO). Both phases:have different optical and electrical characteristics that make them interesting for applications such as solar cells or resistive switching devices. For a given application, it is necessary to selectively control oxide thickness and cupric/cuprous oxide phase volume fraction. The thickness and composition of a copper oxide film growing on the surface of copper widely depend on the characteristics of as-deposited copper. In this Research Article, two samples, copper films prepared by two different deposition techniques, electron-beam evaporation and, sputtering, were studied. As the core part of the study, the formation of the oxidized copper was analyzed routinely over a period of 253 days using spectroscopic polarized reflectometry-spectroscopic ellipsometry (RE). An effective medium approximation (EMA) model was used to fit the RE data. The RE measurements were complemented and validated by using X-ray photoelectron spectroscopy (XPS), atomic force microscopy (AFM) and X-ray diffraction (XRD). Our results show that the two samples oxidized under identical laboratory ambient conditions (RTSP, 87% average relative humidity) developed unique oxide films following an inverse-logarithmic growth rate with thickness and composition different from each other over time. Discussion is focused on the ability of RE to simultaneously extract thickness (i.e., growth rate) and composition of copper oxide films and on plausible physical mechanisms responsible for unique oxidation habits observed in the two copper samples. It appears that extended surface characteristics (i.e., surface roughness and grain boundaries) and preferential crystalline orientation of as deposited polycrystalline copper films control the growth kinetics of the copper oxide film. Analysis based on a noncontact and nondestructive measurement, such as RE, to extract key material parameters is beneficial for conveniently understanding the oxidation process that would ultimately enable copper oxide-based devices at manufacturing scales.
C1 [Leon, Juan J. Diaz; Fryauf, David M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Leon, Juan J. Diaz; Fryauf, David M.; 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.
[Cormia, Robert D.] Foothill Coll, Los Altos, CA 94022 USA.
[Zhang, Min-Xian Max; Samuels, Kathryn; Williams, R. Stanley] Hewlett Packard Labs, Palo Alto, CA 94304 USA.
RP Leon, JJD (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.; Leon, JJD (reprint author), Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jdiazleo@ucsc.edu
RI Williams, R. Stanley/A-8281-2009
OI Williams, R. Stanley/0000-0003-0213-4259
FU NSF [DMR-1126845]
FX We would like to acknowledge the Scott Oliver lab at the University of
California Santa Cruz for the work of Jesse Hauser in X-ray
diffractometry using a Rigaku SmartLab X-ray diffractometer, funded by
the NSF Major Research Instrument (MRI) Program under Grant DMR-1126845.
We would also like to thank Vince Crist (XPS international) for helpful
assistance in interpreting the XPS data.
NR 36
TC 0
Z9 0
U1 30
U2 30
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD AUG 31
PY 2016
VL 8
IS 34
BP 22337
EP 22344
DI 10.1021/acsami.6b06626
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA DU9CP
UT WOS:000382514100060
ER
PT J
AU Nedoluha, GE
Connor, BJ
Mooney, T
Barrett, JW
Parrish, A
Gomez, RM
Boyd, I
Allen, DR
Kotkamp, M
Kremser, S
Deshler, T
Newman, P
Santee, ML
AF Nedoluha, Gerald E.
Connor, Brian J.
Mooney, Thomas
Barrett, James W.
Parrish, Alan
Gomez, R. Michael
Boyd, Ian
Allen, Douglas R.
Kotkamp, Michael
Kremser, Stefanie
Deshler, Terry
Newman, Paul
Santee, Michelle L.
TI 20 years of ClO measurements in the Antarctic lower stratosphere
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID CHLORINE MONOXIDE; SPRING STRATOSPHERE; LOW ALTITUDES; OZONE;
REANALYSIS; SATELLITE; CHEMISTRY; CIO
AB We present 20 years (1996-2015) of austral springtime measurements of chlorine monoxide (ClO) over Antarctica from the Chlorine Oxide Experiment (ChlOE1) ground-based millimeter wave spectrometer at Scott Base, Antarctica, as well 12 years (2004-2015) of ClO measurements from the Aura Microwave Limb Sounder (MLS). From August onwards we observe a strong increase in lower stratospheric ClO, with a peak column amount usually occurring in early September. From mid-September onwards we observe a strong decrease in ClO. In order to study interannual differences, we focus on a 3-week period from 28 August to 17 September for each year and compare the average column ClO anomalies. These column ClO anomalies are shown to be highly correlated with the average ozone mass deficit for September and October of each year. We also show that anomalies in column ClO are strongly anti-correlated with 30 hPa temperature anomalies, both on a daily and an interannual timescale. Making use of this anti-correlation we calculate the linear dependence of the interannual variations in column ClO on interannual variations in temperature. By making use of this relationship, we can better estimate the underlying trend in the total chlorine (Cl-y = HCl + ClONO2 + HOCl + 2 x Cl-2 + 2 x Cl2O2 + ClO + Cl). The resultant trends in Cl-y, which determine the long-term trend in ClO, are estimated to be -0.5 +/- 0.2, -1.4 +/- 0.9, and -0.6 +/- 0.4% year(-1), for zonal MLS, Scott Base MLS (both 2004-2015), and ChlOE (1996-2015) respectively. These trends are within 1 sigma of trends in stratospheric Cl-y previously found at other latitudes. The decrease in ClO is consistent with the trend expected from regulations enacted under the Montreal Protocol.
C1 [Nedoluha, Gerald E.; Gomez, R. Michael; Allen, Douglas R.] Naval Res Lab, Washington, DC 20375 USA.
[Connor, Brian J.; Mooney, Thomas; Boyd, Ian] BC Sci Consulting LLC, Stony Brook, NY USA.
[Barrett, James W.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Parrish, Alan] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Kotkamp, Michael] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Kremser, Stefanie] Bodeker Sci, Alexandra, New Zealand.
[Deshler, Terry] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Newman, Paul] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nedoluha, GE (reprint author), Naval Res Lab, Washington, DC 20375 USA.
EM nedoluha@nrl.navy.mil
OI /0000-0002-3573-7083
FU NASA under the Upper Atmosphere Research Program; Naval Research
Laboratory; Office of Naval Research; National Aeronautics and Space
Administration
FX This project was funded by NASA under the Upper Atmosphere Research
Program, by the Naval Research Laboratory, and by the Office of Naval
Research. We would like to acknowledge the many Antarctica New Zealand
technicians who have supported the daily operation of ChlOE over two
decades of measurements. We also acknowledge the logistical support that
Antarctica New Zealand has supplied over this period. Work at the Jet
Propulsion Laboratory, California Institute of Technology, was carried
out under a contract with the National Aeronautics and Space
Administration. Sonde temperature data were collected under support from
the National Science Foundation.
NR 30
TC 1
Z9 1
U1 5
U2 5
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 30
PY 2016
VL 16
IS 16
BP 10725
EP 10734
DI 10.5194/acp-16-10725-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6EZ
UT WOS:000383743600002
ER
PT J
AU Dolant, C
Langlois, A
Montpetit, B
Brucker, L
Roy, A
Royer, A
AF Dolant, Caroline
Langlois, Alexandre
Montpetit, Benoit
Brucker, Ludovic
Roy, Alexandre
Royer, Alain
TI Development of a rain-on-snow detection algorithm using passive
microwave radiometry
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snow; passive microwave; rain-on-snow; extreme winter events
ID THERMAL-CONDUCTIVITY; ACTIVE LAYER; IMPACTS; TEMPERATURE; SVALBARD;
CLIMATE; EVENTS; MODEL; ICE
AB Currently observed climate warming in the Arctic has numerous consequences. Of particular relevance, the precipitation regime is modified where mixed and liquid precipitation can occur during the winter season leading to rain-on-snow (ROS) events. This phenomenon is responsible for ice crust formation, which has a significant impact on ecosystems (such as biological, hydrological, ecological and physical processes). The spatially and temporally sporadic nature of ROS events makes the phenomenon difficult to monitor using meteorological observations. This paper focuses on the detection of ROS events using passive microwave (PMW) data from a modified brightness temperature (T-B) gradient approach at 19 and 37GHz. The approach presented here was developed empirically for observed ROS events with coincident ground-based PMW measurements in Sherbrooke, Quebec, Canada. It was then tested in Nunavik, Quebec, with the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E). We obtained a detection accuracy of 57, 71 and 89% for ROS detection for three AMSR-E grid cells with a maximum error of 7% when considering all omissions and commissions with regard to the total number of AMSR-E passes throughout the winter period. Copyright (c) 2016 John Wiley & Sons, Ltd.
C1 [Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Roy, Alexandre; Royer, Alain] Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
[Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Royer, Alain] Ctr Etud Nord, Kuujjuarapik, PQ, Canada.
[Montpetit, Benoit] Environm Canada, Canadian Ice Serv, Ottawa, ON, Canada.
[Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA.
[Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA.
RP Dolant, C (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
EM caroline.dolant@USherbrooke.ca
RI Brucker, Ludovic/A-8029-2010
OI Brucker, Ludovic/0000-0001-7102-8084
FU Natural Sciences and Engineering Research Council of Canada (NSERC);
Centre for Northern Studies; EnviroNorth; Canadian Foundation for
Innovation (CFI)
FX Funding for this research was provided by the Natural Sciences and
Engineering Research Council of Canada (NSERC), the Centre for Northern
Studies, EnviroNorth and the Canadian Foundation for Innovation (CFI).
Thanks to the National Snow and Ice Data Center (NSIDC) for satellite
data access. The authors would also like to thank the Universite de
Sherbrooke and the Centre d'Applications et de Recherches en
TELedetection (CARTEL) for logistical and administrative support.
NR 46
TC 3
Z9 3
U1 10
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD AUG 30
PY 2016
VL 30
IS 18
BP 3184
EP 3196
DI 10.1002/hyp.10828
PG 13
WC Water Resources
SC Water Resources
GA DW2IU
UT WOS:000383466900006
ER
PT J
AU Bonnett, C
Troxel, MA
Hartley, W
Amara, A
Leistedt, B
Becker, MR
Bernstein, GM
Bridle, SL
Bruderer, C
Busha, MT
Kind, MC
Childress, MJ
Castander, FJ
Chang, C
Crocce, M
Davis, TM
Eifler, TF
Frieman, J
Gangkofner, C
Gaztanaga, E
Glazebrook, K
Gruen, D
Kacprzak, T
King, A
Kwan, J
Lahav, O
Lewis, G
Lidman, C
Lin, H
MacCrann, N
Miquel, R
O'Neill, CR
Palmese, A
Peiris, HV
Refregier, A
Rozo, E
Rykoff, ES
Sadeh, I
Sanchez, C
Sheldon, E
Uddin, S
Wechsler, RH
Zuntz, J
Abbott, T
Abdalla, FB
Allam, S
Armstrong, R
Banerji, M
Bauer, AH
Benoit-Levy, A
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Capozzi, D
Rosell, AC
Carretero, J
Cunha, CE
D'Andrea, CB
da Costa, LN
DePoy, DL
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Neto, AF
Fernandez, E
Flaugher, B
Fosalba, P
Gerdes, DW
Gruendl, RA
Honscheid, K
Jain, B
James, DJ
Jarvis, M
Kim, AG
Kuehn, K
Kuropatkin, N
Li, TS
Lima, M
Maia, MAG
March, M
Marshall, JL
Martini, P
Melchior, P
Miller, CJ
Neilsen, E
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Reil, K
Romer, AK
Roodman, A
Sako, M
Sanchez, E
Santiago, B
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Vikram, V
Walker, AR
AF Bonnett, C.
Troxel, M. A.
Hartley, W.
Amara, A.
Leistedt, B.
Becker, M. R.
Bernstein, G. M.
Bridle, S. L.
Bruderer, C.
Busha, M. T.
Kind, M. Carrasco
Childress, M. J.
Castander, F. J.
Chang, C.
Crocce, M.
Davis, T. M.
Eifler, T. F.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Glazebrook, K.
Gruen, D.
Kacprzak, T.
King, A.
Kwan, J.
Lahav, O.
Lewis, G.
Lidman, C.
Lin, H.
MacCrann, N.
Miquel, R.
O'Neill, C. R.
Palmese, A.
Peiris, H. V.
Refregier, A.
Rozo, E.
Rykoff, E. S.
Sadeh, I.
Sanchez, C.
Sheldon, E.
Uddin, S.
Wechsler, R. H.
Zuntz, J.
Abbott, T.
Abdalla, F. B.
Allam, S.
Armstrong, R.
Banerji, M.
Bauer, A. H.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Capozzi, D.
Carnero Rosell, A.
Carretero, J.
Cunha, C. E.
D'Andrea, C. B.
da Costa, L. N.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Gerdes, D. W.
Gruendl, R. A.
Honscheid, K.
Jain, B.
James, D. J.
Jarvis, M.
Kim, A. G.
Kuehn, K.
Kuropatkin, N.
Li, T. S.
Lima, M.
Maia, M. A. G.
March, M.
Marshall, J. L.
Martini, P.
Melchior, P.
Miller, C. J.
Neilsen, E.
Nichol, R. C.
Nord, B.
Ogando, R.
Plazas, A. A.
Reil, K.
Romer, A. K.
Roodman, A.
Sako, M.
Sanchez, E.
Santiago, B.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Vikram, V.
Walker, A. R.
CA Dark Energy Survey Collaboration
TI Redshift distributions of galaxies in the Dark Energy Survey Science
Verification shear catalogue and implications for weak lensing
SO PHYSICAL REVIEW D
LA English
DT Article
ID STAR-FORMING GALAXIES; LARGE-SCALE STRUCTURE; PHOTO-Z PERFORMANCE; VLT
DEEP SURVEY; PHOTOMETRIC REDSHIFTS; DATA RELEASE; PRECISION COSMOLOGY;
SURVEY REQUIREMENTS; SHAPE MEASUREMENT; NEURAL-NETWORKS
AB We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model-or machine learning-based photometric redshift methods-ANNZ2, BPZ calibrated against BCC-Ufig simulations, SKYNET, and TPZ-are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 +/- 0.01 over the range 0.3 < z < 1.3, we construct three tomographic bins with means of z = {0.45; 0.67; 1.00}. These bins each have systematic uncertainties delta z <= 0.05 in the mean of the fiducial SKYNET photo-z (dz). We propagate the errors in the redshift distributions through to their impact on cosmological parameters estimated with cosmic shear, and find that they cause shifts in the value of sigma(8) of approximately 3%. This shift is within the one sigma statistical errors on sigma(8) for the DES SV shear catalogue. We further study the potential impact of systematic differences on the critical surface density, Sigma(crit), finding levels of bias safely less than the statistical power of DES SV data. We recommend a final Gaussian prior for the photo-z bias in the mean of n(z) of width 0.05 for each of the three tomographic bins, and show that this is a sufficient bias model for the corresponding cosmology analysis.
C1 [Bonnett, C.; Miquel, R.; Sanchez, C.; Carretero, J.; Fernandez, E.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Troxel, M. A.; Bridle, S. L.; MacCrann, N.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Hartley, W.; Amara, A.; Bruderer, C.; Chang, C.; Kacprzak, T.; Refregier, A.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland.
[Leistedt, B.; Lahav, O.; Palmese, A.; Peiris, H. V.; Sadeh, I.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Becker, M. R.; Busha, M. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Becker, M. R.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Cunha, C. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Bernstein, G. M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[King, A.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[Castander, F. J.; Crocce, M.; Gaztanaga, E.; Bauer, A. H.; Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain.
[Eifler, T. F.; Abdalla, F. B.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Frieman, J.; Lin, H.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kwan, J.; Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA.
[Lidman, C.; Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Glazebrook, K.; Uddin, S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.
[Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Bertin, E.] Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst Eastron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Desai, S.] Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Gangkofner, C.; Sheldon, E.; Desai, S.; Dietrich, J. P.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Gruen, D.; Dietrich, J. P.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Gerdes, D. W.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Kim, A. G.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.] CIEMAT, Madrid, Spain.
[Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Lewis, G.] South East Phys Network, SEPnet, Southampton, Hants, England.
[Davis, T. M.; O'Neill, C. R.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Childress, M. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA.
[Gangkofner, C.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
RP Bonnett, C (reprint author), Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Davis,
Tamara/A-4280-2008; Gaztanaga, Enrique/L-4894-2014;
OI Ogando, Ricardo/0000-0003-2120-1154; Davis, Tamara/0000-0002-4213-8783;
Gaztanaga, Enrique/0000-0001-9632-0815; Abdalla,
Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658
FU European Research Council [240672]; DFG Cluster of Excellence Origin and
Structure of the Universe; 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; Center for Cosmology and Astro-Particle Physics
at the Ohio State University; Mitchell Institute for Fundamental Physics
and Astronomy at Texas AM University; Financiadora de Estudos e
Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do
Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche
Forschungsgemeinschaft; National Science Foundation [AST-1138766];
MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de
Excelencia Severo Ochoa [SEV-2012-0234]; ERDF funds from the European
Union; Argonne National Laboratory; University of California at Santa
Cruz; University of Cambridge; Centro de Investigaciones Energeticas,
Medioambientales y Tecnologicas-Madrid; University of Chicago;
University College London; DES-Brazil Consortium; Eidgenossische
Technische Hochschule (ETH) Zurich; Fermi National Accelerator
Laboratory; University of Edinburgh; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat and the 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; Australian Astronomical Observatory [A/2013B/012];
Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Swiss National Science Foundation
[200021_14944, 200021_143906]; 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; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Pennsylvania
State University; Princeton University; Spanish Participation Group;
University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; University of Washington; Yale University; ESO
Telescopes at the La Silla Paranal Observatory [179.A-2004, 177.A-3016]
FX We are grateful for the extraordinary contributions of our CTIO
colleagues and the DECam Construction, 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 group. M. T., S. B., N. M., and J. Z. acknowledge
support from the European Research Council in the form of a Starting
Grant with number 240672. D. G. acknowledges the support by the DFG
Cluster of Excellence Origin and Structure of the Universe. 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, the Center for Cosmology and Astro-Particle
Physics at the Ohio State University, the Mitchell Institute for
Fundamental Physics and Astronomy at Texas A&M University, Financiadora
de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa
do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the
Deutsche Forschungsgemeinschaft and the Collaborating Institutions in
the Dark Energy Survey. C. G. acknowledges the support by the DFG
Cluster of Excellence Origin and Structure of the Universe. The DES data
management system is supported by the National Science Foundation under
Grant Number AST-1138766. The DES participants from Spanish institutions
are partially supported by MINECO under grants AYA2012-39559,
ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa
SEV-2012-0234, some of which include ERDF funds from the European Union.
The Collaborating Institutions are Argonne National Laboratory, the
University of California at Santa Cruz, the University of Cambridge,
Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat and the associated Excellence Cluster
Universe, the University of Michigan, the National Optical Astronomy
Observatory, the University of Nottingham, The Ohio State University,
the University of Pennsylvania, the University of Portsmouth, SLAC
National Accelerator Laboratory, Stanford University, the University of
Sussex, and Texas A&M University. Based in part on observations taken at
the Australian Astronomical Observatory under program A/2013B/012. Parts
of this research were conducted by the Australian Research Council
Centre of Excellence for All-sky Astrophysics (CAASTRO), through project
number CE110001020. This work was supported in part by grants
200021_14944 and 200021_143906 from the Swiss National Science
Foundation. 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.; r 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. Based on observations made with ESO Telescopes at the La
Silla Paranal Observatory under programme ID 179.A-2004. Based on
observations made with ESO Telescopes at the La Silla Paranal
Observatory under programme ID 177.A-3016. This paper is Fermilab
publication FERMILAB-PUB-15-306 and DES publication DES2015-0060. This
paper has gone through internal review by the DES Collaboration.
NR 95
TC 10
Z9 10
U1 5
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 30
PY 2016
VL 94
IS 4
AR 042005
DI 10.1103/PhysRevD.94.042005
PG 26
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DU4IW
UT WOS:000382177300001
ER
PT J
AU Frankenberg, C
Thorpe, AK
Thompson, DR
Hulley, G
Kort, EA
Vance, N
Borchardt, J
Krings, T
Gerilowski, K
Sweeney, C
Conley, S
Bue, BD
Aubrey, AD
Hook, S
Green, RO
AF Frankenberg, Christian
Thorpe, Andrew K.
Thompson, David R.
Hulley, Glynn
Kort, Eric Adam
Vance, Nick
Borchardt, Jakob
Krings, Thomas
Gerilowski, Konstantin
Sweeney, Colm
Conley, Stephen
Bue, Brian D.
Aubrey, Andrew D.
Hook, Simon
Green, Robert O.
TI Airborne methane remote measurements reveal heavy-tail flux distribution
in Four Corners region
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE methane; Four Corners; remote sensing; heavy-tail
ID IMAGING SPECTROMETER AVIRIS; MATCHED-FILTER DETECTION; GAS PRODUCTION
SITES; EMISSION RATES; UNITED-STATES; TRACE GASES; RETRIEVAL;
QUANTIFICATION; SPECTROSCOPY; CO2
AB Methane (CH4) impacts climate as the second strongest anthropogenic greenhouse gas and air quality by influencing tropospheric ozone levels. Space-based observations have identified the Four Corners region in the Southwest United States as an area of large CH4 enhancements. We conducted an airborne campaign in Four Corners during April 2015 with the next-generation Airborne Visible/Infrared Imaging Spectrometer (near-infrared) and Hyperspectral Thermal Emission Spectrometer (thermal infrared) imaging spectrometers to better understand the source of methane by measuring methane plumes at 1-to 3-m spatial resolution. Our analysis detected more than 250 individual methane plumes from fossil fuel harvesting, processing, and distributing infrastructures, spanning an emission range from the detection limit similar to 2 kg/h to 5 kg/h through similar to 5,000 kg/h. Observed sources include gas processing facilities, storage tanks, pipeline leaks, and well pads, as well as a coal mine venting shaft. Overall, plume enhancements and inferred fluxes follow a lognormal distribution, with the top 10% emitters contributing 49 to 66% to the inferred total point source flux of 0.23 Tg/y to 0.39 Tg/y. With the observed confirmation of a lognormal emission distribution, this airborne observing strategy and its ability to locate previously unknown point sources in real time provides an efficient and effective method to identify and mitigate major emissions contributors over a wide geographic area. With improved instrumentation, this capability scales to spaceborne applications [Thompson DR, et al. (2016) Geophys Res Lett 43(12): 6571-6578]. Further illustration of this potential is demonstrated with two detected, confirmed, and repaired pipeline leaks during the campaign.
C1 [Frankenberg, Christian] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Frankenberg, Christian; Thorpe, Andrew K.; Thompson, David R.; Hulley, Glynn; Vance, Nick; Bue, Brian D.; Aubrey, Andrew D.; Hook, Simon; Green, Robert O.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kort, Eric Adam] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Borchardt, Jakob; Krings, Thomas; Gerilowski, Konstantin] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
[Sweeney, Colm] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Sweeney, Colm] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Conley, Stephen] Sci Aviat, Boulder, CO 80301 USA.
[Conley, Stephen] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
RP Frankenberg, C (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM cfranken@caltech.edu
RI Kort, Eric/F-9942-2012; Frankenberg, Christian/A-2944-2013
OI Kort, Eric/0000-0003-4940-7541; Frankenberg,
Christian/0000-0002-0546-5857
FU NASA Headquarters; state of Bremen; University of Bremen; National
Oceanic and Atmospheric Administration AC4 program [NA14OAR0110139]
FX We thank the AVIRIS-NG flight and instrument teams, including Michael
Eastwood, Sarah Lundeen, Scott Nolte, Mark Helmlinger, and Betina Pavri.
Didier Keymeulen and Joseph Boardman assisted with the real-time system.
We also thank the HyTES flight and instrument teams, including Bjorn
Eng, Jonathan Mihaly, Seth Chazanoff, and Bill Johnson. We thank the
organizers and all the participants in the TOPDOWN campaign for the
fruitful collaboration. We thank NASA Headquarters, in particular Jack
Kaye, for funding this flight campaign, which augmented the overall Twin
Otter Projects Defining Oil/Gas Well Emissions (TOPDOWN) campaign. J.B.,
T.K., and K.G. were funded by the state of Bremen and University of
Bremen. E.A.K. and C.S. were supported, in part, by the National Oceanic
and Atmospheric Administration AC4 program under Grant NA14OAR0110139.
NR 23
TC 3
Z9 3
U1 9
U2 9
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 30
PY 2016
VL 113
IS 35
BP 9734
EP 9739
DI 10.1073/pnas.1605617113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV7BL
UT WOS:000383090700039
PM 27528660
ER
PT J
AU Zhang, RY
Peng, JF
Wang, Y
Hu, M
AF Zhang, Renyi
Peng, Jianfei
Wang, Yuan
Hu, Min
TI Rate and timescale of black carbon aging regulate direct radiative
forcing
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
ID AEROSOLS; IMPACTS; CHINA
C1 [Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.
[Zhang, Renyi; Peng, Jianfei; Hu, Min] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
[Wang, Yuan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.; Zhang, RY (reprint author), Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.; Zhang, RY; Hu, M (reprint author), Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
EM renyi-zhang@tamu.edu; minhu@pku.edu.cn
RI Peng, Jianfei/F-1438-2015
NR 10
TC 0
Z9 0
U1 32
U2 32
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 30
PY 2016
VL 113
IS 35
BP E5094
EP E5095
DI 10.1073/pnas.1610241113
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV7BL
UT WOS:000383090700002
PM 27555593
ER
PT J
AU Feyhl-Buska, J
Chen, YF
Jia, CL
Wang, JX
Zhang, CLL
Boyd, ES
AF Feyhl-Buska, Jayme
Chen, Yufei
Jia, Chengling
Wang, Jin-Xiang
Zhang, Chuanlun L.
Boyd, Eric S.
TI Influence of Growth Phase, pH, and Temperature on the Abundance and
Composition of Tetraether Lipids in the Thermoacidophile Picrophilus
torridus
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Article
DE tetraether; GDGT; GTGT; growth phase; temperature; pH; thermoacidophile;
stress
ID FATTY-ACID-COMPOSITION; TERRESTRIAL HOT-SPRINGS; LOWER PEARL RIVER;
SOUTH CHINA SEA; MEMBRANE-LIPIDS; POLAR LIPIDS;
NITROSOPUMILUS-MARITIMUS; ARCHAEBACTERIAL LIPIDS; THERMOPHILIC ARCHAEA;
MASS-SPECTROMETRY
AB The abundance and composition of glycerol dibiphytanyl glycerol tetraether (GDGT) and glycerol tribiphytanyl glycerol tetraether (GTGT) lipids were determined as a function of growth phase as a proxy for nutrient availability, the pH of growth medium, and incubation temperature in cultures of the thermoacidophile Picrophilus torridus. Regardless of the cultivation condition, the abundance of GDGTs and GTGTs was greater in the polar than core fraction, with a marked decrease in core GDGTs in cultures harvested during log phase growth. These data are consistent with previous suggestions indicating that core GDGTs are re-functionalized during polar lipid synthesis. Under all conditions examined, polar lipids were enriched in a GDGT with 2 cyclopentyl rings (GDGT-2), indicating GDGT-2 is the preferred lipid in this taxon. However, lag or stationary phase grown cells or cells subjected to pH or thermal stress were enriched in GDGTs with 4, 5, or 6 rings and depleted in GDGTs with 1, 2, 3, rings relative to log phase cells grown under optimal conditions. Variation in the composition of polar GDGT lipids in cells harvested during various growth phases tended to be greater than in cells cultivated over a pH range of 0.31.1 and a temperature range of 5363 degrees C. These results suggest that the growth phase, the pH of growth medium, and incubation temperature are all important factors that shape the composition of tetraether lipids in Picrophilus. The similarity in enrichment of GDGTs with more rings in cultures undergoing nutrient, pH, and thermal stress points to GDGT cyclization as a generalized physiological response to stress in this taxon.
C1 [Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
[Chen, Yufei; Jia, Chengling; Wang, Jin-Xiang; Zhang, Chuanlun L.] Tongji Univ, State Key Lab Marine Geol, Shanghai, Peoples R China.
[Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94043 USA.
[Feyhl-Buska, Jayme] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA.
[Wang, Jin-Xiang] Univ Bremen, MARUM Ctr Marine Environm Sci, Bremen, Germany.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.; Boyd, ES (reprint author), NASA, Astrobiol Inst, Mountain View, CA 94043 USA.
EM eboyd@montana.edu
FU National Science Foundation [PIRE-0968421]; National Natural Science
Foundation of China [40972211, 41373072]; National Science Foundation
Research Experience for Undergraduates grant [DBI REU 1005223]; NASA
Astrobiology Institute [NNA15BB02A]; NASA Exobiology and Evolutionary
Biology Program [NNX13AI11G]
FX This work was supported by grants from the National Science Foundation
(PIRE-0968421) to CZ and EB and from the National Natural Science
Foundation of China (40972211 and 41373072) to CZ. A National Science
Foundation Research Experience for Undergraduates grant (DBI REU
1005223) supported JF during the completion of this work. EB
acknowledges support from the NASA Astrobiology Institute (NNA15BB02A)
and the NASA Exobiology and Evolutionary Biology Program (NNX13AI11G).
Two reviewers are acknowledged for comments which significantly improved
this manuscript.
NR 60
TC 0
Z9 0
U1 8
U2 8
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1664-302X
J9 FRONT MICROBIOL
JI Front. Microbiol.
PD AUG 30
PY 2016
VL 7
AR 1323
DI 10.3389/fmicb.2016.01323
PG 12
WC Microbiology
SC Microbiology
GA DU3KC
UT WOS:000382108200001
PM 27625636
ER
PT J
AU Mandra, S
Zhu, Z
Wang, WL
Perdomo-Ortiz, A
Katzgraber, HG
AF Mandra, Salvatore
Zhu, Zheng
Wang, Wenlong
Perdomo-Ortiz, Alejandro
Katzgraber, Helmut G.
TI Strengths and weaknesses of weak-strong cluster problems: A detailed
overview of state-of-the-art classical heuristics versus quantum
approaches
SO PHYSICAL REVIEW A
LA English
DT Article
ID MONTE-CARLO; SPIN-GLASS; OPTIMIZATION; COMPUTATION; ANNEALERS; QUBITS
AB To date, a conclusive detection of quantum speedup remains elusive. Recently, a team by Google Inc. [V. S. Denchev et al., Phys. Rev. X 6, 031015 (2016)] proposed a weak-strong cluster model tailored to have tall and narrow energy barriers separating local minima, with the aim to highlight the value of finite-range tunneling. More precisely, results from quantum Monte Carlo simulations as well as the D-Wave 2X quantum annealer scale considerably better than state-of-the-art simulated annealing simulations. Moreover, the D-Wave 2X quantum annealer is similar to 10(8) times faster than simulated annealing on conventional computer hardware for problems with approximately 10(3) variables. Here, an overview of different sequential, nontailored, as well as specialized tailored algorithms on the Google instances is given. We show that the quantum speedup is limited to sequential approaches and study the typical complexity of the benchmark problems using insights from the study of spin glasses.
C1 [Mandra, Salvatore] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
[Zhu, Zheng; Wang, Wenlong; Katzgraber, Helmut G.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Perdomo-Ortiz, Alejandro] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
[Perdomo-Ortiz, Alejandro] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Katzgraber, Helmut G.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Katzgraber, Helmut G.] Coventry Univ, Appl Math Res Ctr, Coventry CV1 5FB, W Midlands, England.
RP Mandra, S (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
EM smandra@fas.harvard.edu; zzwtgts@tamu.edu; wenlong@physics.umass.edu;
alejandro.perdomoortiz@nasa.gov; hgk@tamu.edu
FU NSF [DMR-1151387]; NASA [NNX14AF62G]; Office of the Director of National
Intelligence (ODNI), Intelligence Advanced Research Projects Activity
(IARPA), via MIT Lincoln Laboratory Air Force [FA8721-05-C-0002]
FX We thank the Google Quantum A. I. Lab members for sharing their QMC and
SA data, multiple discussions, as well as making the weak-strong cluster
instances available to us. We also thank A. Aspuru-Guzik, F. Hamze, A.J.
Ochoa, and Eleanor G. Rieffel for many fruitful discussions, as well as
H. Munoz-Bauza for help with the graphics. H.G.K. and W.W. acknowledge
support from the NSF (Grant No. DMR-1151387). H.G.K. thanks D. Humm,
M.P. White, T. Keller, H. Blumenthal, and P. Bocuse for inspiration
during the initial stages of the manuscript. S.M. was supported by NASA
(Sponsor Award No. NNX14AF62G). We thank the Texas Advanced Computing
Center (TACC) at The University of Texas at Austin for providing HPC
resources (Stampede Cluster) and Texas A&M University for access to
their Ada and Lonestar clusters. This research is based upon work
supported in part by the Office of the Director of National Intelligence
(ODNI), Intelligence Advanced Research Projects Activity (IARPA), via
MIT Lincoln Laboratory Air Force Contract No. FA8721-05-C-0002.
NR 80
TC 2
Z9 2
U1 1
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD AUG 29
PY 2016
VL 94
IS 2
AR 022337
DI 10.1103/PhysRevA.94.022337
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DU2BR
UT WOS:000382016400003
ER
PT J
AU Matsuyama, I
Nimmo, F
Keane, JT
Chan, NH
Taylor, GJ
Wieczorek, MA
Kiefer, WS
Williams, JG
AF Matsuyama, Isamu
Nimmo, Francis
Keane, James T.
Chan, Ngai H.
Taylor, G. Jeffrey
Wieczorek, Mark A.
Kiefer, Walter S.
Williams, James G.
TI GRAIL, LLR, and LOLA constraints on the interior structure of the Moon
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE lunar interior
ID DEEP LUNAR INTERIOR; SEISMIC DATA; POLYCRYSTALLINE OLIVINE;
FREQUENCY-DEPENDENCE; CHANDLER-WOBBLE; TIDAL RESPONSE; GRAVITY-FIELD;
GIANT IMPACT; MARE BASALTS; MODEL
AB The interior structure of the Moon is constrained by its mass, moment of inertia, and k(2) and h(2) tidal Love numbers. We infer the likely radius, density, and (elastic limit) rigidity of all interior layers by solving the inverse problem using these observational constraints assuming spherical symmetry. Our results do not favor the presence of a low rigidity transition layer between a liquid outer core and mantle. If a transition layer exists, its rigidity is constrained to 43-9+26GPa, with a preference for the high rigidity values. Therefore, if a transition layer exists, it is more likely to have a rigidity similar to that of the mantle (approximate to 70GPa). The total (solid and liquid) core mass fraction relative to the lunar mass is constrained to 0.0098-0.0094+0.0066 and 0.0198-0.0049+0.0026 for interior structures with and without a transition layer, respectively, narrowing the range of possible giant impact formation scenarios.
C1 [Matsuyama, Isamu; Keane, James T.; Chan, Ngai H.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Taylor, G. Jeffrey] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Wieczorek, Mark A.] Inst Phys Globe Paris, Paris, France.
[Kiefer, Walter S.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Williams, James G.] Inst Technol, Jet Prop Lab, Pasadena, CA USA.
RP Matsuyama, I (reprint author), Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM isa@lpl.arizona.edu
RI Wieczorek, Mark/G-6427-2010;
OI Wieczorek, Mark/0000-0001-7007-4222; Matsuyama,
Isamu/0000-0002-2917-8633; Kiefer, Walter/0000-0001-6741-5460
FU NASA's Discovery Program
FX The GRAIL mission is supported by NASA's Discovery Program and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology. A
portion of the research described in this paper was carried out at the
Jet Propulsion Laboratory of the California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Government sponsorship is acknowledged. The data used are listed in the
references and tables.
NR 51
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8365
EP 8375
DI 10.1002/2016GL069952
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800005
ER
PT J
AU Way, MJ
Del Genio, AD
Kiang, NY
Sohl, LE
Grinspoon, DH
Aleinov, I
Kelley, M
Clune, T
AF Way, M. J.
Del Genio, Anthony D.
Kiang, Nancy Y.
Sohl, Linda E.
Grinspoon, David H.
Aleinov, Igor
Kelley, Maxwell
Clune, Thomas
TI Was Venus the first habitable world of our solar system?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ancient Venus; habitability
ID EARTH; ATMOSPHERE; WATER; PLANETS; EVOLUTION; HYDROGEN; OCEAN;
DEUTERIUM; ROTATION; HISTORY
AB Present-day Venus is an inhospitable place with surface temperatures approaching 750K and an atmosphere 90 times as thick as Earth's. Billions of years ago the picture may have been very different. We have created a suite of 3-D climate simulations using topographic data from the Magellan mission, solar spectral irradiance estimates for 2.9 and 0.715 Gya, present-day Venus orbital parameters, an ocean volume consistent with current theory, and an atmospheric composition estimated for early Venus. Using these parameters we find that such a world could have had moderate temperatures if Venus had a prograde rotation period slower than similar to 16 Earth days, despite an incident solar flux 46-70% higher than Earth receives. At its current rotation period, Venus's climate could have remained habitable until at least 0.715 Gya. These results demonstrate the role rotation and topography play in understanding the climatic history of Venus-like exoplanets discovered in the present epoch.
C1 [Way, M. J.; Del Genio, Anthony D.; Kiang, Nancy Y.; Sohl, Linda E.; Aleinov, Igor; Kelley, Maxwell] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Way, M. J.] Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden.
[Sohl, Linda E.; Aleinov, Igor] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Grinspoon, David H.] Planetary Sci Inst, Tucson, AZ USA.
[Clune, Thomas] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Way, MJ (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Way, MJ (reprint author), Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden.
EM michael.j.way@nasa.gov
OI Way, Michael/0000-0003-3728-0475
FU NASA Astrobiology Program through the Nexus for Exoplanet System Science
(NExSS) research coordination network - NASA's Science Mission
Directorate; NASA Goddard Space Flight Center ROCKE-3D Science Task
Group funding
FX This research was supported by the NASA Astrobiology Program through the
Nexus for Exoplanet System Science (NExSS) research coordination network
sponsored by NASA's Science Mission Directorate. This work was also
supported by NASA Goddard Space Flight Center ROCKE-3D Science Task
Group funding. Resources supporting this work were provided by the NASA
High-End Computing (HEC) Program through the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. This research has made
use of NASA's Astrophysics Data System Bibliographic Services. Thanks to
Jeffrey A. Jonas, Kostas Tsigaridis, and David S. Amundsen for their
assistance in this work and thanks to June Wang at Washington University
in St. Louis for help with the Magellan PDS data. We also thank referee
Norman Sleep for his constructive comments. The data products associated
with this paper can be obtained by contacting the first author Michael
J. Way.
NR 53
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8376
EP 8383
DI 10.1002/2016GL069790
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800006
ER
PT J
AU Scheuchl, B
Mouginot, J
Rignot, E
Morlighem, M
Khazendar, A
AF Scheuchl, B.
Mouginot, J.
Rignot, E.
Morlighem, M.
Khazendar, A.
TI Grounding line retreat of Pope, Smith, and Kohler Glaciers, West
Antarctica, measured with Sentinel-1a radar interferometry data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Grounding Line; Synthetic Aperture Radar; Sentinel-1
ID AMUNDSEN SEA EMBAYMENT; ICE-SHEET; PINE ISLAND; SHELF; WIDESPREAD;
STABILITY; GREENLAND; CRYOSAT-2; THWAITES; SURFACE
AB We employ Sentinel-1a C band satellite radar interferometry data in Terrain Observation with Progressive Scans mode to map the grounding line and ice velocity of Pope, Smith, and Kohler glaciers, in West Antarctica, for the years 2014-2016 and compare the results with those obtained using Earth Remote Sensing Satellites (ERS-1/2) in 1992, 1996, and 2011. We observe an ongoing, rapid grounding line retreat of Smith at 2km/yr (40km since 1996), an 11km retreat of Pope (0.5km/yr), and a 2km readvance of Kohler since 2011. The variability in glacier retreat is consistent with the distribution of basal slopes, i.e., fast along retrograde beds and slow along prograde beds. We find that several pinning points holding Dotson and Crosson ice shelves disappeared since 1996 due to ice shelf thinning, which signal the ongoing weakening of these ice shelves. Overall, the results indicate that ice shelf and glacier retreat in this sector remain unabated.
C1 [Scheuchl, B.; Mouginot, J.; Rignot, E.; Morlighem, M.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, E.; Khazendar, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Scheuchl, B (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM bscheuch@uci.edu
FU National Aeronautics and Space Administration's Cryospheric Science
Program; National Aeronautics and Space Administration's MEaSUREs
program
FX This work was performed at the University of California, Irvine, and at
the Jet Propulsion Laboratory, California Institute of Technology, under
a grant from the National Aeronautics and Space Administration's
Cryospheric Science Program and MEaSUREs program. The authors gratefully
acknowledge the European Space Agency and the USGS for providing the
data. SAR data acquisition was coordinated by the Polar Space Task
Group. The 2014 grounding line is available at NSIDC as part of the
updated MEaSUREs InSAR based grounding line product.
NR 39
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U2 12
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8572
EP 8579
DI 10.1002/2016GL069287
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800029
ER
PT J
AU Peyser, CE
Yin, JJ
Landerer, FW
Cole, JE
AF Peyser, Cheryl E.
Yin, Jianjun
Landerer, Felix W.
Cole, Julia E.
TI Pacific sea level rise patterns and global surface temperature
variability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE sea level rise; Pacific; warming hiatus; global temperature
ID WESTERN TROPICAL PACIFIC; OCEAN HEAT UPTAKE; WARMING HIATUS;
INTENSIFICATION; CIRCULATION; ATLANTIC; TRENDS
AB During 1998-2012, climate change and sea level rise (SLR) exhibit two notable features: a slowdown of global surface warming (hiatus) and a rapid SLR in the tropical western Pacific. To quantify their relationship, we analyze the long-term control simulations of 38 climate models. We find a significant and robust correlation between the east-west contrast of dynamic sea level (DSL) in the Pacific and global mean surface temperature (GST) variability on both interannual and decadal time scales. Based on linear regression of the multimodel ensemble mean, the anomalously fast SLR in the western tropical Pacific observed during 1998-2012 indicates suppression of a potential global surface warming of 0.16 degrees 0.06 degrees C. In contrast, the Pacific contributed 0.29 degrees 0.10 degrees C to the significant interannual GST increase in 1997/1998. The Pacific DSL anomalies observed in 2015 suggest that the strong El Nino in 2015/2016 could lead to a 0.21 degrees 0.07 degrees C GST jump.
C1 [Peyser, Cheryl E.; Yin, Jianjun; Cole, Julia E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Landerer, Felix W.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
RP Yin, JJ (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
EM yin@email.arizona.edu
FU Strategic University Research Partnership Program of the NASA Jet
Propulsion Laboratory [1492484/NNN12AA01C]
FX We thank many observation and modeling centers for making their data
available. We thank the anonymous reviewers for detailed reviews and P.
Goddard, S. Griffies, S. Malyshev, J. Pelletier, J. Russell, and R.
Stouffer for discussion. The work was supported by the Strategic
University Research Partnership Program of the NASA Jet Propulsion
Laboratory (grant # 1492484/NNN12AA01C). The work of F.W.L. was
performed at the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. The observational, reanalysis,
and model data used in this study can be accessed from the URLs found in
the section 2. For all other data inquiries, please contact Cheryl
Peyser (peyser@email.arizona.edu).
NR 31
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SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8662
EP 8669
DI 10.1002/2016GL069401
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800039
ER
PT J
AU Lyu, F
Cummer, SA
Briggs, M
Marisaldi, M
Blakeslee, RJ
Bruning, E
Wilson, JG
Rison, W
Krehbiel, P
Lu, GP
Cramer, E
Fitzpatrick, G
Mailyan, B
McBreen, S
Roberts, OJ
Stanbro, M
AF Lyu, Fanchao
Cummer, Steven A.
Briggs, Michael
Marisaldi, Martino
Blakeslee, Richard J.
Bruning, Eric
Wilson, Jennifer G.
Rison, William
Krehbiel, Paul
Lu, Gaopeng
Cramer, Eric
Fitzpatrick, Gerard
Mailyan, Bagrat
McBreen, Sheila
Roberts, Oliver J.
Stanbro, Matthew
TI Ground detection of terrestrial gamma ray flashes from distant radio
signals
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE terrestrial gamma ray flashes; energetic in-cloud pulses; lightning;
ground detection
ID ALTITUDE
AB Terrestrial gamma ray flashes (TGFs) are brief bursts of energetic gammy-ray photons generated during thunderstorms, which have been detected almost exclusively by satellite-based instruments. Here we present three lines of evidence which includes the three out of three simultaneously observed pairs, the same occurrence contexts, and the consistent estimated occurrence rate, which indicate a direct relationship between a subset of TGFs and a class of energetic radio signal easily detectable by ground-based sensors. This connection indicates that these gamma ray and radio emissions are two views of the same phenomenon and further enable detection of these TGFs from ground distant radio signals alone. Besides dramatically increasing the detection rate of TGFs, this ground detection approach can identify TGFs in continental and coastal areas that are at latitudes too high for present TGF-detecting satellites and will provide more insights into the mechanism of TGF production.
C1 [Lyu, Fanchao; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Briggs, Michael; Cramer, Eric; Fitzpatrick, Gerard; Mailyan, Bagrat] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Briggs, Michael; Stanbro, Matthew] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
[Marisaldi, Martino] INAF IASF Bologna, Bologna, Italy.
[Marisaldi, Martino] Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway.
[Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Bruning, Eric] Texas Tech Univ, Dept Geosci, Atmospher Sci Grp, Lubbock, TX 79409 USA.
[Wilson, Jennifer G.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL USA.
[Rison, William; Krehbiel, Paul] New Mexico Inst Min & Technol, Langmuir Lab Atmospher Res, Geophys Res Ctr, Socorro, NM 87801 USA.
[Lu, Gaopeng] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China.
[Lu, Gaopeng] Nanjing Univ Informat Sci & Technol, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China.
[Cramer, Eric] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Fitzpatrick, Gerard; McBreen, Sheila; Roberts, Oliver J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
RP Cummer, SA (reprint author), Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
EM cummer@ee.duke.edu
RI Roberts, Oliver/N-6284-2016
OI Roberts, Oliver/0000-0002-7150-9061
FU National Science Foundation Dynamic and Physical Meteorology program
[ATM-1047588]; DARPA Nimbus program [HR0011-10-10059]; Science
Foundation Ireland [12/IP/1288]
FX The authors would like to acknowledge the support from the National
Science Foundation Dynamic and Physical Meteorology program through
grant ATM-1047588 and the DARPA Nimbus program through grant
HR0011-10-10059. The authors would like to thank those colleges at
Florida Institute of Technology, University of Oklahoma, University of
Mississippi, and Kansas State University which assist us with the
operation of LF networks. We thank Vaisala Inc. for providing the
real-time lightning data which enabled us to start the investigation.
O.J.R. and S.M.B. acknowledge support from Science Foundation Ireland
under grant 12/IP/1288. We thank the Fermi team for providing the
Fermi-GBM gamma ray data
(http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/). The recent TGF
catalog can be accessed on the website
(http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/tgf/). All data are
available by request (cummer@ee.duke.edu). The authors would like to
thank two anonymous reviewers for their comments to improve the paper.
NR 31
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8728
EP 8734
DI 10.1002/2016GL070154
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800047
ER
PT J
AU Kahn, BH
Huang, XL
Stephens, GL
Collins, WD
Feldman, DR
Su, H
Wong, S
Yue, Q
AF Kahn, Brian H.
Huang, Xianglei
Stephens, Graeme L.
Collins, William D.
Feldman, Daniel R.
Su, Hui
Wong, Sun
Yue, Qing
TI ENSO regulation of far- and mid-infrared contributions to clear-sky OLR
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE far infrared; clear sky; tropics; ENSO; upper troposphere; water vapor
ID SEA-SURFACE TEMPERATURE; TROPICAL DEEP CONVECTION; WATER-VAPOR; EL-NINO;
CHANGING CLIMATE; CLOUDS; TROPOSPHERE; DEPENDENCE; SIGNATURE; RADIATION
AB NASA Aqua-derived thermodynamic profiles, calculated spectral clear-sky outgoing longwave radiation (OLR), and vertical velocity fields from meteorological reanalyses are combined to determine the relative proportion of the far-infrared (FIR) and mid-infrared (MIR) spectral contributions to the total clear-sky OLR during different phases of El Nino-Southern Oscillation (ENSO). In the ascending branch of the tropical circulation, the spatial variance of upper tropospheric water vapor is shown to be larger during La Nina than El Nino and is consistent with zonal symmetry changes in the tropical waveguide and associated tropical-extratropical mixing. In the descending branch, upper tropospheric water vapor shows weaker coupling to lower layers that is evidenced by changes in the ratio of FIR to MIR in the clear-sky OLR. Diagnostics from the Geophysical Fluid Dynamics Laboratory AM3 model simulation are generally similar to satellite data, but the ratio of FIR to MIR is 5-10% larger with respect to dynamic regime.
C1 [Kahn, Brian H.; Stephens, Graeme L.; Su, Hui; Wong, Sun; Yue, Qing] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Huang, Xianglei] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Collins, William D.; Feldman, Daniel R.] Lawrence Berkeley Natl Lab, Climate & Ecosyst Div, Berkeley, CA USA.
[Collins, William D.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM brian.h.kahn@jpl.nasa.gov
RI Collins, William/J-3147-2014; Yue, Qing/F-4619-2017
OI Collins, William/0000-0002-4463-9848; Yue, Qing/0000-0002-3559-6508
FU JPL; University of Michigan; NASA [NNX14AJ50G]; U.S. Department of
Energy, Office of Science, Office of Biological and Environmental
Research, Terrestrial Ecosystem Science and Atmospheric System Research
programs [DE-ACO2-05CH11231]
FX A portion of this research was carried out at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with the National Aeronautics and Space Administration. We thank two
anonymous reviewers for very constructive feedback and insights that led
to an improved manuscript. B. Kahn was supported by Strategic University
Research Partnership (SURP) proposal between JPL and the University of
Michigan. X. Huang was supported by NASA under grant NNX14AJ50G awarded
to the University of Michigan. D. Feldman and W. Collins acknowledge
support by the U.S. Department of Energy, Office of Science, Office of
Biological and Environmental Research, Terrestrial Ecosystem Science and
Atmospheric System Research programs, under award DE-ACO2-05CH11231. The
AIRS version 6 data sets were processed by and obtained from the Goddard
Earth Services Data and Information Services Center
(http://daac.gsfc.nasa.gov/). The MERRA data sets were processed by and
obtained from the NASA Goddard's Global Modeling and Assimilation Office
(GMAO). Copyright 2016. All rights reserved. Government sponsorship
acknowledged.
NR 43
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U1 6
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8751
EP 8759
DI 10.1002/2016GL070263
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800050
ER
PT J
AU Wu, LH
Hasekamp, O
van Diedenhoven, B
Cairns, B
Yorks, JE
Chowdhary, J
AF Wu, Lianghai
Hasekamp, Otto
van Diedenhoven, Bastiaan
Cairns, Brian
Yorks, John E.
Chowdhary, Jacek
TI Passive remote sensing of aerosol layer height using near-UV multiangle
polarization measurements
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE aerosol layer height
ID RESEARCH SCANNING POLARIMETER; RADIATIVE-TRANSFER MODEL;
PHOTOPOLARIMETRIC MEASUREMENTS; SPECTRAL-RESOLUTION; OPTICAL-PROPERTIES;
RETRIEVAL; OCEAN; SENSITIVITY; LIDAR; BAND
AB We demonstrate that multiangle polarization measurements in the near-UV and blue part of the spectrum are very well suited for passive remote sensing of aerosol layer height. For this purpose we use simulated measurements with different setups (different wavelength ranges, with and without polarization, different polarimetric accuracies) as well as airborne measurements from the Research Scanning Polarimeter (RSP) obtained over the continental USA. We find good agreement of the retrieved aerosol layer height from RSP with measurements from the Cloud Physics Lidar showing a mean absolute difference of less than 1km. Furthermore, we found that the information on aerosol layer height is provided for large part by the multiangle polarization measurements with high accuracy rather than the multiangle intensity measurements. The information on aerosol layer height is significantly decreased when the shortest RSP wavelength (410nm) is excluded from the retrieval and is virtually absent when 550nm is used as shortest wavelength.
C1 [Wu, Lianghai; Hasekamp, Otto] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[van Diedenhoven, Bastiaan; Cairns, Brian; Chowdhary, Jacek] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Yorks, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Chowdhary, Jacek] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Wu, LH (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands.
EM l.wu@sron.nl
FU NASA Radiation Sciences Program
FX The RSP data are available from NASA Goddard Institute for Space Studies
(http://data.giss.nasa.gov/pub/rsp/). The RSP data from the SEAC4RS and
PODEX field experiments that are used in this study were funded by the
NASA Radiation Sciences Program managed by Hal Maring and by the NASA
Earth Science Division as part of the preformulation study for the
Aerosol Cloud and ocean Ecosystem (ACE) mission. The CPL data are
provided by NASA Goddard Space Flight Center from the Web site at
http://cpl.gsfc.nasa.gov/.
NR 42
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8783
EP 8790
DI 10.1002/2016GL069848
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800054
ER
PT J
AU Newman, PA
Coy, L
Pawson, S
Lait, LR
AF Newman, P. A.
Coy, L.
Pawson, S.
Lait, L. R.
TI The anomalous change in the QBO in 2015-2016
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE QBO
ID QUASI-BIENNIAL OSCILLATION; EQUATORIAL STRATOSPHERE;
GENERAL-CIRCULATION; WIND; MODEL
AB The quasi-biennial oscillation (QBO) is a tropical lower stratospheric, downward propagating zonal wind variation, with an average period of similar to 8months. The QBO has been constantly documented since 1953. Here we describe the evolution of the QBO during the Northern Hemisphere winter of 2015-2016 using radiosonde observations and meteorological reanalyses. Normally, the QBO would show a steady downward propagation of the westerly phase. In 2015-2016, there was an anomalous upward displacement of this westerly phase from similar to 30hPa to 15hPa. These westerlies impinge on or cutoff the normal downward propagation of the easterly phase. In addition, easterly winds develop at 40hPa. Comparisons to tropical wind statistics for the 1953 to present record demonstrate that this 2015-2016 QBO disruption is unprecedented.
C1 [Newman, P. A.; Coy, L.; Pawson, S.; Lait, L. R.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Coy, L.] SSAI, Lanham, MD USA.
[Lait, L. R.] Morgan State Univ, Baltimore, MD 21239 USA.
RP Newman, PA (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA.
EM paul.a.newman@nasa.gov
FU NASA Modeling, Analysis, and Prediction program; NASA Atmospheric
Composition Modeling and Analysis Program
FX The help of Eric R. Nash and Gerald Ziemke is greatly appreciated. This
research was performed with funding from the NASA Modeling, Analysis,
and Prediction program and the NASA Atmospheric Composition Modeling and
Analysis Program. The MERRA-2 reanalysis fields were obtained from the
NASA Earth Observing System Data and Information System
(https://earthdata.nasa.gov). The monthly mean QBO data for the
1953-1978 period were obtained from the Freie Universitat Berlin
(http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/). Daily
global radiosondes have been collected at NASA/GSFC and are provided
from the Global Telecommunications System (available via the NOAA/NCEP
web site: ftp://ftp.cpc.ncep.noaa.gov/wd53rl/rsonde/).
NR 16
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U1 6
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8791
EP 8797
DI 10.1002/2016GL070373
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800055
ER
PT J
AU Mackie, CJ
Candian, A
Huang, XC
Maltseva, E
Petrignani, A
Oomens, J
Mattioda, AL
Buma, WJ
Lee, TJ
Tielens, AGGM
AF Mackie, Cameron J.
Candian, Alessandra
Huang, Xinchuan
Maltseva, Elena
Petrignani, Annemieke
Oomens, Jos
Mattioda, Andrew L.
Buma, Wybren Jan
Lee, Timothy J.
Tielens, Alexander G. G. M.
TI The anharmonic quartic force field infrared spectra of five non-linear
polycyclic aromatic hydrocarbons: Benz[a]anthracene, chrysene,
phenanthrene, pyrene, and triphenylene
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID EMISSION FEATURES; SPECTROSCOPY; PAHS; MOLECULES; GRAPHENE; DATABASE;
RINGS; IONS
AB The study of interstellar polycyclic aromatic hydrocarbons (PAHs) relies heavily on theoretically predicted infrared spectra. Most earlier studies use scaled harmonic frequencies for band positions and the double harmonic approximation for intensities. However, recent high-resolution gas-phase experimental spectroscopic studies have shown that the harmonic approximation is not sufficient to reproduce experimental results. In our previous work, we presented the anharmonic theoretical spectra of three linear PAHs, showing the importance of including anharmonicities into the theoretical calculations. In this paper, we continue this work by extending the study to include five non-linear PAHs (benz[a]anthracene, chrysene, phenanthrene, pyrene, and triphenylene), thereby allowing us to make a full assessment of how edge structure, symmetry, and size influence the effects of anharmonicities. The theoretical anharmonic spectra are compared to spectra obtained under matrix isolation low-temperature conditions, low-resolution, high-temperature gas-phase conditions, and high-resolution, low-temperature gas-phase conditions. Overall, excellent agreement is observed between the theoretical and experimental spectra although the experimental spectra show subtle but significant differences. Published by AIP Publishing.
C1 [Mackie, Cameron J.; Candian, Alessandra; Petrignani, Annemieke; Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Huang, Xinchuan] SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
[Maltseva, Elena; Petrignani, Annemieke; Buma, Wybren Jan] Univ Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Petrignani, Annemieke; Oomens, Jos] Radboud Univ Nijmegen, Toernooiveld 7, NL-6525 ED Nijmegen, Netherlands.
[Mattioda, Andrew L.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mackie, CJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM mackie@strw.leidenuniv.nl
RI Buma, Wybren Jan/F-6691-2011; Lee, Timothy/K-2838-2012; HUANG,
XINCHUAN/A-3266-2013;
OI Buma, Wybren Jan/0000-0002-1265-8016; Petrignani,
Annemieke/0000-0002-6116-5867; Candian, Alessandra/0000-0002-5431-4449
FU Advanced European Research Council [246976]; Spinoza award; Dutch
Astrochemistry Network - Netherlands Organization for Scientific
Research, NWO; NWO Exacte Wetenschappen [MP-270-13, MP-264]; NWO
[639.041.543, 723.014.007]; NASA [12-APRA12-0107]; NASA/SETI
[NNX15AF45A]; National Aeronautics and Space Administration through the
NASA Astrobiology Institute through the Science Mission Directorate
[NNH13ZDA017C]
FX The authors would like to thank the two anonymous reviewers for their
helpful comments that improved the clarity of the manuscript. The
spectroscopic study of interstellar PAHs at Leiden Observatory has been
supported through the Advanced European Research Council Grant No.
246976, a Spinoza award, and through the Dutch Astrochemistry Network
funded by the Netherlands Organization for Scientific Research, NWO.
Computing time has been made available by NWO Exacte Wetenschappen
(Project Nos. MP-270-13 and MP-264) and calculations were performed at
the LISA Linux cluster of the SurfSARA supercomputer center in Almere,
The Netherlands. A.C. acknowledges NWO for a VENI grant (639.041.543).
A.P. acknowledges NWO for a VIDI grant (723.014.007). 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-op Agreement NNX15AF45A. This
material is based upon work supported by the National Aeronautics and
Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice NNH13ZDA017C issued through the Science
Mission Directorate.
NR 44
TC 3
Z9 3
U1 17
U2 17
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD AUG 28
PY 2016
VL 145
IS 8
AR 084313
DI 10.1063/1.4961438
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DW8AL
UT WOS:000383875500034
PM 27586928
ER
PT J
AU Battaglia, A
Mroz, K
Lang, T
Tridon, F
Tanelli, S
Tian, L
Heymsfield, GM
AF Battaglia, A.
Mroz, K.
Lang, Tim
Tridon, F.
Tanelli, S.
Tian, Lin
Heymsfield, Gerald M.
TI Using a multiwavelength suite of microwave instruments to investigate
the microphysical structure of deep convective cores
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DUAL-WAVELENGTH RADAR; HYDROMETEOR IDENTIFICATION ALGORITHM;
RAIN-PROFILING ALGORITHM; MULTIPLE-SCATTERING; PART II; PRECIPITATION
RETRIEVAL; LIQUID WATER; CLOUD; ATTENUATION; RADIOMETER
AB Due to the large natural variability of its microphysical properties, the characterization of solid precipitation is a longstanding problem. Since in situ observations are unavailable in severe convective systems, innovative remote sensing retrievals are needed to extend our understanding of such systems. This study presents a novel technique able to retrieve the density, mass, and effective diameter of graupel and hail in severe convection through the combination of airborne microwave remote sensing instruments. The retrieval is applied to measure solid precipitation properties within two convective cells observed on 23-24 May 2014 over North Carolina during the IPHEx campaign by the NASA ER-2 instrument suite. Between 30 and 40 degrees of freedom of signal are associated with the measurements, which is insufficient to provide full microphysics profiling. The measurements have the largest impact on the retrieval of ice particle sizes, followed by ice water contents. Ice densities are mainly driven by a priori assumptions, though low relative errors in ice densities suggest that in extensive regions of the convective system, only particles with densities larger than 0.4 g/cm(3) are compatible with the observations. This is in agreement with reports of large hail on the ground and with hydrometeor classification derived from ground-based polarimetric radars observations. This work confirms that multiple scattering generated by large ice hydrometeors in deep convection is relevant for airborne radar systems already at Ku band. A fortiori, multiple scattering will play a pivotal role in such conditions also for Ku band spaceborne radars (e.g., the GPM Dual Precipitation Radar).
C1 [Battaglia, A.; Mroz, K.] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.
[Battaglia, A.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England.
[Lang, Tim] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tian, Lin; Heymsfield, Gerald M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Tian, Lin] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA.
RP Battaglia, A (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.; Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England.
EM a.battaglia@leicester.ac.uk
RI 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" - UK NERC [NE/L007169/1]; NASA
ACE Mission formulation; GPM Ground Validation; NASA Airborne Instrument
Technology Transition (AITT); ACE; GPM GV; NASA
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" funded by the UK NERC (NE/L007169/1).
The forward radar model code was courteously provided by R. Hogan
(http://www.met.rdg.ac.uk/clouds/multiscatter/). This research used the
ALICE High Performance Computing Facility at the University of
Leicester. CRS was supported by the NASA ACE Mission formulation. HIWRAP
was supported by GPM Ground Validation. EXRAD was supported by the NASA
Airborne Instrument Technology Transition (AITT). ER-2 flights were
jointly sponsored by GPM ground validation and the ACE Decadal Mission
study. AMPRs participation was supported by GPM GV. Timothy Lang was
supported by GPM GV. The work performed by Simone Tanelli was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA in support to the preformulation phase
studies for the ACE mission concept and to the GPM Science Team. NEXRAD
data were obtained from NOAA via the online data set hosted by Amazon
Web Services. NEXRAD processing code is available from
https://github.com/ARM-DOE/pyart,
https://github.com/CSU-Radarmet/CSU_RadarTools, and
https://github.com/nasa/DualPol. AMPR processing code is available from
https://github.com/nasa/PyAMPR.
NR 62
TC 0
Z9 0
U1 7
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9356
EP 9381
DI 10.1002/2016JD025269
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200006
PM 27708991
ER
PT J
AU Li, JLF
Wang, YH
Lee, T
Waliser, D
Lee, WL
Yu, JY
Chen, YC
Fetzer, E
Hasson, A
AF Li, J. -L. F.
Wang, Yi-Hui
Lee, Tong
Waliser, Duane
Lee, Wei-Liang
Yu, Jia-Yuh
Chen, Yi-Chun
Fetzer, Eric
Hasson, Audrey
TI The impacts of precipitating cloud radiative effects on ocean surface
evaporation, precipitation, and ocean salinity in coupled GCM
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GLOBAL WATER CYCLE; GENERAL-CIRCULATION MODEL; ABRUPT CLIMATE-CHANGE;
THERMOHALINE CIRCULATION; FLUX CORRECTION; PART I; CMIP3; VARIABILITY;
ARGO; INTENSIFICATION
AB The coupled global climate model (GCM) fidelity in representing upper ocean salinity including near sea surface bulk salinity (SSS) is evaluated in this study, with a focus on the Pacific Ocean. The systematic biases in ocean surface evaporation (E) minus precipitation (P) and SSS are found to be fairly similar in the twentieth century simulations of the Coupled Model Intercomparison Phase 3 (CMIP3) and Phase 5 (CMIP5) relative to the observations. One of the potential causes of the CMIP model biases is the missing representation of the radiative effects of precipitating hydrometeors (i.e., snow) in most CMIP models. To examine the radiative effect of cloud snow on SSS, sensitivity experiments with and without such effect are conducted by the National Center for Atmospheric Research-coupled Community Earth System Model (CESM). This study investigates the difference in SSS between sensitivity experiments and its relationship with atmospheric circulation, E - P and air-sea heat fluxes. It is found that the exclusion of the cloud snow radiative effect in CESM produces weaker Pacific trade winds, resulting in enhanced precipitation, reduced evaporation, and a reduction of the upper ocean salinity in the tropical and subtropical Pacific. The latter results in an improved comparison with climatological upper ocean bulk salinity. The introduction of cloud snow also altered the budget terms that maintain the time-mean salinity in the mixed layer.
C1 [Li, J. -L. F.; Wang, Yi-Hui; Lee, Tong; Waliser, Duane; Fetzer, Eric; Hasson, Audrey] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Li, J. -L. F.; Lee, Tong; Waliser, Duane; Fetzer, Eric] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Lee, Wei-Liang; Chen, Yi-Chun] Acad Sinica, Res Ctr Environm Change, Taipei, Taiwan.
[Yu, Jia-Yuh] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Li, JLF (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM Juilin.F.Li@jpl.nasa.gov
FU Earth Science Program, the Modeling, Analysis, and Prediction (MAP)
[NNH12ZDA001N ROSES 2012]; ATMOS COMP [NNH12ZDA001N-CCST]; NDOA;
National Aeronautics and Space Administration (NASA); NASA Physical
Oceanography Program; NASA; Ministry of Science and Technology of Taiwan
[NSC100-2119-M-001-029-MY5, NSC102-2111-M-001-009]
FX We acknowledge PCMDI/DOE and the WCRP's WGCM for their roles in making
CMIP3/CMIP5 available. We thank Qing Yue and Graeme Stephens for their
useful comments. The contribution by J.L.L. and D.E.W. to this study
were carried out on behalf of the Jet Propulsion Laboratory, California
Institute of Technology, under contracts of NNH12ZDA001N ROSES 2012,
Earth Science Program, the Modeling, Analysis, and Prediction (MAP), and
ATMOS COMP 2013 (NNH12ZDA001N-CCST) and J.J.L. under NDOA with the
National Aeronautics and Space Administration (NASA) as well as T.L.
from NASA Physical Oceanography Program. This work has been supported in
part by the NASA Making Earth System Data Records for Use in Research
Environments (MEaSUREs) programs. W.L.L. was supported by Ministry of
Science and Technology of Taiwan under contracts
NSC100-2119-M-001-029-MY5 and NSC102-2111-M-001-009. The subsurface
ocean salinity data from the World Ocean Atlas 2009 (WOA09) is used in
this study and can be found in
http://www.nodc.noaa.gov/OC5/WOA09/pr_woa09.html. The long-term mean
evaporation is based on the Objectively Analyzed air-sea Fluxes (OAFlux)
product [Yu and Weller,]. The OAFlux project began in 1958, and its
utilization of satellite-based, high-resolution ocean surface vector
winds since July 1987 weights the long-term mean in favor of the late
twentieth century and can be found at http://oaflux.whoi.edu/. The
long-term mean precipitation is obtained from the Global Precipitation
Climatology Project (GPCP)
(http://www.esrl.noaa.gov/psd/data/gridded/data.gpcp.html).
NR 72
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9474
EP 9491
DI 10.1002/2016JD024911
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200012
ER
PT J
AU Wen, GY
Marshak, A
Varnai, T
Levy, R
AF Wen, Guoyong
Marshak, Alexander
Varnai, Tamas
Levy, Robert
TI Testing the two-layer model for correcting near-cloud reflectance
enhancement using LES/SHDOM-simulated radiances
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADIATIVE-TRANSFER; CALIPSO OBSERVATIONS; AEROSOL PROPERTIES; BROKEN
CLOUDS; MODIS; PRODUCTS; VALIDATION; SCATTERING; SATELLITE; SURFACE
AB A transition zone exists between cloudy skies and clear sky; such that, clouds scatter solar radiation into clear-sky regions. From a satellite perspective, it appears that clouds enhance the radiation nearby. We seek a simple method to estimate this enhancement, since it is so computationally expensive to account for all three-dimensional (3-D) scattering processes. In previous studies, we developed a simple two-layer model (2LM) that estimated the radiation scattered via cloud-molecular interactions. Here we have developed a new model to account for cloud-surface interaction (CSI). We test the models by comparing to calculations provided by full 3-D radiative transfer simulations of realistic cloud scenes. For these scenes, the Moderate Resolution Imaging Spectroradiometer (MODIS)-like radiance fields were computed from the Spherical Harmonic Discrete Ordinate Method (SHDOM), based on a large number of cumulus fields simulated by the University of California, Los Angeles (UCLA) large eddy simulation (LES) model. We find that the original 2LM model that estimates cloud-air molecule interactions accounts for 64% of the total reflectance enhancement and the new model (2LM + CSI) that also includes cloud-surface interactions accounts for nearly 80%. We discuss the possibility of accounting for cloud-aerosol radiative interactions in 3-D cloud-induced reflectance enhancement, which may explain the remaining 20% of enhancements. Because these are simple models, these corrections can be applied to global satellite observations (e.g., MODIS) and help to reduce biases in aerosol and other clear-sky retrievals.
C1 [Wen, Guoyong; Marshak, Alexander; Varnai, Tamas; Levy, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wen, Guoyong] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Wen, GY (reprint author), Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
EM Guoyong.Wen-1@nasa.gov
RI Marshak, Alexander/D-5671-2012; Levy, Robert/M-7764-2013
OI Levy, Robert/0000-0002-8933-5303
FU NASA Radiation Program; NASA CALIPSO project; NASA Terra/Aqua projects
FX We gratefully acknowledge support for this research by the NASA
Radiation Program managed by Hal Maring, the NASA CALIPSO project
supervised by David Considine, and the NASA Terra/Aqua projects managed
by Paula Bontempi. We also thank Frank Evans for providing the results
of radiative transfer calculations for cumulus fields from Large-Eddy
Simulations.
NR 45
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9661
EP 9674
DI 10.1002/2016JD025021
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200023
ER
PT J
AU Lang, TJ
Lyons, WA
Cummer, SA
Fuchs, BR
Dolan, B
Rutledge, SA
Krehbiel, P
Rison, W
Stanley, M
Ashcraft, T
AF Lang, Timothy J.
Lyons, Walter A.
Cummer, Steven A.
Fuchs, Brody R.
Dolan, Brenda
Rutledge, Steven A.
Krehbiel, Paul
Rison, William
Stanley, Mark
Ashcraft, Thomas
TI Observations of two sprite-producing storms in Colorado
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHARGE MOMENT CHANGES; SEVERE THUNDERSTORM ELECTRIFICATION; MESOSCALE
CONVECTIVE SYSTEMS; CONTINENTAL UNITED-STATES; LIGHTNING FLASH RATE;
PART II; PRECIPITATION; RADAR; STEPS; ELVES
AB Two sprite-producing thunderstorms were observed on 8 and 25 June 2012 in northeastern Colorado by a combination of low-light cameras, a lightning mapping array, polarimetric and Doppler radars, the National Lightning Detection Network, and charge moment change measurements. The 8 June event evolved from a tornadic hailstorm to a larger multicellular system that produced 21 observed positive sprites in 2 h. The majority of sprites occurred during a lull in convective strength, as measured by total flash rate, flash energy, and radar echo volume. Mean flash area spiked multiple times during this period; however, total flash rates still exceeded 60 min(-1), and portions of the storm featured a complex anomalous charge structure, with midlevel positive charge near -20 degrees C. The storm produced predominantly positive cloud-to-ground lightning. All sprite-parent flashes occurred on the northeastern flank of the storm, where strong westerly upper level flow was consistent with advection of charged precipitation away from convection, providing a pathway for stratiform lightning. The 25 June event was another multicellular hailstorm with an anomalous charge structure that produced 26 positive sprites in less than 1 h. The sprites again occurred during a convective lull, with relatively weaker reflectivity and lower total flash rate but relatively larger mean flash area. However, all sprite parents occurred in or near convection and tapped charge layers in adjacent anvil cloud. The results demonstrate the sprite production by convective ground strokes in anomalously charged storms and also indicate that sprite production and convective vigor are inversely related in mature storms.
C1 [Lang, Timothy J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
[Cummer, Steven A.] Duke Univ, Durham, NC USA.
[Fuchs, Brody R.; Dolan, Brenda; Rutledge, Steven A.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Krehbiel, Paul; Rison, William; Stanley, Mark] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
[Ashcraft, Thomas] Heliotown Observ, Lamy, NM USA.
RP Lang, TJ (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM timothy.j.lang@nasa.gov
OI Fuchs, Brody/0000-0002-7629-0687
FU NASA; Defense Advanced Research Project Agency (DARPA); National Science
Foundation (NSF); NSF; National Oceanic and Atmospheric Administration
(NOAA)
FX Pat Kennedy, Dave Brunkow, Jim George, and Bob Bowie all contributed to
the CSU-CHILL and CSU-Pawnee radar scanning on the storm days analyzed
in this study, and thus, important data sets would not have been
available without their help. CSU radar data and COLMA data from DC3 are
available from the National Center for Atmospheric Research (NCAR;
http://data.eol.ucar.edu/master_list/?project=DC3). NEXRAD volumetric
radar data are available from Amazon Web Services
(https://aws.amazon.com/noaa-big-data/nexrad/), while MRMS data are
available from the National Severe Storms Laboratory
(http://www.nssl.noaa.gov/projects/mrms/). NLDN data are available from
the NASA Global Hydrology Resource Center
(https://ghrc.nsstc.nasa.gov/home/). Sounding data were obtained from
the University of Wyoming
(http://weather.uwyo.edu/upperair/sounding.html). Key open source
software packages used in this study include Py-ART
(http://arm-doe.github.io/pyart/), ARTview
(https://github.com/nguy/artview), lmatools
(https://github.com/deeplycloudy/lmatools), CSU_RadarTools
(https://github.com/CSU-Radarmet/CSU_RadarTools), DualPol
(https://github.com/nasa/DualPol), MMM-Py
(https://github.com/nasa/MMM-Py), SkewT
(https://pypi.python.org/pypi/SkewT), and SHARPpy
(http://sharppy.github.io/SHARPpy/). CEDRIC and SPRINT can be obtained
from NCAR (https://wiki.ucar.edu/display/raygridding/Home) along with
other useful radar software, such as Radx
(https://www.ral.ucar.edu/projects/titan/docs/radial_formats/radx.html).
Contact the first author (timothy.j.lang@nasa.gov) for access to other
data sets, such as sprite imagery and CMCN measurements. Lang also can
provide access to customized analysis software, such as CLEAR and XLMA.
Funding for this work was provided by the NASA Lightning Imaging Sensor
(LIS) project, the Defense Advanced Research Project Agency (DARPA)
Nimbus program, and the National Science Foundation (NSF) Physical
Meteorology and Lower Atmosphere Observing Facilities programs. DC3 was
made possible by the financial and logistical support of NSF, NASA, and
the National Oceanic and Atmospheric Administration (NOAA). The views,
opinions, and findings in this report are those of the authors and
should not be construed as an official NASA or U.S. Government position,
policy, or decision.
NR 85
TC 0
Z9 0
U1 7
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9675
EP 9695
DI 10.1002/2016JD025299
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200024
ER
PT J
AU Fast, JD
Berg, LK
Zhang, K
Easter, RC
Ferrare, RA
Hair, JW
Hostetler, CA
Liu, Y
Ortega, I
Sedlacek, A
Shilling, JE
Shrivastava, M
Springston, SR
Tomlinson, JM
Volkamer, R
Wilson, J
Zaveri, RA
Zelenyuk, A
AF Fast, Jerome D.
Berg, Larry K.
Zhang, Kai
Easter, Richard C.
Ferrare, Richard A.
Hair, Johnathan W.
Hostetler, Chris A.
Liu, Ying
Ortega, Ivan
Sedlacek, Arthur, III
Shilling, John E.
Shrivastava, Manish
Springston, Stephen R.
Tomlinson, Jason M.
Volkamer, Rainer
Wilson, Jacqueline
Zaveri, Rahul A.
Zelenyuk, Alla
TI Model representations of aerosol layers transported from North America
over the Atlantic Ocean during the Two-Column Aerosol Project
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; PHASE FRAGMENTATION REACTIONS; CLOUD
MICROPHYSICS SCHEME; SPECTRAL-RESOLUTION LIDAR; CARBON VERTICAL
PROFILES; GLOBAL CLIMATE MODEL; LONG-RANGE TRANSPORT; LOW-VOLATILITY
SOA; BASIS-SET APPROACH; ORGANIC AEROSOL
AB The ability of the Weather Research and Forecasting model with chemistry (WRF-Chem) version 3.7 and the Community Atmosphere Model version 5.3 (CAM5) in simulating profiles of aerosol properties is quantified using extensive in situ and remote sensing measurements from the Two-Column Aerosol Project (TCAP) conducted during July of 2012. TCAP was supported by the U.S. Department of Energy's Atmospheric Radiation Measurement program and was designed to obtain observations within two atmospheric columns; one fixed over Cape Cod, Massachusetts, and the other several hundred kilometers over the ocean. The performance is quantified using most of the available aircraft and surface measurements during July, and 2 days are examined in more detail to identify the processes responsible for the observed aerosol layers. The higher-resolution WRF-Chem model produced more aerosol mass in the free troposphere than the coarser-resolution CAM5 model so that the fraction of aerosol optical thicknessabove the residual layer from WRF-Chem was more consistent with lidar measurements. We found that the free troposphere layers are likely due to mean vertical motions associated with synoptic-scale convergence that lifts aerosols from the boundary layer. The vertical displacement and the time period associated with upward transport in the troposphere depend on the strength of the synoptic system and whether relatively high boundary layer aerosol concentrations are present where convergence occurs. While a parameterization of subgrid scale convective clouds applied in WRF-Chem modulated the concentrations of aerosols aloft, it did not significantly change the overall altitude and depth of the layers.
C1 [Fast, Jerome D.; Berg, Larry K.; Zhang, Kai; Easter, Richard C.; Liu, Ying; Shilling, John E.; Shrivastava, Manish; Tomlinson, Jason M.; Wilson, Jacqueline; Zaveri, Rahul A.; Zelenyuk, Alla] Pacific Northwest Natl Lab, Richland, WA 99352 USA.
[Ferrare, Richard A.; Hair, Johnathan W.; Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ortega, Ivan; Volkamer, Rainer] Univ Colorado, Dept Chem, Boulder, CO 80309 USA.
[Sedlacek, Arthur, III; Springston, Stephen R.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Fast, JD (reprint author), Pacific Northwest Natl Lab, Richland, WA 99352 USA.
EM jerome.fast@pnl.gov
RI Zhang, Kai/F-8415-2010; Volkamer, Rainer/B-8925-2016
OI Zhang, Kai/0000-0003-0457-6368; Volkamer, Rainer/0000-0002-0899-1369
FU Office of Science of the U.S. Department of Energy; DOE ARM
[DE-SC0006730]; National Science Foundation; [DE-A06-76RLO976 1830]
FX This research was supported by the Office of Science of the U.S.
Department of Energy as part of the Atmospheric Radiation Measurement
(ARM) and Atmospheric System Research (ASR) programs. The Pacific
Northwest National Laboratory (PNNL) is operated by DOE by the Battelle
Memorial Institute under contract DE-A06-76RLO976 1830. We thank the
contributions of numerous individuals, including the G-1 flight crew (M.
Hubbell, W. Svancara, J. Hone, and E. Dukes), King Air flight crew (R.
Yasky, L. Kagey, M. Wusk, D. Bowser, S. Sims, D. Riddick, and G.
Slover), staff from the Cape Cod National Seashore (Superintendent G.
Price, L. McKean, C. Skowron, and B. Dougan), Cape Cod National Seashore
Atlantic Research and Learning Center, and the radiosonde launch team
from the Provincetown Center for Coastal Studies (M. Dunn, S. Greene, C.
Hudak, L. Ludwig, J. Melander, D. Minsky, K. Shorr, S. Sollog, D.
Towler, E. Larson, D. Dionne, C. Skowron). Support for the HSRL-2 flight
operations during TCAP was provided by the DOE ARM program, Interagency
Agreement DE-SC0006730, while support for the development of HSRL-2 was
provided by the NASA Science Mission Directorate, ESTO, AITT, and
Radiation Science Programs. The NOAA-MFRSR measurements were supported
by NOAA GOES-R Cal/Val Activities within NOAA's National Environmental
Satellite, Data, and Information Service. We thank Joseph Michalsky
(NOAA) for providing the AOD measurements from the MFRSR instrument,
Louisa Emmons (NCAR) for providing the MOZART global chemistry model
output, Christine Wiedinmyer (NCAR) for providing the fire emissions
inventory, Stuart McKeen (NOAA) for processing the 2011 NEI, Michael
Sprenger and Heini Wernli (ETH) for providing the Lagrangian Analysis
Tool LAGRANTO for the CAM5 back trajectory calculations, and Po-Lun Ma
(PNNL) for assisting with the set up of CAM5. The Environmental
Molecular Science Laboratory (EMSL), a DOE Office of Science User
Facility located at PNNL, provided computational resources for the
WRF-Chem simulations. For the CAM5 simulations, we would like to
acknowledge the computing support from Yellowstone (ark:/85065/d7wd3xhc)
provided by NCAR's Computational and Information Systems Laboratory
(sponsored by the National Science Foundation) and from the PNNL
Institutional Computing (PIC). Data used in this manuscript are
available from the ARM data archive (www.archive.arm.gov) or from the
corresponding author (jerome.fast@pnnl.gov).
NR 108
TC 1
Z9 1
U1 8
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9814
EP 9848
DI 10.1002/2016JD025248
PG 35
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200031
ER
PT J
AU Li, JY
Mao, JQ
Min, KE
Washenfelder, RA
Brown, SS
Kaiser, J
Keutsch, FN
Volkamer, R
Wolfe, GM
Hanisco, TF
Pollack, IB
Ryerson, TB
Graus, M
Gilman, JB
Lerner, BM
Warneke, C
de Gouw, JA
Middlebrook, AM
Liao, J
Welti, A
Henderson, BH
McNeill, VF
Hall, SR
Ullmann, K
Donner, LJ
Paulot, F
Horowitz, LW
AF Li, Jingyi
Mao, Jingqiu
Min, Kyung-Eun
Washenfelder, Rebecca A.
Brown, Steven S.
Kaiser, Jennifer
Keutsch, Frank N.
Volkamer, Rainer
Wolfe, Glenn M.
Hanisco, Thomas F.
Pollack, Ilana B.
Ryerson, Thomas B.
Graus, Martin
Gilman, Jessica B.
Lerner, Brian M.
Warneke, Carsten
de Gouw, Joost A.
Middlebrook, Ann M.
Liao, Jin
Welti, Andre
Henderson, Barron H.
McNeill, V. Faye
Hall, Samuel R.
Ullmann, Kirk
Donner, Leo J.
Paulot, Fabien
Horowitz, Larry W.
TI Observational constraints on glyoxal production from isoprene oxidation
and its contribution to organic aerosol over the Southeast United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADICAL-INITIATED OXIDATION; MASTER CHEMICAL MECHANISM; METHYL VINYL
KETONE; GAS-PHASE; ATMOSPHERIC CHEMISTRY; TROPOSPHERIC DEGRADATION;
HETEROGENEOUS CHEMISTRY; AIRCRAFT MEASUREMENTS; PARTICULATE MATTER;
PEROXY-RADICALS
AB We use a 0-D photochemical box model and a 3-D global chemistry-climate model, combined with observations from the NOAA Southeast Nexus (SENEX) aircraft campaign, to understand the sources and sinks of glyoxal over the Southeast United States. Box model simulations suggest a large difference in glyoxal production among three isoprene oxidation mechanisms (AM3ST, AM3B, and Master Chemical Mechanism (MCM) v3.3.1). These mechanisms are then implemented into a 3-D global chemistry-climate model. Comparison with field observations shows that the average vertical profile of glyoxal is best reproduced by AM3ST with an effective reactive uptake coefficient.glyx of 2 x 10(-3) and AM3B without heterogeneous loss of glyoxal. The two mechanisms lead to 0-0.8 mu gm(-3) secondary organic aerosol (SOA) from glyoxal in the boundary layer of the Southeast U.S. in summer. We consider this to be the lower limit for the contribution of glyoxal to SOA, as other sources of glyoxal other than isoprene are not included in our model. In addition, we find that AM3B shows better agreement on both formaldehyde and the correlation between glyoxal and formaldehyde (RGF = [GLYX]/[HCHO]), resulting from the suppression of d-isoprene peroxy radicals. We also find that MCM v3.3.1 may underestimate glyoxal production from isoprene oxidation, in part due to an underestimated yield from the reaction of isoprene epoxydiol (IEPOX) peroxy radicals with HO2. Our work highlights that the gas-phase production of glyoxal represents a large uncertainty in quantifying its contribution to SOA.
C1 [Li, Jingyi; Mao, Jingqiu; Paulot, Fabien] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Mao, Jingqiu; Donner, Leo J.; Paulot, Fabien; Horowitz, Larry W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Min, Kyung-Eun; Washenfelder, Rebecca A.; Brown, Steven S.; Pollack, Ilana B.; Ryerson, Thomas B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Middlebrook, Ann M.; Liao, Jin; Welti, Andre] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Min, Kyung-Eun; Washenfelder, Rebecca A.; Volkamer, Rainer; Pollack, Ilana B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Liao, Jin; Welti, Andre] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Min, Kyung-Eun] Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Gwangju, South Korea.
[Brown, Steven S.; Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Kaiser, Jennifer; Keutsch, Frank N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Keutsch, Frank N.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Wolfe, Glenn M.; Hanisco, Thomas F.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Pollack, Ilana B.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Graus, Martin] Univ Innsbruck, Inst Atmospher & Cryospher Sci, Innsbruck, Austria.
[Welti, Andre] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Henderson, Barron H.] Univ Florida, Dept Environm Engn Sci, Engn Sch Sustainable Infrastruct & Environm, Gainesville, FL 32611 USA.
[McNeill, V. Faye] Columbia Univ, Dept Chem Engn, New York, NY USA.
[Hall, Samuel R.; Ullmann, Kirk] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
RP Mao, JQ (reprint author), Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.; Mao, JQ (reprint author), NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
EM Jingqiu.Mao@noaa.gov
RI Volkamer, Rainer/B-8925-2016; Graus, Martin/E-7546-2010; Mao,
Jingqiu/F-2511-2010; de Gouw, Joost/A-9675-2008; Gilman,
Jessica/E-7751-2010; Pollack, Ilana/F-9875-2012; Washenfelder,
Rebecca/E-7169-2010; Middlebrook, Ann/E-4831-2011; Wolfe,
Glenn/D-5289-2011; Brown, Steven/I-1762-2013; Manager, CSD
Publications/B-2789-2015
OI Volkamer, Rainer/0000-0002-0899-1369; Graus, Martin/0000-0002-2025-9242;
Mao, Jingqiu/0000-0002-4774-9751; de Gouw, Joost/0000-0002-0385-1826;
Gilman, Jessica/0000-0002-7899-9948; Washenfelder,
Rebecca/0000-0002-8106-3702; Middlebrook, Ann/0000-0002-2984-6304;
FU NOAA Climate Program Office [NA13OAR4310071, NA14OAR4320106]; NOAA
Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program; EPA
[83540601]; NASA [NNH10ZDA001N-SEAC4RS]; NASA Headquarters under the
NASA Earth and Space Science Fellowship Program [NNX14AK97H]; NSF EAGER
[AGS-1452317]; NSF [AGS-1546136]
FX The authors thank Charles A. Brock (NOAA) for providing the aerosol size
data, Vaishali Naik (UCAR/NOAA) for providing the emission inventories
from the SENEX campaign, and William Cooke for the help with convection
scheme of the AM3 model. J.L., J.M., and L.W.H. acknowledge supports by
the NOAA Climate Program Office grant NA13OAR4310071 and NA14OAR4320106.
K.E.M., R.A.W., and S.S.B. acknowledge the support from the NOAA
Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program. J.K.,
F.N.K., G.M.W., and T.F.H. are grateful for the support from EPA Science
to Achieve Results program grant 83540601 and NASA grant
NNH10ZDA001N-SEAC4RS. J. Kaiser acknowledges support from NASA
Headquarters under the NASA Earth and Space Science Fellowship Program
grant NNX14AK97H. R.V. is grateful for the support from NSF EAGER award
AGS-1452317. V.F.M. acknowledges support from NSF (AGS-1546136). We
thank the staff at the NOAA Aircraft Operations Center and the WP-3D
flight crew for their help in instrumenting the aircraft and for
conducting the flights. Special thanks go to Songmiao Fan (NOAA) for the
helpful discussions. This research has not been subjected to any EPA
review and therefore does not necessarily reflect the views of the
agency, and no official endorsement should be inferred. Observational
data sets and modeling results are available upon request to the
corresponding author (Jingqiu.Mao@noaa.gov).
NR 92
TC 0
Z9 0
U1 19
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9849
EP 9861
DI 10.1002/2016JD025331
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200032
ER
PT J
AU Ware, J
Kort, EA
DeCola, P
Duren, R
AF Ware, John
Kort, Eric A.
DeCola, Phil
Duren, Riley
TI Aerosol lidar observations of atmospheric mixing in Los Angeles:
Climatology and implications for greenhouse gas observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BOUNDARY-LAYER HEIGHT; AIR-POLLUTANT TRANSPORT; FIELD-OF-VIEW; CO2
EMISSIONS; COASTAL ENVIRONMENT; SIMULATIONS; BACKSCATTER; DEPENDENCE;
SYSTEM; DEPTH
AB Atmospheric observations of greenhouse gases provide essential information on sources and sinks of these key atmospheric constituents. To quantify fluxes from atmospheric observations, representation of transport-especially vertical mixing-is a necessity and often a source of error. We report on remotely sensed profiles of vertical aerosol distribution taken over a 2 year period in Pasadena, California. Using an automated analysis system, we estimate daytime mixing layer depth, achieving high confidence in the afternoon maximum on 51% of days with profiles from a Sigma Space Mini Micropulse LiDAR (MiniMPL) and on 36% of days with a Vaisala CL51 ceilometer. We note that considering ceilometer data on a logarithmic scale, a standard method, introduces, an offset in mixing height retrievals. The mean afternoon maximum mixing height is 770 m Above Ground Level in summer and 670 m in winter, with significant day-to-day variance (within season sigma = 220 m approximate to 30%). Taking advantage of the MiniMPL's portability, we demonstrate the feasibility of measuring the detailed horizontal structure of the mixing layer by automobile. We compare our observations to planetary boundary layer (PBL) heights from sonde launches, North American regional reanalysis (NARR), and a custom Weather Research and Forecasting (WRF) model developed for greenhouse gas (GHG) monitoring in Los Angeles. NARR and WRF PBL heights at Pasadena are both systematically higher than measured, NARR by 2.5 times; these biases will cause proportional errors in GHG flux estimates using modeled transport. We discuss how sustained lidar observations can be used to reduce flux inversion error by selecting suitable analysis periods, calibrating models, or characterizing bias for correction in post processing.
C1 [Ware, John] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Ware, John; Kort, Eric A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[DeCola, Phil] Sigma Space Corp, Lanham, MD USA.
[Duren, Riley] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Ware, J (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.; Ware, J (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM johnware@umich.edu
RI Kort, Eric/F-9942-2012
OI Kort, Eric/0000-0003-4940-7541
FU NASA [NNN12AA01C]; NASA
FX This work was supported by NASA under grant NNN12AA01C. Portions of this
work were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. We thank Taylor Jones
for assistance in setting up and operating the MiniMPL instrument and
Athena Sparks for help with data preprocessing. We thank Vineet Yadav
for generating and providing WRF model output. NARR data provided by the
NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at
http://www.esrl.noaa.gov/psd/. The authors would also like to thank the
Megacities Carbon Project team for useful discussion and feedback.
Mixing depth data will be available through the Megacities Carbon
Project portal at https://megacities.jpl.nasa.gov. To obtain a copy of
the analysis system used to generate the estimates, please contact the
authors at johnware@umich.edu.
NR 50
TC 0
Z9 0
U1 6
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2016
VL 121
IS 16
BP 9862
EP 9878
DI 10.1002/2016JD024953
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200033
PM 27867786
ER
PT J
AU Mezuman, K
Bauer, SE
Tsigaridis, K
AF Mezuman, Keren
Bauer, Susanne E.
Tsigaridis, Kostas
TI Evaluating secondary inorganic aerosols in three dimensions
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; AQUEOUS-PHASE-TRANSITIONS; TROPOSPHERIC
OZONE; GODDARD-INSTITUTE; ATMOSPHERIC AEROSOLS; AMMONIUM-NITRATE;
UNITED-STATES; GLOBAL-MODEL; MINERAL DUST; EMISSIONS
AB The spatial distribution of aerosols and their chemical composition dictates whether aerosols have a cooling or a warming effect on the climate system. Hence, properly modeling the three-dimensional distribution of aerosols is a crucial step for coherent climate simulations. Since surface measurement networks only give 2-D data, and most satellites supply integrated column information, it is thus important to integrate aircraft measurements in climate model evaluations. In this study, the vertical distribution of secondary inorganic aerosol (i.e., sulfate, ammonium, and nitrate) is evaluated against a collection of 14 AMS flight campaigns and surface measurements from 2000 to 2010 in the USA and Europe. GISS ModelE2 is used with multiple aerosol microphysics (MATRIX, OMA) and thermodynamic (ISOR-ROPIA II, EQSAM) configurations. Our results show that the MATRIX microphysical scheme improves the model performance for sulfate, but that there is a systematic underestimation of ammonium and nitrate over the USA and Europe in all model configurations. In terms of gaseous precursors, nitric acid concentrations are largely underestimated at the surface while overestimated in the higher levels of the model. Heterogeneous reactions on dust surfaces are an important sink for nitric acid, even high in the troposphere. At high altitudes, nitrate formation is calculated to be ammonia limited. The underestimation of ammonium and nitrate in polluted regions is most likely caused by a too simplified treatment of the NH3 / NH4+ partitioning which affects the HNO3 / NO3- partitioning.
C1 [Mezuman, Keren] Columbia Univ, Earth & Environm Sci, New York, NY USA.
[Mezuman, Keren; Bauer, Susanne E.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bauer, Susanne E.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
RP Bauer, SE (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Bauer, SE (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
EM susanne.bauer@columbia.edu
FU NASA; NASA High-End Computing (HEC) Program through NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center; NASA's
Atmospheric Composition Modeling and Analysis Program (ACMAP)
[NNX15AE36G]
FX Climate modeling at GISS is supported by the NASA Modeling, Analysis,
and Prediction program. Resources supporting this work were provided by
the NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center. SEB and KT
acknowledge funding from NASA's Atmospheric Composition Modeling and
Analysis Program (ACMAP), contract number NNX15AE36G. We acknowledge the
IMPROVE monitoring program for providing data. EMEP measurement data
were extracted from the EBAS database, which is maintained and further
developed by the Norwegian Institute for Air Research (NILU). We
acknowledge the Toolsets for Airborne Data (TAD)
website:https://tad.larc.nasa.gov, as well as the site
https://sites.google.com/site/amsglobaldatabase/ maintained by the Zhang
and Jimenez groups.
NR 70
TC 1
Z9 1
U1 15
U2 15
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 26
PY 2016
VL 16
IS 16
BP 10651
EP 10669
DI 10.5194/acp-16-10651-2016
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6EW
UT WOS:000383743200002
ER
PT J
AU Adams, C
Normand, EN
McLinden, CA
Bourassa, AE
Lloyd, ND
Degenstein, DA
Krotkov, NA
Rivas, MB
Boersma, KF
Eskes, H
AF Adams, Cristen
Normand, Elise N.
McLinden, Chris A.
Bourassa, Adam E.
Lloyd, Nicholas D.
Degenstein, Douglas A.
Krotkov, Nickolay A.
Rivas, Maria Belmonte
Boersma, K. Folkert
Eskes, Henk
TI Limb-nadir matching using non-coincident NO2 observations: proof of
concept and the OMI-minus-OSIRIS prototype product
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; NITROGEN-DIOXIDE;
STRATOSPHERIC OZONE; RETRIEVAL ALGORITHM; MIDDLE ATMOSPHERE; COLUMN
RETRIEVAL; SCIAMACHY; SATELLITE; MISSION
AB A variant of the limb-nadir matching technique for deriving tropospheric NO2 columns is presented in which the stratospheric component of the NO2 slant column density (SCD) measured by the Ozone Monitoring Instrument (OMI) is removed using non-coincident profiles from the Optical Spectrograph and InfraRed Imaging System (OSIRIS). In order to correct their mismatch in local time and the diurnal variation of stratospheric NO2 OSIRIS profiles, which were measured just after sunrise, were mapped to the local time of OMI observations using a photochemical box model. Following the profile time adjustment, OSIRIS NO2 stratospheric vertical column densities (VCDs) were calculated. For profiles that did not reach down to the tropopause, VCDs were adjusted using the photochemical model. Using air mass factors from the OMI Standard Product (SP), a new tropospheric NO2 VCD product -referred to as OMI-minus-OSIRIS (OmO) - was generated through limb-nadir matching. To accomplish this, the OMI total SCDs were scaled using correction factors derived from the next-generation SCDs that improve upon the spectral fitting used for the current operational products. One year, 2008, of OmO was generated for 60 degrees S to 60 degrees N and a cursory evaluation was performed. The OmO product was found to capture the main features of tropospheric NO2, including a background value of about 0.3 x 10(15) molecules cm(-2) over the tropical Pacific and values comparable to the OMI operational products over anthropogenic source areas. While additional study is required, these results suggest that a limb-nadir matching approach is feasible for the removal of stratospheric NO2 measured by a polar orbiter from a nadir-viewing instrument in a geostationary orbit such as Tropospheric Emissions: Monitoring of Pollution (TEMPO) or Sentinel-4.
C1 [Adams, Cristen; Normand, Elise N.; Bourassa, Adam E.; Lloyd, Nicholas D.; Degenstein, Douglas A.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada.
[Adams, Cristen] Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada.
[McLinden, Chris A.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada.
[Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Rivas, Maria Belmonte; Boersma, K. Folkert; Eskes, Henk] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
[Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands.
RP Adams, C (reprint author), Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada.; Adams, C (reprint author), Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada.
EM cristenlfadams@gmail.com
RI Boersma, Klaas/H-4559-2012
OI Boersma, Klaas/0000-0002-4591-7635
FU Natural Sciences and Engineering Research Council (Canada); Canadian
Space Agency; Sweden (SNSB); Canada (CSA); France (CNES); Finland
(Tekes)
FX This work was supported by the Natural Sciences and Engineering Research
Council (Canada) and the Canadian Space Agency. Odin is a Swedish-led
satellite project funded jointly by Sweden (SNSB), Canada (CSA), France
(CNES), and Finland (Tekes). The authors thank David Plummer for the
provision of climatological fields from the Canadian Middle Atmosphere
Model. Thanks to Sergey Marchenko for providing the OMI SCD bias
correction factors. Thank you also to Chris Roth for help with the
OSIRIS database.
NR 56
TC 1
Z9 1
U1 3
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 26
PY 2016
VL 9
IS 8
BP 4103
EP 4122
DI 10.5194/amt-9-4103-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW7PH
UT WOS:000383842900001
ER
PT J
AU Aguilar, M
Alpat, B
Alpat, B
Ambrosi, G
Arruda, L
Attig, N
Aupetit, S
Azzarello, P
Bachlechner, A
Barao, F
Barrau, A
Barrin, L
Bartoloni, A
Basara, L
Basegmez-du Pree, S
Battarbee, M
Battiston, R
Bazo, J
Becker, U
Behlmann, M
Beischer, B
Berdugo, J
Bertucci, B
Bindi, V
Boella, G
de Boer, W
Bollweg, K
Bonnivard, V
Borgia, B
Boschini, MJ
Bourquin, M
Bueno, EF
Burger, J
Cadoux, F
Cai, XD
Capell, M
Caroff, S
Casaus, J
Castellini, G
Cernuda, I
Cervelli, F
Chae, MJ
Chang, YH
Chen, AI
Chen, GM
Chen, HS
Cheng, L
Chou, HY
Choumilov, E
Choutko, V
Chung, CH
Clark, C
Clavero, R
Coignet, G
Consolandi, C
Contin, A
Corti, C
Coste, B
Creus, W
Crispoltoni, M
Cui, Z
Dai, YM
Delgado, C
Della Torre, S
Demirkoz, MB
Derome, L
Di Falco, S
Dimiccoli, F
Diaz, C
von Doetinchem, P
Dong, F
Donnini, F
Duranti, M
D'Urso, D
Egorov, A
Eline, A
Eronen, T
Feng, J
Fiandrini, E
Finch, E
Fisher, P
Formato, V
Galaktionov, Y
Gallucci, G
Garcia, B
Garcia-Lopez, RJ
Gargiulo, C
Gast, H
Gebauer, I
Gervasi, M
Ghelfi, A
Giovacchini, F
Goglov, P
Gomez-Coral, DM
Gong, J
Goy, C
Grabski, V
Grandi, D
Graziani, M
Guerri, I
Guo, KH
Habiby, M
Haino, S
Han, KC
He, ZH
Heil, M
Hoffman, J
Hsieh, TH
Huang, H
Huang, ZC
Huh, C
Incagli, M
Ionica, M
Jang, WY
Jinchi, H
Kang, SC
Kanishev, K
Kim, GN
Kim, KS
Kirn, T
Konak, C
Kounina, O
Kounine, A
Koutsenko, V
Krafczyk, MS
La Vacca, G
Laudi, E
Laurenti, G
Lazzizzera, I
Lebedev, A
Lee, HT
Lee, SC
Leluc, C
Li, HS
Li, JQ
Li, JQ
Li, Q
Li, TX
Li, W
Li, ZH
Li, ZY
Lim, S
Lin, CH
Lipari, P
Lippert, T
Liu, D
Liu, H
Lu, SQ
Lu, YS
Luebelsmeyer, K
Luo, F
Luo, JZ
Lv, SS
Majka, R
Mana, C
Marin, J
Martin, T
Martinez, G
Masi, N
Maurin, D
Menchaca-Rocha, A
Meng, Q
Mo, DC
Morescalchi, L
Mott, P
Nelson, T
Ni, JQ
Nikonov, N
Nozzoli, F
Nunes, P
Oliva, A
Orcinha, M
Palmonari, F
Palomares, C
Paniccia, M
Pauluzzi, M
Pensotti, S
Pereira, R
Picot-Clemente, N
Pilo, F
Pizzolotto, C
Plyaskin, V
Pohl, M
Poireau, V
Putze, A
Quadrani, L
Qi, XM
Qin, X
Qu, ZY
Raiha, T
Rancoita, PG
Rapin, D
Ricol, JS
Rodriguez, I
Rosier-Lees, S
Rozhkov, A
Rozza, D
Sagdeev, R
Sandweiss, J
Saouter, P
Schael, S
Schmidt, SM
von Dratzig, AS
Schwering, G
Seo, ES
Shan, BS
Shi, JY
Siedenburg, T
Son, D
Song, JW
Sun, WH
Tacconi, M
Tang, XW
Tang, ZC
Tao, L
Tescaro, D
Ting, SCC
Ting, SM
Tomassetti, N
Torsti, J
Turkoglu, C
Urban, T
Vagelli, V
Valente, E
Vannini, C
Valtonen, E
Acosta, MV
Vecchi, M
Velasco, M
Vialle, JP
Vitale, V
Vitillo, S
Wang, LQ
Wang, NH
Wang, QL
Wang, X
Wang, XQ
Wang, ZX
Wei, CC
Weng, ZL
Whitman, K
Wienkenhover, J
Willenbrock, M
Wu, H
Wu, X
Xia, X
Xiong, RQ
Xu, W
Yan, Q
Yang, J
Yang, M
Yang, Y
Yi, H
Yu, YJ
Yu, ZQ
Zeissler, S
Zhang, C
Zhang, J
Zhang, JH
Zhang, SD
Zhang, SW
Zhang, Z
Zheng, ZM
Zhu, ZQ
Zhuang, HL
Zhukov, V
Zichichi, A
Zimmermann, N
Zuccon, P
AF Aguilar, M.
Alpat, B.
Alpat, B.
Ambrosi, G.
Arruda, L.
Attig, N.
Aupetit, S.
Azzarello, P.
Bachlechner, A.
Barao, F.
Barrau, A.
Barrin, L.
Bartoloni, A.
Basara, L.
Basegmez-du Pree, S.
Battarbee, M.
Battiston, R.
Bazo, J.
Becker, U.
Behlmann, M.
Beischer, B.
Berdugo, J.
Bertucci, B.
Bindi, V.
Boella, G.
de Boer, W.
Bollweg, K.
Bonnivard, V.
Borgia, B.
Boschini, M. J.
Bourquin, M.
Bueno, E. F.
Burger, J.
Cadoux, F.
Cai, X. D.
Capell, M.
Caroff, S.
Casaus, J.
Castellini, G.
Cernuda, I.
Cervelli, F.
Chae, M. J.
Chang, Y. H.
Chen, A. I.
Chen, G. M.
Chen, H. S.
Cheng, L.
Chou, H. Y.
Choumilov, E.
Choutko, V.
Chung, C. H.
Clark, C.
Clavero, R.
Coignet, G.
Consolandi, C.
Contin, A.
Corti, C.
Coste, B.
Creus, W.
Crispoltoni, M.
Cui, Z.
Dai, Y. M.
Delgado, C.
Della Torre, S.
Demirkoz, M. B.
Derome, L.
Di Falco, S.
Dimiccoli, F.
Diaz, C.
von Doetinchem, P.
Dong, F.
Donnini, F.
Duranti, M.
D'Urso, D.
Egorov, A.
Eline, A.
Eronen, T.
Feng, J.
Fiandrini, E.
Finch, E.
Fisher, P.
Formato, V.
Galaktionov, Y.
Gallucci, G.
Garcia, B.
Garcia-Lopez, R. J.
Gargiulo, C.
Gast, H.
Gebauer, I.
Gervasi, M.
Ghelfi, A.
Giovacchini, F.
Goglov, P.
Gomez-Coral, D. M.
Gong, J.
Goy, C.
Grabski, V.
Grandi, D.
Graziani, M.
Guerri, I.
Guo, K. H.
Habiby, M.
Haino, S.
Han, K. C.
He, Z. H.
Heil, M.
Hoffman, J.
Hsieh, T. H.
Huang, H.
Huang, Z. C.
Huh, C.
Incagli, M.
Ionica, M.
Jang, W. Y.
Jinchi, H.
Kang, S. C.
Kanishev, K.
Kim, G. N.
Kim, K. S.
Kirn, Th.
Konak, C.
Kounina, O.
Kounine, A.
Koutsenko, V.
Krafczyk, M. S.
La Vacca, G.
Laudi, E.
Laurenti, G.
Lazzizzera, I.
Lebedev, A.
Lee, H. T.
Lee, S. C.
Leluc, C.
Li, H. S.
Li, J. Q.
Li, J. Q.
Li, Q.
Li, T. X.
Li, W.
Li, Z. H.
Li, Z. Y.
Lim, S.
Lin, C. H.
Lipari, P.
Lippert, T.
Liu, D.
Liu, Hu
Lu, S. Q.
Lu, Y. S.
Luebelsmeyer, K.
Luo, F.
Luo, J. Z.
Lv, S. S.
Majka, R.
Mana, C.
Marin, J.
Martin, T.
Martinez, G.
Masi, N.
Maurin, D.
Menchaca-Rocha, A.
Meng, Q.
Mo, D. C.
Morescalchi, L.
Mott, P.
Nelson, T.
Ni, J. Q.
Nikonov, N.
Nozzoli, F.
Nunes, P.
Oliva, A.
Orcinha, M.
Palmonari, F.
Palomares, C.
Paniccia, M.
Pauluzzi, M.
Pensotti, S.
Pereira, R.
Picot-Clemente, N.
Pilo, F.
Pizzolotto, C.
Plyaskin, V.
Pohl, M.
Poireau, V.
Putze, A.
Quadrani, L.
Qi, X. M.
Qin, X.
Qu, Z. Y.
Raiha, T.
Rancoita, P. G.
Rapin, D.
Ricol, J. S.
Rodriguez, I.
Rosier-Lees, S.
Rozhkov, A.
Rozza, D.
Sagdeev, R.
Sandweiss, J.
Saouter, P.
Schael, S.
Schmidt, S. M.
von Dratzig, A. Schulz
Schwering, G.
Seo, E. S.
Shan, B. S.
Shi, J. Y.
Siedenburg, T.
Son, D.
Song, J. W.
Sun, W. H.
Tacconi, M.
Tang, X. W.
Tang, Z. C.
Tao, L.
Tescaro, D.
Ting, Samuel C. C.
Ting, S. M.
Tomassetti, N.
Torsti, J.
Turkoglu, C.
Urban, T.
Vagelli, V.
Valente, E.
Vannini, C.
Valtonen, E.
Acosta, M. Vazquez
Vecchi, M.
Velasco, M.
Vialle, J. P.
Vitale, V.
Vitillo, S.
Wang, L. Q.
Wang, N. H.
Wang, Q. L.
Wang, X.
Wang, X. Q.
Wang, Z. X.
Wei, C. C.
Weng, Z. L.
Whitman, K.
Wienkenhover, J.
Willenbrock, M.
Wu, H.
Wu, X.
Xia, X.
Xiong, R. Q.
Xu, W.
Yan, Q.
Yang, J.
Yang, M.
Yang, Y.
Yi, H.
Yu, Y. J.
Yu, Z. Q.
Zeissler, S.
Zhang, C.
Zhang, J.
Zhang, J. H.
Zhang, S. D.
Zhang, S. W.
Zhang, Z.
Zheng, Z. M.
Zhu, Z. Q.
Zhuang, H. L.
Zhukov, V.
Zichichi, A.
Zimmermann, N.
Zuccon, P.
CA AMS Collaboration
TI Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of
Elementary Particle Fluxes in Primary Cosmic Rays Measured with the
Alpha Magnetic Spectrometer on the International Space Station
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; GEOMAGNETIC REFERENCE FIELD; DARK-MATTER;
RICH DETECTOR; ANTI-PROTONS; AMS-02 TRD; GEV-C; POSITRONS; NUCLEI;
CARBON
AB A precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio in primary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 x 10(5) antiproton events and 2.42 x 10(9) proton events. The fluxes and flux ratios of charged elementary particles in cosmic rays are also presented. In the absolute rigidity range similar to 60 to similar to 500 GV, the antiproton (p) over bar, proton p, and positron e(+) fluxes are found to have nearly identical rigidity dependence and the electron e(-) flux exhibits a different rigidity dependence. Below 60 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios each reaches a maximum. From similar to 60 to similar to 500 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios show no rigidity dependence. These are new observations of the properties of elementary particles in the cosmos.
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[Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Nikonov, N.; Raiha, T.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhover, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany.
[Demirkoz, M. B.; Konak, C.; Turkoglu, C.] Middle E Tech Univ, Dept Phys, TR-06800 Ankara, Turkey.
[Caroff, S.; Coignet, G.; Goy, C.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vialle, J. P.] CNRS IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France.
[Li, W.; Shan, B. S.; Zheng, Z. M.] Beihang Univ BUAA, Beijing 100191, Peoples R China.
[Dai, Y. M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, Inst Elect Engn IEE, Beijing 100190, Peoples R China.
[Bachlechner, A.; Basegmez-du Pree, S.; Chen, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Wang, X. Q.; Yang, M.; Yu, Z. Q.; Zhang, C.; Zhang, S. W.; Zhuang, H. L.] Chinese Acad Sci, Inst High Energy Phys IHEP, Beijing 100049, Peoples R China.
[Contin, A.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Contin, A.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
[Becker, U.; Behlmann, M.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Choumilov, E.; Choutko, V.; Egorov, A.; Eline, A.; Fisher, P.; Galaktionov, Y.; Goglov, P.; Heil, M.; Hsieh, T. H.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Li, J. Q.; Plyaskin, V.; Rozhkov, A.; Sun, W. H.; Ting, Samuel C. C.; Ting, S. M.; Wang, X.; Weng, Z. L.; Willenbrock, M.; Xu, W.; Yan, Q.; Zhang, J.; Zhang, S. D.; Zhang, Z.; Zhu, Z. Q.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
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[Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
[Picot-Clemente, N.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Huh, C.; Jang, W. Y.; Kang, S. C.; Kim, G. N.; Kim, K. S.; Lim, S.; Son, D.] Kyungpook Natl Univ, CHEP, Daegu 41566, South Korea.
[Castellini, G.] CNR IROE, I-50125 Florence, Italy.
[Barrin, L.; Crispoltoni, M.; Formato, V.; Gargiulo, C.; Laudi, E.; Ting, Samuel C. C.] European Org Nucl Res CERN, CH-1211 Geneva 23, Switzerland.
[Azzarello, P.; Bourquin, M.; Cadoux, F.; Habiby, M.; Leluc, C.; Paniccia, M.; Pohl, M.; Rapin, D.; Saouter, P.; Vitillo, S.; Wu, X.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
[Aupetit, S.; Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] CNRS IN2P3, LPSC, F-38026 Grenoble, France.
[Aupetit, S.; Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] Univ Grenoble Alpes, F-38026 Grenoble, France.
[Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S. S.; Mo, D. C.; Ni, J. Q.; Qi, X. M.; Wang, Z. X.] Sun Yat Sen Univ SYSU, Guangzhou 510275, Guangdong, Peoples R China.
[Bindi, V.; Consolandi, C.; Corti, C.; von Doetinchem, P.; Hoffman, J.; Nelson, T.; Pereira, R.; Whitman, K.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] NASA, Johnson Space Ctr JSC, Jacobs Engn & Business Integra, Houston, TX 77058 USA.
[Attig, N.; Lippert, T.; Schmidt, S. M.] Julich Supercomp Ctr, D-52425 Julich, Germany.
[Attig, N.; Lippert, T.; Schmidt, S. M.] Res Ctr Julich, JARA FAME, D-52425 Julich, Germany.
[de Boer, W.; Gebauer, I.; Zeissler, S.] KIT, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
[Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] IAC, E-38205 San Cristobal la Laguna, Spain.
[Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Arruda, L.; Barao, F.; Nunes, P.; Orcinha, M.] Lab Instrumentacao & Fis Expt Particulas LIP, P-1000 Lisbon, Portugal.
[Han, K. C.; Jinchi, H.] Natl Chung Shan Inst Sci & Technol NCSIST, Taoyuan 32546, Taiwan.
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[Gomez-Coral, D. M.; Grabski, V.; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
[Boella, G.; Boschini, M. J.; Della Torre, S.; Gervasi, M.; Grandi, D.; La Vacca, G.; Pensotti, S.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy.
[Boella, G.; Gervasi, M.; Pensotti, S.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Dong, F.; Gong, J.; Li, J. Q.; Li, Q.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. H.] Southeast Univ SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
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[Battiston, R.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.] Univ Trento, I-38123 Povo, Trento, Italy.
[Bartoloni, A.; Borgia, B.; Lipari, P.; Valente, E.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Borgia, B.; Valente, E.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Bueno, E. F.; Vecchi, M.] Univ Sao Paulo, Inst Fis Sao Carlos, CP 369, BR-13560970 Sao Carlos, SP, Brazil.
[Chae, M. J.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
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[Li, H. S.; Yang, Y.] Natl Cheng Kung Univ, Tainan 70101, Taiwan.
[Lee, H. T.] Acad Sinica Grid Ctr ASGC, Taipei 11529, Taiwan.
[Feng, J.; Haino, S.; Huang, H.; Lee, S. C.; Li, Z. Y.; Lin, C. H.; Liu, D.; Lu, S. Q.; Qu, Z. Y.; Wei, C. C.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
[Battarbee, M.; Eronen, T.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland.
ASI, I-00133 Rome, Italy.
[Bazo, J.] PUCP, Dept Ciencias, Lima 32, Peru.
[Bachlechner, A.; D'Urso, D.; Nozzoli, F.; Pizzolotto, C.; Vitale, V.] ASDC, I-00133 Rome, Italy.
[Feng, J.; Li, Z. Y.; Lu, S. Q.] Sun Yat Sen Univ, Guangzhou 510275, Guangdong, Peoples R China.
[Huang, H.; Zhang, J.] Wuhan Univ, Wuhan 430072, Peoples R China.
[Li, J. Q.; Zhang, S. D.] Harbin Inst Technol HIT, Harbin 150001, Peoples R China.
[Liu, Hu] Huazhong Univ Sci & Technol HUST, Wuhan 430074, Peoples R China.
[Morescalchi, L.] Univ Siena, I-53100 Siena, Italy.
[Putze, A.] CNRS, Lab Annecy le Vieux Phys Theor LAPTh, F-74941 Annecy Le Vieux, France.
[Putze, A.] Univ Savoie Mt Blanc, F-74941 Annecy Le Vieux, France.
[Qin, X.; Xia, X.] Shandong Univ SDU, Jinan 250100, Shandong, Peoples R China.
[Qu, Z. Y.] Nankai Univ, Tianjin 300071, Peoples R China.
[Sun, W. H.] Southeast Univ SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Wei, C. C.] Chinese Acad Sci, Inst Theoretial Phys, Beijing 100190, Peoples R China.
[Zhu, Z. Q.] Jilin Univ, Jilin 130012, Peoples R China.
RI Vecchi, Manuela/J-9180-2014; Sao Carlos Institute of Physics,
IFSC/USP/M-2664-2016; Paniccia, Mercedes/A-4519-2017; Delgado,
Carlos/K-7587-2014;
OI Paniccia, Mercedes/0000-0001-8482-2703; Delgado,
Carlos/0000-0002-7014-4101; Corti, Claudio/0000-0001-9127-7133;
Morescalchi, Luca/0000-0002-7819-8139; Bertucci,
Bruna/0000-0001-7584-293X; La Vacca, Giuseppe/0000-0002-2168-9447; Della
Torre, Stefano/0000-0002-7669-0859
FU Sao Paulo Research Foundation (FAPESP), Brazil [2014/19149-7,
2014/50747-8, 2015-50378-5]; CAS, China; NSFC, China; MOST, China; NLAA,
China; provincial government of Shandong, China; provincial government
of Jiangsu, China; provincial government of Guangdong, China; China
Scholarship Council, China; Finnish Funding Agency for Innovation
(Tekes), Finland [40361/01, 40518/03]; Academy of Finland, Finland
[258963]; CNRS, France; IN2P3, France; CNES, France; Enigmass, France;
ANR, France; Pascale Ehrenfreund, Germany; DLR, Germany; JARA-HPC,
Germany [JARA0052]; INFN, Italy [2013-002-R.0, 2014-037-R.0]; ASI, Italy
[2013-002-R.0, 2014-037-R.0]; CHEP Grants at Kyungpook National
University, Korea [NRF-2009-0080142, NRF-2012-010226]; CHEP Grants at
Ewha Womans University, Korea [NRF-2013-004883]; Consejo Nacional de
Ciencia y Tecnologia, Mexico; UNAM, Mexico; FCT, Portugal
[PTDC/FIS/122567/2010]; CIEMAT, Spain; IAC, Spain; CDTI, Spain;
SEIDI-MINECO, Spain [AYA2012-39526-C02-(01/02),
ESP2015-71662-C2-(1-P/2-P), SEV-2011-0187, SEV-2015-0548,
MDM-2015-0509]; Swiss National Science Foundation (SNSF), federal and
cantonal authorities, Switzerland; Academia Sinica, Taiwan; Ministry of
Science and Technology (MOST), Taiwan [103-2112-M-006-018-MY3,
104-2112-M-001-027, CDA-105-M06]; Turkish Atomic Energy Authority at
METU, Turkey; NSF Grant, USA [1455202]; Wyle Laboratories Grant, USA
[2014/T72497]; NASA NESSF Grant, USA [HELIO15F-0005]
FX We thank former NASA Administrator Daniel S. Goldin for his dedication
to the legacy of the ISS as a scientific laboratory and his decision for
NASA to fly AMS as a DOE payload. We also acknowledge the continuous
support of the NASA leadership including Charles Bolden and William H.
Gerstenmaier and of the JSC and MSFC flight control teams which has
allowed AMS to operate optimally on the ISS for five years. We are
grateful for the support of Jim Siegrist and his staff of the DOE. We
also acknowledge the continuous support from MIT and its School of
Science, Michael Sipser, Marc Kastner, Ernest Moniz, Richard Milner, and
Boleslaw Wyslouch. Research supported by Sao Paulo Research Foundation
(FAPESP) Grants No. 2014/19149-7, No. 2014/50747-8, and No.
2015-50378-5, Brazil; CAS, NSFC, MOST, NLAA, the provincial governments
of Shandong, Jiangsu, Guangdong, and the China Scholarship Council,
China; the Finnish Funding Agency for Innovation (Tekes) Grants No.
40361/01 and No. 40518/03 and the Academy of Finland Grant No. 258963,
Finland; CNRS, IN2P3, CNES, Enigmass, and the ANR, France; Pascale
Ehrenfreund, DLR, and JARA-HPC under Project No. JARA0052, Germany; INFN
and ASI under ASI-INFN Agreements No. 2013-002-R.0 and No. 2014-037-R.0,
Italy; CHEP Grants No. NRF-2009-0080142 and No. NRF-2012-010226 at
Kyungpook National University and No. NRF-2013-004883 at Ewha Womans
University, Korea; the Consejo Nacional de Ciencia y Tecnologia and
UNAM, Mexico; FCT under Grant No. PTDC/FIS/122567/2010, Portugal;
CIEMAT, IAC, CDTI, and SEIDI-MINECO under Grants No.
AYA2012-39526-C02-(01/02), No. ESP2015-71662-C2-(1-P/2-P), No.
SEV-2011-0187, No. SEV-2015-0548, and No. MDM-2015-0509, Spain; the
Swiss National Science Foundation (SNSF), federal and cantonal
authorities, Switzerland; Academia Sinica and the Ministry of Science
and Technology (MOST) under Grants No. 103-2112-M-006-018-MY3, No.
104-2112-M-001-027, and No. CDA-105-M06, former President of Academia
Sinica Yuan-Tseh Lee, and former Ministers of MOST Maw-Kuen Wu and
Luo-Chuan Lee, Taiwan; the Turkish Atomic Energy Authority at METU,
Turkey; and NSF Grant No. 1455202, Wyle Laboratories Grant No.
2014/T72497, and NASA NESSF Grant No. HELIO15F-0005, USA. We gratefully
acknowledge the strong support from CERN including Rolf-Dieter Heuer and
Fabiola Gianotti, from the CERN IT department and Bernd Panzer-Steindel,
and from the European Space Agency including Johann-Dietrich Worner and
Simonetta Di Pippo. We are grateful for important discussions with
Fiorenza Donato, Jonathan Ellis, Jonathan Feng, Igor Moskalenko, Michael
Salamon, Subir Sarkar, Joachim Trumper, Michael S. Turner, Steven
Weinberg, and Arnold Wolfendale.
NR 85
TC 8
Z9 8
U1 27
U2 27
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD AUG 26
PY 2016
VL 117
IS 9
AR 091103
DI 10.1103/PhysRevLett.117.091103
PG 10
WC Physics, Multidisciplinary
SC Physics
GA DU1ZE
UT WOS:000382008900001
PM 27610839
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Godin-Beekmann, S
Haefele, A
Trickl, T
Payen, G
Gabarrot, F
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Godin-Beekmann, Sophie
Haefele, Alexander
Trickl, Thomas
Payen, Guillaume
Gabarrot, Frank
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
1: Vertical resolution
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID RAMAN LIDAR; STRATOSPHERIC OZONE; RAYLEIGH; DIFFERENTIATION; RETRIEVAL;
PROFILES; DENSITY
AB A standardized approach for the definition and reporting of vertical resolution of the ozone and temperature lidar profiles contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. Two standardized definitions homogeneously and unequivocally describing the impact of vertical filtering are recommended.
The first proposed definition is based on the width of the response to a finite-impulse-type perturbation. The response is computed by convolving the filter coefficients with an impulse function, namely, a Kronecker delta function for smoothing filters, and a Heaviside step function for derivative filters. Once the response has been computed, the proposed standardized definition of vertical resolution is given by Delta z = delta z x H-FWHM, where delta z is the lidar's sampling resolution and H-FWHM is the full width at half maximum (FWHM) of the response, measured in sampling intervals.
The second proposed definition relates to digital filtering theory. After applying a Laplace transform to a set of filter coefficients, the filter's gain characterizing the effect of the filter on the signal in the frequency domain is computed, from which the cut-off frequency f(C), defined as the frequency at which the gain equals 0.5, is computed. Vertical resolution is then defined by Delta z = delta z/(2f(C)). Unlike common practice in the field of spectral analysis, a factor 2 f(C) instead of f(C) is used here to yield vertical resolution values nearly equal to the values obtained with the impulse response definition using the same filter coefficients. When using either of the proposed definitions, unsmoothed signals yield the best possible vertical resolution Delta z = delta z (one sampling bin).
Numerical tools were developed to support the implementation of these definitions across all NDACC lidar groups. The tools consist of ready-to-use "plug-in" routines written in several programming languages that can be inserted into any lidar data processing software and called each time a filtering operation occurs in the data processing chain.
When data processing implies multiple smoothing operations, the filtering information is analytically propagated through the multiple calls to the routines in order for the standardized values of vertical resolution to remain theoretically and numerically exact at the very end of data processing.
C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands.
[Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France.
[Haefele, Alexander] Meteoswiss, Payerne, Switzerland.
[Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany.
[Payen, Guillaume; Gabarrot, Frank] Univ Le Reunion, Observ Sci, CNRS, St Denis De La Reunion, Reunion.
[Payen, Guillaume; Gabarrot, Frank] Univ Reunion, UMS3365, St Denis De La Reunion, Reunion.
RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
EM thierry.leblanc@jpl.nasa.gov
RI Trickl, Thomas/F-7331-2010
FU VALID project; Canadian National Sciences and Engineering Research
Council
FX This work was initiated in response to the 2010 call for international
teams of experts in earth and space science by the International Space
Science Institute (ISSI) in Bern, Switzerland. It could not have been
performed without the travel and logistical support of ISSI. Part of the
work described in this report was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under agreements with
the National Aeronautics and Space Administration. Part of this work was
carried out in support of the VALID project. Robert J. Sica would like
to acknowledge the support of the Canadian National Sciences and
Engineering Research Council for support of the University of Western
Ontario lidar work. The team would also like to acknowledge J. Bandoro
for his help in the design of the MATLAB filtering tools.
NR 29
TC 3
Z9 3
U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 25
PY 2016
VL 9
IS 8
BP 4029
EP 4049
DI 10.5194/amt-9-4029-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YY
UT WOS:000383798500001
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Godin-Beekmann, S
Haefele, A
Trickl, T
Payen, G
Liberti, G
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Godin-Beekmann, Sophie
Haefele, Alexander
Trickl, Thomas
Payen, Guillaume
Liberti, Gianluigi
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
2: Ozone DIAL uncertainty budget
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; FOURIER-TRANSFORM SPECTROSCOPY; O-2 HERZBERG
BANDS; STRATOSPHERIC OZONE; RAYLEIGH-SCATTERING; UV SPECTROSCOPY; NM
REGION; NO2; TROPOSPHERE; SPECTRA
AB A standardized approach for the definition, propagation, and reporting of uncertainty in the ozone differential absorption lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One essential aspect of the proposed approach is the propagation in parallel of all independent uncertainty components through the data processing chain before they are combined together to form the ozone combined standard uncertainty.
The independent uncertainty components contributing to the overall budget include random noise associated with signal detection, uncertainty due to saturation correction, background noise extraction, the absorption cross sections of O-3, NO2, SO2, and O-2, the molecular extinction cross sections, and the number densities of the air, NO2, and SO2. The expression of the individual uncertainty components and their step-by-step propagation through the ozone differential absorption lidar (DIAL) processing chain are thoroughly estimated. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which requires knowledge of the covariance matrix when the lidar signal is vertically filtered. In addition, the covariance terms must be taken into account if the same detection hardware is shared by the lidar receiver channels at the absorbed and non-absorbed wavelengths.
The ozone uncertainty budget is presented as much as possible in a generic form (i.e., as a function of instrument performance and wavelength) so that all NDACC ozone DIAL investigators across the network can estimate, for their own instrument and in a straightforward manner, the expected impact of each reviewed uncertainty component. In addition, two actual examples of full uncertainty budget are provided, using nighttime measurements from the tropospheric ozone DIAL located at the Jet Propulsion Laboratory (JPL) Table Mountain Facility, California, and nighttime measurements from the JPL stratospheric ozone DIAL located at Mauna Loa Observatory, Hawai'i.
C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands.
[Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France.
[Haefele, Alexander] Meteoswiss, Payerne, Switzerland.
[Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany.
[Payen, Guillaume] Univ La Reunion, Observ Sci, CNRS, St Denis De La Reunion, France.
[Payen, Guillaume] Univ Reunion, UMS3365, St Denis De La Reunion, France.
[Liberti, Gianluigi] ISAC CNR, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
EM thierry.leblanc@jpl.nasa.gov
RI Trickl, Thomas/F-7331-2010
FU European Space Agency VALID project; Canadian National Sciences and
Engineering Research Council
FX This work was initiated in response to the 2010 call for international
teams of experts in Earth and Space Science by the International Space
Science Institute (ISSI) in Bern, Switzerland. It could not have been
performed without the travel and logistical support of ISSI. Part of the
work described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under agreements with
the National Aeronautics and Space Administration. Part of this work was
carried out in support of the European Space Agency VALID project.
Robert J. Sica would like to acknowledge the support of the Canadian
National Sciences and Engineering Research Council for support of the
University of Western Ontario lidar work.
NR 58
TC 2
Z9 2
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 25
PY 2016
VL 9
IS 8
BP 4051
EP 4078
DI 10.5194/amt-9-4051-2016
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YY
UT WOS:000383798500002
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Haefele, A
Payen, G
Liberti, G
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Haefele, Alexander
Payen, Guillaume
Liberti, Gianluigi
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
3: Temperature uncertainty budget
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; RAYLEIGH-SCATTER; RAMAN LIDAR; MIDDLE
ATMOSPHERE; NO2 ABSORPTION; NM REGION; SPECTRA; MODEL; VALIDATION; RANGE
AB A standardized approach for the definition, propagation, and reporting of uncertainty in the temperature lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One important aspect of the proposed approach is the ability to propagate all independent uncertainty components in parallel through the data processing chain. The individual uncertainty components are then combined together at the very last stage of processing to form the temperature combined standard uncertainty.
The identified uncertainty sources comprise major components such as signal detection, saturation correction, background noise extraction, temperature tie-on at the top of the profile, and absorption by ozone if working in the visible spectrum, as well as other components such as molecular extinction, the acceleration of gravity, and the molecular mass of air, whose magnitudes depend on the instrument, data processing algorithm, and altitude range of interest.
The expression of the individual uncertainty components and their step-by-step propagation through the temperature data processing chain are thoroughly estimated, taking into account the effect of vertical filtering and the merging of multiple channels. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which means that covariance terms must be taken into account when vertical filtering is applied and when temperature is integrated from the top of the profile. Quantitatively, the uncertainty budget is presented in a generic form (i.e., as a function of instrument performance and wavelength), so that any NDACC temperature lidar investigator can easily estimate the expected impact of individual uncertainty components in the case of their own instrument.
Using this standardized approach, an example of uncertainty budget is provided for the Jet Propulsion Laboratory (JPL) lidar at Mauna Loa Observatory, Hawai'i, which is typical of the NDACC temperature lidars transmitting at 355 nm. The combined temperature uncertainty ranges between 0.1 and 1 K below 60 km, with detection noise, saturation correction, and molecular extinction correction being the three dominant sources of uncertainty. Above 60 km and up to 10 km below the top of the profile, the total uncertainty increases exponentially from 1 to 10 K due to the combined effect of random noise and temperature tie-on. In the top 10 km of the profile, the accuracy of the profile mainly depends on that of the tie-on temperature. All other uncertainty components remain below 0.1K throughout the entire profile (1590 km), except the background noise correction uncertainty, which peaks around 0.3-0.5 K. It should be kept in mind that these quantitative estimates may be very different for other lidar instruments, depending on their altitude range and the wavelengths used.
C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands.
[Haefele, Alexander] Meteoswiss, Payerne, Switzerland.
[Payen, Guillaume] Univ La Reunion, CNRS, Observ Sci, St Denis De La Reunion, France.
[Payen, Guillaume] Univ Reunion, UMS3365, St Denis De La Reunion, France.
[Liberti, Gianluigi] ISAC CNR, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
EM thierry.leblanc@jpl.nasa.gov
FU VALID project; Canadian National Sciences and Engineering Research
Council
FX This work was initiated in response to the 2010 call for international
teams of experts in Earth and Space Science by the International Space
Science Institute (ISSI) in Bern, Switzerland. It could not have been
performed without the travel and logistical support of ISSI. Part of the
work described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under agreements with
the National Aeronautics and Space Administration. Part of this work was
carried out in support of the VALID project. Robert J. Sica would like
to acknowledge the support of the Canadian National Sciences and
Engineering Research Council for support of the University of Western
Ontario lidar work.
NR 47
TC 2
Z9 2
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 25
PY 2016
VL 9
IS 8
BP 4079
EP 4101
DI 10.5194/amt-9-4079-2016
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YY
UT WOS:000383798500003
ER
PT J
AU Mills, JD
Ben-Nun, M
Rollin, K
Bromley, MWJ
Li, JB
Hinde, RJ
Winstead, CL
Sheehy, JA
Boatz, JA
Langhoff, PW
AF Mills, Jeffrey D.
Ben-Nun, Michal
Rollin, Kyle
Bromley, Michael W. J.
Li, Jiabo
Hinde, Robert J.
Winstead, Carl L.
Sheehy, Jeffrey A.
Boatz, Jerry A.
Langhoff, Peter W.
TI Atomic Spectral Methods for Ab Initio Molecular Electronic Energy
Surfaces: Transitioning From Small-Molecule to Biomolecular-Suitable
Approaches
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID DIATOMICS-IN-MOLECULES; DENSITY-FUNCTIONAL THEORY; NON-HERMITIAN
FORMULATION; SLATER-TYPE ORBITALS; VALENCE-BOND; GENERAL-THEORY;
DYNAMICS SIMULATIONS; PERTURBATION-THEORY; HYDROGEN MOLECULE;
EXCITED-STATES
AB Continuing attention has addressed incorportation of the electronically dynamical attributes of biomolecules in the largely static first-generation molecular-mechanical force fields commonly employed in molecular-dynamics simulations. We describe here a universal quantum mechanical approach to calculations of the electronic energy surfaces of both small molecules and large aggregates on a common basis which can include such electronic attributes, and which also seems well-suited to adaptation in ab initio molecular-dynamics applications. In contrast to the more familiar orbital-product-based methodologies employed in traditional small-molecule computational quantum chemistry, the present approach is based on an "ex-post-facto" method in which Hamiltonian matrices are evaluated prior to wave function antisymmetrization, implemented here in the support of a Hilbert space of orthonormal products of many-electron atomic spectral eigenstates familiar from the van der Waals theory of long-range interactions. The general theory in its various forms incorporates the early semiempirical atoms- and diatomics-in-molecules approaches of Moffitt, Ellison, Tully, Kuntz, and others in a comprehensive mathematical setting, and generalizes the developments of Eisenschitz, London, Claverie, and others addressing electron permutation symmetry adaptation issues, completing these early attempts to treat van der Waals and chemical forces on a common basis. Exact expressions are obtained for molecular Hamiltonian matrices and for associated energy eigenvalues as sums of separate atomic and interaction-energy terms, similar in this respect to the forms of classical force fields. The latter representation is seen to also provide a long-missing general definition of the energies of individual atoms and of their interactions within molecules and matter free from subjective additional constraints. A computer code suite is described for calculations of the many-electron atomic eigenspectra and the pairwise-atomic Hamiltonian matrices required for practical applications. These matrices can be retained as functions of scalar atomic-pair separations and employed in assembling aggregate Hamiltonian matrices, with Wigner rotation matrices providing analytical representations of their angular degrees of freedom. In this way, ab initio potential energy surfaces are obtained in the complete absence of repeated evaluations and transformations of the one- and two-electron integrals at different molecular geometries required in most ab inito molecular calculations, with large Hamiltonian matrix assembly simplified and explicit diagonalizations avoided employing partitioning and Brillouin-Wigner or Rayleigh-Schrodinger perturbation theory. Illustrative applications of the important components of the formalism, selected aspects of the scaling of the approach, and aspects of "on-the-fly" interfaces with Monte Carlo and molecular-dynamics methods are described in anticipation of subsequent applications to biomolecules and other large aggregates.
C1 [Mills, Jeffrey D.; Boatz, Jerry A.] US Air Force, Res Lab, 10 East Saturn Blvd, Edwards Afb, CA 93524 USA.
[Ben-Nun, Michal] Predict Sci Inc, 9990 Mesa Rim Rd 170, San Diego, CA 92121 USA.
[Rollin, Kyle] Northrup Grumman Corp, 1 Rancho Carmel Dr, San Diego, CA 92128 USA.
[Bromley, Michael W. J.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Li, Jiabo] Accelrys Inc, 10188 Telesis Court 100, San Diego, CA 92121 USA.
[Hinde, Robert J.] Univ Tennessee, Dept Chem, Knoxville, TN 37996 USA.
[Winstead, Carl L.] CALTECH, AA Noyes Lab Chem Phys, Pasadena, CA 91125 USA.
[Sheehy, Jeffrey A.] NASA Headquarters, 300 E St SW,Suite 5R30, Washington, DC USA.
[Langhoff, Peter W.] Univ Calif San Diego, Dept Chem & Biochem, 9500 Gilman Dr,MS 0365, La Jolla, CA 92093 USA.
RP Langhoff, PW (reprint author), Univ Calif San Diego, Dept Chem & Biochem, 9500 Gilman Dr,MS 0365, La Jolla, CA 92093 USA.
EM planghoff@mail.ucsd.edu
RI Bromley, Michael/A-9453-2010
OI Bromley, Michael/0000-0002-3817-7296
FU Air Force Research Laboratory [FA9300-09-C-2001, FA9300-07-M-301]; US
Air Force Office of Scientific Research [F07-206-0375]; European Office
of Aerospace Research and Development [FA8655-09-1-3069]; American
Society of Engineering Education; National Research Council of the
National Academy of Science; Department of Chemistry and Biochemistry
FX The financial support of the Air Force Research Laboratory
(FA9300-09-C-2001, FA9300-07-M-301), the US Air Force Office of
Scientific Research (F07-206-0375), the European Office of Aerospace
Research and Development (FA8655-09-1-3069), the American Society of
Engineering Education, and the National Research Council of the National
Academy of Science is gratefully acknowledged. Access to computational
facilities was provided by the National Science Foundation under the
auspices of TeraGrid and XSEDE allocations. We acknowledge the valuable
assistance and advice provided by Professors R. Lopez and J. F. Rico and
their co-workers at various stages of the investigation, and thank Mr.
W. Kalliomaa and Dr. Steve Rodgers of AFRL for continuing encouragement
and support. It is a pleasure to thank Professor J. A. McCammon and
other colleagues at the University of California San Diego for their
hospitality and support in the Department of Chemistry and Biochemistry.
NR 164
TC 0
Z9 0
U1 4
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD AUG 25
PY 2016
VL 120
IS 33
BP 8321
EP 8337
DI 10.1021/acs.jpcb.6b02021
PG 17
WC Chemistry, Physical
SC Chemistry
GA DU4JZ
UT WOS:000382180200026
PM 27232159
ER
PT J
AU de Miranda, BC
Garcia, GA
Gaie-Levrel, F
Mahjoub, A
Gautier, T
Fleury, B
Nahon, L
Pernot, P
Carrasco, N
AF de Miranda, Barbara Cunha
Garcia, Gustavo A.
Gaie-Levrel, Francois
Mahjoub, Ahmed
Gautier, Thomas
Fleury, Benjamin
Nahon, Laurent
Pernot, Pascal
Carrasco, Nathalie
TI Molecular Isomer Identification of Titan's Tholins Organic Aerosols by
Photoelectron/Photoion Coincidence Spectroscopy Coupled to VUV
Synchrotron Radiation
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID PHOTO-ELECTRON SPECTRA; SUM-RULE CONSIDERATION; GAS-PHASE;
MASS-SPECTROMETRY; HIGH-RESOLUTION; ATMOSPHERIC AEROSOLS;
ANGULAR-DISTRIBUTION; PENNING IONIZATION; HEI PHOTOELECTRON; IONIC
STATES
AB The chemical composition of Titan organic haze is poorly known. To address this issue, laboratory analogues named tholins are synthesized and analyzed by methods often requiring an extraction process in a carrier solvent. These methods exclude the analysis of the insoluble tholins' fraction and assume a hypothetical chemical equivalence between soluble and insoluble fractions. In this work, we present a powerful complementary analysis method recently developed on the DESIRS VUV synchrotron beamline at SOLEIL. It involves soft pyrolysis of tholins at similar to 230 degrees C and electron/ion coincidence analysis of the emitted volatile compounds photoionized by tunable synchrotron radiation. By comparison with reference photoelectron spectra (PES), the spectral information collected on the detected molecules yields their isomeric structure. The method is more readily applied to light species (m/z <= 69), while for heavier ones, the number of possibilities and the lack of PES reference spectra in the literature limit its analysis. A notable pattern in the analyzed tholins is the presence of species containing adjacent doubly bonded N atoms, which might be a signature of heterogeneous incorporation of N-2 in tholins.
C1 [de Miranda, Barbara Cunha; Garcia, Gustavo A.; Gaie-Levrel, Francois; Nahon, Laurent] Synchrotron SOLEIL, DESIRS Beamline, F-91192 Gif Sur Yvette, France.
[Gaie-Levrel, Francois] Natl Metrol Inst, Gas & Aerosol Metrol Dept, Chem & Biol Div, Lab Natl Metrol & Essais LNE, 1 Rue Gaston Boissier, F-75724 Paris 15, France.
[Gaie-Levrel, Francois] Testing Lab, 1 Rue Gaston Boissier, F-75724 Paris 15, France.
[Mahjoub, Ahmed; Gautier, Thomas; Fleury, Benjamin; Carrasco, Nathalie] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS INSU,LATMOS IPSL, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Gautier, Thomas] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA.
[Pernot, Pascal] Univ Paris 11, CNRS, UMR8000, Chim Phys Lab, F-91405 Orsay, France.
[Carrasco, Nathalie] Inst Univ France, 103 Blvd St Michel, F-75005 Paris, France.
[de Miranda, Barbara Cunha] Univ Paris 06, Lab Chim Phys Mat & Rayonnement, 11 Rue Pierre & Marie Curie, F-75231 Paris 05, France.
RP Carrasco, N (reprint author), Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS INSU,LATMOS IPSL, 11 Blvd Alembert, F-78280 Guyancourt, France.; Carrasco, N (reprint author), Inst Univ France, 103 Blvd St Michel, F-75005 Paris, France.
EM nathalie.carrasco@latmos.ipsl.fr
RI Carrasco, Nathalie/D-2365-2012
OI Carrasco, Nathalie/0000-0002-0596-6336
FU Region Ile-de-France (DIM-ACAV program); European Research Council (ERC
Starting Grant PRIMCHEM) [636829]; [20110728]; [20120953]
FX We would like to thank the general technical staff of SOLEIL for running
the facility under project no 20110728 and 20120953. The authors wish to
thank Isabelle Schmitz-Afonso and David Touboul from the Institut de
Chimie des Substances Naturelles (ICSN) for the OHR-MS measurements.
B.F.'s Ph.D. grant is supported by Region Ile-de-France (DIM-ACAV
program). N.C. acknowledges the European Research Council for their
financial support (ERC Starting Grant PRIMCHEM, grant agreement
no636829).
NR 94
TC 0
Z9 0
U1 11
U2 11
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD AUG 25
PY 2016
VL 120
IS 33
BP 6529
EP 6540
DI 10.1021/acs.jpca.6b03346
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DU4JQ
UT WOS:000382179300004
ER
PT J
AU van den Hurk, B
Kim, HJ
Krinner, G
Seneviratne, SI
Derksen, C
Oki, T
Douville, H
Colin, J
Ducharne, A
Cheruy, F
Viovy, N
Puma, MJ
Wada, Y
Li, WP
Jia, BH
Alessandri, A
Lawrence, DM
Weedon, GP
Ellis, R
Hagemann, S
Mao, JF
Flanner, MG
Zampieri, M
Materia, S
Law, RM
Sheffield, J
AF van den Hurk, Bart
Kim, Hyungjun
Krinner, Gerhard
Seneviratne, Sonia I.
Derksen, Chris
Oki, Taikan
Douville, Herve
Colin, Jeanne
Ducharne, Agnes
Cheruy, Frederique
Viovy, Nicholas
Puma, Michael J.
Wada, Yoshihide
Li, Weiping
Jia, Binghao
Alessandri, Andrea
Lawrence, Dave M.
Weedon, Graham P.
Ellis, Richard
Hagemann, Stefan
Mao, Jiafu
Flanner, Mark G.
Zampieri, Matteo
Materia, Stefano
Law, Rachel M.
Sheffield, Justin
TI LS3MIP (v1.0) contribution to CMIP6: the Land Surface, Snow and Soil
moisture Model Intercomparison Project - aims, setup and expected
outcome
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID EARTH SYSTEM MODELS; CLIMATE-CHANGE; CARBON-DIOXIDE; INTERANNUAL
VARIABILITY; ALBEDO FEEDBACK; BIASES; WATER; PREDICTABILITY; CRYOSPHERE;
TRENDS
AB The Land Surface, Snow and Soil Moisture Model Intercomparison Project (LS3MIP) is designed to provide a comprehensive assessment of land surface, snow and soil moisture feedbacks on climate variability and climate change, and to diagnose systematic biases in the land modules of current Earth system models (ESMs). The solid and liquid water stored at the land surface has a large influence on the regional climate, its variability and predictability, including effects on the energy, water and carbon cycles. Notably, snow and soil moisture affect surface radiation and flux partitioning properties, moisture storage and land surface memory. They both strongly affect atmospheric conditions, in particular surface air temperature and precipitation, but also large-scale circulation patterns. However, models show divergent responses and representations of these feedbacks as well as systematic biases in the underlying processes. LS3MIP will provide the means to quantify the associated uncertainties and better constrain climate change projections, which is of particular interest for highly vulnerable regions (densely populated areas, agricultural regions, the Arctic, semi-arid and other sensitive terrestrial ecosystems).
The experiments are subdivided in two components, the first addressing systematic land biases in offline mode ("LMIP", building upon the 3rd phase of Global Soil Wetness Project; GSWP3) and the second addressing land feedbacks attributed to soil moisture and snow in an integrated framework ("LFMIP", building upon the GLACE-CMIP blueprint).
C1 [van den Hurk, Bart] KNMI, De Bilt, Netherlands.
[Kim, Hyungjun; Oki, Taikan] Univ Tokyo, Inst Ind Sci, Tokyo, Japan.
[Krinner, Gerhard] CNRS, LGGE, Grenoble, France.
[Seneviratne, Sonia I.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[Derksen, Chris] Environm & Climate Change, Div Climate Res, Toronto, ON, Canada.
[Douville, Herve; Colin, Jeanne] Meteo France, CNRM, Toulouse, France.
[Cheruy, Frederique] Univ Paris 06, Ecole Polytech, Ecole Normale Super, LMD IPSL,CNRS, Paris, France.
[Viovy, Nicholas] LSCE IPSL CEA CNRS UVSQ, Gif Sur Yvette, France.
[Puma, Michael J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Wada, Yoshihide] Int Inst Appl Syst Anal, Laxenburg, Austria.
[Li, Weiping] China Meteorol Adm, Natl Climate Ctr, Lab Climate Studies, Beijing, Peoples R China.
[Jia, Binghao] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Numer Modeling Atmospher Sci & Geop, Beijing, Peoples R China.
[Alessandri, Andrea] Agenzia Nazl Nuove Tecnol Energia & Sviluppo Econ, Rome, Italy.
[Lawrence, Dave M.] Natl Ctr Atmospher Res, Climate & Global Dynam Lab, POB 3000, Boulder, CO 80307 USA.
[Weedon, Graham P.] Met Off JCHMR, Maclean Bldg, Wallingford, Oxon, England.
[Ellis, Richard] Ctr Ecol & Hydrol, Maclean Bldg, Wallingford, Oxon, England.
[Hagemann, Stefan] Max Planck Inst Meteorol, Hamburg, Germany.
[Mao, Jiafu] Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA.
[Mao, Jiafu] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN USA.
[Flanner, Mark G.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Zampieri, Matteo; Materia, Stefano] Euromediterranean Ctr Climate Change CMCC, Climate Simulat & Predict Div, Bologna, Italy.
[Law, Rachel M.] CSIRO Oceans & Atmosphere, Aspendale, Vic, Australia.
[Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Sheffield, Justin] Univ Southampton, Geog & Environm, Southampton, Hants, England.
[Ducharne, Agnes] UPMC CNRS EPHE, Sorbonne Univ, UMR METIS 7619, Paris, France.
RP van den Hurk, B (reprint author), KNMI, De Bilt, Netherlands.
EM hurkvd@knmi.nl
RI Oki, Taikan/E-5778-2010; Krinner, Gerhard/A-6450-2011; Weedon,
Graham/B-7574-2008; Flanner, Mark/C-6139-2011; Mao, Jiafu/B-9689-2012;
Law, Rachel/A-1969-2012
OI Oki, Taikan/0000-0003-4067-4678; Krinner, Gerhard/0000-0002-2959-5920;
Weedon, Graham/0000-0003-1262-9984; Flanner, Mark/0000-0003-4012-174X;
Mao, Jiafu/0000-0002-2050-7373; Law, Rachel/0000-0002-7346-0927
FU Joint UK DECC/Defra Met Office Hadley Climate Centre Programme
[GA01101]; Biogeochemistry-Climate Feedbacks Scientific Focus Area
project funded through the Regional and Global Climate Modeling Program
in Climate and Environmental Sciences Division (CESD) of the (BER)
Program in the; DOE [DE-AC05-00OR22725]; Japan Society for the Promotion
of Science KAKENHI [16H06291]
FX The authors thank the CMIP panel of the WCRP Working Group on Climate
Modelling for their efforts in coordinating the CMIP6 enterprise. Graham
R Weedon was supported by the Joint UK DECC/Defra Met Office Hadley
Climate Centre Programme (GA01101). Jiafu Mao is supported by the
Biogeochemistry-Climate Feedbacks Scientific Focus Area project funded
through the Regional and Global Climate Modeling Program in Climate and
Environmental Sciences Division (CESD) of the Biological and
Environmental Research (BER) Program in the U.S. Department of Energy
(DOE) Office of Science. Oak Ridge National Laboratory is managed by
UT-BATTELLE for DOE under contract DE-AC05-00OR22725. H. Kim and T. Oki
were supported by Japan Society for the Promotion of Science KAKENHI
(16H06291). Hanna Lee (NorESM) has expressed intention to participate in
LS3MIP when feasible, but has not contributed to this manuscript.
NR 107
TC 1
Z9 1
U1 11
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD AUG 24
PY 2016
VL 9
IS 8
BP 2809
EP 2832
DI 10.5194/gmd-9-2809-2016
PG 24
WC Geosciences, Multidisciplinary
SC Geology
GA DW6ZQ
UT WOS:000383800400002
ER
PT J
AU Everroad, RC
Stuart, RK
Bebout, BM
Detweiler, AM
Lee, JZ
Woebken, D
Prufert-Bebout, L
Pett-Ridge, J
AF Everroad, R. Craig
Stuart, Rhona K.
Bebout, Brad M.
Detweiler, Angela M.
Lee, Jackson Z.
Woebken, Dagmar
Prufert-Bebout, Leslie
Pett-Ridge, Jennifer
TI Permanent draft genome of strain ESFC-1: ecological genomics of a newly
discovered lineage of filamentous diazotrophic cyanobacteria
SO STANDARDS IN GENOMIC SCIENCES
LA English
DT Article
DE Cyanobacteria; Nitrogen fixation; Hydrogenase; Intertidal microbial mat
ID PHOTOSYNTHETIC MICROBIAL MATS; OXYGENIC PHOTOSYNTHESIS; HYDROGEN
METABOLISM; MAXIMUM-LIKELIHOOD; DIVERSITY; IDENTIFICATION; PHYLOGENIES;
ALGORITHMS; ORGANISMS; FIXATION
AB The nonheterocystous filamentous cyanobacterium, strain ESFC-1, is a recently described member of the order Oscillatoriales within the Cyanobacteria. ESFC-1 has been shown to be a major diazotroph in the intertidal microbial mat system at Elkhorn Slough, CA, USA. Based on phylogenetic analyses of the 16S RNA gene, ESFC-1 appears to belong to a unique, genus-level divergence; the draft genome sequence of this strain has now been determined. Here we report features of this genome as they relate to the ecological functions and capabilities of strain ESFC-1. The 5,632,035 bp genome sequence encodes 4914 protein-coding genes and 92 RNA genes. One striking feature of this cyanobacterium is the apparent lack of either uptake or bi-directional hydrogenases typically expected within a diazotroph. Additionally, a large genomic island is found that contains numerous low GC-content genes and genes related to extracellular polysaccharide production and cell wall synthesis and maintenance.
C1 [Everroad, R. Craig; Bebout, Brad M.; Detweiler, Angela M.; Lee, Jackson Z.; Woebken, Dagmar; Prufert-Bebout, Leslie] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Everroad, R. Craig; Detweiler, Angela M.; Lee, Jackson Z.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Stuart, Rhona K.; Pett-Ridge, Jennifer] Lawrence Livermore Natl Lab, Phys & Life Sci Directorate, Livermore, CA USA.
[Woebken, Dagmar] Univ Vienna, Res Network Chem Meets Microbiol, Div Microbial Ecol, Dept Microbiol & Ecosyst Sci, Vienna, Austria.
RP Everroad, RC (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.; Everroad, RC (reprint author), Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
EM craig.everroad@nasa.gov
OI Woebken, Dagmar/0000-0002-1314-9926; Stuart, Rhona/0000-0001-5916-9693
FU US. DOE Genomic Science Program [SCW1039]; Community Sequencing Project
'Microbial Interactions in Extremophilic Mat Communities' at the DOE JGI
[701]; Office of Science of the U.S. DOE [DE-AC02-05CH11231]; US DOE at
Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX Funding was provided by the US. DOE Genomic Science Program under
contract SCW1039. Sequencing and support was provided by Community
Sequencing Project #701 'Microbial Interactions in Extremophilic Mat
Communities' at the DOE JGI. Work conducted by the U.S. DOE-JGI was
supported by the Office of Science of the U.S. DOE Under Contract No.
DE-AC02-05CH11231. Work at LLNL was performed under the auspices of the
US DOE at Lawrence Livermore National Laboratory under Contract
DE-AC52-07NA27344. We thank Jeff Cann, Associate Wildlife Biologist,
Central Region, California Department of Fish and Wildlife, for
coordinating our access to the Moss Landing Wildlife Area.
NR 45
TC 0
Z9 0
U1 4
U2 4
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1944-3277
J9 STAND GENOMIC SCI
JI Stand. Genomic Sci.
PD AUG 24
PY 2016
VL 11
AR 53
DI 10.1186/s40793-016-0174-6
PG 8
WC Genetics & Heredity; Microbiology
SC Genetics & Heredity; Microbiology
GA DW8PU
UT WOS:000383918800002
PM 27559430
ER
PT J
AU Chen, DL
Tian, YD
Yao, TD
Ou, TH
AF Chen, Deliang
Tian, Yudong
Yao, Tandong
Ou, Tinghai
TI Satellite measurements reveal strong anisotropy in spatial coherence of
climate variations over the Tibet Plateau
SO SCIENTIFIC REPORTS
LA English
DT Article
ID AIR-TEMPERATURE; ICE CORE; SURFACE-TEMPERATURE; SOIL-MOISTURE;
PRECIPITATION; VARIABILITY; HIMALAYA; RESOLUTION; SCALES; GAUGE
AB This study uses high-resolution, long-term satellite observations to evaluate the spatial scales of the climate variations across the Tibet Plateau (TP). Both land surface temperature and precipitation observations of more than 10 years were analysed with a special attention to eight existing ice-core sites in the TP. The temporal correlation for the monthly or annual anomalies between any two points decreases exponentially with their spatial distance, and we used the e-folding decay constant to quantify the spatial scales. We found that the spatial scales are strongly direction-dependent, with distinctive patterns in the west-east and south-north orientations, for example. Meanwhile, in the same directions the scales are largely symmetric backward and forward. Focusing on the west-east and south-north directions, we found the spatial coherence in the first is generally stronger than in the second. The annual surface temperature had typical spatial scales of 302-480 km, while the annual precipitation showed smaller scales of 111-182 km. The majority of the eight ice-core sites exhibit scales much smaller than the typical scales over the TP as a whole. These results provide important observational basis for the selection of appropriate downscaling strategies, deployment of climate-data collection networks, and interpreting paleoclimate reconstructions.
C1 [Chen, Deliang; Ou, Tinghai] Univ Gothenburg, Dept Earth Sci, Reg Climate Grp, S-40530 Gothenburg, Sweden.
[Tian, Yudong] Univ Maryland, NASA, GSFC, College Pk, MD 20742 USA.
[Tian, Yudong] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Yao, Tandong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100101, Peoples R China.
RP Chen, DL (reprint author), Univ Gothenburg, Dept Earth Sci, Reg Climate Grp, S-40530 Gothenburg, Sweden.; Yao, TD (reprint author), Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100101, Peoples R China.
EM deliang@gvc.gu.se; tdyao@itpcas.ac.cn
RI Chen, Deliang/A-5107-2013
OI Chen, Deliang/0000-0003-0288-5618
FU Swedish Research Council grant [621-2014-5320]; Swedish national
strategic research program BECC; Swedish national strategic research
program MERGE; Chinese Academy of Sciences [XDB03000000]
FX The reanalysis data used in this study are from the Research Data
Archive (RDA) that is maintained by the Computational and Information
Systems Laboratory (CISL) at the National Center for Atmospheric
Research (NCAR). D. Chen is supported by a Swedish Research Council
grant (621-2014-5320) and the Swedish national strategic research
programs BECC and MERGE. T. Yao was supported by the Chinese Academy of
Sciences (XDB03000000). Y. Tian acknowledges the hospitality of
University Gothenburg, and appreciates the assistance of Peng Zhang
during his summer visit. The authors wish to acknowledge the two
anonymous reviewers for their detailed and helpful comments which
significantly improved the clarity of the paper.
NR 42
TC 1
Z9 1
U1 8
U2 11
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD AUG 24
PY 2016
VL 6
AR 30304
DI 10.1038/srep30304
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DT9UV
UT WOS:000381848700001
PM 27553388
ER
PT J
AU Ortega, I
Coburn, S
Berg, LK
Lantz, K
Michalsky, J
Ferrare, RA
Hair, J
Hostetler, CA
Volkamer, R
AF Ortega, Ivan
Coburn, Sean
Berg, Larry K.
Lantz, Kathy
Michalsky, Joseph
Ferrare, Richard A.
Hair, JohnathanW.
Hostetler, Chris A.
Volkamer, Rainer
TI The CU 2-D-MAX-DOAS instrument - Part 2: Raman scattering probability
measurements and retrieval of aerosol optical properties
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SKY BRIGHTNESS MEASUREMENTS; RADIATIVE-TRANSFER MODELS; SPECTROSCOPY
MAX-DOAS; ABSORPTION SPECTROSCOPY; MULTIPLE-SCATTERING; SOLAR TRACKER;
IN-SITU; AERONET; DEPTH; DISTRIBUTIONS
AB The multiannual global mean of aerosol optical depth at 550 nm (AOD(550))over land is similar to 0.19, and that over oceans is similar to 0.13. About 45% of the Earth surface shows AOD550 smaller than 0.1. There is a need for measurement techniques that are optimized to measure aerosol optical properties under low AOD conditions. We present an inherently calibrated retrieval (i.e., no need for radiance calibration) to simultaneously measure AOD and the aerosol phase function parameter, g, based on measurements of azimuth distributions of the Raman scattering probability (RSP), the near-absolute rotational Raman scattering (RRS) intensity. We employ radiative transfer model simulations to show that for solar azimuth RSP measurements at solar elevation and solar zenith angle (SZA) smaller than 80 degrees, RSP is insensitive to the vertical distribution of aerosols and maximally sensitive to changes in AOD and g under near-molecular scattering conditions. The University of Colorado two-dimensional Multi-AXis Differential Optical Absorption Spectroscopy (CU 2-D-MAX-DOAS) instrument was deployed as part of the Two Column Aerosol Project (TCAP) at Cape Cod, MA, during the summer of 2012 to measure direct sun spectra and RSP from scattered light spectra at solar relative azimuth angles (SRAAs) between 5 and 170 degrees. During two case study days with (1) high aerosol load (17 July, 0.3 < AOD(430) < 0.6) and (2) near-molecular scattering conditions (22 July, AOD(430) < 0.13) we compare RSP-based retrievals of AOD(430) and g with data from a co-located CIMEL sun photometer, Multi-Filter Rotating Shadowband Radiometer (MFRSR), and an airborne High Spectral Resolution Lidar (HSRL-2). The average difference (relative to DOAS) for AOD(430) is + 0.012 +/- 0.023 (CIMEL), -0.012 +/- 0.024 (MFRSR), -0.011 +/- 0.014 (HSRL-2), and +0.023 +/- 0.013 (CIMELAOD - MFRSRAOD) and yields the following expressions for correlations between different instruments: DOAS(AOD) = -(0.019 +/- 0.006) + (1.03 +/- 0.02) X CIMELAOD (R-2 = 0.98), DOAS(AOD) = -(0.006 +/- 0.005) +. 1.08 +/- 0.02) x MFRSRAOD (R-2 = 0.98), and CIMELAOD = (0.013 +/- 0.004) + (1.05 +/- 0.01) x MFRSRAOD (R-2 = 0.99). The average g measured by DOAS on both days was 0.66 +/- 0.03, with a difference of 0.014 +/- 0.05 compared to CIMEL. Active steps to minimize the error in the RSP help to reduce the uncertainty in retrievals of AOD and g. As AOD decreases and SZA increases, the RSP signal-to-noise ratio increases. At AOD(430) similar to 0.4 and 0.10 the absolute AOD errors are similar to 0.014 and 0.003 at 70 degrees SZA and 0.02 and 0.004 at 35 degrees SZA. Inherently calibrated, precise AOD and g measurements are useful to better characterize the aerosol direct effect in urban polluted and remote pristine environments.
C1 [Ortega, Ivan; Coburn, Sean; Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Ortega, Ivan; Coburn, Sean; Lantz, Kathy; Michalsky, Joseph; Volkamer, Rainer] CIRES, Boulder, CO 80309 USA.
[Berg, Larry K.] Pacific Northwest Natl Lab, Richland, WA USA.
[Lantz, Kathy; Michalsky, Joseph] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA.
[Ferrare, Richard A.; Hair, JohnathanW.; Hostetler, Chris A.] NASA Langley Res Ctr, Hampton, VA USA.
RP Volkamer, R (reprint author), Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.; Volkamer, R (reprint author), CIRES, Boulder, CO 80309 USA.
EM rainer.volkamer@colorado.edu
RI Volkamer, Rainer/B-8925-2016
OI Volkamer, Rainer/0000-0002-0899-1369
FU NSF-CAREER [ATM-0847793]; US Department of Energy (DOE) [DE-SC0006080];
NASA Earth Science graduate fellowship; DOE Atmospheric System Research
(ASR) Program; Battelle Memorial Institute [DE-AC06-76RLO 1830]; DOE ARM
program: Interagency Agreement [DE-SC0006730]
FX The instrument was developed with support from the NSF-CAREER award
ATM-0847793; US Department of Energy (DOE) award DE-SC0006080 supported
the TCAP deployment (RV). Ivan Ortega is the recipient of a NASA Earth
Science graduate fellowship. Larry Berg is supported by the DOE
Atmospheric System Research (ASR) Program. The Pacific Northwest
National Laboratory is operated by Battelle Memorial Institute under
contract DE-AC06-76RLO 1830. Support for the HSRL-2 light operations
during TCAP was provided by the DOE ARM program: Interagency Agreement
DE-SC0006730. We are grateful to Tim Deutschmann for providing support
with the McArtim RTM. We thank Caroline Fayt and Michel van Roozendael
for providing the WinDOAS software and Thomas Wagner for helpful
discussions.
NR 61
TC 0
Z9 0
U1 3
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 23
PY 2016
VL 9
IS 8
BP 3893
EP 3910
DI 10.5194/amt-9-3893-2016
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YI
UT WOS:000383796900001
ER
PT J
AU Lubken, FJ
Baumgarten, G
Hildebrand, J
Schmidlin, FJ
AF Luebken, Franz-Josef
Baumgarten, Gerd
Hildebrand, Jens
Schmidlin, Francis J.
TI Simultaneous and co-located wind measurements in the middle atmosphere
by lidar and rocket-borne techniques
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID METEOROLOGICAL ROCKETSONDE; RAYLEIGH/MIE/RAMAN LIDAR; CAMPAIGN; CLOUDS
AB We present the first comparison of a new lidar technique to measure winds in the middle atmosphere, called DoRIS (Doppler Rayleigh Iodine Spectrometer), with a rocket-borne in situ method, which relies on measuring the horizontal drift of a target ("starute") by a tracking radar. The launches took place from the Andoya Space Center (ASC), very close to the ALOMAR observatory (Arctic Lidar Observatory for Middle Atmosphere Research) at 69 degrees N. DoRIS is part of a steerable twin lidar system installed at ALOMAR. The observations were made simultaneously and with a horizontal distance between the two lidar beams and the starute trajectories of typically 0-40 km only. DoRIS measured winds from 14 March 2015, 17:00 UTC, to 15 March 2015, 11:30 UTC. A total of eight starute flights were launched successfully from 14 March, 19:00 UTC, to 15 March, 00:19 UTC. In general there is excellent agreement between DoRIS and the in situ measurements, considering the combined range of uncertainties. This concerns not only the general height structures of zonal and meridional winds and their temporal developments, but also some wavy structures. Considering the comparison between all starute flights and all DoRIS observations in a time period of +/- 20 min around each individual starute flight, we arrive at mean differences of typically +/- 5-10 m s(-1) for both wind components. Part of the remaining differences are most likely due to the detection of different wave fronts of gravity waves. There is no systematic difference between DoRIS and the in situ observations above 30 km. Below similar to 30 km, winds from DoRIS are systematically too large by up to 10-20 m s(-1), which can be explained by the presence of aerosols. This is proven by deriving the backscatter ratios at two different wavelengths. These ratios are larger than unity, which is an indication of the presence of aerosols.
C1 [Luebken, Franz-Josef; Baumgarten, Gerd; Hildebrand, Jens] Leibniz Inst Atmospher Phys, Schloss Str 6, Kuhlungsborn, Germany.
[Schmidlin, Francis J.] NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA.
RP Lubken, FJ (reprint author), Leibniz Inst Atmospher Phys, Schloss Str 6, Kuhlungsborn, Germany.
EM luebken@iap-kborn.de
OI Baumgarten, Gerd/0000-0002-6727-284X
FU German Space Agency (DLR) [50 OE 1001]; European Union [653980]
FX The support of the German MORABA team (DLR) and the Andoya Space Center
for preparing and launching the meteorological rockets is highly
appreciated. We thank Boris Strelnikov for leading the launch operation.
This work was supported by the German Space Agency (DLR) under grant 50
OE 1001 (Project WADIS). DoRIS was partly supported by the European
Union's Horizon 2020 research and innovation programme under grant
agreement no. 653980. The authors wish to thank the National Aeronautics
and Space Administration for providing the small meteorological rockets.
NR 24
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 23
PY 2016
VL 9
IS 8
BP 3911
EP 3919
DI 10.5194/amt-9-3911-2016
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YI
UT WOS:000383796900002
ER
PT J
AU Scheepmaker, RA
aan de Brugh, J
Hu, HL
Borsdorff, T
Frankenberg, C
Risi, C
Hasekamp, O
Aben, I
Landgraf, J
AF Scheepmaker, Remco A.
aan de Brugh, Joost
Hu, Haili
Borsdorff, Tobias
Frankenberg, Christian
Risi, Camille
Hasekamp, Otto
Aben, Ilse
Landgraf, Jochen
TI HDO and H2O total column retrievals from TROPOMI shortwave infrared
measurements
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SCIAMACHY HDO/H2O MEASUREMENTS; GENERAL-CIRCULATION MODEL; HEXAGONAL ICE
CRYSTALS; WATER-VAPOR; SENTINEL-5 PRECURSOR; OBSERVING NETWORK; STABLE
ISOTOPES; SPECTRA; SPECTROSCOPY; TEMPERATURE
AB The TROPOspheric Monitoring Instrument (TROPOMI) on board the European Space Agency Sentinel-5 Precursor mission is scheduled for launch in the last quarter of 2016. As part of its operational processing the mission will provide CH4 and CO total columns using backscattered sunlight in the shortwave infrared band (2.3 mu m). By adapting the CO retrieval algorithm, we have developed a non-scattering algorithm to retrieve total column HDO and H2O from the same measurements under clear-sky conditions. The isotopologue ratio HDO/H2O is a powerful diagnostic in the efforts to improve our understanding of the hydrological cycle and its role in climate change, as it provides an insight into the source and transport history of water vapour, nature's strongest greenhouse gas. Due to the weak reflectivity over water surfaces, we need to restrict the retrieval to cloud-free scenes over land. We exploit a novel 2-band filter technique, using strong vs. weak water or methane absorption bands, to prefilter scenes with medium-to-high-level clouds, cirrus or aerosol and to significantly reduce processing time. Scenes with cloud top heights. 1 km, very low fractions of high-level clouds or an aerosol layer above a high surface albedo are not filtered out. We use an ensemble of realistic measurement simulations for various conditions to show the efficiency of the cloud filter and to quantify the performance of the retrieval. The single-measurement precision in terms of delta D is better than 15-25 parts per thousand for even the lowest surface albedo (2-4 parts per thousand for high albedos), while a small bias remains possible of up to similar to 20 parts per thousand due to remaining aerosol or up to similar to 70 parts per thousand due to remaining cloud contamination. We also present an analysis of the sensitivity towards prior assumptions, which shows that the retrieval has a small but significant sensitivity to the a priori assumption of the atmospheric trace gas profiles. Averaging multiple measurements over time and space, however, will reduce these errors, due to the quasi-random nature of the profile uncertainties. The sensitivity of the retrieval with respect to instrumental parameters within the expected instrument performance is <3 parts per thousand, which represents only a small contribution to the overall error budget. Spectroscopic uncertainties of the water lines, however, can have a larger and more systematic impact on the performance of the retrieval and warrant further reassessment of the water line parameters. With TROPOMI's high radiometric sensitivity, wide swath (resulting in daily global coverage) and efficient cloud filtering, in combination with a spatial resolution of 7 x 7 km(2), we will greatly increase the amount of useful data on HDO, H2O and their ratio HDO/H2O. We showcase the overall performance of the retrieval algorithm and cloud filter with an accurate simulation of TROPOMI measurements from a single overpass over parts of the USA and Mexico, based on MODIS satellite data and realistic conditions for the surface, atmosphere and chemistry (including isotopologues). This shows that TROPOMI will pave the way for new studies of the hydrological cycle, both globally and locally, on timescales of mere days and weeks instead of seasons and years and will greatly extend the HDO/H2O datasets from the SCIAMACHY and GOSAT missions.
C1 [Scheepmaker, Remco A.; aan de Brugh, Joost; Hu, Haili; Borsdorff, Tobias; Hasekamp, Otto; Aben, Ilse; Landgraf, Jochen] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Risi, Camille] CNRS, Insitut Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France.
RP Landgraf, J (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands.
EM j.landgraf@sron.nl
RI Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
FU TROPOMI national programme from the Netherlands Space Office (NSO)
FX H. Hu and J. aan de Brugh are in part financed by the TROPOMI national
programme from the Netherlands Space Office (NSO). LMDZiso simulations
used the computing resources of IDRIS under the allocation 0292 made by
GENCI. We thank the two anonymous referees for their useful comments
that improved this paper.
NR 59
TC 2
Z9 2
U1 3
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 23
PY 2016
VL 9
IS 8
BP 3921
EP 3937
DI 10.5194/amt-9-3921-2016
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YK
UT WOS:000383797100001
ER
PT J
AU Joiner, J
Yoshida, Y
Guanter, L
Middleton, EM
AF Joiner, Joanna
Yoshida, Yasuko
Guanter, Luis
Middleton, Elizabeth M.
TI New methods for the retrieval of chlorophyll red fluorescence from
hyperspectral satellite instruments: simulations and application to
GOME-2 and SCIAMACHY
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SUN-INDUCED FLUORESCENCE; GROSS PRIMARY PRODUCTION; MONITORING
INSTRUMENT; SENTINEL-5 PRECURSOR; CANOPY FLUORESCENCE; RAMAN-SCATTERING;
COASTAL WATERS; A FLUORESCENCE; B-BANDS; SPACE
AB Global satellite measurements of solar-induced fluorescence (SIF) from chlorophyll over land and ocean have proven useful for a number of different applications related to physiology, phenology, and productivity of plants and phytoplankton. Terrestrial chlorophyll fluorescence is emitted throughout the red and far-red spectrum, producing two broad peaks near 683 and 736 nm. From ocean surfaces, phytoplankton fluorescence emissions are entirely from the red region (683 nm peak). Studies using satellite-derived SIF over land have focused almost exclusively on measurements in the far red (wavelengths >712 nm), since those are the most easily obtained with existing instrumentation. Here, we examine new ways to use existing hyperspectral satellite data sets to retrieve red SIF (wavelengths <712 nm) over both land and ocean. Red SIF is thought to provide complementary information to that from the far red for terrestrial vegetation. The satellite instruments that we use were designed to make atmospheric trace-gas measurements and are therefore not optimal for observing SIF; they have coarse spatial resolution and only moderate spectral resolution (0.5 nm). Nevertheless, these instruments, the Global Ozone Monitoring Instrument 2 (GOME-2) and the SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY (SCIAMACHY), offer a unique opportunity to compare red and far-red terrestrial SIF at regional spatial scales. Terrestrial SIF has been estimated with ground-, aircraft-, or satellite-based instruments by measuring the filling-in of atmospheric and/or solar absorption spectral features by SIF. Our approach makes use of the oxygen (O-2) gamma band that is not affected by SIF. The SIF-free O-2 gamma band helps to estimate absorption within the spectrally variable O-2 B band, which is filled in by red SIF. SIF also fills in the spectrally stable solar Fraunhofer lines (SFLs) at wavelengths both inside and just outside the O-2 B band, which further helps to estimate red SIF emission. Our approach is then an extension of previous approaches applied to satellite data that utilized only the filling-in of SFLs by red SIF. We conducted retrievals of red SIF using an extensive database of simulated radiances covering a wide range of conditions. Our new algorithm produces good agreement between the simulated truth and retrievals and shows the potential of the O-2 bands for noise reduction in red SIF retrievals as compared with approaches that rely solely on SFL filling. Biases seen with existing satellite data, most likely due to instrumental artifacts that vary in time, space, and with instrument, must be addressed in order to obtain reasonable results. Our 8-year record of red SIF observations over land with the GOME-2 allows for the first time reliable global mapping of monthly anomalies. These anomalies are shown to have similar spatiotemporal structure as those in the far red, particularly for drought-prone regions. There is a somewhat larger percentage response in the red as compared with the far red for these areas that are drought sensitive. We also demonstrate that good-quality ocean fluorescence line height retrievals can be achieved with GOME-2, SCIAMACHY, and similar instruments by utilizing the full complement of radiance measurements that span the red SIF emission feature.
C1 [Joiner, Joanna; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA.
[Guanter, Luis] Helmholtz Ctr, Potsdam, Germany.
RP Joiner, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joanna.joiner@nasa.gov
FU NASA; Emmy Noether Programme (GlobFluo project) of the German Research
Foundation
FX Funding for this work was provided by NASA and the Emmy Noether
Programme (GlobFluo project) of the German Research Foundation. The
authors are indebted to Phil Durbin, Ghassan Taha, and Michael Yan for
their assistance with the satellite data sets. We gratefully acknowledge
the European Meteorological Satellite (EUMETSAT) program, ESA, and NASA,
particularly the MODIS data processing team, for making available the
GOME-2, SCIAMACHY, and MODIS data used here. We also thank Alexander
Vasilkov, Karl (Fred) Huemmrich, William Cook, Qingyuan Zhang, Rose
Munro, Rudiger Lang, Joseph Berry, John Burrows, P. K. Bhartia, Petya
Campbell, Lawrence Corp, Kelly Chance, and Arlindo da Silva for helpful
discussions. Finally, we thank the two anonymous reviewers for comments
and suggestions that helped to improve the manuscript.
NR 99
TC 2
Z9 2
U1 23
U2 23
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 23
PY 2016
VL 9
IS 8
BP 3939
EP 3967
DI 10.5194/amt-9-3939-2016
PG 29
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YM
UT WOS:000383797300001
ER
PT J
AU Colose, CM
LeGrande, AN
Vuille, M
AF Colose, Christopher M.
LeGrande, Allegra N.
Vuille, Mathias
TI Hemispherically asymmetric volcanic forcing of tropical hydroclimate
during the last millennium
SO EARTH SYSTEM DYNAMICS
LA English
DT Article
ID INTERTROPICAL CONVERGENCE ZONE; STRATOSPHERIC AEROSOLS; PAST MILLENNIUM;
GLACIAL MAXIMUM; HEAT-TRANSPORT; ENERGY BUDGET; ITCZ LOCATION;
ERUPTIONS; CLIMATE; OCEAN
AB Volcanic aerosols exert the most important natural radiative forcing of the last millennium. State-of-the-art paleoclimate simulations of this interval are typically forced with diverse spatial patterns of volcanic forcing, leading to different responses in tropical hydroclimate. Recently, theoretical considerations relating the intertropical convergence zone (ITCZ) position to the demands of global energy balance have emerged in the literature, allowing for a connection to be made between the paleoclimate simulations and recent developments in the understanding of ITCZ dynamics. These energetic considerations aid in explaining the well-known historical, paleoclimatic, and modeling evidence that the ITCZ migrates away from the hemisphere that is energetically deficient in response to asymmetric forcing.
Here we use two separate general circulation model (GCM) suites of experiments for the last millennium to relate the ITCZ position to asymmetries in prescribed volcanic sulfate aerosols in the stratosphere and related asymmetric radiative forcing. We discuss the ITCZ shift in the context of atmospheric energetics and discuss the ramifications of transient ITCZ migrations for other sensitive indicators of changes in the tropical hydrologic cycle, including global streamflow. For the first time, we also offer insight into the large-scale fingerprint of water isotopologues in precipitation (delta O-18(p)) in response to asymmetries in radiative forcing.
The ITCZ shifts away from the hemisphere with greater volcanic forcing. Since the isotopic composition of precipitation in the ITCZ is relatively depleted compared to areas outside this zone, this meridional precipitation migration results in a large-scale enrichment (depletion) in the isotopic composition of tropical precipitation in regions the ITCZ moves away from (toward). Our results highlight the need for careful consideration of the spatial structure of volcanic forcing for interpreting volcanic signals in proxy records and therefore in evaluating the skill of Common Era climate model output.
C1 [Colose, Christopher M.; Vuille, Mathias] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
[LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Colose, CM (reprint author), SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
EM ccolose@albany.edu
FU NOAA [C2D2 NA10OAR4310126]; NSF [AGS-1003690, AGS-1303828]; NASA
[GISS-E2]; NASA High-End Computing (HEC) Program through the NASA Center
for Climate Simulation (NCCS) at Goddard Space Flight Center
FX This study was funded by NOAA C2D2 NA10OAR4310126 and NSF awards
AGS-1003690 and AGS-1303828. We would like to thank NASA GISS-E2 for
institutional support. Computing resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center. We
acknowledge the CESM1(CAM5) Last Millennium Ensemble Community Project
and supercomputing resources provided by NSF/CISL/Yellowstone.
NR 74
TC 3
Z9 3
U1 8
U2 8
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 2190-4979
EI 2190-4987
J9 EARTH SYST DYNAM
JI Earth Syst. Dynam.
PD AUG 23
PY 2016
VL 7
IS 3
BP 681
EP 696
DI 10.5194/esd-7-681-2016
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA DW6ZM
UT WOS:000383799900001
ER
PT J
AU Yuan, P
Koppelmans, V
Reuter-Lorenz, PA
De Dios, YE
Gadd, NE
Wood, SJ
Riascos, R
Kofman, IS
Bloomberg, JJ
Mulavara, AP
Seidler, RD
AF Yuan, Peng
Koppelmans, Vincent
Reuter-Lorenz, Patricia A.
De Dios, Yiri E.
Gadd, Nichole E.
Wood, Scott J.
Riascos, Roy
Kofman, Igor S.
Bloomberg, Jacob J.
Mulavara, Ajitkumar P.
Seidler, Rachael D.
TI Increased Brain Activation for Dual Tasking with 70-Days Head-Down Bed
Rest
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Article
DE dual task; head-down bed rest; fMRI; microgravity analog; brain activity
ID SENSORIMOTOR PERFORMANCE; COGNITIVE PERFORMANCE; MENTAL PERFORMANCE;
SPACE MISSION; SHORT-TERM; METAANALYSIS; SPACEFLIGHT; CEREBELLUM;
DURATION; CORTEX
AB Head-down tilt bed rest (HDBR) has been used as a spaceflight analog to simulate the effects of microgravity exposure on human physiology, sensorimotor function, and cognition on Earth. Previous studies have reported that concurrent performance of motor and cognitive tasks can be impaired during space missions. Understanding the consequences of HDBR for neural control of dual tasking may possibly provide insight into neural efficiency during spaceflight. In the current study, we evaluated how dual task performance and the underlying brain activation changed as a function of HDBR. Eighteen healthy men participated in this study. They remained continuously in the 6 degrees head-down tilt position for 70 days. Functional MRI for bimanual finger tapping was acquired during both single task and dual task conditions, and repeated at 7 time points pre-, during- and post-HDBR. Another 12 healthy males participated as controls who did not undergo HDBR. A widely distributed network involving the frontal, parietal, cingulate, temporal, and occipital cortices exhibited increased activation for dual tasking and increased activation differences between dual and single task conditions during HDBR relative to pre- or post-HDBR. This HDBR-related brain activation increase for dual tasking implies that more neurocognitive control is needed for dual task execution during HDBR compared to pre- and post-HDBR. We observed a positive correlation between pre-to-post HDBR changes in dual-task cost of reaction time and pre-to-post HDBR change in dual-task cost of brain activation in several cerebral and cerebellar regions. These findings could be predictive of changes in dual task processing during spaceflight.
C1 [Yuan, Peng; Koppelmans, Vincent; Seidler, Rachael D.] Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA.
[Reuter-Lorenz, Patricia A.; Seidler, Rachael D.] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA.
[De Dios, Yiri E.; Gadd, Nichole E.; Kofman, Igor S.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Wood, Scott J.] Azusa Pacific Univ, Dept Psychol, Azusa, CA USA.
[Riascos, Roy] Univ Texas Hlth Sci Ctr Houston, Houston, TX 77030 USA.
[Bloomberg, Jacob J.; Mulavara, Ajitkumar P.] NASA, Johnson Space Ctr, Houston, TX USA.
[Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA.
[Seidler, Rachael D.] Univ Michigan, Sch Med, Neurosci Program, Ann Arbor, MI 48109 USA.
RP Seidler, RD (reprint author), Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA.; Seidler, RD (reprint author), Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA.; Seidler, RD (reprint author), Univ Michigan, Sch Med, Neurosci Program, Ann Arbor, MI 48109 USA.
EM rseidler@umich.edu
OI Riascos, Roy/0000-0002-3081-0413
FU National Space Biomedical Research Institute [NASA NCC 9-58, MA02701,
PF04101, NNX11AR02G]; NASA Flight Analogs Project; National Institutes
of Health; National Center for Advancing Translational Sciences
[1UL1RR029876-01]
FX This work is supported by grants from the National Space Biomedical
Research Institute (NASA NCC 9-58, MA02701, and PF04101), from the
National Aeronautics and Space Administration (NASA; NNX11AR02G) and
NASA Flight Analogs Project, and the National Institutes of Health, and
National Center for Advancing Translational Sciences, 1UL1RR029876-01.
NR 46
TC 1
Z9 1
U1 0
U2 0
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD AUG 23
PY 2016
VL 10
AR 71
DI 10.3389/fnsys.2016.00071
PG 14
WC Neurosciences
SC Neurosciences & Neurology
GA DT9DK
UT WOS:000381795600002
PM 27601982
ER
PT J
AU Nicholson, JW
DeSantolo, A
Yan, MF
Wisk, P
Mangan, B
Puc, G
Yu, AW
Stephen, MA
AF Nicholson, J. W.
DeSantolo, A.
Yan, M. F.
Wisk, P.
Mangan, B.
Puc, G.
Yu, A. W.
Stephen, M. A.
TI High energy, 1572.3 nm pulses for CO2 LIDAR from a
polarization-maintaining, very-large-mode-area, Er-doped fiber amplifier
SO OPTICS EXPRESS
LA English
DT Article
ID PEAK-POWER; MU-M; LASER; AMPLIFICATION; MJ
AB We demonstrate the first polarization-maintaining, very-large-mode-area, Er-doped fiber amplifier with similar to 1100 mu m(2) effective area. The amplifier is core pumped by a Raman fiber laser and is used to generate single-frequency, one-microsecond, pulses with pulse energy of 541 mu J, peak power of 700 W, M-2 of 1.1, and polarization extinction >20 dB. The amplifier operates at 1572.3 nm, a wavelength useful for trace atmospheric CO2 detection. (C) 2016 Optical Society of America
C1 [Nicholson, J. W.; DeSantolo, A.; Yan, M. F.; Wisk, P.; Mangan, B.; Puc, G.] OFS Labs, 19 Schoolhouse Rd,Suite 105, Somerset, NJ 08873 USA.
[Yu, A. W.; Stephen, M. A.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Nicholson, JW (reprint author), OFS Labs, 19 Schoolhouse Rd,Suite 105, Somerset, NJ 08873 USA.
EM jwn@ofsoptics.com
NR 21
TC 1
Z9 1
U1 5
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 AUG 22
PY 2016
VL 24
IS 17
BP 19961
EP 19968
AR 268882
DI 10.1364/OE.24.019961
PG 8
WC Optics
SC Optics
GA DY6KV
UT WOS:000385227100106
PM 27557271
ER
PT J
AU Harrison, JJ
Chipperfield, MP
Boone, CD
Dhomse, SS
Bernath, PF
Froidevaux, L
Anderson, J
Russell, J
AF Harrison, Jeremy J.
Chipperfield, Martyn P.
Boone, Christopher D.
Dhomse, Sandip S.
Bernath, Peter F.
Froidevaux, Lucien
Anderson, John
Russell, James, III
TI Satellite observations of stratospheric hydrogen fluoride and
comparisons with SLIMCAT calculations
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID MIDLATITUDE OZONE CHANGES; CHEMICAL-TRANSPORT MODEL; HCL; SIMULATIONS;
CIRCULATION; VALIDATION; CHEMISTRY; COLUMN; HF
AB The vast majority of emissions of fluorine-containing molecules are anthropogenic in nature, e.g. chlorofluorocarbons (CFCs), hydrochlorofluorocarbons (HCFCs), and hydrofluorocarbons (HFCs). Many of these fluorine-containing species deplete stratospheric ozone and are regulated by the Montreal Protocol. Once in the atmosphere they slowly degrade, ultimately leading to the formation of hydrogen fluoride (HF), the dominant reservoir of stratospheric fluorine due to its extreme stability. Monitoring the growth of stratospheric HF is therefore an important marker for the success of the Montreal Protocol.
We report the comparison of global distributions and trends of HF measured in the Earth's atmosphere by the satellite remote-sensing instruments ACE-FTS (Atmospheric Chemistry Experiment Fourier transform spectrometer), which has been recording atmospheric spectra since 2004, and HALOE (HALogen Occultation Experiment), which recorded atmospheric spectra between 1991 and 2005, with the output of SLIMCAT, a state-of-the-art three-dimensional chemical transport model. In general the agreement between observation and model is good, although the ACE-FTS measurements are biased high by similar to 10% relative to HALOE. The observed global HF trends reveal a substantial slowing down in the rate of increase of HF since the 1990s: 4.97 +/- 0.12% year(-1) (1991-1997; HALOE), 1.12 +/- 0.08% year(-1) (1998-2005; HALOE), and 0.52 +/- 0.03% year(-1) (2004-2012; ACE-FTS). In comparison, SLIMCAT calculates trends of 4.01, 1.10, and 0.48% year(-1), respectively, for the same periods; the agreement is very good for all but the earlier of the two HALOE periods. Furthermore, the observations reveal variations in the HF trends with latitude and altitude; for example, between 2004 and 2012 HF actually decreased in the Southern Hemisphere below similar to 35 km. An additional SLIMCAT simulation with repeating meteorology for the year 2000 produces much cleaner trends in HF with minimal variations with latitude and altitude. Therefore, the variations with latitude and altitude in the observed HF trends are due to variability in stratospheric dynamics on the timescale of a few years. Overall, the agreement between observation and model points towards the ongoing success of the Montreal Protocol and the usefulness of HF as a metric for stratospheric fluorine.
C1 [Harrison, Jeremy J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Harrison, Jeremy J.] Univ Leicester, Natl Ctr Earth Observat, Leicester LE1 7RH, Leics, England.
[Chipperfield, Martyn P.; Dhomse, Sandip S.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Chipperfield, Martyn P.; Dhomse, Sandip S.] Univ Leeds, Sch Earth & Environm, Natl Ctr Earth Observat, Leeds LS2 9JT, W Yorkshire, England.
[Boone, Christopher D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA.
[Froidevaux, Lucien] Jet Prop Lab, Pasadena, CA 91109 USA.
[Anderson, John; Russell, James, III] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
RP Harrison, JJ (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.; Harrison, JJ (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester LE1 7RH, Leics, England.
EM jh592@leicester.ac.uk
RI Bernath, Peter/B-6567-2012; Dhomse, Sandip/C-8198-2011
OI Bernath, Peter/0000-0002-1255-396X; Dhomse, Sandip/0000-0003-3854-5383
FU UK Natural Environment Research Council (NERC) [NE/I022663/1]; National
Centre for Earth Observation (NCEO); Canadian Space Agency (CSA); NASA
FX The authors wish to thank the UK Natural Environment Research Council
(NERC) for supporting Jeremy J. Harrison through grant NE/I022663/1 and
through the National Centre for Earth Observation (NCEO). The ACE
satellite mission is funded primarily by the Canadian Space Agency
(CSA). HALOE was funded by NASA. Martyn P. Chipperfield and Sandip S.
Dhomse thank Wuhu Feng (the National Centre for Atmospheric Science;
NCAS) for help with SLIMCAT. Martyn P. Chipperfield is a Royal Society
Wolfson Research Merit Award holder. Work at the Jet Propulsion
Laboratory was performed under contract with the National Aeronautics
and Space Administration (NASA). We thank the ECMWF for providing the
ERA-Interim reanalyses used by the SLIMCAT model.
NR 32
TC 0
Z9 0
U1 3
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 22
PY 2016
VL 16
IS 16
BP 10501
EP 10519
DI 10.5194/acp-16-10501-2016
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6ES
UT WOS:000383742800002
ER
PT J
AU Cheung, SH
Miki, K
Prudencio, E
Simmons, C
AF Cheung, Sai Hung
Miki, Kenji
Prudencio, Ernesto
Simmons, Chris
TI Uncertainty quantification and robust predictive system analysis for
high temperature kinetics of HCN/O-2/Ar mixture
SO CHEMICAL PHYSICS
LA English
DT Article
DE Bayesian approach; Stochastic system; Uncertainty quantification; Robust
predictive analysis; Arrhenius form; Deterministic model; Stochastic
model; Reaction rate; Experimental error; Modeling error
ID THERMAL-DECOMPOSITION; HYDROGEN-CYANIDE; SHOCK-WAVES; ARRHENIUS
PARAMETERS; METHANE COMBUSTION; MODEL; NO; OXIDATION; HCN;
IDENTIFICATION
AB In this paper, a stochastic system based Bayesian approach is applied to quantify the uncertainties involved in the modeling of the HCN/O-2/Ar mixture kinetics proposed by Thielen and Roth (1987). This enables more robust predictions of quantities of interest such as rate coefficients of HCN + Ar -> H + CN + Ar and O-2 + CN -> NCO + O by using a stochastic Arrhenius form calibrated against their experimental data. This Bayesian approach requires the evaluation of multidimensional integrals, which cannot be done analytically. Here a recently developed stochastic simulation algorithm, which allows for efficient sampling in the high-dimensional parameter space, is used. We quantify the uncertainties in the modeling of the HCN/O-2/Ar mixture kinetics and in turn the two rate coefficients and the other relevant rate coefficients. The uncertainty in the error including both the experimental measurement error and physical modeling error is also quantified. The effect of the number of uncertain parameters on the uncertainties is investigated. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Cheung, Sai Hung; Prudencio, Ernesto; Simmons, Chris] Univ Texas Austin, Inst Computat Engn & Sci, 1 Univ Stn, Austin, TX 78712 USA.
[Miki, Kenji] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Miki, K (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM saihung@ices.utexas.edu; kmiki@usra.edu; prudenci@ices.utexas.edu;
csim@ices.utexas.edu
RI Cheung , Sai Hung/A-3781-2011
FU Department of Energy [National Nuclear Security Administration]
[DE-FC52-08NA28615]
FX We are very grateful to Professor Philip L. Varghese at the University
of Texas at Austin for his helpful discussions and comments on the
manuscript. This material is based upon work supported by the Department
of Energy [National Nuclear Security Administration] under Award Number
[DE-FC52-08NA28615].
NR 60
TC 1
Z9 1
U1 5
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-0104
EI 1873-4421
J9 CHEM PHYS
JI Chem. Phys.
PD AUG 22
PY 2016
VL 475
BP 136
EP 152
DI 10.1016/j.chemphys.2016.05.026
PG 17
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DT6IR
UT WOS:000381588400018
ER
PT J
AU Alonso, D
Louis, T
Bull, P
Ferreira, PG
AF Alonso, David
Louis, Thibaut
Bull, Philip
Ferreira, Pedro G.
TI Reconstructing cosmic growth with kinetic Sunyaev-Zel'dovich
observations in the era of stage IV experiments
SO PHYSICAL REVIEW D
LA English
DT Article
ID EARLY-TYPE GALAXIES; PECULIAR VELOCITIES; COSMOLOGICAL CONSTRAINTS;
NONTHERMAL PRESSURE; CLUSTER PHYSICS; POWER SPECTRUM; IA SUPERNOVAE;
DARK ENERGY; LOCAL GROUP; CATALOG
AB Future ground-based cosmic microwave background (CMB) experiments will generate competitive large-scale structure data sets by precisely characterizing CMB secondary anisotropies over a large fraction of the sky. We describe a method for constraining the growth rate of structure to sub-1% precision out to z approximate to 1, using a combination of galaxy cluster peculiar velocities measured using the kinetic Sunyaev-Zel'dovich (kSZ) effect, and the velocity field reconstructed from galaxy redshift surveys. We consider only thermal SZ-selected cluster samples, which will consist of O(10(4)-10(5)) sources for Stage 3 and 4 CMB experiments respectively. Three different methods for separating the kSZ effect from the primary CMB are compared, including a novel blind "constrained realization" method that improves signal-to-noise by a factor of similar to 2 over a commonly-used aperture photometry technique. Assuming a correlation between the integrated tSZ y-parameter and the cluster optical depth, it should then be possible to break the kSZ velocity-optical depth degeneracy. The effects of including CMB polarization and SZ profile uncertainties are also considered. In the absence of systematics, a combination of future Stage 4 experiments should be able to measure the product of the growth and expansion rates, alpha equivalent to fH, to better than 1% in bins of Delta z = 0.1 out to z approximate to 1-competitive with contemporary redshift-space distortion constraints from galaxy surveys. We conclude with a discussion of the likely impact of various systematics.
C1 [Alonso, David; Ferreira, Pedro G.] Univ Oxford, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Louis, Thibaut] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bull, Philip] CALTECH, Pasadena, CA 91125 USA.
[Bull, Philip] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
RP Alonso, D (reprint author), Univ Oxford, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
FU Beecroft Trust; ERC [259505, 267117]; STFC; Higgs Centre in Edinburgh;
NASA
FX We are grateful to Nicholas Battaglia, Jo Dunkley, Simone Ferraro,
Sigurd Naess, and Emmanuel Schaan for useful comments and discussion. We
also thank the anonymous referee, whose input improved the quality of
the paper. D. A. is supported by the Beecroft Trust and ERC Grant No.
259505. T. L. is supported by ERC Grant No. 267117 (DARK) hosted by
Universite Pierre et Marie Curie- Paris 6. P. B.'s research was
supported by an appointment to the NASA Postdoctoral Program at the Jet
Propulsion Laboratory, California Institute of Technology, administered
by Universities Space Research Association under contract with NASA. P.
G. F. acknowledges support from STFC, the Beecroft Trust and the Higgs
Centre in Edinburgh.
NR 71
TC 1
Z9 1
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 22
PY 2016
VL 94
IS 4
AR 043522
DI 10.1103/PhysRevD.94.043522
PG 17
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DU0LA
UT WOS:000381894400004
ER
PT J
AU Daigle, S
Kelly, KJ
Champagne, AE
Buckner, MQ
Iliadis, C
Howard, C
AF Daigle, S.
Kelly, K. J.
Champagne, A. E.
Buckner, M. Q.
Iliadis, C.
Howard, C.
TI Measurement of the E-r(c.m.)=259 ke V resonance in the N-14(p,gamma)O-15
reaction
SO PHYSICAL REVIEW C
LA English
DT Article
ID HEAVY-ION COLLISIONS; LIGHT-NUCLEI; SOLAR NEUTRINOS; CROSS-SECTION;
ENERGY-LEVELS; S-FACTOR; GAMMA)O-15; N-14(P; DETECTOR; SYSTEM
AB The N-14(p,gamma)(15) O reaction regulates the power generated by the CN cycle and thus impacts the structure and evolution of every star at some point in its life. The lowest positive-energy resonance in this reaction is located at E-r(c.m.) = 259 keV, too high in energy to strongly influence quiescent stellar burning. However, the strength of this resonance is used as a cross-section normalization for lower-energy measurements of this reaction. We report on new measurements of the energy, strength, and gamma-ray branching ratios for the 259-keV resonance, using different detection and data-analysis schemes. We have also reevaluated previous results, where possible. Our new recommended strength of omega gamma = 12.6(3) meV is in agreement with the previous value of 13.1(6) meV, but is more precise and thus provides a more reliable normalization for low-energy (p,gamma) measurements.
C1 [Daigle, S.] Univ N Carolina, Chapel Hill, NC 27599 USA.
Triangle Univ Nucl Lab, Durham, NC 27708 USA.
[Daigle, S.] NASA Marshall Space Flight Ctr, NASA Postdoctoral Program, Huntsville, AL 35812 USA.
[Buckner, M. Q.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Howard, C.] Nordion, 447 March Rd, Kanata, ON K2K 1X8, Canada.
RP Daigle, S (reprint author), Univ N Carolina, Chapel Hill, NC 27599 USA.; Daigle, S (reprint author), NASA Marshall Space Flight Ctr, NASA Postdoctoral Program, Huntsville, AL 35812 USA.
EM stephen.daigle@nasa.gov
FU US Department of Energy [DE-FG02-97ER41041]; U.S. Department of Energy
National Nuclear Security Administration [DE-FC52-08NA28752]
FX This work was supported in part by the US Department of Energy under
Contract No. DE-FG02-97ER41041 and by the U.S. Department of Energy
National Nuclear Security Administration under Contract No.
DE-FC52-08NA28752. We would like to thank J. R. Dermigny for his
assistance with the fraction fits.
NR 59
TC 0
Z9 0
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9985
EI 2469-9993
J9 PHYS REV C
JI Phys. Rev. C
PD AUG 22
PY 2016
VL 94
IS 2
AR 025803
DI 10.1103/PhysRevC.94.025803
PG 13
WC Physics, Nuclear
SC Physics
GA DU0KL
UT WOS:000381892200008
ER
PT J
AU Dell'Agli, F
Di Criscienzo, M
Boyer, ML
Garcia-Hernandez, DA
AF Dell'Agli, F.
Di Criscienzo, M.
Boyer, M. L.
Garcia-Hernandez, D. A.
TI Evolved stars in the Local Group galaxies - I. AGB evolution and dust
production in IC 1613
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: abundances; stars: AGB and post-AGB; ISM: abundances
ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE
DIAGRAMS; INTERMEDIATE-MASS STARS; LOW-METALLICITY; STELLAR WINDS;
MINERAL FORMATION; CARBON STARS; CIRCUMSTELLAR ENVELOPES; FORMATION
HISTORY
AB We used models of thermally-pulsing asymptotic giant branch (AGB) stars, that also describe the dust-formation process in the wind, to interpret the combination of near- and mid-infrared photometric data of the dwarf galaxy IC 1613. This is the first time that this approach is extended to an environment different from the Milky Way and the Magellanic Clouds (MCs). Our analysis, based on synthetic population techniques, shows a nice agreement between the observations and the expected distribution of stars in the colour-magnitude diagrams obtained with JHK and Spitzer bands. This allows a characterization of the individual stars in the AGB sample in terms of mass, chemical composition, and formation epoch of the progenitors. We identify the stars exhibiting the largest degree of obscuration as carbon stars evolving through the final AGB phases, descending from 1-1.25Msun objects of metallicity Z=0.001 and from 1.5-2.5Msun stars with Z=0.002. Oxygen-rich stars constitute the majority of the sample (65%), mainly low mass stars (<2Msun) that produce a negligible amount of dust (<10<^>{-7}Msun/yr). We predict the overall dust-production rate from IC 1613, mostly determined by carbon stars, to be 6x10<^>{-7}Msun/yr with an uncertainty of 30%. The capability of the current generation of models to interpret the AGB population in an environment different from the MCs opens the possibility to extend this kind of analysis to other Local Group galaxies.
C1 [Dell'Agli, F.; Di Criscienzo, M.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, CRESST, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Garcia-Hernandez, D. A.] Inst Astrofis Canarias, Via Lactea S-N, E-38200 San Cristobal la Laguna, Spain.
[Garcia-Hernandez, D. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
RP Dell'Agli, F (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy.
EM flaviadellagli@gmail.com
FU Observatory of Rome; European Commission [312725]; Ramon y Cajal
fellowship [RYC-2013-14182]; Spanish Ministry of Economy and
Competitiveness (MINECO) [AYA-2014-58082-P]
FX The authors are indebted to the anonymous referee for the careful
reading of the manuscript and for the several comments, which help
improving significantly the quality of this work. FDA acknowledges
support from the Observatory of Rome. MDC acknowledges Adriano Fontana
and the contribution of the FP7 SPACE project ASTRODEEP (Ref. No.
312725) supported by the European Commission. DAGH was funded by the
Ramon y Cajal fellowship number RYC-2013-14182, and he acknowledges
support provided by the Spanish Ministry of Economy and Competitiveness
(MINECO) under grant AYA-2014-58082-P.
NR 83
TC 1
Z9 1
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 AUG 21
PY 2016
VL 460
IS 4
BP 4230
EP 4241
DI 10.1093/mnras/stw1276
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT8AV
UT WOS:000381711100063
ER
PT J
AU Heywood, I
Jarvis, MJ
Baker, AJ
Bannister, KW
Carvalho, CS
Hardcastle, M
Hilton, M
Moodley, K
Smirnov, OM
Smith, DJB
White, SV
Wollack, EJ
AF Heywood, I.
Jarvis, M. J.
Baker, A. J.
Bannister, K. W.
Carvalho, C. S.
Hardcastle, M.
Hilton, M.
Moodley, K.
Smirnov, O. M.
Smith, D. J. B.
White, S. V.
Wollack, E. J.
TI A deep/wide 1-2 GHz snapshot survey of SDSS Stripe 82 using the Karl G.
Jansky Very Large Array in a compact hybrid configuration
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; radio continuum: general
ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION HISTORY; DEEP FIELD-SOUTH;
INFRARED EXTRAGALACTIC FIELD; SPECTRAL INDEX PROPERTIES; RADIO-AGN
POPULATION; VLA-COSMOS SURVEY; 2ND DATA RELEASE; SKY SURVEY; SOURCE
CATALOG
AB We have used the Karl G. Jansky Very Large Array to image similar to 100 deg(2) of SDSS Stripe 82 at 1-2 GHz. The survey consists of 1026 snapshot observations of 2.5 min duration, using the hybrid CnB configuration. The survey has good sensitivity to diffuse, low surface brightness structures and extended radio emission, making it highly synergistic with existing 1.4 GHz radio observations of the region. The principal data products are continuum images, with 16 x 10 arcsec resolution, and a catalogue containing 11 782 point and Gaussian components resulting from fits to the thresholded Stokes-I brightness distribution, forming approximately 8948 unique radio sources. The typical effective 1 sigma noise level is 88 mu Jy beam(-1). Spectral index estimates are included, as derived from the 1 GHz of instantaneous bandwidth. Astrometric and photometric accuracy are in excellent agreement with existing narrowband observations. A large-scale simulation is used to investigate clean bias, which we extend into the spectral domain. Clean bias remains an issue for snapshot surveys with the VLA, affecting our total intensity measurements at the similar to 1 sigma level. Statistical spectral index measurements are in good agreement with existing measurements derived from matching separate surveys at two frequencies. At flux densities below similar to 35 sigma the median in-band spectral index measurements begin to exhibit a bias towards flatness that is dependent on both flux density and the intrinsic spectral index. In-band spectral curvature measurements are likely to be unreliable for all but the very brightest components. Image products and catalogues are publicly available via an FTP server.
C1 [Heywood, I.; Bannister, K. W.] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
[Heywood, I.; Smirnov, O. M.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Jarvis, M. J.; White, S. V.] Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, Private Bag X17, ZA-7535 Bellville, South Africa.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
[Carvalho, C. S.] Univ Lisbon, Inst Astrophys & Space Sci, P-1349018 Lisbon, Portugal.
[Carvalho, C. S.] Acad Athens, Res Ctr Astron & Appl Math, Soranou Efessiou 4, Athens 11527, Greece.
[Hardcastle, M.; Smith, D. J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Hilton, M.; Moodley, K.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Smirnov, O. M.] SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa.
[White, S. V.] Curtin Univ, ICRAR, Bentley, WA 6102, Australia.
[Wollack, E. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
RP Heywood, I (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.; Heywood, I (reprint author), Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
EM ian.heywood@csiro.au
RI Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Hardcastle,
Martin/0000-0003-4223-1117
FU Australian Government; Government of Western Australia; National Science
Foundation [ACI-1440620]; National Aeronautics and Space
Administration's Earth Science Technology Office [NCC5-626]
FX We thank the anonymous referee and the MNRAS editorial staff for
providing very useful comments on this paper. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
This work was supported by resources provided by the Pawsey
Supercomputing Centre with funding from the Australian Government and
the Government of Western Australia. IH thanks the Rhodes Centre for
Radio Astronomy Techniques and Technologies (RATT) for the provision of
computing facilities. This research has made use of NASA's Astrophysics
Data System. This research made use of Montage. It is funded by the
National Science Foundation under Grant Number ACI-1440620, and was
previously funded by the National Aeronautics and Space Administration's
Earth Science Technology Office, Computation Technologies Project, under
Cooperative Agreement Number NCC5-626 between NASA and the California
Institute of Technology. Some figures in this paper were created using
the PYTHON package APLpy, an open-source plotting package for PYTHON
hosted at http://aplpy.github.com. IH acknowledges useful discussions
with Natasha Maddox. IH thanks the participants of the SAGE workshop,
and SKA South Africa for their hospitality during this event.
NR 89
TC 0
Z9 0
U1 4
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 21
PY 2016
VL 460
IS 4
BP 4433
EP 4452
DI 10.1093/mnras/stw1250
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT8AV
UT WOS:000381711100079
ER
PT J
AU Drouin, BJ
Tang, A
Schlecht, E
Brageot, E
Gu, QJ
Ye, Y
Shu, R
Chang, MCF
Kim, Y
AF Drouin, Brian J.
Tang, Adrian
Schlecht, Erich
Brageot, Emily
Gu, Q. Jane
Ye, Y.
Shu, R.
Chang, Mau-Chung Frank
Kim, Y.
TI A CMOS millimeter-wave transceiver embedded in a semi-confocal
Fabry-Perot cavity for molecular spectroscopy
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID RINGDOWN SPECTROSCOPY; MICROWAVE
AB The extension of radio frequency complementary metal oxide semiconductor (CMOS) circuitry into millimeter wavelengths promises the extension of spectroscopic techniques in compact, power efficient systems. We are now beginning to use CMOS millimeter devices for low-mass, low-power instrumentation capable of remote or in situ detection of gas composition during space missions. We have chosen to develop a Flygare-Balle type spectrometer, with a semi-confocal Fabry-Perot cavity to amplify the pump power of a mm-wavelength CMOS transmitter that is directly coupled to the planar mirror of the cavity. We have built a pulsed transceiver system at 92-105 GHz inside a 3 cm base length cavity and demonstrated quality factor up to 4680, allowing for modes with 20 MHz bandwidth, with a sufficient cavity amplification factor for mW class transmitters. This work describes the initial gas measurements and outlines the challenges and next steps. Published by AIP Publishing.
C1 [Drouin, Brian J.; Tang, Adrian; Schlecht, Erich; Brageot, Emily] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gu, Q. Jane; Ye, Y.; Shu, R.] Univ Calif Davis, Davis, CA 95616 USA.
[Chang, Mau-Chung Frank; Kim, Y.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brian.j.drouin@jpl.nasa.gov
FU National Aeronautics and Space Administration [NNN13D485 T]
FX This material is based upon work supported by the National Aeronautics
and Space Administration under Grant No. NNN13D485 T issued through the
Planetary Science Division PICASSO program. Portions of the research
described in this paper were performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration, government sponsorship
acknowledged.
NR 15
TC 0
Z9 0
U1 6
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD AUG 21
PY 2016
VL 145
IS 7
AR 074201
DI 10.1063/1.4961020
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DT7QG
UT WOS:000381680700019
PM 27544098
ER
PT J
AU Carlberg, JK
Cunha, K
Smith, VV
AF Carlberg, Joleen K.
Cunha, Katia
Smith, Verne V.
TI LITHIUM INVENTORY OF 2 M-circle dot RED CLUMP STARS IN OPEN CLUSTERS: A
TEST OF THE HELIUM FLASH MECHANISM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (Collinder 110, NGC 2204, NGC
2506, NGC 6583); stars: abundances; stars: late-type
ID OLD OPEN CLUSTERS; AGE OPEN CLUSTERS; GIANT STARS; RADIAL-VELOCITIES;
CHEMICAL-COMPOSITION; MAIN-SEQUENCE; NGC 7789; LI; EVOLUTION; ABUNDANCE
AB The temperature distribution of field Li-rich red giants suggests the presence of a population of Li-rich red clump (RC) stars. One proposed explanation for this population is that all stars with masses near 2 M-circle dot experience a shortlived phase of Li-richness at the onset of core He-burning. Many of these stars have low C-12/C-13, a signature of deep mixing that is presumably associated with the Li regeneration. To test this purported mechanism of Li enrichment, we measured abundances in 38 RC stars and 6 red giant branch (RGB) stars in four open clusters selected to have RC masses near 2 M-circle dot. We find six Li-rich stars (A(Li) >= 1.50 dex) of which only two may be RC stars. None of the RC stars have Li exceeding the levels observed in the RGB stars, but given the brevity of the suggested Li-rich phase and the modest sample size, it is probable that stars with larger Li-enrichments were missed simply by chance. However, we find very few stars in our sample with low C-12/C-13. Such low C-12/C-13, seen in many field Li-rich stars, should persist even after lithium has returned to normal low levels. Thus, if Li synthesis during the He flash occurs, it is a rare, but potentially long-lived occurrence rather than a short-lived phase for all stars. We estimate a conservative upper limit of the fraction of stars going through a Li-rich phase to be < 47%, based on stars that have low C-12/C-13 for their observed A(Li).
C1 [Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
[Cunha, Katia] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Smith, Verne V.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA.
RP Carlberg, JK (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
EM joleen.k.carlberg@nasa.gov
FU NASA Postdoctoral Program at the Goddard Space Flight Center; NASA
FX We are grateful to S. H. Lee and H. B. Ann for providing us their
optical photometry of the NGC 2506 red giants in this study. We also
thank the referee for valuable feedback that improved this manuscript.
JKC acknowledges support by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Universities
Space Research Association through a contract with NASA. This paper
includes data gathered with the 6.5 m Magellan Telescopes located at Las
Campanas Observatory, Chile and made use of the WEBDA database, operated
at the Department of Theoretical Physics and Astrophysics of the Masaryk
University.
NR 54
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
IS 2
AR 129
DI 10.3847/0004-637X/827/2/129
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600041
ER
PT J
AU Fischer, WJ
Padgett, DL
Stapelfeldt, KL
Sewilo, M
AF Fischer, William J.
Padgett, Deborah L.
Stapelfeldt, Karl L.
Sewilo, Marta
TI A WISE CENSUS OF YOUNG STELLAR OBJECTS IN CANIS MAJOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: formation; stars:
protostars Supporting material: figure set, machine-readable table
ID INFRARED-SURVEY-EXPLORER; SPACE-TELESCOPE SURVEY; (CO)-C-13 J=1-0
SURVEY; STAR-FORMING REGIONS; MOLECULAR CLOUDS; SPITZER SURVEY; CARINA
NEBULA; OUTER GALAXY; MILKY-WAY; HI-GAL
AB With the Wide-field Infrared Survey Explorer (WISE), we searched for young stellar objects (YSOs) in a 100 deg(2) region centered on the lightly studied Canis Major star-forming region. Applying stringent magnitude cuts to exclude the majority of extragalactic contaminants, we find 144 Class I candidates and 335 Class II candidates. The sensitivity to Class II candidates is limited by their faintness at the distance to Canis Major (assumed as 1000 pc). More than half the candidates (53%) are found in 16 groups of more than four members, including four groups with more than 25 members each. The ratio of Class II to Class I objects, N-II/N-I, varies from 0.4 to 8.3 in just the largest four groups. We compare our results to those obtainable with combined Two Micron All Sky Survey and post-cryogenic Spitzer Space Telescope data; the latter approach recovers missing Class II sources. Via a comparison to protostars characterized with the Herschel Space Observatory, we propose new WISE color criteria for flat-spectrum and Class 0 protostars, finding 80 and 7. of these, respectively. The distribution of YSOs in CMa OB1 is consistent with supernova-induced star formation, although the diverse N-II/N-I ratios are unexpected if this parameter traces age and the YSOs are due to the same supernova. Less massive clouds feature larger N-II/N-I ratios, suggesting that initial conditions play a role in determining this quantity.
C1 [Fischer, William J.; Padgett, Deborah L.; Sewilo, Marta] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stapelfeldt, Karl L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Fischer, WJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM william.j.fischer@nasa.gov
OI Fischer, William J/0000-0002-3747-2496
FU University of California, Los Angeles; National Aeronautics and Space
Administration (NASA); NASA Postdoctoral Program at Goddard Space Flight
Center; NASA; National Science Foundation [ACI-1440620]
FX This paper 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 (JPL/Caltech), funded by the National
Aeronautics and Space Administration (NASA). The work of W. J. F. and M.
S. was supported by appointments to the NASA Postdoctoral Program at
Goddard Space Flight Center. This research made use of the NASA/Infrared
Processing and Analysis Center Infrared Science Archive, which is
operated by JPL/Caltech under contract with NASA. This research also
made use of Montage, which is funded by the National Science Foundation
under Grant Number ACI-1440620, and was previously funded by NASA's
Earth Science Technology Office, Computation Technologies Project, under
Cooperative Agreement Number NCC5-626 between NASA and Caltech.
NR 55
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
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AR 96
DI 10.3847/0004-637X/827/2/96
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600008
ER
PT J
AU Flock, M
Fromang, S
Turner, NJ
Benisty, M
AF Flock, M.
Fromang, S.
Turner, N. J.
Benisty, M.
TI RADIATION HYDRODYNAMICS MODELS OF THE INNER RIM IN PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; magnetohydrodynamics (MHD); radiative
transfer; techniques: interferometric
ID HERBIG AE/BE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; STRATIFIED ACCRETION
DISKS; INTERMEDIATE-MASS STARS; CIRCUMSTELLAR DISKS; PLANET FORMATION;
CONVECTIVE OVERSTABILITY; PROTOSTELLAR DISKS; SOLAR NEBULA; DEAD ZONES
AB Many stars host planets orbiting within a few astronomical units (AU). The occurrence rate and distributions of masses and orbits vary greatly with the host star's mass. These close planets' origins are a mystery that motivates investigating protoplanetary disks' central regions. A key factor governing the conditions near the star is the silicate sublimation front, which largely determines where the starlight is absorbed, and which is often called the inner rim. We present the first radiation hydrodynamical modeling of the sublimation front in the disks around the young intermediate-mass stars called Herbig Ae stars. The models are axisymmetric. and include starlight heating;. silicate grains sublimating and condensing to equilibrium at the local, time-dependent temperature and density;. and accretion stresses parameterizing the results of MHD magnetorotational turbulence models. The results compare well with radiation hydrostatic solutions. and prove to be dynamically stable. Passing the model disks into Monte Carlo radiative transfer calculations, we show that the models satisfy observational constraints on the inner rim's location. A small optically thin halo of hot dust naturally arises between the inner rim and the star. The inner rim has a substantial radial extent, corresponding to several disk scale heights. While the front's overall position varies with the stellar luminosity, its radial extent depends on the mass accretion rate. A pressure maximum develops near the location of thermal ionization at temperatures of. about 1000 K. The pressure maximum is capable of halting solid pebbles' radial drift and concentrating them in a zone where temperatures are sufficiently high for annealing to form crystalline silicates.
C1 [Flock, M.; Turner, N. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Flock, M.; Fromang, S.] Univ Paris 07, CEA Saclay, Irfu, Lab AIM,CEA,DSM,CNRS,Serv Astrophys, F-91191 Gif sur Yvette, France.
[Benisty, M.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
RP Flock, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Flock, M (reprint author), Univ Paris 07, CEA Saclay, Irfu, Lab AIM,CEA,DSM,CNRS,Serv Astrophys, F-91191 Gif sur Yvette, France.
EM mflock@caltech.edu
FU European Research Council under the European Union's Seventh Framework
Programme (FP7)/ERC [258729]; National Aeronautics and Space
Administration; NASA Exoplanet Research program [14XRP14_20153]
FX The authors thank Antonella Natta, Wlad Lyra, Rafael Millan-Gabet, Gijs
Mulders, and Satoshi Okuzumi for useful comments on the manuscript. We
thank Andrea Mignone for supporting and advising us with the newest
PLUTO code. Parallel computations have been performed on the Genci
supercomputer "curie" at the calculation center of CEA TGCC and on the
zodiac supercomputer at JPL. For this work, S.F. and M.F. received
funding from the European Research Council under the European Union's
Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement nr.
258729. This research was carried out in part at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration and with the support
of the NASA Exoplanet Research program via grant 14XRP14_20153.
Copyright 2016 California Institute of Technology. Government
sponsorship acknowledged.
NR 77
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
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IS 2
AR 144
DI 10.3847/0004-637X/827/2/144
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600056
ER
PT J
AU Hankins, MJ
Lau, RM
Morris, MR
Sanchez-Bermudez, J
Pott, JU
Adams, JD
Herter, TL
AF Hankins, M. J.
Lau, R. M.
Morris, M. R.
Sanchez-Bermudez, J.
Pott, J. U.
Adams, J. D.
Herter, T. L.
TI INFRARED OBSERVATIONS OF THE QUINTUPLET PROPER MEMBERS USING
SOFIA/FORCAST AND GEMINI/TReCS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; stars: evolution; stars: massive; stars: Wolf-Rayet
ID WOLF-RAYET STARS; GALACTIC-CENTER; MASSIVE STARS; MIDINFRARED CAMERA;
PINWHEEL NEBULA; DUST; CLUSTERS; INTERFEROMETRY; EXTINCTION; FORCAST
AB Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in nature. Originally dubbed the "cocoon stars" due to their cool featureless spectra, high-resolution near-infrared imaging observations have shown that at least two of the objects exhibit "pinwheel" nebulae consistent with binary systems with a carbon-rich Wolf-Rayet star and O/B companion. In this paper, we present 19.7, 25.2, 31.5, and 37.1 mu m observations of the QPMs (with an angular resolution of 3.2 ''-3.8 '') taken with the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST) in conjunction with high-resolution (similar to 0.1 ''-0.2 '') images at 8.8 and 11.7 mu m from the Thermal-Region Camera Spectrograph (TReCS). DUSTY models of the thermal dust emission of two of the four detected QPMs, Q2 and Q3, are fitted by radial density profiles that. are consistent with constant mass-loss rates (rho(d) alpha r(-2)). For the two remaining sources, Q1 and Q9, extended structures (similar to 1 '') are detected around these objects in high-resolution imaging data. Based on the fitted dust masses, Q9 has an unusually large dust reservoir (M-d = 1.3(-0.4)(+0.8) x 10(-3) M-circle dot) compared to typical dusty Wolf-Rayet stars, which suggests that it may have recently undergone an episode of enhanced mass loss.
C1 [Hankins, M. J.; Lau, R. M.; Adams, J. D.; Herter, T. L.] Cornell Univ, Dept Astron, 202 Space Sci Bldg, Ithaca, NY 14853 USA.
[Lau, R. M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Morris, M. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Sanchez-Bermudez, J.; Pott, J. U.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Sanchez-Bermudez, J.] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain.
[Adams, J. D.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Armstrong Flight Res Ctr, 2825 East Ave P, Palmdale, CA 93550 USA.
RP Hankins, MJ (reprint author), Cornell Univ, Dept Astron, 202 Space Sci Bldg, Ithaca, NY 14853 USA.
OI Morris, Mark/0000-0002-6753-2066
FU NASA [NAS2-97001, 8500-98-014]; DLR [50 OK 0901]; National Science
Foundation Graduate Research Fellowship [DGE-1144153]; Spanish Ministry
of Economy and Competitiveness (MINECO) [AYA2012-38491-CO2-02]; FEDER
funds; European Commission [312430]; OPTICON initiative
FX We would like to thank the rest of the FORCAST team, George Gull, Justin
Schoenwald, Chuck Henderson, and Jason Wang, the USRA Science and
Mission Ops teams, and the entire SOFIA staff. This work is based on
observations made with the NASA/DLR Stratospheric Observatory for
Infrared Astronomy (SOFIA). SOFIA science mission operations are
conducted jointly by the Universities Space Research Association, Inc.
(USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut
(DSI) under DLR contract 50 OK 0901. Financial support for FORCAST was
provided by NASA through award 8500-98-014 issued by USRA. This material
is based on work supported by the National Science Foundation Graduate
Research Fellowship under grant no. DGE-1144153. J.S.-B acknowledges
support by grants AYA2012-38491-CO2-02 of the Spanish Ministry of
Economy and Competitiveness (MINECO) cofounded with FEDER funds, and the
OPTICON initiative, which is supported by the European Commission's FP7
Capacities program (grant no. 312430).
NR 47
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
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AR 136
DI 10.3847/0004-637X/827/2/136
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600048
ER
PT J
AU Haqq-Misra, J
Kopparapu, RK
Batalha, NE
Harman, CE
Kasting, JF
AF Haqq-Misra, Jacob
Kopparapu, Ravi Kumar
Batalha, Natasha E.
Harman, Chester E.
Kasting, James F.
TI LIMIT CYCLES CAN REDUCE THE WIDTH OF THE HABITABLE ZONE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; extraterrestrial intelligence; planets and satellites:
atmospheres; planets and satellites: terrestrial planets
ID EARTH-LIKE PLANETS; MAIN-SEQUENCE STARS; CARBON-DIOXIDE CLOUDS;
MOLECULAR SPECTROSCOPIC DATABASE; EARLY MARTIAN CLIMATE; CO2 ICE CLOUDS;
ATMOSPHERIC CO2; PLATE-TECTONICS; SUPER-EARTHS; EXTRASOLAR PLANETS
AB The liquid water habitable zone (HZ) describes the orbital distance at which a terrestrial planet can maintain above-freezing conditions through regulation by the carbonate-silicate cycle. Recent calculations have suggested that planets in the outer regions of the HZ cannot maintain stable, warm climates, but rather should oscillate between long, globally glaciated states and shorter periods of climatic warmth. Such conditions, similar to "Snowball Earth" episodes experienced on Earth, would be inimical to the development of complex land life, including intelligent life. Here, we build on previous studies with an updated. energy balance climate model to calculate this "limit cycle" region of the HZ where such cycling would occur. We argue that an abiotic Earth would have a greater CO2 partial pressure than today because plants and other biota help to enhance the storage of CO2 in soil. When we tune our abiotic model accordingly, we find that limit cycles can occur but that previous calculations have overestimated their importance. For G stars like the Sun, limit cycles occur only for planets with CO2 outgassing rates less than that on modern Earth. For K-and M-star planets, limit cycles should not occur; however, M-star planets may be inhospitable to life for other reasons. Planets orbiting late G-type and early K-type stars retain the greatest potential for maintaining warm, stable conditions. Our results suggest that host star type, planetary volcanic activity, and seafloor weathering are all important factors in determining whether planets will be prone to limit cycling.
C1 [Haqq-Misra, Jacob; Kopparapu, Ravi Kumar] Blue Marble Space Inst Sci, 1001 4th Ave,Suite 3201, Seattle, WA 98154 USA.
[Haqq-Misra, Jacob; Kopparapu, Ravi Kumar; Batalha, Natasha E.; Harman, Chester E.; Kasting, James F.] NASA, Astrobiol Inst, Virtual Planetary Lab, POB 351580, Seattle, WA 98195 USA.
[Kopparapu, Ravi Kumar] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Stop 699-0,Bldg 34, Greenbelt, MD 20771 USA.
[Kopparapu, Ravi Kumar] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Batalha, Natasha E.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Batalha, Natasha E.; Harman, Chester E.; Kasting, James F.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Harman, Chester E.; Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Haqq-Misra, J (reprint author), Blue Marble Space Inst Sci, 1001 4th Ave,Suite 3201, Seattle, WA 98154 USA.; Haqq-Misra, J (reprint author), NASA, Astrobiol Inst, Virtual Planetary Lab, POB 351580, Seattle, WA 98195 USA.
OI Harman, Chester/0000-0003-2281-1990; Haqq-Misra,
Jacob/0000-0003-4346-2611
FU NASA Habitable Worlds program [NNX15AQ82G, NNX16AB61G]; NASA
Astrobiology Institute's Virtual Planetary Laboratory lead team; NASA
[NNH05ZDA001C]; National Science Foundation [DGE1255832]
FX The authors thank Darren Williams for assistance with model development,
as well as Dorian Abbot, Ray Pierrehumbert, Aomawa Shields, and Russell
Deitrick for helpful discussions. The authors also thank an anonymous
reviewer for thoughtful comments. that greatly improved the manuscript.
J.H.-M. acknowledges funding from the NASA Habitable Worlds program
under award NNX15AQ82G. R.K.K. and J.F.K. acknowledge funding from NASA
Astrobiology Institute's Virtual Planetary Laboratory lead team,
supported by NASA under cooperative agreement NNH05ZDA001C. R.K.K. and
J.H.-M. also acknowledge funding from the NASA Habitable Worlds program
under award NNX16AB61G. This material is based on work supported by the
National Science Foundation under Grant No. DGE1255832 to N.E.B. Any
opinions, findings, and conclusions or recommendations expressed in this
material are those of the authors and do not necessarily reflect the
views of NASA or the National Science Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
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SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600032
ER
PT J
AU Kerr, GS
Fletcher, L
Russell, AJB
Allred, JC
AF Kerr, Graham S.
Fletcher, Lyndsay.
Russell, Alexander J. B.
Allred, Joel C.
TI SIMULATIONS OF THE MG II K AND CA II 8542 LINES FROM AN ALFVEN
WAVE-HEATED FLARE CHROMOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; Sun: atmosphere; Sun: chromosphere; Sun: flares;
Sun: UV radiation; waves
ID WHITE-LIGHT FLARES; REGION-IMAGING-SPECTROGRAPH; SOLAR-FLARES; MODEL
CHROMOSPHERES; ATOMIC DATABASE; RAY-EMISSION; SPECTRA; IRIS;
REDISTRIBUTION; DISSIPATION
AB We use radiation hydrodynamic simulations to examine two models of solar flare chromospheric heating: Alfven wave dissipation and electron beam collisional losses. Both mechanisms are capable of strong chromospheric heating, and we show that the distinctive atmospheric evolution in the mid-to-upper chromosphere results in Mg II k-line emission that should be observably different between wave-heated and beam-heated simulations. We also present Ca II 8542 angstrom profiles that are formed slightly deeper in the chromosphere. The Mg. II k-line profiles from our wave-heated simulation are quite different from those from a beam-heated model and are more consistent with Interface Region Imaging Spectrograph observations. The predicted differences between the Ca II 8542 angstrom in the two models are small. We conclude that careful observational and theoretical study of lines formed in the mid-to-upper chromosphere holds genuine promise for distinguishing between competing models for chromospheric heating in flares.
C1 [Kerr, Graham S.; Fletcher, Lyndsay.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Russell, Alexander J. B.] Univ Dundee, Sch Sci & Engn, Dundee DD1 4HN, Scotland.
[Allred, Joel C.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Code 671,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Kerr, GS (reprint author), Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
EM g.kerr.2@research.gla.ac.uk; Lyndsay.Fletcher@glasgow.ac.uk;
arussell@maths.dundee.ac.uk; joel.c.allred@nasa.gov
FU College of Science and Engineering, University of Glasgow; STFC
consolidated grant [ST/L000741/1, ST/K000993/1]; European Community's
Seventh Framework Programme (F-CHROMA) [606862]; NASA Heliophysics
Supporting Research; NASA Living with a Star programs
FX The authors would like to thank Dr. J. Reep and Dr. A. Kowalski for
helpful discussions, and Dr. J. Leenaarts for help with the RH code. We
would like to thank Dr. M. Carlsson, who wrote RADYN, for help using the
RADYN code and for some analysis software that we made use of. G.S.K.
would like to acknowledge the financial support of a PhD scholarship
from the College of Science and Engineering, University of Glasgow. L.F.
acknowledges support from STFC consolidated grant ST/L000741/1. The
research leading these results has received funding from the European
Community's Seventh Framework Programme (FP7/2007-2013) under grant
agreement no. 606862 (F-CHROMA). A.J.B.R. acknowledges support from STFC
consolidated grant ST/K000993/1. A.J.B.R. and L.F. acknowledge support
from ISSI (Switzerland) for the International Team on 'Magnetic Waves in
Solar Flares: Beyond the "Standard" Flare Model'. J.C.A. acknowledges
funding support through the NASA Heliophysics Supporting Research and
NASA Living with a Star programs.
NR 53
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
PD AUG 20
PY 2016
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SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600013
ER
PT J
AU Loeffler, MJ
Moore, MH
Gerakines, PA
AF Loeffler, M. J.
Moore, M. H.
Gerakines, P. A.
TI THE EFFECTS OF EXPERIMENTAL CONDITIONS ON THE REFRACTIVE INDEX AND
DENSITY OF LOW-TEMPERATURE ICES: SOLID CARBON DIOXIDE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; planetary nebulae: general; methods: laboratory:
molecular; methods: laboratory: solid state; radiative transfer;
techniques: spectroscopic
ID INFRARED BAND STRENGTHS; OPTICAL-CONSTANTS; MOLECULAR CLOUDS; CO2;
SPECTRA; H2O; CH4; SPECTROSCOPY; GASES; FILMS
AB We present the first study on the effects of the. deposition technique on the measurements of the visible refractive index and the density of a low-temperature ice. using solid carbon dioxide (CO2) at 14-70 K as an example. While our measurements generally agree with previous studies that show a dependence of index and density on temperature below 50 K, we also find that the measured values depend on the method used to create each sample. Below 50 K, we find that the refractive index varied by as much as 4% and the density by as much as 16% at a single temperature depending on the deposition method. We also show that the Lorentz-Lorenz approximation is valid for solid CO2 across the full 14-70 K temperature range, regardless of the deposition method used. Since the refractive index and density are important in calculations of optical constants and infrared (IR) band strengths of materials, our results suggest that the deposition method must be considered in cases where n(vis) and rho are not measured in the same experimental setup where the IR spectral measurements are made.
C1 [Loeffler, M. J.; Moore, M. H.; Gerakines, P. A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
[Moore, M. H.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Code 691, Greenbelt, MD 20771 USA.
RP Loeffler, MJ (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
RI Loeffler, Mark/C-9477-2012; Gerakines, Perry/D-2226-2012
OI Gerakines, Perry/0000-0002-9667-5904
FU NASA Goddard's Technical Equipment fund; NASA's Astrophysics Research
and Analysis (APRA) program
FX The construction of the ultra-high vacuum chamber used in this study was
partially supported by NASA Goddard's Technical Equipment fund. This
work was supported by NASA's Astrophysics Research and Analysis (APRA)
program. The authors thank Reggie Hudson for assistance in day-to-day
operations in the laboratory and for his comments on this manuscript.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
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IS 2
AR 98
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SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600010
ER
PT J
AU Makela, P
Gopalswamy, N
Reiner, MJ
Akiyama, S
Krupar, V
AF Makela, P.
Gopalswamy, N.
Reiner, M. J.
Akiyama, S.
Krupar, V.
TI SOURCE REGIONS OF THE TYPE II RADIO BURST OBSERVED DURING A CME-CME
INTERACTION ON 2013 MAY 22
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: radio radiation
ID CORONAL MASS EJECTIONS; PARTICLE EVENTS; STEREO MISSION; MARCH 5; WAVE;
TRIANGULATION; SPACECRAFT; EMISSIONS; TRACKING; MODEL
AB We report on our study of radio source regions during the type II radio burst on 2013 May 22 based on direction-finding analysis of the Wind/WAVES and STEREO/WAVES (SWAVES) radio observations at decameter-hectometric wavelengths. The type II emission showed an enhancement that coincided with the interaction of two coronal mass ejections (CMEs) launched in sequence along closely spaced trajectories. The triangulation of the SWAVES source directions posited the ecliptic projections of the radio sources near the line connecting the Sun and the STEREO-A spacecraft. The WAVES and SWAVES source directions revealed shifts in the latitude of the radio source, indicating that the spatial location of the dominant source of the type II emission varies during the CME-CME interaction. The WAVES source directions close to 1 MHz frequencies matched the location of the leading edge of the primary CME seen in the images of the LASCO/C3 coronagraph. This correspondence of spatial locations at both wavelengths confirms that the CME-CME interaction region is the source of the type II enhancement. Comparison of radio and white-light observations also showed that at lower frequencies scattering significantly affects radio wave propagation.
C1 [Makela, P.; Reiner, M. J.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Makela, P.; Gopalswamy, N.; Reiner, M. J.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krupar, V.] Imperial Coll London, Blackett Lab, London SW7 2AZ, England.
[Krupar, V.] Inst Atmospher Phys CAS, Prague 14131, Czech Republic.
RP Makela, P (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.; Makela, P (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM pertti.makela@nasa.gov
RI Krupar, Vratislav/H-6237-2014;
OI Krupar, Vratislav/0000-0001-6185-3945; Makela,
Pertti/0000-0002-8182-4559
FU NSF [AGS-1358274]; Czech Academy of Sciences; Czech Science Foundation
[GAP209/12/2394]
FX We are grateful to J.C. Martinez Oliveros for providing his version of
the STEREO/WAVES direction-finding code. SOHO is an international
cooperation project between ESA and NASA. P.M. and S.A. were partially
supported by NSF grant AGS-1358274. V.K. thanks the support of the
Praemium Academiae award of the Czech Academy of Sciences and the Czech
Science Foundation grant GAP209/12/2394.
NR 37
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
IS 2
AR 141
DI 10.3847/0004-637X/827/2/141
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600053
ER
PT J
AU Pon, A
Kaufman, MJ
Johnstone, D
Caselli, P
Fontani, F
Butler, MJ
Jimenez-Serra, I
Palau, A
Tan, JC
AF Pon, A.
Kaufman, M. J.
Johnstone, D.
Caselli, P.
Fontani, F.
Butler, M. J.
Jimenez-Serra, I.
Palau, A.
Tan, J. C.
TI MID-J CO SHOCK TRACING OBSERVATIONS OF INFRARED DARK CLOUDS. III. SLED
FITTING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: molecules; shock waves; stars: formation; turbulence
ID YOUNG STELLAR OBJECTS; MASSIVE STARLESS CORES; MOLECULAR ION SPECTRA;
LOW-VELOCITY SHOCKS; MAGNETIC-FIELD; TURBULENT DISSIPATION; INTERSTELLAR
CLOUDS; MAGNETOHYDRODYNAMIC TURBULENCE; PHOTODISSOCIATION REGIONS;
MILKY-WAY
AB Giant molecular clouds contain supersonic turbulence that can locally heat small fractions of gas to over 100 K. We run shock models for low-velocity, C-type shocks propagating into gas with densities between 10(3) and 10(5) cm(-3) and find that CO lines are the most important cooling lines. Comparison to photodissociation region (PDR) models indicates that mid-J CO lines (J = 8 -> 7 and higher) should be dominated by emission from shocked gas. In Papers I and II we presented CO J = 3 -> 2, 8 -> 7, and 9 -> 8 observations toward. four primarily quiescent clumps within infrared dark clouds. Here. we fit PDR models to the combined spectral line energy distributions and show that the PDR models that best fit the low-J CO emission underpredict the mid-J CO emission by orders of magnitude, strongly hinting at a hot gas component within these clumps. The low-J CO data clearly show that the integrated intensities. of both the CO J = 8 -> 7 and 9 -> 8 lines are anomalously high, such that the line ratio can be used to characterize the hot gas component. Shock models are reasonably consistent with the observed mid-J CO emission, with models with densities near 10(4.5) cm(-3) providing the best agreement. Where this mid-J CO is detected, the mean volume filling factor of the hot gas is 0.1%. Much of the observed mid-J CO emission, however, is also associated with known protostars and may be due to protostellar feedback.
C1 [Pon, A.] Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada.
[Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 USA.
[Kaufman, M. J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
[Johnstone, D.] NRC Herzberg Inst Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, POB 3055 STN CSC, Victoria, BC V8W 3P6, Canada.
[Caselli, P.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Fontani, F.] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
[Butler, M. J.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Jimenez-Serra, I.] UCL, Dept Phys & Astron, 132 Hampstead Rd, London NW1 2PS, England.
[Palau, A.] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, POB 3-72, Morelia 58090, Michoacan, Mexico.
[Tan, J. C.] Univ Florida, Dept Phys & Astron, Gainesville, FL 32611 USA.
RP Pon, A (reprint author), Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada.
EM apon@uwo.ca
OI Fontani, Francesco/0000-0003-0348-3418; Palau, Aina/0000-0002-9569-9234
FU Canadian Institute for Theoretical Astrophysics (CITA) National
Fellowship; European Research Council (ERC) [320620]; Natural Sciences
and Engineering Research Council (NSERC) Discovery Grant; STFC through
an Ernest Rutherford Fellowship [ST/L004801/1]; UNAM-DGAPA-PAPIIT,
Mexico [IA102815]
FX We would like to thank our anonymous referee for many useful changes to
this paper. The authors would like to thank Dr. J. Bailey, Dr. N.
Bailey, Dr. J. D. Henshaw, and Dr. D. Stock for many insightful
conversations regarding the data presented in this paper. Partial salary
support for A. Pon was provided by a Canadian Institute for Theoretical
Astrophysics (CITA) National Fellowship. P.C. acknowledges 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 financial
support received from the STFC through an Ernest Rutherford Fellowship
(proposal number ST/L004801/1). A.P. acknowledges financial support from
UNAM-DGAPA-PAPIIT IA102815 grant, Mexico. This research has made use of
the Smithsonian Astrophysical Observatory (SAO)/National Aeronautics and
Space Administration's (NASA's) Astrophysics Data System (ADS). This
research has made use of the astro-ph archive.
NR 90
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
IS 2
AR 107
DI 10.3847/0004-637X/827/2/107
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600019
ER
PT J
AU Sahai, R
Scibelli, S
Morris, MR
AF Sahai, R.
Scibelli, S.
Morris, M. R.
TI HIGH-SPEED BULLET EJECTIONS DURING THE AGB-TO-PLANETARY NEBULA
TRANSITION: HST OBSERVATIONS OF THE CARBON STAR, V HYDRAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; circumstellar matter; stars: AGB and post; AGB; stars:
individual (V Hydrae); stars: jets; stars: mass-loss
ID PREPLANETARY NEBULA; CRL 618; ASTROPHYSICAL JETS; BIPOLAR OUTFLOW;
EPISODIC JET; MASS-LOSS; DISCOVERY; SIMULATIONS; ENVELOPE; BINARY
AB The well-studied carbon star, V Hya, showing evidence for high-speed, collimated outflows and dense equatorial structures, is a key object in the study of the poorly understood transition of AGB stars into aspherical planetary nebulae. Using the Space Telescope Imaging Spectrograph instrument on board the Hubble Space Telescope, we have obtained high spatial-resolution long-slit optical spectra of V Hya that show high-velocity emission in [S (II)]and [Fe (II)] lines. Our data set, spanning three epochs spaced apart by a year during each of two periods (in 2002-2004 and 2011-2013), shows that V Hya ejects high-speed (similar to 200-250 km s(-1)) bullets once every similar to 8.5 years. The ejection axis flip-flops around a roughly eastern direction, both in and perpendicular to the sky-plane, and the radial velocities of the ejecta also vary in concert between low and high values. We propose a model in which the bullet ejection is associated with the periastron passage of a binary companion in an eccentric orbit around V Hya with an orbital period of similar to 8.5 years. The flip-flop phenomenon is likely the result of collimated ejection from an accretion disk (produced by gravitational capture of material from the primary) that is warped and precessing, and/or that has a magnetic field that is misaligned with that of the companion or the primary star. We show how a previously observed 17 year period in V Hya's light-cycle can also be explained in our model. Additionally, we describe how the model proposed here can be extended to account for multipolar nebulae.
C1 [Sahai, R.; Scibelli, S.] CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
[Scibelli, S.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Morris, M. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
EM raghvendra.sahai@jpl.nasa.gov
OI Morris, Mark/0000-0002-6753-2066
FU NASA; STScI HST award [GO 12227.01]
FX R.S.'s contribution to the research described here was carried out at
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with NASA, with financial support was provided by NASA,
in part from an STScI HST award (GO 12227.01). S.S.'s contribution was
carried out during her tenure as a NASA Undergraduate Intern (UI) at
JPL.
NR 34
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
IS 2
AR 92
DI 10.3847/0004-637X/827/2/92
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600004
ER
PT J
AU Sleator, CC
Tomsick, JA
King, AL
Miller, JM
Boggs, SE
Bachetti, M
Barret, D
Chenevez, J
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Rahoui, F
Stern, DK
Walton, DJ
Zhang, WW
AF Sleator, Clio C.
Tomsick, John A.
King, Ashley L.
Miller, Jon M.
Boggs, Steven E.
Bachetti, Matteo
Barret, Didier
Chenevez, Jerome
Christensen, Finn E.
Craig, William W.
Hailey, Charles J.
Harrison, Fiona A.
Rahoui, Farid
Stern, Daniel K.
Walton, Dominic J.
Zhang, William W.
TI A NuSTAR OBSERVATION OF THE REFLECTION SPECTRUM OF THE LOW-MASS X-RAY
BINARY 4U 1728-34
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: neutron; X-rays: binaries
ID INNER ACCRETION DISKS; NEUTRON-STAR; BLACK-HOLES; AQUILA X-1;
XMM-NEWTON; PULSARS; LINES; SPECTROSCOPY; CONSTRAINTS; TELESCOPE
AB We report on a simultaneous NuSTAR and Swift observation of the neutron star low-mass X-ray binary 4U 1728-34. We identified and removed four Type I X-ray bursts during the observation in order to study the persistent emission. The continuum spectrum is hard and described well by a blackbody with kT = 1.5 keV and a cutoff power law with Gamma = 1.5, and a cutoff temperature of 25 keV. Residuals between 6 and 8 keV provide strong evidence of a broad Fe K alpha line. By modeling the spectrum with a relativistically blurred reflection model, we find an upper limit for the inner disk radius of R-in <= 2R(ISCO). Consequently, we find that R-NS <= 23 km, assuming M =1.4 M-circle dot and alpha = 0.15. We also find an upper limit on the magnetic field of B <= 2 x 10(8) G.
C1 [Sleator, Clio C.; Tomsick, John A.; Boggs, Steven E.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[King, Ashley L.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA.
[Miller, Jon M.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
[Bachetti, Matteo; Barret, Didier] Univ Toulouse, UPS OMP, Toulouse, France.
[Bachetti, Matteo; Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Chenevez, Jerome; Christensen, Finn E.] Tech Univ Denmark, DTU Space, Elektrovej 327-328, Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Craig, William W.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA.
[Craig, William W.; Hailey, Charles J.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA.
[Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Rahoui, Farid] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Rahoui, Farid] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA.
[Stern, Daniel K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sleator, CC (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
OI Bachetti, Matteo/0000-0002-4576-9337
FU ESA/PRODEX; NASA
FX We thank Michael Parker and Andy Fabian for the particular version of
the reflionx model used in this analysis. We thank Kristin Madsen for
her help identifying the calibration issue in the NuSTAR data between
3-4.5 keV. J.C. thanks ESA/PRODEX for financial support. This work is
based on data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by NASA.
NR 45
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
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AR 134
DI 10.3847/0004-637X/827/2/134
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600046
ER
PT J
AU Troja, E
Sakamoto, T
Cenko, SB
Lien, A
Gehrels, N
Castro-Tirado, AJ
Ricci, R
Capone, J
Toy, V
Kutyrev, A
Kawai, N
Cucchiara, A
Fruchter, A
Gorosabel, J
Jeong, S
Levan, A
Perley, D
Sanchez-Ramirez, R
Tanvir, N
Veilleux, S
AF Troja, E.
Sakamoto, T.
Cenko, S. B.
Lien, A.
Gehrels, N.
Castro-Tirado, A. J.
Ricci, R.
Capone, J.
Toy, V.
Kutyrev, A.
Kawai, N.
Cucchiara, A.
Fruchter, A.
Gorosabel, J.
Jeong, S.
Levan, A.
Perley, D.
Sanchez-Ramirez, R.
Tanvir, N.
Veilleux, S.
TI AN ACHROMATIC BREAK IN THE AFTERGLOW OF THE SHORT GRB 140903A: EVIDENCE
FOR A NARROW JET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 140903A); X-rays: bursts
ID GAMMA-RAY BURSTS; NEUTRON-STAR MERGERS; COMPACT OBJECT MERGERS; MASS
BLACK-HOLES; LIGHT CURVES; ENERGY INJECTION; MILLISECOND MAGNETAR;
OPTICAL AFTERGLOWS; ALERT TELESCOPE; CENTRAL ENGINE
AB We report the results of our observing campaign on GRB. 140903A, a nearby (z = 0.351) short-duration (T-90 similar to 0.3 s) gamma-ray burst discovered by Swift. We monitored the X-ray afterglow with Chandra up to 15 days after the burst. and detected a steeper decay of the X-ray flux after t(j) approximate to 1 day. Continued monitoring at optical and radio wavelengths showed a similar decay in flux at nearly the same time, and we interpret it as evidence of a narrowly collimated jet. By using the standard fireball model to describe the afterglow evolution, we derive a jet opening angle theta(j) approximate to 5 degrees and a collimation-corrected total energy release E approximate to 2 x 10(50) erg. We further discuss the nature of the GRB progenitor system. Three main lines disfavor a massive star progenitor: the properties of the prompt gamma-ray emission, the age and low star formation rate of the host galaxy, and the lack of a bright supernova. We conclude that this event. likely originated from a compact binary merger.
C1 [Troja, E.; Capone, J.; Toy, V.; Kutyrev, A.; Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Troja, E.; Cenko, S. B.; Lien, A.; Gehrels, N.; Kutyrev, A.; Cucchiara, A.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Aoyama Gakuin Univ, Dept Math & Phys, Coll Sci & Engn, Chuo Ku, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2525258, Japan.
[Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Lien, A.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Castro-Tirado, A. J.; Jeong, S.; Sanchez-Ramirez, R.] Inst Astrofis Andalucia IAA CSIC, POB 03004, E-18008 Granada, Spain.
[Castro-Tirado, A. J.] Univ Malaga, Unidad Asociada Dept Ingn & Sistemas Automat, ETS Ingn Ind, Campus Teatinos,Arquitecto Francisco Penalosa,6, E-29010 Malaga, Spain.
[Ricci, R.] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
[Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 H-29 Ookayama, Tokyo 1528551, Japan.
[Cucchiara, A.; Fruchter, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Gorosabel, J.] Univ Pas Vasco UPV EHU, Unidad Asociada Grp Ciencias Planetarias UPV EHU, IAA CSIC, Dept Fis Aplicada 1,ETS Ingn, Alameda Urquijo S-N, E-48013 Bilbao, Spain.
[Gorosabel, J.] Basque Fdn Sci, Ikerbasque, Alameda Urquijo 36-5, E-48008 Bilbao, Spain.
[Gorosabel, J.] Univ Basque Country, Bilbao, Spain.
[Jeong, S.] Sunkgkyunkwan Univ, 25-2 Sungkyunkwan Ro, Seoul 1398, South Korea.
[Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Perley, D.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Tanvir, N.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Troja, E (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Troja, E (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
OI Sanchez-Ramirez, Ruben/0000-0002-7158-5099
FU National Aeronautics and Space Administration through Chandra Awards
[GO4-15072A, GO4-15067A]; National Aeronautics Space Administration
[NAS8-03060]; Discovery Communications; National Science Foundation
[AST-1005313]; Spanish Ministry Projects [AYA2012-39727-C03-01,
2015-71718R]
FX The scientific results reported in this article are based in part on
observations made by the Chandra X-ray Observatory. Support for this
work was provided by the National Aeronautics and Space Administration
through Chandra Awards GO4-15072A and GO4-15067A issued by the Chandra
X-ray. Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060. These results also made use of
Lowell Observatory's Discovery Channel Telescope. 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 the Lowell Observatory using funds from the National Science
Foundation (AST-1005313). This paper is partly based on observations
obtained at the Gemini Observatory, which is operated by the Association
of Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the National Research Council
(Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e
Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia
e Inovacao (Brazil). Observations were also carried out with the 10.4 m
Gran Telescopio Canarias installed in the Spanish Observatorio del Roque
de los Muchachos of the Instituto de Astrofisica de Canarias in the
island of La Palma (GTC59-14B) and with the 3.5 m CAHA telescope at the
German-Spanish Calar Alto Observatory operated by the IAA-CSIC. A.J.C.T.
acknowledges support from the Spanish Ministry Projects
AYA2012-39727-C03-01 and 2015-71718R.
NR 97
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2016
VL 827
IS 2
AR 102
DI 10.3847/0004-637X/827/2/102
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9SA
UT WOS:000384001600014
ER
PT J
AU Hayes, LA
Gallagher, PT
Dennis, BR
Ireland, J
Inglis, AR
Ryan, DF
AF Hayes, L. A.
Gallagher, P. T.
Dennis, B. R.
Ireland, J.
Inglis, A. R.
Ryan, D. F.
TI QUASI-PERIODIC PULSATIONS DURING THE IMPULSIVE AND DECAY PHASES OF AN
X-CLASS FLARE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: flares; Sun: oscillations; Sun: X-rays, gamma rays
ID RAY BURST MONITOR; SOLAR-FLARE; SAUSAGE OSCILLATIONS; LOOPS;
ACCELERATION; MICROWAVE; RECONNECTION; PARAMETERS; EMISSION; RADIO
AB Quasi-periodic pulsations (QPPs) are often observed in X-ray emission from solar flares. To date, it is unclear what their physical origins are. Here, we present a multi-instrument investigation of the nature of QPP during the impulsive and decay phases of the X1.0 flare of 2013 October 28. We focus on the character of the fine structure pulsations evident in the soft X-ray (SXR) time derivatives and compare this variability with structure across multiple wavelengths including hard X-ray and microwave emission. We find that during the impulsive phase of the flare, high correlations between pulsations in the thermal and non-thermal emissions are seen. A characteristic timescale of similar to 20 s is observed in all channels and a second timescale of similar to 55 s is observed in the non-thermal emissions. SXR pulsations are seen to persist into the decay phase of this flare, up to 20 minutes after the non-thermal emission has ceased. We find that these decay phase thermal pulsations have very small amplitude and show an increase in characteristic timescale from similar to 40 s up to similar to 70 s. We interpret the bursty nature of the coexisting multi-wavelength QPPs during the impulsive phase in terms of episodic particle acceleration and plasma heating. The persistent thermal decay phase QPPs are most likely connected with compressive magnetohydrodynamic processes in the post-flare loops such as the fast sausage mode or the vertical kink mode.
C1 [Hayes, L. A.; Gallagher, P. T.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.
[Hayes, L. A.; Dennis, B. R.; Ireland, J.; Inglis, A. R.; Ryan, D. F.] NASA, Heliophys Sci Div, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hayes, L. A.; Ireland, J.] ADNET Syst Inc, Bethesda, MD USA.
[Inglis, A. R.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ryan, D. F.] Royal Observ Belgium, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium.
RP Hayes, LA (reprint author), Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.; Hayes, LA (reprint author), NASA, Heliophys Sci Div, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Hayes, LA (reprint author), ADNET Syst Inc, Bethesda, MD USA.
OI Dennis, Brian/0000-0001-8585-2349; Gallagher, Peter/0000-0001-9745-0400
FU Irish Research Council (IRC); Solar-Terrestrial Centre of Excellence;
SIDC Data Exploitation; NASA
FX This work has been supported by Enterprise Partnership Scheme
studentship from the Irish Research Council (IRC) between Trinity
College Dublin and Adnet System Inc. D. Ryan thanks the
Solar-Terrestrial Centre of Excellence and the SIDC Data Exploitation
and the NASA Postdoctoral Program administered by the Universities Space
Research Association for their financial support. The support of the
PROBA2 Guest Investigator Program provided opportunity to collaborate
with the PROBA2 team at the Royal Observatory Belgium. This research has
made use of SunPy, an open-source and free community-developed solar
data analysis package written in Python (SunPy Community et al. 2015).
We also acknowledge the anonymous referee whose comments helped to
improve the Letter.
NR 43
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2016
VL 827
IS 2
AR L30
DI 10.3847/2041-8205/827/2/L30
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW5UI
UT WOS:000383712100009
ER
PT J
AU Marshall, FE
Guillemot, L
Harding, AK
Martin, P
Smith, DA
AF Marshall, F. E.
Guillemot, L.
Harding, A. K.
Martin, P.
Smith, D. A.
TI A NEW, LOW BRAKING INDEX FOR THE LMC PULSAR B0540-69
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: individual (PSR B0540-69)
ID LARGE-MAGELLANIC-CLOUD; 50 MILLISECOND PULSAR; MAGNETIC-FIELD; PSR
B0540-69; SPIN-DOWN; ACTIVE PULSAR; DISCOVERY; TELESCOPE; BEHAVIOR
AB We report the results of a 16 month monitoring campaign using the Swift satellite of PSR B0540-69, a young pulsar in the Large Magellanic Cloud. Phase connection was maintained throughout the campaign so that a reliable ephemeris could be determined, and the length of the campaign is adequate to accurately determine the spin frequency. and its first and second derivatives. The braking index n is 0.031. +/-. 0.013 (90% confidence), a value much lower than previously reported for B0540-69 and almost all other young pulsars. We use data from the extensive monitoring campaign with Rossi X-ray Timing Explorer to show that timing noise is unlikely to significantly affect the measurement. This is the first measurement of the braking index in the pulsar's recently discovered high spin-down state. We discuss possible mechanisms for producing the low braking index.
C1 [Marshall, F. E.; Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guillemot, L.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans, France.
[Guillemot, L.] CNRS, Observ Paris, Stn Radioastron Nancay, INSU, F-18330 Nancay, France.
[Martin, P.] UPS, CNRS, UMR5277, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Smith, D. A.] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, BP120, F-33175 Gradignan, France.
RP Marshall, FE (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM frank.marshall@nasa.gov
OI Smith, David/0000-0002-7833-0275
NR 30
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2016
VL 827
IS 2
AR L39
DI 10.3847/2041-8205/827/2/L39
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW5UI
UT WOS:000383712100018
ER
PT J
AU Veres, P
Preece, RD
Goldstein, A
Meszaros, P
Burns, E
Connaughton, V
AF Veres, P.
Preece, R. D.
Goldstein, A.
Meszaros, P.
Burns, E.
Connaughton, V.
TI GRAVITATIONAL-WAVE OBSERVATIONS MAY CONSTRAIN GAMMA-RAY BURST MODELS:
THE CASE OF GW150914-GBM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; gravitational waves
ID BLACK-HOLE MERGERS; EVENT GW150914; EMISSION; PHOTOSPHERE; SYNCHROTRON;
AFTERGLOW; SHOCKS; SWIFT; GRBS; LONG
AB The possible short gamma-ray burst (GRB) observed by Fermi/GBM in coincidence with the first gravitational-wave (GW) detection offers new ways to test GRB prompt emission models. GW observations provide previously inaccessible physical parameters for the black hole central engine such as its horizon radius and rotation parameter. Using a minimum jet launching radius from the Advanced LIGO measurement of GW. 150914, we calculate photospheric and internal shock models and find that they are marginally inconsistent with the GBM data, but cannot be definitely ruled out. Dissipative photosphere models, however, have no problem explaining the observations. Based on the peak energy and the observed flux, we find that the external shock model gives a natural explanation, suggesting a low interstellar density (similar to 10(-3) cm(-3)) and a high Lorentz factor (similar to 2000). We only speculate on the exact nature of the system producing the gamma-rays, and study the parameter space of a generic Blandford-Znajek model. If future joint observations confirm the GW-short-GRB association we can provide similar but more detailed tests for prompt emission models.
C1 [Veres, P.] Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Preece, R. D.] Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Goldstein, A.; Connaughton, V.] Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA.
[Goldstein, A.] NASA, Astrophys Off, ZP12, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Burns, E.] Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35805 USA.
RP Veres, P (reprint author), Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM peter.veres@uah.edu
OI Preece, Robert/0000-0003-1626-7335; Veres, Peter/0000-0002-2149-9846
FU Fermi grant [NNM11AA01A]; NASA [NNX13AH50G]
FX We thank Tyson Littenberg and Michael Briggs for discussions. This study
was supported by Fermi grant NNM11AA01A. P.M. acknowledges support from
NASA NNX13AH50G.
NR 54
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 AUG 20
PY 2016
VL 827
IS 2
AR L34
DI 10.3847/2041-8205/827/2/L34
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW5UI
UT WOS:000383712100013
ER
PT J
AU Behrangi, A
Fetzer, EJ
Granger, SL
AF Behrangi, Ali
Fetzer, Eric J.
Granger, Stephanie L.
TI Early detection of drought onset using near surface temperature and
humidity observed from space
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID METEOROLOGICAL DROUGHT; SEASONAL PREDICTION; PRECIPITATION; INFORMATION;
WEATHER; CLIMATE; TRENDS
AB Drought is associated with severe societal impacts ranging from shortages of water for human consumption to agricultural failure and famine. An important aspect of drought forecast is determining the onset, which is critical for early warning efforts and water resources and agriculture planning. Indices of precipitation shortage have been widely used to detect the onset of drought because precipitation deficits often lead to shortages in other hydrologic variables such as soil moisture and runoff. The present work demonstrates that atmospheric temperature and humidity observations from the Atmospheric Infrared Sounder (AIRS) contain information that can be used to detect drought onset earlier than that obtained from precipitation deficit. By calculating the standardized indices for precipitation, near-surface temperature, vapour pressure deficit, and relative humidity, we show that in many regions of the world signals of drought onset can be detected from near-surface temperature and humidity data a few months earlier than those obtained from precipitation deficit. In particular, vapour pressure deficit showed higher effectiveness than relative humidity or temperature only. The outcome was generally consistent for the three- and six-month accumulations studied here. Further analysis using 65years (1960-2014) of monthly temperature and humidity data derived from the Parameter-elevation Regressions on Independent Slopes Model (PRISM) data set over the continental United States suggests that there is a good agreement between drought early detection signals obtained from AIRS and that from ground stations during the overlapped (2003-2014) period. Analysis using longer record suggests that the frequency of successful early detection of drought onset using temperature and humidity data shows regional shift towards eastern United States in the recent years.
C1 [Behrangi, Ali; Fetzer, Eric J.; Granger, Stephanie L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Ali.Behrangi@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology; National Aeronautics and Space Administration.
NR 31
TC 0
Z9 0
U1 10
U2 12
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD AUG 20
PY 2016
VL 37
IS 16
BP 3911
EP 3923
DI 10.1080/01431161.2016.1204478
PG 13
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA DS8QT
UT WOS:000381048600018
ER
PT J
AU Kataoka, R
Ngwira, C
AF Kataoka, Ryuho
Ngwira, Chigomezyo
TI Extreme geomagnetically induced currents
SO PROGRESS IN EARTH AND PLANETARY SCIENCE
LA English
DT Review
DE Geomagnetically induced currents; Magnetic storms; Auroral substorms;
Sudden commencements; Solar energetic particles
ID 1-2 SEPTEMBER 1859; CORONAL MASS EJECTION; SOLAR-WIND; MAGNETIC STORM;
SUDDEN COMMENCEMENTS; STATISTICAL-ANALYSIS; EVENT; PRESSURE; SYSTEMS;
LIMITS
AB We propose an emergency alert framework for geomagnetically induced currents (GICs), based on the empirically extreme values and theoretical upper limits of the solar wind parameters and of dB/dt, the time derivative of magnetic field variations at ground. We expect this framework to be useful for preparing against extreme events. Our analysis is based on a review of various papers, including those presented during Extreme Space Weather Workshops held in Japan in 2011, 2012, 2013, and 2014. Large-amplitude dB/dt values are the major cause of hazards associated with three different types of GICs: (1) slow dB/dt with ring current evolution (RC-type), (2) fast dB/dt associated with auroral electrojet activity (AE-type), and (3) transient dB/dt of sudden commencements (SC-type). We set "caution," " warning," and "emergency" alert levels during the main phase of superstorms with the peak Dst index of less than -300 nT (once per 10 years), -600 nT (once per 60 years), or -900 nT (once per 100 years), respectively. The extreme dB/dt values of the AE-type GICs are 2000, 4000, and 6000 nT/min at caution, warning, and emergency levels, respectively. For the SC-type GICs, a "transient alert" is also proposed for dB/dt values of 40 nT/s at low latitudes and 110 nT/s at high latitudes, especially when the solar energetic particle flux is unusually high.
C1 [Kataoka, Ryuho] Natl Inst Polar Res, Tokyo, Japan.
[Kataoka, Ryuho] SOKENDAI, Dept Polar Sci, Tokyo, Japan.
[Ngwira, Chigomezyo] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD USA.
RP Kataoka, R (reprint author), Natl Inst Polar Res, Tokyo, Japan.; Kataoka, R (reprint author), SOKENDAI, Dept Polar Sci, Tokyo, Japan.
EM kataoka.ryuho@nipr.ac.jp
OI Kataoka, Ryuho/0000-0001-9400-1765
NR 57
TC 1
Z9 1
U1 2
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 AUG 19
PY 2016
VL 3
AR UNSP 23
DI 10.1186/s40645-016-0101-x
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DU0XD
UT WOS:000381927300001
ER
PT J
AU Chu, T
Fong, H
Kumar, P
Pfeiffer, HP
Boyle, M
Hemberger, DA
Kidder, LE
Scheel, MA
Szilagyi, B
AF Chu, Tony
Fong, Heather
Kumar, Prayush
Pfeiffer, Harald P.
Boyle, Michael
Hemberger, Daniel A.
Kidder, Lawrence E.
Scheel, Mark A.
Szilagyi, Bela
TI On the accuracy and precision of numerical waveforms: effect of waveform
extraction methodology
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE numerical relativity; binary black holes; gravitational-wave astronomy;
gravitational wave extraction; LIGO; general relativity; advanced LIGO
ID GRAVITATIONAL-RADIATION; GENERAL RELATIVITY; EINSTEIN EQUATIONS
AB We present a new set of 95 numerical relativity simulations of non-precessing binary black holes (BBHs). The simulations sample comprehensively both black-hole spins up to spin magnitude of 0.9, and cover mass ratios 1-3. The simulations cover on average 24 inspiral orbits, plus merger and ringdown, with low initial orbital eccentricities e < 10(-4). A subset of the simulations extends the coverage of non-spinning BBHs up to mass ratio q = 10. Gravitational waveforms at asymptotic infinity are computed with two independent techniques: extrapolation and Cauchy characteristic extraction. An error analysis based on noise-weighted inner products is performed. We find that numerical truncation error, error due to gravitational wave extraction, and errors due to the Fourier transformation of signals with finite length of the numerical waveforms are of similar magnitude, with gravitational wave extraction errors dominating at noise-weighted mismatches of similar to 3 x 10(-4). This set of waveforms will serve to validate and improve aligned-spin waveform models for gravitational wave science.
C1 [Chu, Tony] Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Chu, Tony; Fong, Heather; Kumar, Prayush; Pfeiffer, Harald P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Fong, Heather] Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada.
[Pfeiffer, Harald P.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Potsdam, Germany.
[Pfeiffer, Harald P.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada.
[Boyle, Michael; Kidder, Lawrence E.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Hemberger, Daniel A.; Scheel, Mark A.; Szilagyi, Bela] CALTECH, Theoret Astrophys 350 17, Pasadena, CA 91125 USA.
[Szilagyi, Bela] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Fong, H (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.; Fong, H (reprint author), Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada.
EM hfong@physics.utoronto.ca
FU NSERC of Canada; Ontario Early Researcher Awards Program; Canada
Research Chairs Program; Canadian Institute for Advanced Research;
Sherman Fairchild Foundation; NSF [PHY-1404569, AST-1333520,
PHY-1306125, AST-1333129, PHY-1305682, PHY-0960291]; Simons Foundation;
Canada Foundation for Innovation (CFI) under Compute Canada; Government
of Ontario; Ontario Research Fund (ORF)-Research Excellence; University
of Toronto; Canada Foundation for Innovation (CFI); Ministere de
l'Economie, de l'Innovation et des Exportations du Quebec (MEIE); RMGA;
Fonds de recherche du Quebec-Nature et Technologies (FRQ-NT); NSF XSEDE
network [TG-PHY990007N]; NSF PRAC Award [ACI-1440083]
FX We gratefully acknowledge support for this research at CITA from NSERC
of Canada, the Ontario Early Researcher Awards Program, the Canada
Research Chairs Program, and the Canadian Institute for Advanced
Research; at Caltech from the Sherman Fairchild Foundation and NSF
grants PHY-1404569 and AST-1333520; at Cornell from the Sherman
Fairchild Foundation and NSF grants PHY-1306125 and AST-1333129; and at
Princeton from NSF grant PHY-1305682 and the Simons Foundation.
Calculations were performed at the GPC supercomputer at the SciNet HPC
Consortium [88]; SciNet is funded by: the Canada Foundation for
Innovation (CFI) under the auspices of Compute Canada; the Government of
Ontario; Ontario Research Fund (ORF)-Research Excellence; and the
University of Toronto. Further calculations were performed on the
Briaree cluster at Sherbrooke University, managed by Calcul Quebec and
Compute Canada and with operation funded by the Canada Foundation for
Innovation (CFI), Ministere de l'Economie, de l'Innovation et des
Exportations du Quebec (MEIE), RMGA and the Fonds de recherche du
Quebec-Nature et Technologies (FRQ-NT); on the Zwicky cluster at
Caltech, which is supported by the Sherman Fairchild Foundation and by
NSF award PHY-0960291; on the NSF XSEDE network under grant
TG-PHY990007N; on the NSF/NCSA Blue Waters at the University of Illinois
with allocation jr6 under NSF PRAC Award ACI-1440083. HP and PK thank
the Albert-Einstein Institute, Potsdam, for hospitality during part of
the time where this research was completed.
NR 76
TC 6
Z9 6
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD AUG 18
PY 2016
VL 33
IS 16
AR 165001
DI 10.1088/0264-9381/33/16/165001
PG 21
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA DU5OX
UT WOS:000382262300003
ER
PT J
AU Zanchettin, D
Khodri, M
Timmreck, C
Toohey, M
Schmidt, A
Gerber, EP
Hegerl, G
Robock, A
Pausata, FSR
Ball, WT
Bauer, SE
Bekki, S
Dhomse, SS
LeGrande, AN
Mann, GW
Marshall, L
Mills, M
Marchand, M
Niemeier, U
Poulain, V
Rozanov, E
Rubino, A
Stenke, A
Tsigaridis, K
Tummon, F
AF Zanchettin, Davide
Khodri, Myriam
Timmreck, Claudia
Toohey, Matthew
Schmidt, Anja
Gerber, Edwin P.
Hegerl, Gabriele
Robock, Alan
Pausata, Francesco S. R.
Ball, William T.
Bauer, Susanne E.
Bekki, Slimane
Dhomse, Sandip S.
LeGrande, Allegra N.
Mann, Graham W.
Marshall, Lauren
Mills, Michael
Marchand, Marion
Niemeier, Ulrike
Poulain, Virginie
Rozanov, Eugene
Rubino, Angelo
Stenke, Andrea
Tsigaridis, Kostas
Tummon, Fiona
TI The Model Intercomparison Project on the climatic response to Volcanic
forcing (VolMIP): experimental design and forcing input data for CMIP6
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID MT. PINATUBO ERUPTION; NORTH-ATLANTIC OCEAN; ATMOSPHERIC CIRCULATION;
AEROSOL-CHEMISTRY; LAST MILLENNIUM; LAKI ERUPTION; TREE-RINGS; IMPACT;
TEMPERATURES; SENSITIVITY
AB The enhancement of the stratospheric aerosol layer by volcanic eruptions induces a complex set of responses causing global and regional climate effects on a broad range of timescales. Uncertainties exist regarding the climatic response to strong volcanic forcing identified in coupled climate simulations that contributed to the fifth phase of the Coupled Model Intercomparison Project (CMIP5). In order to better understand the sources of these model diversities, the Model Intercomparison Project on the climatic response to Volcanic forcing (VolMIP) has defined a coordinated set of idealized volcanic perturbation experiments to be carried out in alignment with the CMIP6 protocol. VolMIP provides a common stratospheric aerosol data set for each experiment to minimize differences in the applied volcanic forcing. It defines a set of initial conditions to assess how internal climate variability contributes to determining the response. VolMIP will assess to what extent volcanically forced responses of the coupled ocean-atmosphere system are robustly simulated by state-of-the-art coupled climate models and identify the causes that limit robust simulated behavior, especially differences in the treatment of physical processes. This paper illustrates the design of the idealized volcanic perturbation experiments in the VolMIP protocol and describes the common aerosol forcing input data sets to be used.
C1 [Zanchettin, Davide; Rubino, Angelo] Univ Venice, Dept Environm Sci Informat & Stat, Venice, Italy.
[Khodri, Myriam; Poulain, Virginie] IRD IPSL Lab Oceanog & Climat, Paris, France.
[Timmreck, Claudia; Toohey, Matthew; Niemeier, Ulrike] Max Planck Inst Meteorol, Hamburg, Germany.
[Toohey, Matthew] GEOMAR Helmholtz Ctr Ocean Res Kiel, Kiel, Germany.
[Schmidt, Anja; Dhomse, Sandip S.; Mann, Graham W.; Marshall, Lauren] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Gerber, Edwin P.] NYU, Courant Inst Math Sci, New York, NY USA.
[Hegerl, Gabriele] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
[Robock, Alan] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ USA.
[Pausata, Francesco S. R.] Stockholm Univ, Dept Meteorol, Stockholm, Sweden.
[Pausata, Francesco S. R.] Bolin Ctr Climate Res, Stockholm, Sweden.
[Ball, William T.; Rozanov, Eugene] PMOD WRC, Davos, Switzerland.
[Ball, William T.; Stenke, Andrea; Tummon, Fiona] ETH, Dept Environm Syst Sci, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[Bauer, Susanne E.; LeGrande, Allegra N.; Tsigaridis, Kostas] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY USA.
[Bauer, Susanne E.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Bekki, Slimane; Marchand, Marion] UPMC, LATMOS IPSL, UVSQ Univ Paris Saclay, CNRS, Guyancourt, France.
[Mann, Graham W.] Univ Leeds, Natl Ctr Atmospher Sci, Leeds, W Yorkshire, England.
[Mills, Michael] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
RP Zanchettin, D (reprint author), Univ Venice, Dept Environm Sci Informat & Stat, Venice, Italy.
EM davide.zanchettin@unive.it
RI Toohey, Matthew/G-3129-2010; Schmidt, Anja/C-9617-2012; Rozanov,
Eugene/A-9857-2012; Dhomse, Sandip/C-8198-2011;
OI Toohey, Matthew/0000-0002-7070-405X; Rozanov,
Eugene/0000-0003-0479-4488; Dhomse, Sandip/0000-0003-3854-5383; Schmidt,
Anja/0000-0001-8759-2843
FU World Climate Research Programme (WCRP); LABEX L-IPSL; French Agence
Nationale de la Recherche under the "Programme d'Investissements
d'Avenir" [ANR-10-LABX-18-01]; Agence Nationale de la Recherche
MORDICUS, under the "Programme Environnement et Societe"
[ANR-13-SENV-0002-02]; German Federal Ministry of Education (BMBF),
research program "MiKlip" [FKZ: 01LP1517B/01LP1130A]; European Project
[603557, FP7-ENV. 2013.6.1-2]; BMBF, research program "MiKlip" [FKZ:
01LP1130B]; US National Science Foundation (NSF) [AGS-1430051]; NSF
[AGS-1264195]; Academic Research Fellowship from the University of
Leeds; NERC [NE/N006038/1]; Swiss National Science Foundation [149182,
163206, CRSII2_147659]; ERC project TITAN [EC-320691]; NCAS; Wolfson
Foundation; Royal Society as a Royal Society Wolfson Research Merit
Award [WM130060]
FX VolMIP is dedicated to the memory of Thomas Crowley (1948-2014), whose
pioneering work on volcanic forcing on climate has inspired many
researchers and strongly contributed to the foundation upon which VolMIP
was built. We thank the broad scientific community for the stimulating
discussions that motivated VolMIP and for their contribution to the
definition of the experiments and the comments on this draft. We thank
the climate modeling groups who have committed to perform the VolMIP
experiments. We are grateful to the CMIP6 Panel who guided our work
throughout the endorsement process, in particular concerning their
recommendation to upgrade the volc-pinatubo-strat/surf experiments,
which led to a stronger Tier 1 experimental palette. We thank Christoph
Raible and an anonymous reviewer for their helpful comments on the
manuscript and on the VolMIP protocol. The volc-cluster-21C experiment
was added to the VolMIP protocol following a suggestion by Ingo Bethke.
We thank Martin Juckes for his assistance in preparing the CMIP6 data
request and Karl Taylor for his assistance throughout the endorsement
process. We thank Andrew Schurer for discussion about solar forcing. We
acknowledge the support provided by the World Climate Research Programme
(WCRP), which is responsible for the CMIP5. M. Khodri acknowledges grant
support from the LABEX L-IPSL, funded by the French Agence Nationale de
la Recherche under the "Programme d'Investissements d'Avenir"(grant no.
ANR-10-LABX-18-01), a grant from the Agence Nationale de la Recherche
MORDICUS, under the "Programme Environnement et Societe" (rant no.
ANR-13-SENV-0002-02) and benefited from the IPSL data access PRODIGUER.
C. Timmreck acknowledges support from the German Federal Ministry of
Education (BMBF), research program "MiKlip" (FKZ: 01LP1517B/01LP1130A)
and the European Project 603557-STRATOCLIM under program FP7-ENV.
2013.6.1-2; STRAOCLIM also partially supported S. Bekki's work. M.
Toohey acknowledges support from the BMBF, research program "MiKlip"
(FKZ: 01LP1130B). A. Robock is supported by US National Science
Foundation (NSF) grant AGS-1430051. E. P. Gerber acknowledges NSF grant
AGS-1264195. A. Schmidt was supported by an Academic Research Fellowship
from the University of Leeds and NERC grant NE/N006038/1. W. T. Ball was
funded by the Swiss National Science Foundation projects 149182 and
163206. G. Hegerl is supported by the ERC project TITAN (EC-320691), by
NCAS and the Wolfson Foundation and the Royal Society as a Royal Society
Wolfson Research Merit Award (WM130060) holder. E. Rozanov was partially
supported by the Swiss National Science Foundation under grant
CRSII2_147659 (FUPSOL II).
NR 92
TC 8
Z9 8
U1 14
U2 14
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD AUG 17
PY 2016
VL 9
IS 8
BP 2701
EP 2719
DI 10.5194/gmd-9-2701-2016
PG 19
WC Geosciences, Multidisciplinary
SC Geology
GA DW6XH
UT WOS:000383794200001
ER
PT J
AU Weeraddana, D
Premaratne, M
Gunapala, SD
Andrews, DL
AF Weeraddana, Dilusha
Premaratne, Malin
Gunapala, Sarath D.
Andrews, David L.
TI Quantum electrodynamical theory of high-efficiency excitation energy
transfer in laser-driven nanostructure systems
SO PHYSICAL REVIEW B
LA English
DT Article
ID BUILDING-BLOCKS; DOTS; ABSORPTION; NANOWIRES; EMISSION; DEVICES
AB A fundamental theory is developed for describing laser-driven resonance energy transfer (RET) in dimensionally constrained nanostructureswithin the framework of quantum electrodynamics. The process of RET communicates electronic excitation between suitably disposed emitter and detector particles in close proximity, activated by the initial excitation of the emitter. Here, we demonstrate that the transfer rate can be significantly increased by propagation of an auxiliary laser beam through a pair of nanostructure particles. This is due to the higher order perturbative contribution to the Forster-type RET, in which laser field is applied to stimulate the energy transfer process. We construct a detailed picture of how excitation energy transfer is affected by an off-resonant radiation field, which includes the derivation of second and fourth order quantum amplitudes. The analysis delivers detailed results for the dependence of the transfer rates on orientational, distance, and laser intensity factor, providing a comprehensive fundamental understanding of laser-driven RET in nanostructures. The results of the derivations demonstrate that the geometry of the system exercises considerable control over the laser-assisted RET mechanism. Thus, under favorable conformational conditions and relative spacing of donor-acceptor nanostructures, the effect of the auxiliary laser beam is shown to produce up to 70% enhancement in the energy migration rate. This degree of control allows optical switching applications to be identified.
C1 [Weeraddana, Dilusha; Premaratne, Malin] Monash Univ, Adv Comp & Simulat Lab AxL, Dept Elect & Comp Syst Engn, Clayton, Vic 3800, Australia.
[Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Andrews, David L.] Univ East Anglia, Sch Chem, Norwich Res Pk, Norwich NR4 7TJ, Norfolk, England.
RP Weeraddana, D (reprint author), Monash Univ, Adv Comp & Simulat Lab AxL, Dept Elect & Comp Syst Engn, Clayton, Vic 3800, Australia.
EM dilusha.weeraddana@monash.edu; malin.premaratne@monash.edu;
Sarath.D.Gunapala@jpl.nasa.gov; d.l.andrews@uea.ac.uk
FU Monash University Institute of Graduate Research; Australian Research
Council [DP140100883]
FX The work of D.W. is supported by the Monash University Institute of
Graduate Research. The work of M.P. is supported by the Australian
Research Council, through its Discovery Grant No. DP140100883.
NR 53
TC 0
Z9 0
U1 7
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD AUG 17
PY 2016
VL 94
IS 8
AR 085133
DI 10.1103/PhysRevB.94.085133
PG 11
WC Physics, Condensed Matter
SC Physics
GA DT4XX
UT WOS:000381485900003
ER
PT J
AU Turner, DL
Fennell, JF
Blake, JB
Clemmons, JH
Mauk, BH
Cohen, IJ
Jaynes, AN
Craft, JV
Wilder, FD
Baker, DN
Reeves, GD
Gershman, DJ
Avanov, LA
Dorelli, JC
Giles, BL
Pollock, CJ
Schmid, D
Nakamura, R
Strangeway, RJ
Russell, CT
Artemyev, AV
Runov, A
Angelopoulos, V
Spence, HE
Torbert, RB
Burch, JL
AF Turner, D. L.
Fennell, J. F.
Blake, J. B.
Clemmons, J. H.
Mauk, B. H.
Cohen, I. J.
Jaynes, A. N.
Craft, J. V.
Wilder, F. D.
Baker, D. N.
Reeves, G. D.
Gershman, D. J.
Avanov, L. A.
Dorelli, J. C.
Giles, B. L.
Pollock, C. J.
Schmid, D.
Nakamura, R.
Strangeway, R. J.
Russell, C. T.
Artemyev, A. V.
Runov, A.
Angelopoulos, V.
Spence, H. E.
Torbert, R. B.
Burch, J. L.
TI Energy limits of electron acceleration in the plasma sheet during
substorms: A case study with the Magnetospheric Multiscale (MMS) mission
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE energetic particle injections; particle acceleration; magnetotail;
plasma sheet; reconnection; substorm
ID BURSTY BULK FLOWS; DIPOLARIZATION EVENTS; PARTICLE INJECTIONS;
RECONNECTION; SIMULATION; FIELD
AB We present multipoint observations of earthward moving dipolarization fronts and energetic particle injections from NASA's Magnetospheric Multiscale mission with a focus on electron acceleration. From a case study during a substorm on 02 August 2015, we find that electrons are only accelerated over a finite energy range, from a lower energy threshold at similar to 7-9keV up to an upper energy cutoff in the hundreds of keV range. At energies lower than the threshold energy, electron fluxes decrease, potentially due to precipitation by strong parallel electrostatic wavefields or initial sources in the lobes. Electrons at energies higher than the threshold are accelerated cumulatively by a series of impulsive magnetic dipolarization events. This case demonstrates how the upper energy cutoff increases, in this case from similar to 130keV to >500keV, with each dipolarization/injection during sustained activity. We also present a simple model accounting for these energy limits that reveals that electron energization is dominated by betatron acceleration.
C1 [Turner, D. L.; Fennell, J. F.; Blake, J. B.; Clemmons, J. H.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
[Mauk, B. H.; Cohen, I. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Jaynes, A. N.; Craft, J. V.; Wilder, F. D.; Baker, D. N.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Gershman, D. J.; Avanov, L. A.; Dorelli, J. C.; Giles, B. L.; Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Pollock, C. J.] Denali Sci, Healy, AK USA.
[Schmid, D.; Nakamura, R.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
[Strangeway, R. J.; Russell, C. T.; Artemyev, A. V.; Runov, A.; Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Spence, H. E.; Torbert, R. B.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
RP Turner, DL (reprint author), Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
EM drew.lawson.turner@gmail.com
RI NASA MMS, Science Team/J-5393-2013; Cohen, Ian/K-3038-2015; Mauk,
Barry/E-8420-2017;
OI NASA MMS, Science Team/0000-0002-9504-5214; Cohen,
Ian/0000-0002-9163-6009; Mauk, Barry/0000-0001-9789-3797; Clemmons,
James/0000-0002-5298-5222
FU NASA (MMS) [NNG04EB99C]; International Space Science Institute's
International Teams program
FX The authors are thankful to all of the MMS, THEMIS, Van Allen Probes,
ACE, Wind, and OMNI teams for making their data available to the public.
In addition to coauthors' contributions, we thank from THEMIS, K.H.
Glassmeier, U. Auster, and W. Baumjohann (under contract 50 OC 0302); D.
Larson and R. P. Lin; and C. W. Carlson and J. P. McFadden for FGM, SST,
and ESA data, respectively; from Van Allen Probes, C. Kletzing and team
for EMFISIS data; from ACE, Wind, and OMNI, J. H. King, N.
Papatashvilli, and team for OMNI solar wind data; the SPEDAS team and
contributors for their open source library of data analysis tools; and
NASA CDAWeb and mission specific online databases. MMS data are
available at < https://lasp.colorado.edu/mms/sdc >; data from this
particular event, which occurred during commissioning, may be requested
from the authors or from the SDC. THEMIS data and SPEDAS tools are
freely available at < http://themis.ssl.berkeley.edu/index.shtml >. Van
Allen Probes data are available at <
http://rbspgway.jhuapl.edu/data_instrumentationSOC >. This work was
primarily supported by funding from NASA (MMS contract NNG04EB99C) and
research supported by the International Space Science Institute's
International Teams program.
NR 40
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 7785
EP 7794
DI 10.1002/2016GL069691
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300001
ER
PT J
AU Wang, S
Chen, LJ
Hesse, M
Bessho, N
Gershman, DJ
Dorelli, J
Giles, B
Torbert, RB
Pollock, CJ
Strangeway, R
Ergun, RE
Burch, JL
Avanov, L
Lavraud, B
Moore, TE
Saito, Y
AF Wang, Shan
Chen, Li-Jen
Hesse, Michael
Bessho, Naoki
Gershman, Daniel J.
Dorelli, John
Giles, Barbara
Torbert, Roy B.
Pollock, Craig J.
Strangeway, Robert
Ergun, Robert E.
Burch, James L.
Avanov, Levon
Lavraud, Benoit
Moore, Thomas E.
Saito, Yoshifumi
TI Two-scale ion meandering caused by the polarization electric field
during asymmetric reconnection
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ion meandering motion; magnetic reconnection; polarization electric
field
ID DIFFUSION REGION; MAGNETIC RECONNECTION; CURRENT SHEET; ACCELERATION;
MAGNETOPAUSE; MAGNETOTAIL; EVOLUTION; TAIL
AB Ion velocity distribution functions (VDFs) from a particle-in-cell simulation of asymmetric reconnection are investigated to reveal a two-scale structure of the ion diffusion region (IDR). Ions bouncing in the inner IDR are trapped mainly by the electric field normal to the current sheet (N direction), while those reaching the outer IDR are turned back mainly by the magnetic force. The resulting inner layer VDFs have counter-streaming populations along N with decreasing counter-streaming speeds away from the midplane while maintaining the out-of-plane speed, and the outer layer VDFs exhibit crescent shapes toward the out-of-plane direction. Observations of the above VDF features and the normal electric fields provide evidence for the two-scale meandering motion.
C1 [Wang, Shan; Chen, Li-Jen; Bessho, Naoki] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wang, Shan; Chen, Li-Jen; Hesse, Michael; Bessho, Naoki; Gershman, Daniel J.; Dorelli, John; Giles, Barbara; Pollock, Craig J.; Avanov, Levon; Moore, Thomas E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Torbert, Roy B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Strangeway, Robert] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Ergun, Robert E.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Burch, James L.] Southwest Res Inst San Antonio, San Antonio, TX USA.
[Lavraud, Benoit] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.
[Lavraud, Benoit] CNRS, UMR 5277, Toulouse, France.
[Saito, Yoshifumi] Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
RP Wang, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Wang, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM swang90@umd.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NSF [AGS-1543598, AGS-1202537, AGS-1552142]; NASA; CNES; CNRS
FX The research is supported in part by NSF grants AGS-1543598,
AGS-1202537, and AGS-1552142 and NASA grants to the MMS Theory and
Modeling and FPI at GSFC. IRAP contribution to MMS was supported by CNES
and CNRS. MMS data are available at MMS Science Data Center
(https://lasp.colorado.edu/mms/sdc/).
NR 25
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SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 7831
EP 7839
DI 10.1002/2016GL069842
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300006
ER
PT J
AU Huang, SY
Sahraoui, F
Retino, A
Le Contel, O
Yuan, ZG
Chasapis, A
Aunai, N
Breuillard, H
Deng, XH
Zhou, M
Fu, HS
Pang, Y
Wang, DD
Torbert, RB
Goodrich, KA
Ergun, RE
Khotyaintsev, YV
Lindqvist, PA
Russell, CT
Strangeway, RJ
Magnes, W
Bromund, K
Leinweber, H
Plaschke, F
Anderson, BJ
Pollock, CJ
Giles, BL
Moore, TE
Burch, JL
AF Huang, S. Y.
Sahraoui, F.
Retino, A.
Le Contel, O.
Yuan, Z. G.
Chasapis, A.
Aunai, N.
Breuillard, H.
Deng, X. H.
Zhou, M.
Fu, H. S.
Pang, Y.
Wang, D. D.
Torbert, R. B.
Goodrich, K. A.
Ergun, R. E.
Khotyaintsev, Y. V.
Lindqvist, P. -A.
Russell, C. T.
Strangeway, R. J.
Magnes, W.
Bromund, K.
Leinweber, H.
Plaschke, F.
Anderson, B. J.
Pollock, C. J.
Giles, B. L.
Moore, T. E.
Burch, J. L.
TI MMS observations of ion-scale magnetic island in the magnetosheath
turbulent plasma
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetic island; magnetosheath; electrostatic solitary waves; lower
hybrid drift waves; electron beams; multiscale coupling
ID ELECTROSTATIC SOLITARY WAVES; EARTHS MAGNETOTAIL; FLUX ROPE; CLUSTER;
RECONNECTION; REGION; FIELD; GENERATION; FREQUENCY; SPECTRA
AB In this letter, first observations of ion-scale magnetic island from the Magnetospheric Multiscale mission in the magnetosheath turbulent plasma are presented. The magnetic island is characterized by bipolar variation of magnetic fields with magnetic field compression, strong core field, density depletion, and strong currents dominated by the parallel component to the local magnetic field. The estimated size of magnetic island is about 8 d(i), where d(i) is the ion inertial length. Distinct particle behaviors and wave activities inside and at the edges of the magnetic island are observed: parallel electron beam accompanied with electrostatic solitary waves and strong electromagnetic lower hybrid drift waves inside the magnetic island and bidirectional electron beams, whistler waves, weak electromagnetic lower hybrid drift waves, and strong broadband electrostatic noise at the edges of the magnetic island. Our observations demonstrate that highly dynamical, strong wave activities and electron-scale physics occur within ion-scale magnetic islands in the magnetosheath turbulent plasma.
C1 [Huang, S. Y.; Yuan, Z. G.; Wang, D. D.] Wuhan Univ, Sch Elect Informat, Wuhan, Peoples R China.
[Huang, S. Y.; Sahraoui, F.; Retino, A.; Le Contel, O.; Aunai, N.; Breuillard, H.] UPMC, Ecole Polytech, CNRS, Lab Phys Plasmas, Palaiseau, France.
[Chasapis, A.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Chasapis, A.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Deng, X. H.; Pang, Y.] Nanchang Univ, Inst Space Sci & Technol, Nanchang, Peoples R China.
[Zhou, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Fu, H. S.] Beihang Univ, Sch Space & Environm, Beijing, Peoples R China.
[Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Goodrich, K. A.; Ergun, R. E.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Khotyaintsev, Y. V.] Swedish Inst Space Phys, Uppsala, Sweden.
[Lindqvist, P. -A.] Royal Inst Technol, Stockholm, Sweden.
[Russell, C. T.; Strangeway, R. J.; Leinweber, H.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Magnes, W.; Plaschke, F.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
[Bromund, K.; Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Pollock, C. J.; Giles, B. L.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
RP Huang, SY (reprint author), Wuhan Univ, Sch Elect Informat, Wuhan, Peoples R China.; Huang, SY (reprint author), UPMC, Ecole Polytech, CNRS, Lab Phys Plasmas, Palaiseau, France.
EM shiyonghuang@whu.edu.cn
RI NASA MMS, Science Team/J-5393-2013;
OI NASA MMS, Science Team/0000-0002-9504-5214; Retino,
Alessandro/0000-0001-5824-2852
FU National Natural Science Foundation of China [41374168, 41404132];
Program for New Century Excellent Talents in University [NCET-13-0446];
China Postdoctoral Science Foundation Funded Project [2015 T80830];
project THESOW [ANR-11-JS56-0008]; LABEX Plas@Par as part of the program
"Investissements d'Avenir" [ANR-11-IDEX-0004-02]; CNES through the grant
"Allocations de recherche postdoctorale"
FX We thank the entire MMS team and instrument leads for the data access
and support. This work was supported by the National Natural Science
Foundation of China (41374168 and 41404132), Program for New Century
Excellent Talents in University (NCET-13-0446), and China Postdoctoral
Science Foundation Funded Project (2015 T80830). S.Y.H. and F.S.
acknowledge the financial support from the project THESOW, grant
ANR-11-JS56-0008, and from LABEX Plas@Par through a grant managed by the
Agence Nationale de la Recherche (ANR), as part of the program
"Investissements d'Avenir" under the reference ANR-11-IDEX-0004-02.
H.B.'s work has been supported by CNES through the grant "Allocations de
recherche postdoctorale." Data are publicly available from the MMS
Science Data Center at http://lasp.colorado.edu/mms/sdc/. The French
involvement (SCM) on MMS is supported by CNES and CNRS.
NR 49
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U1 5
U2 5
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 7850
EP 7858
DI 10.1002/2016GL070033
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300008
ER
PT J
AU Koskinen, TT
Moses, JI
West, RA
Guerlet, S
Jouchoux, A
AF Koskinen, T. T.
Moses, J. I.
West, R. A.
Guerlet, S.
Jouchoux, A.
TI The detection of benzene in Saturn's upper atmosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Saturn; photochemistry
ID POLAR ATMOSPHERE; HAZE FORMATION; THERMOSPHERE; OCCULTATIONS; JUPITER;
STRATOSPHERE; IONOSPHERE; MESOSPHERE; CHEMISTRY; EVOLUTION
AB The stratosphere of Saturn contains a photochemical haze that appears thicker at the poles and may originate from chemistry driven by the aurora. Models suggest that the formation of hydrocarbon haze is initiated at high altitudes by the production of benzene, which is followed by the formation of heavier ring polycyclic aromatic hydrocarbons. Until now there have been no observations of hydrocarbons or photochemical haze in the production region to constrain these models. We report the first vertical profiles of benzene and constraints on haze opacity in the upper atmosphere of Saturn retrieved from Cassini Ultraviolet Imaging Spectrograph stellar occultations. We detect benzene at several different latitudes and find that the observed abundances of benzene can be produced by solar-driven ion chemistry that is enhanced at high latitudes in the northern hemisphere during spring. We also detect evidence for condensation and haze at high southern latitudes in the polar night.
C1 [Koskinen, T. T.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Moses, J. I.] Space Sci Inst, Boulder, CO USA.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Guerlet, S.] Univ Paris 06, Sorbonne Univ, CNRS, Lab Meteorol Dynam IPSL, Paris, France.
[Jouchoux, A.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
RP Koskinen, TT (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM tommi@lpl.arizona.edu
RI Moses, Julianne/I-2151-2013
OI Moses, Julianne/0000-0002-8837-0035
FU NASA Cassini Data Analysis and Participating Scientist grant
[NNX14AD51G]; NASA Solar System Workings grant [NNX16AG10G]; Cassini
Project; CNES
FX T.T.K. was supported by the NASA Cassini Data Analysis and Participating
Scientist grant NNX14AD51G. J.I.M. gratefully acknowledges support from
NASA Solar System Workings grant NNX16AG10G. Part of this work was
performed by the Jet Propulsion Laboratory, California Institute of
Technology, with funding from the Cassini Project for R.A.W. S.G. was
supported by CNES. This work is based on observations with the UVIS and
CIRS instruments onboard Cassini. The retrieval results and atmosphere
models discussed in this work can be obtained from the authors by
emailing T.T.K.
NR 25
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 7895
EP 7901
DI 10.1002/2016GL070000
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300013
ER
PT J
AU Barnhart, TB
Molotch, NP
Livneh, B
Harpold, AA
Knowles, JF
Schneider, D
AF Barnhart, Theodore B.
Molotch, Noah P.
Livneh, Ben
Harpold, Adrian A.
Knowles, John F.
Schneider, Dominik
TI Snowmelt rate dictates streamflow
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE water; snowmelt; streamflow; modeling; hydroclimatology; Budyko
ID WESTERN UNITED-STATES; MEAN ANNUAL EVAPOTRANSPIRATION; HYDROLOGICALLY
BASED DATASET; LAND-SURFACE FLUXES; NORTH-AMERICA; CLIMATE-CHANGE; WATER
AVAILABILITY; SNOWPACK; CATCHMENT; RUNOFF
AB Declining mountain snowpack and earlier snowmelt across the western United States has implications for downstream communities. We present a possible mechanism linking snowmelt rate and streamflow generation using a gridded implementation of the Budyko framework. We computed an ensemble of Budyko streamflow anomalies (BSAs) using Variable Infiltration Capacity model-simulated evapotranspiration, potential evapotranspiration, and estimated precipitation at 1/16 degrees resolution from 1950 to 2013. BSA was correlated with simulated baseflow efficiency (r(2)=0.64) and simulated snowmelt rate (r(2)=0.42). The strong correlation between snowmelt rate and baseflow efficiency (r(2)=0.73) links these relationships and supports a possible streamflow generation mechanism wherein greater snowmelt rates increase subsurface flow. Rapid snowmelt may thus bring the soil to field capacity, facilitating below-root zone percolation, streamflow, and a positive BSA. Previous works have shown that future increases in regional air temperature may lead to earlier, slower snowmelt and hence decreased streamflow production via the mechanism proposed by this work.
C1 [Barnhart, Theodore B.; Molotch, Noah P.; Schneider, Dominik] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Barnhart, Theodore B.; Molotch, Noah P.; Knowles, John F.; Schneider, Dominik] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Livneh, Ben] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
[Livneh, Ben] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Harpold, Adrian A.] Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA.
RP Barnhart, TB (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA.; Barnhart, TB (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
EM theodore.barnhart@colorado.edu
RI Molotch, Noah/C-8576-2009;
OI Knowles, John/0000-0002-3697-9439; Schneider,
Dominik/0000-0002-5846-5033; Harpold, Adrian/0000-0002-2566-9574
FU USDA-NSF Water Sustainability and Climate grant [2012-67003-19802]; NSF
Boulder Creek CZO [EAR-9810218]; NSF Hydrological Sciences
[EAR-1141764]; NSF [EAR-1144894]; USDA NIFA [NEV05293]; NSF Niwot Ridge
LTER [DEB-1027341]; NASA Earth and Space Science Fellowship
FX We would like to thank Paul Brooks for his comments on an early version
of this work, M. Bayani Cardenas for his suggestion to include an
ensemble of Budyko-type equations, and Jeff Dozier for his comments on
the manuscript. This work was supported by the USDA-NSF Water
Sustainability and Climate grant (2012-67003-19802), NSF Boulder Creek
CZO (EAR-9810218), NSF Hydrological Sciences (EAR-1141764), NSF
(EAR-1144894), USDA NIFA (NEV05293), NSF Niwot Ridge LTER (DEB-1027341),
and a NASA Earth and Space Science Fellowship to D.S. This analysis was
conducted in iPython 2.7 (https://ipython.org/) using Jupyter
(http://jupyter.org/), Pandas (http://pandas.pydata.org/), Numpy
(http://www.numpy.org/), Matplotlib (http://matplotlib.org/), and
Statsmodels (http://statsmodels.sourceforge.net/devel/). Data used for
this analysis are available at
ftp://192.12.137.7/pub/dcp/archive/OBS/livneh2014.1_16deg/ and are cited
in section 2.
NR 68
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 8006
EP 8016
DI 10.1002/2016GL069690
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300026
ER
PT J
AU Shellito, PJ
Small, EE
Colliander, A
Bindlish, R
Cosh, MH
Berg, AA
Bosch, DD
Caldwell, TG
Goodrich, DC
McNairn, H
Prueger, JH
Starks, PJ
van der Velde, R
Walker, JP
AF Shellito, Peter J.
Small, Eric E.
Colliander, Andreas
Bindlish, Rajat
Cosh, Michael H.
Berg, Aaron A.
Bosch, David D.
Caldwell, Todd G.
Goodrich, David C.
McNairn, Heather
Prueger, John H.
Starks, Patrick J.
van der Velde, Rogier
Walker, Jeffrey P.
TI SMAP soil moisture drying more rapid than observed in situ following
rainfall events
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Soil Moisture Active Passive (SMAP); validation; drydown; in situ
monitoring
ID ATMOSPHERE COUPLING EXPERIMENT; VALIDATION; DYNAMICS; STABILITY; SMOS;
PERSISTENCE; GLACE
AB We examine soil drying rates by comparing surface soil moisture observations from the NASA Soil Moisture Active Passive (SMAP) mission to those from networks of in situ probes upscaled to SMAP's sensing footprint. SMAP and upscaled in situ probes record different soil drying dynamics after rainfall. We modeled this process by fitting an exponential curve to 63 drydown events: the median SMAP drying timescale is 44% shorter and the magnitude of drying is 35% greater than in situ measurements. We also calculated drying rates between consecutive observations from 193 events. For 6days after rainfall, soil moisture from SMAP dries at twice the rate of in situ measurements. Restricting in situ observations to times of SMAP observations does not change the drying timescale, magnitude, or rate. Therefore, observed differences are likely due to differences in sensing depths: SMAP measures shallower soil moisture than in situ probes, especially after rainfall.
C1 [Shellito, Peter J.; Small, Eric E.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Colliander, Andreas] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Bindlish, Rajat; Cosh, Michael H.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD USA.
[Berg, Aaron A.] Univ Guelph, Dept Geog, Guelph, ON, Canada.
[Bosch, David D.] USDA ARS, Southeast Watershed Res Lab, Tifton, GA 31793 USA.
[Caldwell, Todd G.] Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX USA.
[Goodrich, David C.] USDA ARS, Southwest Watershed Res Ctr, Tucson, AZ USA.
[McNairn, Heather] Agr & Agri Food Canada, Ottawa, ON, Canada.
[Prueger, John H.] USDA ARS, Natl Lab Agr & Environm, Ames, IA USA.
[Starks, Patrick J.] USDA ARS, Grazinglands Res Lab, El Reno, OK USA.
[van der Velde, Rogier] Univ Twente, Fac Geoinformat Sci & Earth Observat ITC, Enschede, Netherlands.
[Walker, Jeffrey P.] Monash Univ, Dept Civil Engn, Melbourne, Vic, Australia.
RP Shellito, PJ (reprint author), Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
EM peter.shellito@colorado.edu
RI Caldwell, Todd/H-5129-2011
OI Caldwell, Todd/0000-0003-4068-0648
FU NASA [NNX13AF43G]; Environment Canada from the Canadian Space Agency
FX This research was supported by NASA grant NNX13AF43G. SMAP data on the
validation grid were provided by the SMAP passive soil moisture team
members: R. Bindlish, S. Chan, T. Jackson, P. O'Neill, and E. Njoku.
Precipitation data used in this study were acquired as part of the
mission of NASA's Earth Science Division and archived and distributed by
the Goddard Earth Sciences Data and Information Services Center. Thanks
to all who have provided high-quality in situ soil moisture data,
including Mark Seyfried and the Reynolds Creek Experimental Watershed;
Stan Livingston of the St. Joseph's Experimental Watershed
(USDA-Agricultural Research Service); Jose Martinez-Fernandez and the
REMEDHUS network; Mahta Moghaddam and the Tonzi Ranch SoilSCAPE project;
and Ernesto Lopez-Baeza and the Valencia network. The Kenaston network
is supported by Environment Canada from grants from the Canadian Space
Agency; Tracy Rowlandson and Erica Tetlock are acknowledged for their
work with the network. The data used are listed and provided in the
supporting information.
NR 43
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 8068
EP 8075
DI 10.1002/2016GL069946
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300033
ER
PT J
AU Colgan, W
Machguth, H
MacFerrin, M
Colgan, JD
van As, D
MacGregor, JA
AF Colgan, William
Machguth, Horst
MacFerrin, Mike
Colgan, Jeff D.
van As, Dirk
MacGregor, Joseph A.
TI The abandoned ice sheet base at Camp Century, Greenland, in a warming
climate
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Camp Century; Greenland; ice sheet
ID MELTWATER STORAGE; SECURITY; FIRN
AB In 1959 the U.S. Army Corps of Engineers built Camp Century beneath the surface of the northwestern Greenland Ice Sheet. There they studied the feasibility of deploying ballistic missiles within the ice sheet. The base and its wastes were abandoned with minimal decommissioning in 1967, under the assumption they would be preserved for eternity by perpetually accumulating snowfall. Here we show that a transition in ice sheet surface mass balance at Camp Century from net accumulation to net ablation is plausible within the next 75years, under a business-as-usual anthropogenic emissions scenario (Representative Concentration Pathway 8.5). Net ablation would guarantee the eventual remobilization of physical, chemical, biological, and radiological wastes abandoned at the site. While Camp Century and four other contemporaneous ice sheet bases were legally established under a Danish-U.S. treaty, the potential remobilization of their abandoned wastes, previously regarded as sequestered, represents an entirely new pathway of political dispute resulting from climate change.
C1 [Colgan, William] York Univ, Lassonde Sch Engn, Toronto, ON, Canada.
[Colgan, William; MacFerrin, Mike] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Machguth, Horst] Univ Zurich, Dept Geog, Zurich, Switzerland.
[Machguth, Horst] Univ Fribourg, Dept Geosci, Fribourg, Switzerland.
[Colgan, Jeff D.] Brown Univ, Watson Inst, Providence, RI 02912 USA.
[van As, Dirk] Geol Survey Denmark & Greenland, Dept Glaciol & Climate, Copenhagen, Denmark.
[MacGregor, Joseph A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab Code 615, Greenbelt, MD USA.
RP Colgan, W (reprint author), York Univ, Lassonde Sch Engn, Toronto, ON, Canada.; Colgan, W (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM colgan@yorku.ca
RI Colgan, William/H-1570-2014
OI Colgan, William/0000-0001-6334-1660
NR 40
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U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 8091
EP 8096
DI 10.1002/2016GL069688
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300036
ER
PT J
AU Kwok, R
Cunningham, GF
AF Kwok, R.
Cunningham, G. F.
TI Contributions of growth and deformation to monthly variability in sea
ice thickness north of the coasts of Greenland and the Canadian Arctic
Archipelago
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE sea ice; deformation; growth; Arctic Ocean
ID FREEBOARD; VOLUME; RADAR
AB Regional variability in monthly CryoSat-2 sea ice thickness is partitioned into contributions from dynamics and thermodynamics using ice deformation calculated from large-scale ice drift. For five winters (December to April, 2011-2015), over a region of persistent convergence north of the coasts of Greenland and the Canadian Arctic Archipelago, deformation explains similar to 34% of the overall variance (up to 69% in 2014/2015) in monthly thickness changes. Approximately 42-56% (or similar to 0.6m) of the seasonal changes in mean regional ice thickness can be attributed to divergence and shear. The estimated area-averaged growth of 0.120.03m/month compares favorably with measurements from ice mass balance buoys. Examination of the time-variable thickness distributions shows areas covered by ice <3m are reduced, while areas of thicker ice (>3m) increased. Albeit at fairly coarse resolution, this coupled analysis of thickness changes and deformation offered a first look at the character of the regional thickness redistribution process.
C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ron.kwok@jpl.nasa.gov
NR 16
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U1 6
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 AUG 16
PY 2016
VL 43
IS 15
BP 8097
EP 8105
DI 10.1002/2016GL069333
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300037
ER
PT J
AU Ray, RD
Susanto, RD
AF Ray, Richard D.
Susanto, R. Dwi
TI Tidal mixing signatures in the Indonesian seas from high-resolution sea
surface temperature data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE tidal mixing; sea surface temperatures
ID SATELLITE-OBSERVATIONS; PILOT PROJECT; SULU SEA; OCEAN; VARIABILITY;
THROUGHFLOW; ARCHIPELAGO; MODULATION; CALIFORNIA; OKHOTSK
AB The presence of significant tidal mixing in the Indonesian seas is well established from both observations and numerical modeling. One indicator is a clear spring-neap cycle in satellite sea surface temperature (SST) measurements, as first shown by Ffield and Gordon. Their early results are here updated with SST data of considerably higher spatial and temporal resolution. The largest fortnightly signals are found to be localized to relatively small straits, channels, and sills, while the deep basin of the Banda Sea displays little significant signal. A broader region of somewhat enhanced signal surrounds the Seram Sea. The high resolution of the modern SST data is especially critical for mapping the complex fortnightly signals that arise in, and especially south of, the major straits of the Lesser Sunda Island chain.
C1 [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Susanto, R. Dwi] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Susanto, R. Dwi] Surya Univ, Ctr Oceanog & Marine Technol, Tangerang, Indonesia.
RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012
FU Physical Oceanography program of the U.S. National Aeronautics and Space
Administration
FX We thank Arnold Gordon for fruitful discussions and two reviewers for
useful comments. This work was supported by the Physical Oceanography
program of the U.S. National Aeronautics and Space Administration. The
Group for High-Resolution Sea Surface Temperature (GHRSST) Multiscale
Ultrahigh Resolution (MUR) SST data were obtained from the NASA EOSDIS
Physical Oceanography Distributed Active Archive Center at the Jet
Propulsion Laboratory, Pasadena, CA.
NR 38
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 8115
EP 8123
DI 10.1002/2016GL069485
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300039
ER
PT J
AU Winchell, TS
Barnard, DM
Monson, RK
Burns, SP
Molotch, NP
AF Winchell, Taylor S.
Barnard, David M.
Monson, Russell K.
Burns, Sean P.
Molotch, Noah P.
TI Earlier snowmelt reduces atmospheric carbon uptake in midlatitude
subalpine forests
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE net ecosystem exchange; snow ablation period; carbon uptake
ID ECOSYSTEM CO2 EXCHANGE; WESTERN NORTH-AMERICA; HIGH-ELEVATION;
INTERANNUAL VARIABILITY; WATER AVAILABILITY; UNITED-STATES; CLIMATE;
TEMPERATURE; AUTUMN; TRENDS
AB Previous work demonstrates conflicting evidence regarding the influence of snowmelt timing on forest net ecosystem exchange (NEE). Based on 15years of eddy covariance measurements in Colorado, years with earlier snowmelt exhibited less net carbon uptake during the snow ablation period, which is a period of high potential for productivity. Earlier snowmelt aligned with colder periods of the seasonal air temperature cycle relative to later snowmelt. We found that the colder ablation-period air temperatures during these early snowmelt years lead to reduced rates of daily NEE. Hence, earlier snowmelt associated with climate warming, counterintuitively, leads to colder atmospheric temperatures during the snow ablation period and concomitantly reduced rates of net carbon uptake. Using a multilinear-regression (R-2=0.79, P<0.001) relating snow ablation period mean air temperature and peak snow water equivalent (SWE) to ablation-period NEE, we predict that earlier snowmelt and decreased SWE may cause a 45% reduction in midcentury ablation-period net carbon uptake.
C1 [Winchell, Taylor S.; Barnard, David M.; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Winchell, Taylor S.] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
[Monson, Russell K.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA.
[Monson, Russell K.] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA.
[Burns, Sean P.; Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Burns, Sean P.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Winchell, TS (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.; Winchell, TS (reprint author), Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
EM taylor.winchell@colorado.edu
RI Molotch, Noah/C-8576-2009
FU U.S. National Science Foundation (NSF) Graduate Research Fellowship
(NSF) [DGE 1144083]; NSF-U.S. Department of Agriculture (USDA) joint
program for Water Sustainability and Climate (USDA) [2012-67003-19802];
NSF Hydrological Sciences Program (NSF) [EAR1141764]; U.S. Department of
Energy (DOE); USDA; NSF Niwot Ridge Long-Term Ecological Research
program; DOE Office of Science through the AmeriFlux Management Project
(AMP) at Lawrence Berkeley National Laboratory [7094866]
FX This material is based upon work supported by the U.S. National Science
Foundation (NSF) Graduate Research Fellowship (NSF grant DGE 1144083),
the NSF-U.S. Department of Agriculture (USDA) joint program for Water
Sustainability and Climate (USDA grant: 2012-67003-19802), and the NSF
Hydrological Sciences Program (NSF Grant: EAR1141764). Data collection
was funded by the U.S. Department of Energy (DOE), the USDA, and the NSF
Niwot Ridge Long-Term Ecological Research program. The US-NR1 AmeriFlux
site is supported by the DOE Office of Science through the AmeriFlux
Management Project (AMP) at Lawrence Berkeley National Laboratory under
award 7094866. We offer thanks to Peter Blanken and all others involved
in the AmeriFlux data collection efforts. Additionally, we are very
thankful to David Schimel and one anonymous reviewer for their
constructive reviews of the manuscript. All data used are listed in the
supporting information and can be found at
http://urquell.colorado.edu/data_ameriflux/ and
http://www.wcc.nrcs.usda.gov/nwcc/site?sitenum=663.
NR 32
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2016
VL 43
IS 15
BP 8160
EP 8168
DI 10.1002/2016GL069769
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DV9VM
UT WOS:000383290300044
ER
PT J
AU Geller, MA
Zhou, TH
Yuan, W
AF Geller, Marvin A.
Zhou, Tiehan
Yuan, Wei
TI The QBO, gravity waves forced by tropical convection, and ENSO
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE QBO amplitudes and periods; gravity waves forced by tropical convection;
ENSO
ID QUASI-BIENNIAL OSCILLATION; MODEL; STRATOSPHERE
AB By means of theory, a simplified cartoon illustrating wave forcing of the stratospheric quasi-biennial oscillation (QBO), and general circulation modeling of the QBO, it is argued that the period of the QBO is mainly controlled by the magnitude of the gravity wave (GW) vertical fluxes of horizontal momentum (GWMF) forcing the QBO, while the QBO amplitude is mainly determined by the phase speeds of the GWs that make up this momentum flux. It is furthermore argued that it is the zonally averaged GWMF that principally determines the QBO period irrespective of the longitudinal distribution of this GW momentum flux. These concepts are used to develop a hypothesis for the cause of a previously reported El Nino-Southern Oscillation (ENSO) modulation of QBO periods and amplitudes. Some observational evidence is reported for the ENSO modulation of QBO amplitudes to have been different before the 1980s than after about 1990. A hypothesis is also given to explain this in terms of the different ENSO modulation of tropical deep convection that took place before the 1980s from that which occurred after about 1990. The observational evidence, while consistent with our hypotheses, does not prove that our hypotheses are correct given the small number of El Ninos and La Ninas that occurred in the early and later periods. Further research is needed to support or refute our hypotheses.
C1 [Geller, Marvin A.; Yuan, Wei] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Zhou, Tiehan] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
RP Geller, MA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
EM marvin.geller@stonybrook.edu
FU National Science Foundation (NSF) [ATM-0836539, ATM-1101258]; NASA's
Modeling, Analysis and Prediction (MAP) Program
FX This work was supported by the National Science Foundation (NSF) under
grants ATM-0836539 and ATM-1101258 and by the NASA's Modeling, Analysis
and Prediction (MAP) Program. The model results were made possible by
the NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center. Data from the
GISS climate model are available from Tiehan Zhou (tz2131@columbia.edu).
The authors acknowledge four very helpful anonymous reviews, which
resulted in a significantly improved paper.
NR 24
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U1 3
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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 AUG 16
PY 2016
VL 121
IS 15
BP 8886
EP 8895
DI 10.1002/2015JD024125
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0ZN
UT WOS:000383372400009
ER
PT J
AU Toth, TD
Zhang, JL
Campbell, JR
Reid, JS
Vaughan, MA
AF Toth, Travis D.
Zhang, Jianglong
Campbell, James R.
Reid, Jeffrey S.
Vaughan, Mark A.
TI Temporal variability of aerosol optical thickness vertical distribution
observed from CALIOP
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol
ID LONG-TERM TREND; DATA-ASSIMILATION; DEPTH RETRIEVALS; MODIS-AQUA;
AERONET; CALIPSO; PRODUCTS; LAND; MISR; DUST
AB Temporal variability in the vertical distribution of aerosol optical thickness (AOT) derived from the 0.532 mu m aerosol extinction coefficient is described using Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) observations over 8.5years (June 2006 to December 2014). Temporal variability of CALIOP column-integrated AOT is largely consistent with total column AOT trends from several passive satellite sensors, such as the Moderate Resolution Imaging Spectroradiometer, Multiangle Imaging Spectroradiometer, and the Sea-viewing Wide Field-of-view Sensor. Globally, a 0.0002 AOT per year positive trend in deseasonalized CALIOP total column AOT for daytime conditions is attributed to corresponding changes in near-surface (i.e., 0.0-0.5km or 0.5-1.0km above ground level (agl)) aerosol particle loading, while a -0.0006 AOT per year trend during nighttime is attributed to elevated (i.e., 1.0-2.0km or >2.0km agl) aerosols. Regionally, increasing daytime CALIOP AOTs are found over Southern Africa and India, mostly due to changes in aerosol loading at the 1.0-2.0km and 0.0-0.5km agl layers, respectively. Decreasing daytime CALIOP AOTs are observed over Northern Africa, Eastern U.S., and South America (due mostly to elevated aerosol loading), while the negative CALIOP AOT trends found over Eastern China, Europe, and Western U.S. are due mostly to aerosol layers nearer the surface. To our knowledge, this study is the first to provide both a globally comprehensive estimation of the temporal variation in aerosol vertical distribution and an insight into passive sensor column AOT trends in the vertical domain.
C1 [Toth, Travis D.; Zhang, Jianglong] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
[Campbell, James R.; Reid, Jeffrey S.] Naval Res Lab, Aerosol & Radiat Sci Sect, Marine Meteorol Div, Monterey, CA USA.
[Vaughan, Mark A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Toth, TD (reprint author), Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
EM travis.toth@und.edu
RI Campbell, James/C-4884-2012; Reid, Jeffrey/B-7633-2014
OI Campbell, James/0000-0003-0251-4550; Reid, Jeffrey/0000-0002-5147-7955
FU Office of Naval Research [322]; NASA [NNX14AJ13G, IAARPO201422]
FX This research was funded through the support of the Office of Naval
Research Code 322. Author J.Z. and T.D.T. acknowledge the support from
NASA grant NNX14AJ13G. Author J.R.C. acknowledges the support of the
NASA Interagency Agreement IAARPO201422 on behalf of the CALIPSO Science
Team. CALIPSO data were obtained from the NASA Langley Research Center
Atmospheric Science Data Center (eos-web.larc.nasa.gov). MODIS data were
obtained from NASA Goddard Space Flight Center
(ladsweb.nascom.nasa.gov). AERONET data were obtained from the project
website (aeronet.gsfc.nasa.gov). We acknowledge the AERONET program, and
the contributing principal investigators and their staff, for
coordinating the sites and data used for this investigation. We thank
Jason Tackett for his guidance with the Level 3.0 aerosol profile data
and Chip Trepte for his suggestions in improving this work.
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SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 16
PY 2016
VL 121
IS 15
BP 9117
EP 9139
DI 10.1002/2015JD024668
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0ZN
UT WOS:000383372400022
ER
PT J
AU Gautam, R
Gatebe, CK
Singh, MK
Varnai, T
Poudyal, R
AF Gautam, Ritesh
Gatebe, Charles K.
Singh, Manoj K.
Varnai, Tamas
Poudyal, Rajesh
TI Radiative characteristics of clouds embedded in smoke derived from
airborne multiangular measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; cloud; remote sensing; radiative interactions
ID AEROSOL OPTICAL DEPTH; ABSORBING AEROSOLS; SENSITIVITY-ANALYSIS;
SOUTHEAST ATLANTIC; EFFECTIVE RADIUS; MODIS; RETRIEVAL; LAYERS;
ABSORPTION; SCATTERING
AB Clouds in the presence of absorbing aerosols result in their apparent darkening, observed at the top of atmosphere (TOA), which is associated with the radiative effects of aerosol absorption. Owing to the large radiative effect and potential impacts on regional climate, above-cloud aerosols have recently been characterized in multiple satellite-based studies. While satellite data are particularly useful in showing the radiative impact of above-cloud aerosols at the TOA, recent literature indicates large uncertainties in satellite retrievals of above-cloud aerosol optical depth (AOD) and single scattering albedo (SSA), which are among the most important parameters in the assessment of associated radiative effects. In this study, we analyze radiative characteristics of clouds in the presence of wildfire smoke using airborne data primarily from NASA's Cloud Absorption Radiometer, collected during the Arctic Research of the Composition of the Troposphere from Aircraft and Satellites campaign in Canada during the 2008 summer season. We found a strong positive reflectance (R) gradient in the UV-visible (VIS)-near infrared (NIR) spectrum for clouds embedded in dense smoke, as opposed to an (expected) negative gradient for cloud-free smoke and a flat spectrum for smoke-free cloud cover. Several cases of clouds embedded in thick smoke were found, when the aircraft made circular/spiral measurements, which not only allowed the complete characterization of angular distribution of smoke scattering but also provided the vertical distribution of smoke and clouds (within 0.5-5km). Specifically, the largest darkening by smoke was found in the UV/VIS, with R-0.34m reducing to 0.2 (or 20%), in contrast to 0.8 at NIR wavelengths (e.g., 1.27 mu m). The observed darkening is associated with large AODs (0.5-3.0) and moderately low SSA (0.85-0.93 at 0.53 mu m), resulting in a significantly large instantaneous aerosol forcing efficiency of 25447Wm(-2-1). Our observations of smoke-cloud radiative interactions were found to be physically consistent with theoretical plane-parallel 1-D and Monte Carlo 3-D radiative transfer calculations, capturing the observed gradient across UV-VIS-NIR. Results from this study offer insights into aerosol-cloud radiative interactions and may help in better constraining satellite retrieval algorithms.
C1 [Gautam, Ritesh; Singh, Manoj K.] Indian Inst Technol, Ctr Studies Resources Engn, Bombay, Maharashtra, India.
[Gautam, Ritesh] Indian Inst Technol, Interdisciplinary Program Climate Studies, Mumbai, Maharashtra, India.
[Gatebe, Charles K.] Univ Space Res Assoc, Columbia, MD USA.
[Gatebe, Charles K.; Varnai, Tamas] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA.
[Poudyal, Rajesh] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Gautam, R (reprint author), Indian Inst Technol, Ctr Studies Resources Engn, Bombay, Maharashtra, India.; Gautam, R (reprint author), Indian Inst Technol, Interdisciplinary Program Climate Studies, Mumbai, Maharashtra, India.
EM rgautam@iitb.ac.in
FU NASA Radiation Sciences program
FX This research is supported by NASA Radiation Sciences program, managed
by Hal Maring. We are grateful to several instrument Principal
Investigators for the provision of airborne data used in this study:
Jens Redemann/NASA ARC (spectral AOD data from AATS measurements),
Anthony Bucholtz/NRL, Monterey (solar radiation flux data from BBR
measurements), and Antony Clarke/University of Hawaii (in situ aerosol
optical properties). Data sets used in this paper are available from the
ARCTAS data archive at
http://www-air.larc.nasa.gov/missions/arctas/arctas.html and CAR data
archive at http://car.gsfc.nasa.gov/. We thank three anonymous reviewers
for their comments and suggestions which helped improve an earlier
version of the manuscript.
NR 44
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SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 16
PY 2016
VL 121
IS 15
BP 9140
EP 9152
DI 10.1002/2016JD025309
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0ZN
UT WOS:000383372400023
ER
PT J
AU Bardeen, CG
Marsh, DR
Jackman, CH
Hervig, ME
Randall, CE
AF Bardeen, C. G.
Marsh, D. R.
Jackman, C. H.
Hervig, M. E.
Randall, C. E.
TI Impact of the January 2012 solar proton event on polar mesospheric
clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE solar proton event; polar mesospheric cloud; noctilucent cloud; CIPS;
SOFIE; WACCM
ID NITRIC-OXIDE; MODEL; OZONE; ICE
AB We use data from the Aeronomy of Ice in the Mesosphere mission and simulations using the Whole Atmosphere Community Climate Model to determine the impact of the 23-30 January 2012 solar proton event (SPE) on polar mesospheric clouds (PMCs) and mesospheric water vapor. We see a small heating and loss of ice mass on 26 January that is consistent with prior results but is not statistically significant. We also find a previously unreported but statistically significant similar to 10% increase in ice mass and in water vapor in the sublimation area in the model that occurs in the 7 to 14days following the start of the event. The magnitude of the response to the January 2012 SPE is small compared to other sources of variability like gravity waves and planetary waves; however, sensitivity tests suggest that with larger SPEs this delayed increase in ice mass will increase, while there is little change in the loss of ice mass early in the event. The PMC response to SPEs in models is dependent on the gravity wave parameterization, and temperature anomalies from SPEs may be useful in evaluating and tuning gravity wave parameterizations.
C1 [Bardeen, C. G.; Marsh, D. R.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Jackman, C. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hervig, M. E.] GATS Inc, Driggs, ID USA.
[Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Randall, C. E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
RP Bardeen, CG (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM bardeenc@ucar.edu
RI Marsh, Daniel/A-8406-2008; Jackman, Charles/D-4699-2012; Randall,
Cora/L-8760-2014
OI Marsh, Daniel/0000-0001-6699-494X; Randall, Cora/0000-0002-4313-4397
FU NASA Living With a Star Targeted Research and Technology program
[10-LWSTRT10-0109]; AIM program; NASA through the Small Explorer program
[NAS5-03132]; NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center; National
Science Foundation; Office of Science (BER) of the U.S. Department of
Energy
FX Funding for C. Bardeen, C. Jackman, and D. Marsh is from the NASA Living
With a Star Targeted Research and Technology program, grant
10-LWSTRT10-0109. Funding for C. Randall and M. Hervig is from the AIM
program. AIM is funded by NASA through the Small Explorer program under
contract NAS5-03132. The CIPS and SOFIE observations, including
documentation and software for reading the data, are available at the
AIM website, aim.hamptonu.edu. SOFIE data are also available at the GATS
website, sofie.gats-inc.com. Model data will be made available upon
request to bardeenc@ucar.edu. We thank the AIM mission operations and
data processing teams for their excellent support. Computing 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. The CESM project is supported by the National Science
Foundation and the Office of Science (BER) of the U.S. Department of
Energy. NCAR is sponsored by the National Science Foundation.
NR 30
TC 0
Z9 0
U1 5
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 AUG 16
PY 2016
VL 121
IS 15
BP 9165
EP 9173
DI 10.1002/2016JD024820
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0ZN
UT WOS:000383372400025
ER
PT J
AU Thompson, DR
McCubbin, I
Gao, BC
Green, RO
Matthews, AA
Mei, F
Meyer, KG
Platnick, S
Schmid, B
Tomlinson, J
Wilcox, E
AF Thompson, David R.
McCubbin, Ian
Gao, Bo Cai
Green, Robert O.
Matthews, Alyssa A.
Mei, Fan
Meyer, Kerry G.
Platnick, Steven
Schmid, Beat
Tomlinson, Jason
Wilcox, Eric
TI Measuring cloud thermodynamic phase with shortwave infrared imaging
spectroscopy
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE imaging spectroscopy; remote sensing; cloud phase; shortwave infrared;
AVIRIS-C; Arm Airborne Facility
ID RADIATIVE-TRANSFER; OPTICAL-THICKNESS; SPECTROMETER DATA; EFFECTIVE
RADIUS; LIQUID WATER; MU-M; ICE; AIRBORNE; RETRIEVAL; WAVELENGTHS
AB Shortwave Infrared imaging spectroscopy enables accurate remote mapping of cloud thermodynamic phase at high spatial resolution. We describe a measurement strategy to exploit signatures of liquid and ice absorption in cloud top apparent reflectance spectra from 1.4 to 1.8m. This signal is generally insensitive to confounding factors such as solar angles, view angles, and surface albedo. We first evaluate the approach in simulation and then apply it to airborne data acquired in the Calwater-2/ACAPEX campaign of Winter 2015. Here NASA's Classic Airborne Visible Infrared Imaging Spectrometer (AVIRIS-C) remotely observed diverse cloud formations while the U.S. Department of Energy ARM Aerial Facility G-1 aircraft measured cloud integral and microphysical properties in situ. The coincident measurements demonstrate good separation of the thermodynamic phases for relatively homogeneous clouds.
C1 [Thompson, David R.; McCubbin, Ian; Green, Robert O.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[McCubbin, Ian; Wilcox, Eric] Desert Res Inst, Reno, NV USA.
[Gao, Bo Cai] Naval Res Lab, Washington, DC 20375 USA.
[Matthews, Alyssa A.; Mei, Fan; Schmid, Beat; Tomlinson, Jason] Pacific Northwest Natl Lab, Richland, WA USA.
[Meyer, Kerry G.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Meyer, Kerry G.; Platnick, Steven] NASA Goddard Space Flight Ctr, Greenland, MD USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM david.r.thompson@jpl.nasa.gov
RI Platnick, Steven/J-9982-2014; Meyer, Kerry/E-8095-2016;
OI Platnick, Steven/0000-0003-3964-3567; Meyer, Kerry/0000-0001-5361-9200;
Thompson, David/0000-0003-1100-7550
FU National Oceanographic and Atmospheric Administration; Department of
Energy; Scripps Institute for Oceanography; California Energy Commission
FX The data used in this paper are available from
http://aviris.jpl.nasa.gov/publications/. The research described in this
paper was performed by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. Copyright 2016 California Institute of
Technology. Government sponsorship acknowledged. We appreciate the vital
assistance of the DOE Atmospheric Radiation Measurement (ARM) program
and the ARM Airborne Facility (AAF) team. We specifically acknowledge
the WCM-2000 sensor team including John Hubbe (deployment and
calibration). We also acknowledge and thank Jennifer Comstock of PNNL
and Chris Roden of SPEC. David Diner and Felix Seidel led the ER-2
observations and coordinated the AAF and the ER-2 flights. We thank the
ER-2 aircraft team at the NASA Armstrong Flight Research Laboratory, and
the Jet Propulsion Laboratory AVIRIS-C instrument team including Michael
Eastwood, Chuck Sarture, Scott Nolte, Mark Helmlinger, Sarah Lundeen,
and others. We acknowledge the help and support of NASA Earth Science
and the joint Calwater-2/ACAPEX investigation sponsored by the National
Oceanographic and Atmospheric Administration, the Department of Energy,
Scripps Institute for Oceanography, and the California Energy
Commission.
NR 47
TC 0
Z9 0
U1 5
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 AUG 16
PY 2016
VL 121
IS 15
BP 9174
EP 9190
DI 10.1002/2016JD024999
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0ZN
UT WOS:000383372400026
ER
PT J
AU Dammers, E
Palm, M
Van Damme, M
Vigouroux, C
Smale, D
Conway, S
Toon, GC
Jones, N
Nussbaumer, E
Warneke, T
Petri, C
Clarisse, L
Clerbaux, C
Hermans, C
Lutsch, E
Strong, K
Hannigan, JW
Nakajima, H
Morino, I
Herrera, B
Stremme, W
Grutter, M
Schaap, M
Kruit, RJW
Notholt, J
Coheur, PF
Erisman, JW
AF Dammers, Enrico
Palm, Mathias
Van Damme, Martin
Vigouroux, Corinne
Smale, Dan
Conway, Stephanie
Toon, Geoffrey C.
Jones, Nicholas
Nussbaumer, Eric
Warneke, Thorsten
Petri, Christof
Clarisse, Lieven
Clerbaux, Cathy
Hermans, Christian
Lutsch, Erik
Strong, Kim
Hannigan, James W.
Nakajima, Hideaki
Morino, Isamu
Herrera, Beatriz
Stremme, Wolfgang
Grutter, Michel
Schaap, Martijn
Kruit, Roy J. Wichink
Notholt, Justus
Coheur, Pierre-F.
Erisman, Jan Willem
TI An evaluation of IASI-NH3 with ground-based Fourier transform infrared
spectroscopy measurements
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID ATMOSPHERIC AMMONIA NH3; SATELLITE-OBSERVATIONS; CARBON-MONOXIDE; FTIR
MEASUREMENTS; HIGH-RESOLUTION; GLOBAL DISTRIBUTIONS; TROPOSPHERIC
AMMONIA; REACTIVE NITROGEN; UNITED-STATES; TES AMMONIA
AB Global distributions of atmospheric ammonia (NH3) measured with satellite instruments such as the Infrared Atmospheric Sounding Interferometer (IASI) contain valuable information on NH3 concentrations and variability in regions not yet covered by ground-based instruments. Due to their large spatial coverage and (bi-)daily overpasses, the satellite observations have the potential to increase our knowledge of the distribution of NH3 emissions and associated seasonal cycles. However the observations remain poorly validated, with only a handful of available studies often using only surface measurements without any vertical information. In this study, we present the first validation of the IASI-NH3 product using ground-based Fourier transform infrared spectroscopy (FTIR) observations. Using a recently developed consistent retrieval strategy, NH3 concentration profiles have been retrieved using observations from nine Network for the Detection of Atmospheric Composition Change (NDACC) stations around the world between 2008 and 2015. We demonstrate the importance of strict spatiotemporal collocation criteria for the comparison. Large differences in the regression results are observed for changing intervals of spatial criteria, mostly due to terrain characteristics and the short lifetime of NH3 in the atmosphere. The seasonal variations of both datasets are consistent for most sites. Correlations are found to be high at sites in areas with considerable NH3 levels, whereas correlations are lower at sites with low atmospheric NH3 levels close to the detection limit of the IASI instrument. A combination of the observations from all sites (N-obs = 547) give a mean relative difference of -32.4 +/- (56.3) %, a correlation r of 0.8 with a slope of 0.73. These results give an improved estimate of the IASI-NH3 product performance compared to the previous upper-bound estimates (-50 to + 100 %).
C1 [Dammers, Enrico; Van Damme, Martin; Erisman, Jan Willem] Vrije Univ Amsterdam, Dept Earth Sci, Cluster Earth & Climate, Amsterdam, Netherlands.
[Palm, Mathias; Warneke, Thorsten; Petri, Christof; Notholt, Justus] Univ Bremen, Inst Umweltphys, Bremen, Germany.
[Van Damme, Martin; Clarisse, Lieven; Clerbaux, Cathy; Coheur, Pierre-F.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, Spect Atmosphere, Brussels, Belgium.
[Vigouroux, Corinne; Hermans, Christian] Royal Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Smale, Dan] Natl Inst Water & Atmosphere, Lauder, New Zealand.
[Conway, Stephanie; Lutsch, Erik; Strong, Kim] Univ Toronto, Toronto, ON, Canada.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Jones, Nicholas] Univ Wollongong, Ctr Atmospher Chem, Wollongong, NSW, Australia.
[Nussbaumer, Eric; Hannigan, James W.] NCAR, Boulder, CO USA.
[Nakajima, Hideaki] NIES, Atmospher Environm Div, Tsukuba, Ibaraki, Japan.
[Morino, Isamu] Natl Inst Environm Studies, 16-2 Onogawa, Tsukuba, Ibaraki 3058506, Japan.
[Herrera, Beatriz; Stremme, Wolfgang; Grutter, Michel] Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City, DF, Mexico.
[Schaap, Martijn] TNO Built Environm & Geosci, Dept Air Qual & Climate, Utrecht, Netherlands.
[Kruit, Roy J. Wichink] Natl Inst Publ Hlth & Environm RIVM, Bilthoven, Netherlands.
[Erisman, Jan Willem] Louis Bolk Inst, Driebergen, Netherlands.
RP Dammers, E (reprint author), Vrije Univ Amsterdam, Dept Earth Sci, Cluster Earth & Climate, Amsterdam, Netherlands.
EM e.dammers@vu.nl
RI Morino, Isamu/K-1033-2014; Notholt, Justus/P-4520-2016
OI Morino, Isamu/0000-0003-2720-1569; Notholt, Justus/0000-0002-3324-885X
FU Netherlands Organisation for Scientific Research (NWO) [GO/12-36]; New
Zealand government's core research grant framework from the Ministry of
Business, Innovation and Employment; CNRS [LACy-UMR8105, UMS3365];
CAFTON project - Canadian Space Agency's FAST programme; NASA; Belgian
Science Policy Office through the IASI Flow Prodex arrangement;
FRS-FNRS; CNES; National Science Foundation; Atmospheric Chemistry
Observations & Modeling Division of NCAR; Australian Research Council
[DP110101948, LE0668470]; UNAM-DGAPA [109914]; CONACYT [249374, 239618]
FX This work is part of the research programme GO/12-36, which is financed
by the Netherlands Organisation for Scientific Research (NWO). The
Lauder NIWA FTIR programme is funded through the New Zealand
government's core research grant framework from the Ministry of
Business, Innovation and Employment. We thank the Lauder FTIR team for
their contribution. We acknowledge the Universite de La Reunion and CNRS
(LACy-UMR8105 and UMS3365) for their support of the Reunion Island
measurements. The Reunion Island data analysis has mainly been supported
by the A3C project (PRODEX Programme of the Belgian Science Policy
Office, BELSPO, Brussels). The University of Toronto's NDACC
contribution has been supported by the CAFTON project, funded by the
Canadian Space Agency's FAST programme. Measurements were made at the
University of Toronto Atmospheric Observatory (TAO), which has been
supported by CF-CAS, ABB Bomem, CFI, CSA, EC, NSERC, ORDCF, PREA, and
the University of Toronto. Part of this research was performed at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. IASI has been developed and built under the
responsibility of the "Centre national d'etudes spatiales" (CNES,
France). It is flown on-board the Metop satellites as part of the
EU-METSAT Polar System. The IASI L1 data were received through the
EUMETCast near-real-time data distribution service.; The IASI-related
activities in Belgium were funded by Belgian Science Policy Office
through the IASI Flow Prodex arrangement (2014-2018). Pierre.-F. Coheur,
Lieven Clarisse, and Martin Van Damme also thank the FRS-FNRS for
financial support. Lieven Clarisse is a research associate with the
Belgian F.R.S-FNRS. Cathy Clerbaux is grateful to CNES for scientific
collaboration and financial support. The National Center for Atmospheric
Research is supported by the National Science Foundation. The Boulder
observation programme is supported in part by the Atmospheric Chemistry
Observations & Modeling Division of NCAR. The measurement programme and
NDACC site at Wollongong have been supported by the Australian Research
Council for many years, most recently by grants DP110101948 and
LE0668470. The Mexico City site was funded through projects UNAM-DGAPA
(109914) and CONACYT (249374, 239618). A. Bezanilla, J. Baylon, and E.
Plaza are acknowledged for their participation in the measurements and
analysis. We would like to thank David Griffith, Clare Murphy, and
Voltaire Velazco at the School of Chemistry, University of Wollongong,
for maintaining Fourier transform spectroscopy (FTS) instrumentation and
conducting FTS measurements. We are grateful to the many colleagues who
have contributed to FTIR data acquisition at the various sites.
NR 72
TC 2
Z9 2
U1 11
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 16
PY 2016
VL 16
IS 16
BP 10351
EP 10368
DI 10.5194/acp-16-10351-2016
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV8PJ
UT WOS:000383198600003
ER
PT J
AU Smith, DD
Luckay, HA
Chang, H
Myneni, K
AF Smith, David D.
Luckay, H. A.
Chang, Hongrok
Myneni, Krishna
TI Quantum-noise-limited sensitivity enhancement of a passive optical
cavity by a fast-light medium
SO PHYSICAL REVIEW A
LA English
DT Article
ID GRAVITATIONAL-WAVE DETECTORS; RING-RESONATOR; INTERFEROMETERS
AB We demonstrate that for a passive optical cavity containing a dispersive atomic medium, the increase in scale factor near the critical anomalous dispersion is not canceled by mode broadening or attenuation, resulting in an overall increase in the predicted quantum-noise-limited sensitivity. Enhancements of over two orders of magnitude are measured in the scale factor, which translates to greater than an order-of-magnitude enhancement in the predicted quantum-noise-limited measurement precision, by temperature-tuning a low-pressure vapor of noninteracting atoms in a low-finesse cavity close to the critical anomalous dispersion condition. The predicted enhancement in sensitivity is confirmed through Monte Carlo numerical simulations.
C1 [Smith, David D.] NASA, Marshall Space Flight Ctr, Space Syst Dept, ES34, Huntsville, AL 35812 USA.
[Luckay, H. A.] Torch Technol, 4035 Chris Dr,Suite C, Huntsville, AL 35802 USA.
[Chang, Hongrok] Gen Atom Electromagnet Syst, 678 Discovery Dr, Huntsville, AL 35806 USA.
[Myneni, Krishna] US Army, Aviat & Missile Res Dev & Engn Ctr, RDMR WDS MRI, Redstone Arsenal, AL 35898 USA.
RP Smith, DD (reprint author), NASA, Marshall Space Flight Ctr, Space Syst Dept, ES34, Huntsville, AL 35812 USA.
EM david.d.smith@nasa.gov
FU NASA Space Technology Mission Directorate Game Changing Development
Office; U.S. Army Aviation and Missile Research Development and
Engineering Center (AMRDEC) Missile ST Program
FX This work was sponsored by the NASA Space Technology Mission Directorate
Game Changing Development Office as well as the U.S. Army Aviation and
Missile Research Development and Engineering Center (AMRDEC) Missile S&T
Program. H. A. Luckay was affiliated with Jacobs ESSSA Group, Jacobs
Technology Inc., while performing the majority of this work.
NR 25
TC 0
Z9 0
U1 4
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD AUG 16
PY 2016
VL 94
IS 2
AR 023828
DI 10.1103/PhysRevA.94.023828
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DT4TE
UT WOS:000381473100002
ER
PT J
AU Field, RD
van der Werf, GR
Fanin, T
Fetzer, EJ
Fuller, R
Jethva, H
Levy, R
Livesey, NJ
Luo, M
Torres, O
Worden, HM
AF Field, Robert D.
van der Werf, Guido R.
Fanin, Thierry
Fetzer, Eric J.
Fuller, Ryan
Jethva, Hiren
Levy, Robert
Livesey, Nathaniel J.
Luo, Ming
Torres, Omar
Worden, Helen M.
TI Indonesian fire activity and smoke pollution in 2015 show persistent
nonlinear sensitivity to El Nino-induced drought
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Indonesia; biomass burning; haze; pollution; El Nino
ID SOUTHEAST-ASIA; FOREST-FIRES; PEAT FIRES; TROPOSPHERIC OZONE; TROPICAL
PEATLANDS; AEROSOL PRODUCTS; EMISSIONS; MODIS; KALIMANTAN; LAND
AB The 2015 fire season and related smoke pollution in Indonesia was more severe than the major 2006 episode, making it the most severe season observed by the NASA Earth Observing System satellites that go back to the early 2000s, namely active fire detections from the Terra and Aqua Moderate Resolution Imaging Spectroradiometers (MODIS), MODIS aerosol optical depth, Terra Measurement of Pollution in the Troposphere (MOPITT) carbon monoxide (CO), Aqua Atmospheric Infrared Sounder (AIRS) CO, Aura Ozone Monitoring Instrument (OMI) aerosol index, and Aura Microwave Limb Sounder (MLS) CO. The MLS CO in the upper troposphere showed a plume of pollution stretching from East Africa to the western Pacific Ocean that persisted for 2 mo. Longer-term records of airport visibility in Sumatra and Kalimantan show that 2015 ranked after 1997 and alongside 1991 and 1994 as among the worst episodes on record. Analysis of yearly dry season rainfall from the Tropical Rainfall Measurement Mission (TRMM) and rain gauges shows that, due to the continued use of fire to clear and prepare land on degraded peat, the Indonesian fire environment continues to have nonlinear sensitivity to dry conditions during prolonged periods with less than 4 mm/d of precipitation, and this sensitivity appears to have increased over Kalimantan. Without significant reforms in land use and the adoption of early warning triggers tied to precipitation forecasts, these intense fire episodes will reoccur during future droughts, usually associated with El Nino events.
C1 [Field, Robert D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[van der Werf, Guido R.; Fanin, Thierry] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands.
[Fetzer, Eric J.; Fuller, Ryan; Livesey, Nathaniel J.; Luo, Ming] CALTECH, Jet Prop Lab, Earth Sci Sect, Pasadena, CA 91109 USA.
[Jethva, Hiren; Levy, Robert; Torres, Omar] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jethva, Hiren] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[Worden, Helen M.] Natl Ctr Atmospher Res, Boulder, CO 80301 USA.
RP Field, RD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Field, RD (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
EM robert.field@columbia.edu
RI Levy, Robert/M-7764-2013
OI Levy, Robert/0000-0002-8933-5303
FU NASA Earth Observing System Program; National Science Foundation; NASA
Atmospheric Chemistry Modeling and Analysis Program; European Research
Council; NASA High-End Computing Program through the NASA Center for
Climate Simulation at Goddard Space Flight Center
FX The MODIS, MOPITT, AIRS, MLS, and OMI projects are supported by the NASA
Earth Observing System Program. The National Center for Atmospheric
Research is sponsored by the National Science Foundation. R.D.F. was
supported by the NASA Atmospheric Chemistry Modeling and Analysis
Program and the NASA Precipitation Measurement Missions Science Team,
and G.R.v.d.W. and T.F. were supported by the European Research Council.
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. 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. AIRS CO,
MODIS AOD, and TRMM precipitation data were obtained from the NASA
Giovanni system. All data in the study can be obtained by contacting the
lead author.
NR 50
TC 3
Z9 3
U1 34
U2 37
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 16
PY 2016
VL 113
IS 33
BP 9204
EP 9209
DI 10.1073/pnas.1524888113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DT3RS
UT WOS:000381399200042
PM 27482096
ER
PT J
AU Rothschild, LJ
AF Rothschild, Lynn J.
TI Synthetic biology meets bioprinting: enabling technologies for humans on
Mars (and Earth)
SO BIOCHEMICAL SOCIETY TRANSACTIONS
LA English
DT Article
DE applied microbiology; biological materials; human exploration; synthetic
biology
ID HIERARCHICAL STRUCTURE
AB Human exploration off planet is severely limited by the cost of launching materials into space and by resupply. Thus materials brought from Earth must be light, stable and reliable at destination. Using traditional approaches, a lunar or Mars base would require either transporting a hefty store of metals or heavy manufacturing equipment and construction materials for in situ extraction; both would severely limit any other mission objectives. Long-term human space presence requires periodic replenishment, adding a massive cost overhead. Even robotic missions often sacrifice science goals for heavy radiation and thermal protection. Biology has the potential to solve these problems because life can replicate and repair itself, and perform a wide variety of chemical reactions including making food, fuel and materials. Synthetic biology enhances and expands life's evolved repertoire. Using organisms as feedstock, additive manufacturing through bioprinting will make possible the dream of producing bespoke tools, food, smart fabrics and even replacement organs on demand. This new approach and the resulting novel products will enable human exploration and settlement on Mars, while providing new manufacturing approaches for life on Earth.
C1 [Rothschild, Lynn J.] NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
RP Rothschild, LJ (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM Lynn.J.Rothschild@nasa.gov
FU NASA Ames Research Center Director's Discretionary fund; NASA
Headquarters; Brown University; Stanford University; Rhode Island Space
[NASA] [NNX10A195H, NNX15AI06H]; Center Innovation Fund; NASA Innovative
Advanced Concepts programs; NASA's Advanced Exploration Systems program
FX This work was supported by the NASA Ames Research Center Director's
Discretionary fund; NASA Headquarters; Brown University; the Stanford
University; the Rhode Island Space [NASA Grant NNX10A195H, NASA Grant
NNX15AI06H]; the Center Innovation Fund; the NASA Innovative Advanced
Concepts programs; and the NASA's Advanced Exploration Systems program.
NR 13
TC 0
Z9 0
U1 2
U2 3
PU PORTLAND PRESS LTD
PI LONDON
PA CHARLES DARWIN HOUSE, 12 ROGER STREET, LONDON WC1N 2JU, ENGLAND
SN 0300-5127
EI 1470-8752
J9 BIOCHEM SOC T
JI Biochem. Soc. Trans.
PD AUG 15
PY 2016
VL 44
BP 1158
EP 1164
DI 10.1042/BST20160067
PN 4
PG 7
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA EI8BC
UT WOS:000392728300024
PM 27528764
ER
PT J
AU Radebaugh, J
Lopes, RM
Howell, RR
Lorenz, RD
Turtle, EP
AF Radebaugh, Jani
Lopes, Rosaly M.
Howell, Robert R.
Lorenz, Ralph D.
Turtle, Elizabeth P.
TI Eruptive behavior of the Marum/Mbwelesu lava lake, Vanuatu and
comparisons with lava lakes on Earth and Io
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Marum; Lava lake; Thermal camera; Camcorder; Near-infrared; Remote
sensing
ID VOLCANIC ACTIVITY; WATER-VAPOR; TEMPERATURE-MEASUREMENTS; ACTIVE
VOLCANISM; GALILEO NIMS; ASO VOLCANO; ISLAND-ARC; MOON IO; PELE;
INSTRUMENT
AB Observations from field remote sensing of the morphology, kinematics and temperature of the Marum/Mbwelesu lava lake in the Vanuatu archipelago in 2014 reveal a highly active, vigorously erupting lava lake. Active degassing and fountaining observed at the similar to 50 m lava lake led to large areas of fully exposed lavas and rapid (similar to 5 m/s) movement of lava from the centers of upwelling outwards to the lake margins. These rapid lava speeds precluded the formation of thick crust; there was never more than 30% non-translucent crust. The lava lake was observed with several portable, handheld, low-cost, near-infrared imagers, all of which measured temperatures near 1000 degrees C and one as high as 1022 degrees C, consistent with basaltic temperatures. Fine-scale structure in the lava fountains and cooled crust was visible in the near infrared at similar to 5 cm/pixel from 300 m above the lake surface. The temperature distribution across the lake surface is much broader than at more quiescent lava lakes, peaking similar to 850 degrees C, and is attributed to the highly exposed nature of the rapidly circulating lake. This lava lake has many characteristics in common with other active lava lakes, such as Erta Ale in Ethiopia, being confined, persistent and high-temperature; however it was much more active than is typical for Erta Ale, which often has >90% crust. Furthermore, it is a good analogue for the persistent, high-temperature lava lakes contained within volcanic depressions on Jupiter's moon Io, such as Pele, also believed from spacecraft and ground-based observations to exhibit similar behavior of gas emission, rapid overturn and fountaining. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, S-389 ESC, Provo, UT 84602 USA.
[Lopes, Rosaly M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Howell, Robert R.] Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA.
[Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Radebaugh, J (reprint author), Brigham Young Univ, S-389 ESC, Provo, UT 84602 USA.
EM janirad@byu.edu; rosaly.m.lopes@jpl.nasa.gov; rhowell@uwyo.edu;
ralph.lorenz@jhuapl.edu; elizabeth.turtle@jhuapl.edu
RI Lopes, Rosaly/D-1608-2016
OI Lopes, Rosaly/0000-0002-7928-3167
FU Brazil's Globo TV; Brigham Young University College of Physical and
Mathematical Sciences; Brigham Young University Department of Geological
Sciences
FX We would like to thank Brazil's Globo TV (Planeta Extremo series) for
their support of this research and field study, and Pascal Guillet at
Vanuatu Ecotours for local arrangements and field support. We thank
Brigham Young University's College of Physical and Mathematical Sciences
and Department of Geological Sciences for funding and field support. We
thank John Turtle for support of the Canon camera procurement, and
technical support at Canon USA for advice on aspects of the camera
function. Part of this work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
NR 69
TC 0
Z9 0
U1 3
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD AUG 15
PY 2016
VL 322
SI SI
BP 105
EP 118
DI 10.1016/j.jvolgeores.2016.03.019
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA EB2MJ
UT WOS:000387196200008
ER
PT J
AU Turtle, EP
Lopes, RMC
Lorenz, RD
Radebaugh, J
Howell, RR
AF Turtle, E. P.
Lopes, R. M. C.
Lorenz, R. D.
Radebaugh, J.
Howell, R. R.
TI Temporal behavior and temperatures of Yasur volcano, Vanuatu from field
remote sensing observations, May 2014
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Yasur; Vanuatu; Stratovolcano; Strombolian eruption; MODIS radiance
ID STROMBOLIAN EXPLOSIONS; FLUX
AB We documented eruption activity at three primary vents at Yasur volcano, Tanna Island, Vanuatu using portable instrumentation in the field over a period of 5 h on 21 May 2014, and acquired aerial images of the craters and vents on 22 May 2014. Although limited in duration, our observations of eruption intervals, durations, temperatures, and speeds of ejected material illustrate the characteristics of the activity at the time at each of the primary vents, providing a useful snapshot of eruption behavior and revealing continued variability at Yasur in comparison to other observation campaigns. Hand-held, high-resolution, near-infrared observations of one of the vents gave peak temperatures of 850 degrees C to 930 degrees C for ejected clasts, with a maximum temperature of 1033 degrees C. These temperatures are significantly higher than previous measurements because exposed lavas could be resolved at timescales less than a second. Our aerial near-infrared images allowed us to estimate the combined area of the active vents within the crater to be similar to 150 m(2), and comparison to MODIS radiance measurements in the same time frame yields temperatures, averaged over the combined vent area, of 530-730 degrees C. In the context of previous observations at Yasur, the activity in May 2014 exhibited lower overall intensity, as well as differences in the nature of the eruptions at the various vents, providing insight regarding the temporal variability of Yasur's activity. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Turtle, E. P.; Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, 11,100 Johns Hopkins Rd, Laurel, MD 20723 USA.
[Lopes, R. M. C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Radebaugh, J.] Brigham Young Univ, Dept Geol Sci, S-389 ESC, Provo, UT 84602 USA.
[Howell, R. R.] Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA.
RP Turtle, EP (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11,100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM elizabeth.turtle@jhuapl.edu; rosaly.m.lopes@jptnasa.gov;
ralph.lorenz@jhuapl.edu; janirad@byu.edu; rhowell@uwyo.edu
RI Lopes, Rosaly/D-1608-2016
OI Lopes, Rosaly/0000-0002-7928-3167
NR 20
TC 2
Z9 2
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD AUG 15
PY 2016
VL 322
SI SI
BP 158
EP 167
DI 10.1016/j.jvolgeores.2016.02.030
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA EB2MJ
UT WOS:000387196200011
ER
PT J
AU Lorenz, RD
Turtle, EP
Howell, R
Radebaugh, J
Lopes, RMC
AF Lorenz, Ralph D.
Turtle, Elizabeth P.
Howell, Robert
Radebaugh, Jani
Lopes, Rosaly M. C.
TI The roar of Yasur: Handheld audio recorder monitoring of Vanuatu
volcanic vent activity
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Yasur; Vanuatu; Acoustic; Data analysis; Periodicity
ID ACOUSTIC MEASUREMENTS; SHISHALDIN VOLCANO; INFRASOUND; VELOCITY; ALASKA;
JETS
AB We describe how near-field audio recording using a pocket digital sound recorder can usefully document volcanic activity, demonstrating the approach at Yasur, Vanuatu in May 2014. Prominent emissions peak at 263 Hz, interpreted as an organ-pipe mode. High-pass filtering was found to usefully discriminate volcano vent noise from wind noise, and autocorrelation of the high pass acoustic power reveals a prominent peak in exhalation intervals of similar to 2.5,4 and 8 s, with a number of larger explosive events at similar to 200 s intervals. We suggest that this compact and inexpensive audio instrumentation can usefully supplement other field monitoring such as seismic or infrasound. A simple estimate of acoustic power interpreted with a dipole jet noise model yielded vent velocities too low to be compatible with pyroclast emission, suggesting difficulties with this approach at audio frequencies (perhaps due to acoustic absorption by volcanic gases). (C) 2015 Elsevier B.V. All rights reserved.
C1 [Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
[Howell, Robert] Univ Wyoming, Laramie, WY 82071 USA.
[Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Lopes, Rosaly M. C.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Ralph.lorenz@jhuapl.edu
RI Lopes, Rosaly/D-1608-2016
OI Lopes, Rosaly/0000-0002-7928-3167
NR 21
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD AUG 15
PY 2016
VL 322
SI SI
BP 168
EP 174
DI 10.1016/j.jvolgeores.2015.06.019
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EB2MJ
UT WOS:000387196200012
ER
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Zuraw, S. E.
Zweizig, J.
CA LIGO Sci Collaboration
Virgo Collaboration
TI Comprehensive all-sky search for periodic gravitational waves in the
sixth science run LIGO data
SO PHYSICAL REVIEW D
LA English
DT Article
AB We report on a comprehensive all-sky search for periodic gravitational waves in the frequency band 100-1500 Hz and with a frequency time derivative in the range of [-1.18; +1.00] x 10(-8) Hz/s. Such a signal could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our galaxy. This search uses the data from the initial LIGO sixth science run and covers a larger parameter space with respect to any past search. A Loosely Coherent detection pipeline was applied to follow up weak outliers in both Gaussian (95% recovery rate) and non-Gaussian (75% recovery rate) bands. No gravitational wave signals were observed, and upper limits were placed on their strength. Our smallest upper limit on worst-case (linearly polarized) strain amplitude h(0) is 9.7 x 10(-25) near 169 Hz, while at the high end of our frequency range we achieve a worst-case upper limit of 5.5 x 10(-24). Both cases refer to all sky locations and entire range of frequency derivative values.
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[Cominsky, L.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Coughlin, S. B.; Kalogera, V.; Klein, B.; Miller, B. B.; Pankow, C.; Perri, L. M.; Sandeen, B.; Shahriar, M. S.; Yablon, J.; Zevin, M.; Zhou, M.; Zhou, Z.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA.
[Crowder, S. G.; Mandic, V.; Meyers, P. M.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Darman, N. S.; Melatos, A.; Sun, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Dasgupta, A.; Gaur, G.; Gupta, A.; Khan, Z.; Kumar, R.; Srivastava, A. K.; Sunil, S.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Daw, E. J.; Edo, T. B.; Kennedy, R.; Tomlinson, C.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Creighton, T.; Diaz, M. C.; Geng, P.; Key, J. S.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Torres, C. V.; Tuyenbayev, D.; Valdes, G.] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA.
[Di Giovanni, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Di Giovanni, M.; Leonardi, M.; Prodi, G. A.; Tiwari, S.; Tringali, M. C.] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy.
[Everett, R.; Hanna, C.; Meacher, D.; Messick, C.] Penn State Univ, University Pk, PA 16802 USA.
[Fairhurst, S.; Fays, M.; Hannam, M. D.; Hopkins, P.; Kalaghatgi, C. V.; Khan, S.; London, L. T.; Muir, A. W.; Ohme, F.; Pannarale, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Tiwari, V.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Favata, M.; Moore, B. C.] Montclair State Univ, Montclair, NJ 07043 USA.
[Fenyvesi, E.; Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Flaminio, R.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Gair, J. R.] Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland.
[Gaur, G.; Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary.
[Gill, K.; Hughey, B.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Grado, A.] Osserv Astron Capodimonte, Ist Nazl Fis Nucl, I-80131 Naples, Italy.
[Gustafson, R.; Neunzert, A.; Riles, K.; Sauter, O. E. S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Henry, J.; Lange, J.; O'Shaughnessy, R.; Rizzo, M.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Huerta, E. A.] Univ Illinois, NCSA, Urbana, IL 61801 USA.
[Husa, S.; Jimenez-Forteza, F.; Keitel, D.; Oliver, M.; Sintes, A. M.] Univ Illes Balears, IAC3 IEEC, E-07122 Palma de Mallorca, Spain.
[Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland.
[Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[Kehl, M. S.; Kumar, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 136791, South Korea.
[Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Lasky, P. D.; Levin, Y.; Qiu, S.; Sammut, L.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Li, T. G. F.] Chinese Univ Hong Kong, Shatin, Hong Kong, Peoples R China.
[Littenberg, T. B.] Univ Alabama, Huntsville, AL 35899 USA.
[Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA.
[Loriette, V.; Maksimovic, I.] ESPCI, CNRS, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP, South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil.
[Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea.
[Pedurand, R.] Univ Lyon, F-69361 Lyon, France.
[Penn, S.] Hobart & William Smith Colleges, Geneva, NY 14456 USA.
[Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland.
[Sakellariadou, M.] Univ London, Kings Coll London, London WC2R 2LS, England.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Trozzo, L.] Univ Siena, I-53100 Siena, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Ciani,
Giacomo/G-1036-2011; Sigg, Daniel/I-4308-2015; Di Virgilio, Angela Dora
Vittoria/E-9078-2015; Garufi, Fabio/K-3263-2015; Sergeev,
Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Tiwari,
Shubhanshu/R-8546-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; prodi,
giovanni/B-4398-2010; Leonardi, Matteo/G-9694-2015; Ferrante,
Isidoro/F-1017-2012; Cesarini, Elisabetta/C-4507-2017; Danilishin,
Stefan/K-7262-2012; Hild, Stefan/A-3864-2010; Steinlechner,
Sebastian/D-5781-2013; Chow, Jong/A-3183-2008; Frey,
Raymond/E-2830-2016; Iyer, Bala R./E-2894-2012; Bell, Angus/E-7312-2011;
Strain, Kenneth/D-5236-2011; Sorrentino, Fiodor/M-6662-2016; Travasso,
Flavio/J-9595-2016; Marchesoni, Fabio/A-1920-2008; Vecchio,
Alberto/F-8310-2015; Rocchi, Alessio/O-9499-2015; Gemme,
Gianluca/C-7233-2008; Strigin, Sergey/I-8337-2012; McClelland,
David/E-6765-2010; Costa, Cesar/G-7588-2012; Losurdo,
Giovanni/K-1241-2014
OI Nelemans, Gijs/0000-0002-0752-2974; Nitz, Alexander/0000-0002-1850-4587;
Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X;
Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628;
Del Pozzo, Walter/0000-0003-3978-2030; Granata,
Massimo/0000-0003-3275-1186; Berry, Christopher/0000-0003-3870-7215;
Piccinni, Ornella Juliana/0000-0001-5478-3950; Kanner,
Jonah/0000-0001-8115-0577; Gammaitoni, Luca/0000-0002-4972-7062; Ciani,
Giacomo/0000-0003-4258-9338; Sigg, Daniel/0000-0003-4606-6526; Di
Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Garufi,
Fabio/0000-0003-1391-6168; Callister, Thomas/0000-0001-9892-177X; Bondu,
Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Tiwari,
Shubhanshu/0000-0003-1611-6625; Punturo, Michele/0000-0001-8722-4485;
Cella, Giancarlo/0000-0002-0752-0338; prodi,
giovanni/0000-0001-5256-915X; Ferrante, Isidoro/0000-0002-0083-7228;
Cesarini, Elisabetta/0000-0001-9127-3167; Danilishin,
Stefan/0000-0001-7758-7493; Steinlechner, Sebastian/0000-0003-4710-8548;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Iyer,
Bala R./0000-0002-4141-5179; Bell, Angus/0000-0003-1523-0821; Strain,
Kenneth/0000-0002-2066-5355; Sorrentino, Fiodor/0000-0002-9605-9829;
Travasso, Flavio/0000-0002-4653-6156; Marchesoni,
Fabio/0000-0001-9240-6793; Vecchio, Alberto/0000-0002-6254-1617; Rocchi,
Alessio/0000-0002-1382-9016; Gemme, Gianluca/0000-0002-1127-7406;
McClelland, David/0000-0001-6210-5842; Losurdo,
Giovanni/0000-0003-0452-746X
FU EGO consortium; Council of Scientific and Industrial Research of India;
Department of Science and Technology, India; Science & Engineering
Research Board (SERB), India; Ministry of Human Resource Development,
India; Spanish Ministerio de Economia y Competitividad; Conselleria
d'Economia i Competitivitat of the Govern de les Illes Balears;
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears; National Science Centre of Poland; European Commission;
Royal Society; Scottish Funding Council; Scottish Universities Physics
Alliance; Hungarian Scientific Research Fund (OTKA); Lyon Institute of
Origins (LIO); National Research Foundation of Korea through the
Ministry of Economic Development and Innovation; Industry Canada through
the Ministry of Economic Development and Innovation; Province of Ontario
through the Ministry of Economic Development and Innovation; Natural
Science and Engineering Research Council Canada; Canadian Institute for
Advanced Research; Brazilian Ministry of Science, Technology, and
Innovation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo
(FAPESP); Russian Foundation for Basic Research; Leverhulme Trust;
Research Corporation; Ministry of Science and Technology (MOST), Taiwan;
Kavli Foundation
FX The authors gratefully acknowledge the support of the U. S. National
Science Foundation (NSF) for the construction and operation of the LIGO
Laboratory and Advanced LIGO as well as the Science and Technology
Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society
(MPS), and the State of Niedersachsen/Germany for support of the
construction of Advanced LIGO and construction and operation of the
GEO600 detector. Additional support for Advanced LIGO was provided by
the Australian Research Council. The authors gratefully acknowledge the
Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre
National de la Recherche Scientifique (CNRS) and the Foundation for
Fundamental Research on Matter supported by the Netherlands Organisation
for Scientific Research, for the construction and operation of the Virgo
detector and the creation and support of the EGO consortium. The authors
also gratefully acknowledge research support from these agencies as well
as by the Council of Scientific and Industrial Research of India,
Department of Science and Technology, India, Science & Engineering
Research Board (SERB), India, Ministry of Human Resource Development,
India, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia i Competitivitat and Conselleria d'Educacio,
Cultura i Universitats of the Govern de les Illes Balears, the National
Science Centre of Poland, the European Commission, the Royal Society,
the Scottish Funding Council, the Scottish Universities Physics
Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon
Institute of Origins (LIO), the National Research Foundation of Korea,
Industry Canada and the Province of Ontario through the Ministry of
Economic Development and Innovation, the Natural Science and Engineering
Research Council Canada, Canadian Institute for Advanced Research, the
Brazilian Ministry of Science, Technology, and Innovation, Fundacao de
Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Russian Foundation
for Basic Research, the Leverhulme Trust, the Research Corporation,
Ministry of Science and Technology (MOST), Taiwan and the Kavli
Foundation. The authors gratefully acknowledge the support of the NSF,
STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for
provision of computational resources.
NR 25
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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 AUG 15
PY 2016
VL 94
IS 4
AR 042002
DI 10.1103/PhysRevD.94.042002
PG 14
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DT4ZW
UT WOS:000381491300001
ER
PT J
AU Venumadhav, T
Cyr-Racine, FY
Abazajian, KN
Hirata, CM
AF Venumadhav, Tejaswi
Cyr-Racine, Francis-Yan
Abazajian, Kevork N.
Hirata, Christopher M.
TI Sterile neutrino dark matter: Weak interactions in the strong coupling
epoch
SO PHYSICAL REVIEW D
LA English
DT Article
ID MILKY-WAY SATELLITES; 3.5 KEV LINE; X-RAY; EXPANDING UNIVERSE; MASSIVE
NEUTRINOS; FINITE-TEMPERATURE; GALAXY CLUSTERS; QCD; MODELS; QUARK
AB We perform a detailed study of the weak interactions of standard model neutrinos with the primordial plasma and their effect on the resonant production of sterile neutrino dark matter. Motivated by issues in cosmological structure formation on small scales, and reported x-ray signals that could be due to sterile neutrino decay, we consider 7 keV-scale sterile neutrinos. Oscillation-driven production of such sterile neutrinos occurs at temperatures T greater than or similar to 100 MeV, where we study two significant effects of weakly charged species in the primordial plasma: (1) the redistribution of an input lepton asymmetry; (2) the opacity for active neutrinos. We calculate the redistribution analytically above and below the quark-hadron transition, and match with lattice QCD calculations through the transition. We estimate opacities due to tree-level processes involving leptons and quarks above the quark-hadron transition, and the most important mesons below the transition. We report final sterile neutrino dark matter phase space densities that are significantly influenced by these effects, and yet relatively robust to remaining uncertainties in the nature of the quark-hadron transition. We also provide transfer functions for cosmological density fluctuations with cutoffs at k similar or equal to 10h Mpc(-1), that are relevant to galactic structure formation.
C1 [Venumadhav, Tejaswi; Cyr-Racine, Francis-Yan] CALTECH, Mail Code 350-17, Pasadena, CA 91125 USA.
[Cyr-Racine, Francis-Yan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Abazajian, Kevork N.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Hirata, Christopher M.] Ohio State Univ, CCAPP, 191 West Woodruff Lane, Columbus, OH 43210 USA.
[Venumadhav, Tejaswi] Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA.
[Cyr-Racine, Francis-Yan] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Venumadhav, T (reprint author), CALTECH, Mail Code 350-17, Pasadena, CA 91125 USA.; Venumadhav, T (reprint author), Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA.
FU David and Lucile Packard Foundation; Simons Foundation; U.S. Department
of Energy; W. M. Keck Foundation; NSF CAREER Grant [PHY-1159224]; NSF
Grant [PHY-1316792]; Institute for Nuclear Theory program "Neutrino
Astrophysics and Fundamental Properties" [15-2a]
FX We thank Olivier Dore and Roland de Putter for fruitful discussions. We
are grateful to Mikko Laine for providing us the data for the plasma's
equation of state. T. V. and C. M. H. are supported by the David and
Lucile Packard Foundation, the Simons Foundation, and the U.S.
Department of Energy. The work of F.-Y. C.-R. was performed in part at
the California Institute of Technology for the Keck Institute for Space
Studies, which is funded by the W. M. Keck Foundation. Part of the
research described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration (NASA). K. N. A. is
partially supported by NSF CAREER Grant No. PHY-1159224 and NSF Grant
No. PHY-1316792. K. N. A. acknowledges support from the Institute for
Nuclear Theory program "Neutrino Astrophysics and Fundamental
Properties" 15-2a where part of this work was done.
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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 AUG 15
PY 2016
VL 94
IS 4
AR 043515
DI 10.1103/PhysRevD.94.043515
PG 28
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DT4ZW
UT WOS:000381491300002
ER
PT J
AU Heldmann, JL
Colaprete, A
Elphic, RC
Lim, D
Deans, M
Cook, A
Roush, T
Skok, JR
Button, NE
Karunatillake, S
Stoker, C
Marquez, JJ
Shirley, M
Kobayashi, L
Lees, D
Bresina, J
Hunt, R
AF Heldmann, Jennifer L.
Colaprete, Anthony
Elphic, Richard C.
Lim, Darlene
Deans, Matthew
Cook, Amanda
Roush, Ted
Skok, J. R.
Button, Nicole E.
Karunatillake, S.
Stoker, Carol
Marquez, Jessica J.
Shirley, Mark
Kobayashi, Linda
Lees, David
Bresina, John
Hunt, Rusty
TI Lunar polar rover science operations: Lessons learned and mission
architecture implications derived from the Mojave Volatiles Prospector
(MVP) terrestrial field campaign
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Moon; Volatiles; Rover; Missions
ID CALIFORNIA; NEUTRON; SURFACE; DESERT; WATER; MOON
AB The Mojave Volatiles Prospector (MVP) project is a science-driven field program with the goal of producing critical knowledge for conducting robotic exploration of the Moon. Specifically, MVP focuses on studying a lunar mission analog to characterize the form and distribution of lunar volatiles. Although lunar volatiles are known to be present near the poles of the Moon, the three dimensional distribution and physical characteristics of lunar polar volatiles are largely unknown. A landed mission with the ability to traverse the lunar surface is thus required to characterize the spatial distribution of lunar polar volatiles. NASA's Resource Prospector (RP) mission is a lunar polar rover mission that will operate primarily in sunlit regions near a lunar pole with near-real time operations to characterize the vertical and horizontal distribution of volatiles. The MVP project was conducted as a field campaign relevant to the RP lunar mission to provide science, payload, and operational lessons learned to the development of a real-time, short-duration lunar polar volatiles prospecting mission. To achieve these goals, the MVP project conducted a simulated lunar rover mission to investigate the composition and distribution of surface and subsurface volatiles in a natural environment with an unknown volatile distribution within the Mojave Desert, improving our understanding of how to find, characterize, and access volatiles on the Moon. (C) 2016 Published by Elsevier Ltd on behalf of COSPAR.
C1 [Heldmann, Jennifer L.; Colaprete, Anthony; Elphic, Richard C.; Lim, Darlene; Deans, Matthew; Cook, Amanda; Roush, Ted; Stoker, Carol; Marquez, Jessica J.; Shirley, Mark; Kobayashi, Linda; Lees, David; Bresina, John; Hunt, Rusty] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lim, Darlene] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Skok, J. R.; Button, Nicole E.; Karunatillake, S.] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA.
RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94305 USA.
EM Jennifer.Heldmann@nasa.gov
RI Karunatillake, Suniti/A-5934-2009
OI Karunatillake, Suniti/0000-0001-9891-1432
FU NASA's Science Mission Directorate's MMAMA (Moon Mars Analog Mission
Activities) program; SSERVI (Solar System Exploration Research Virtual
Institute); NASA's Human Exploration and Operations Mission
Directorate's Advanced Exploration Systems (AES)
FX The MVP team acknowledges support from NASA's Science Mission
Directorate's MMAMA (Moon Mars Analog Mission Activities) program and
SSERVI (Solar System Exploration Research Virtual Institute) as well as
NASA's Human Exploration and Operations Mission Directorate's Advanced
Exploration Systems (AES).
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD AUG 15
PY 2016
VL 58
IS 4
BP 545
EP 559
DI 10.1016/j.asr.2016.05.011
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DS1WY
UT WOS:000380417000008
ER
PT J
AU Zheng, XY
Beard, BL
Reddy, TR
Roden, EE
Johnson, CM
AF Zheng, Xin-Yuan
Beard, Brian L.
Reddy, Thiruchelvi R.
Roden, Eric E.
Johnson, Clark M.
TI Abiologic silicon isotope fractionation between aqueous Si and
Fe(III)-Si gel in simulated Archean seawater: Implications for Si
isotope records in Precambrian sedimentary rocks
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Si isotopes; Fe-Si system; Fractionation factor; Precambrian; BIFs;
Chert
ID BANDED IRON FORMATIONS; MULTI-DIRECTION APPROACH; STABLE-ISOTOPES; ATOM
EXCHANGE; FE(II)-FE(III) ELECTRON; CRYSTAL-CHEMISTRY; AMORPHOUS SILICA;
OXIDE REDUCTION; LOW-TEMPERATURE; WEST GREENLAND
AB Precambrian Si-rich sedimentary rocks, including cherts and banded iron formations (BIFs), record a >7% spread in Si-30/Si-28 ratios (delta Si-30 values), yet interpretation of this large variability has been hindered by the paucity of data on Si isotope exchange kinetics and equilibrium fractionation factors in systems that are pertinent to Precambrian marine conditions. Using the three-isotope method and an enriched Si-29 tracer, a series of experiments were conducted to constrain Si isotope exchange kinetics and fractionation factors between amorphous Fe(III)-Si gel, a likely precursor to Precambrian jaspers and BIFs, and aqueous Si in artificial Archean seawater under anoxic conditions. Experiments were conducted at room temperature, and in the presence and absence of aqueous Fe(II) (Fe(II)(aq)).
Results of this study demonstrate that Si solubility is significantly lower for Fe-Si gel than that of amorphous Si, indicating that seawater Si concentrations in the Precambrian may have been lower than previous estimates. The experiments reached similar to 70-90% Si isotope exchange after a period of 53-126 days, and the highest extents of exchange were obtained where Fe(II) aq was present, suggesting that Fe(II)-Fe(III) electron-transfer and atom-exchange reactions catalyze Si isotope exchange through breakage of Fe-Si bonds. All experiments except one showed little change in the instantaneous solid-aqueous Si isotope fractionation factor with time, allowing extraction of equilibrium Si isotope fractionation factors through extrapolation to 100% isotope exchange. The equilibrium Si-30/Si-28 fractionation between Fe(III)-Si gel and aqueous Si (Delta Si-30(gel-aqueous)) is -2.30 similar to 0.25% (2 sigma) in the absence of Fe(II) aq. In the case where Fe(II)(aq) was present, which resulted in addition of similar to 10% Fe(II) in the final solid, creating a mixed Fe(II)-Fe(III) Si gel, the equilibrium fractionation between Fe(II)-Fe(III)-Si gel and aqueous Si (Delta Si-30(gel-aqueous)) is -3.23 +/- 0.37% (2 sigma). Equilibrium Si isotope fractionation for Fe-Si gel systems is significantly larger in magnitude than estimates of a near-zero solid-aqueous fractionation factor between pure Si gel and aqueous Si, indicating a major influence of Fe atoms on Si-O bonds, and hence the isotopic properties, of Fe-Si gel. Larger Si isotope fractionation in the Fe(II)-bearing systems may be caused by incorporation of Fe(II) into the solid structure, which may further weaken Fe-Si bonds and thus change the Si isotope fractionation factor. The relatively large Si isotope fractionation for Fe-Si gel, relative to pure Si gel, provides a new explanation for the observed contrast in delta Si-30 values in the Precambrian BIFs and cherts, as well as an explanation for the relatively negative delta Si-30 values in BIFs, in contrast to previous proposals that the more negative delta Si-30 values in BIFs reflect hydrothermal sources of Si or sorption to Fe oxides/hydroxides. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Zheng, Xin-Yuan] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
NASA, Astrobiol Inst, Mountain View, CA USA.
RP Zheng, XY (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
EM xzheng75@wisc.edu
OI Zheng, Xin-Yuan/0000-0002-7959-8046
FU NASA Astrobiology Institute [NNA13AA94A]; National Science Foundation
[1122855]
FX We thank Dr. Rosalind Armytage for sharing her expertise during the
process of setting up protocols for Si isotope measurement at
UW-Madison, Prof. Mark Brzezinski for sharing the Si isotope reference
materials (Big Batch, Diatomite and Big Batch), Ms. Janice Jones for
shipping the reference materials, and Dr. Elizabeth Percak-Dennett for
advice on Fe-Si gel synthesis. Comments made by Dr. L. Trower, two
anonymous reviewers and AE E. Schauble have improved the manuscript.
This work was supported by the NASA Astrobiology Institute under grant
NNA13AA94A, and National Science Foundation grant 1122855.
NR 99
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U1 7
U2 15
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 AUG 15
PY 2016
VL 187
BP 102
EP 122
DI 10.1016/j.gca.2016.05.012
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DR2ME
UT WOS:000379737800005
ER
PT J
AU McLeod, CL
Brandon, AD
Fernandes, VA
Peslier, AH
Fritz, J
Lapen, T
Shafer, JT
Butcher, AR
Irving, AJ
AF McLeod, Claire L.
Brandon, Alan D.
Fernandes, Vera A.
Peslier, Anne H.
Fritz, Joerg
Lapen, Thomas
Shafer, John T.
Butcher, Alan R.
Irving, Anthony J.
TI Constraints on formation and evolution of the lunar crust from
feldspathic granulitic breccias NWA 3163 and 4881
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Lunar crust; Meteorite; Lunar evolution; Geochronology
ID LASER ARGON-40-ARGON-39 AGE; NORITIC ANORTHOSITE CLAST; CANYON SANIDINE
STANDARD; K-40 DECAY CONSTANTS; MOON-FORMING IMPACT; ET-AL. 2010;
MAGMA-OCEAN; AR-40/AR-39 GEOCHRONOLOGY; HIGHLAND METEORITES; JOINT
DETERMINATION
AB Lunar granulitic meteorites provide new constraints on the composition and evolution of the lunar crust as they are potentially derived from outside the Apollo and Luna landing sites. Northwest Africa (NWA) 3163, the focus of this study, and its paired stones NWA 4881 and NWA 4483, are shocked granulitic noritic anorthosites. They are petrographically and compositionally distinct from the Apollo granulites and noritic anorthosites. Northwest Africa 3163 is REE-depleted by an order of magnitude compared to Apollo granulites and is one of the most trace element depleted lunar samples studied to date. New in-situ mineral compositional data and Rb-Sr, Ar-Ar isotopic systematics are used to evaluate the petrogenetic history of NWA 3163 (and its paired stones) within the context of early lunar evolution and the bulk composition of the lunar highlands crust. The NWA 3163 protolith was the likely product of reworked lunar crust with a previous history of heavy REE depletion. The bulk feldspathic and pyroxene-rich fragments have Sr-87/Sr-86 that are indistinguishable and average 0.699282 +/- 0.000007 (2 sigma). A calculated source model Sr T-RD age of 4.340 +/- 0.057 Ga is consistent with (1) the recently determined young FAS (Ferroan Anorthosite) age of 4.360 +/- 0.003 Ga for FAS 60025, (2) Nd-142 model ages for the closure of the Sm-Nd system for the mantle source reservoirs of the Apollo mare basalts (4.355-4.314 Ga) and (3) a prominent age peak in the Apollo lunar zircon record (c. 4.345 Ga). These ages are similar to 100 Myr younger than predicted timescales for complete LMO crystallization (similar to 10 Myrs after Moon formation, Elkins-Tanton et al., 2011). This supports a later, major event during lunar evolution associated with crustal reworking due to magma ocean cumulate overturn, serial magmatism, or a large impact event leading to localized or global crustal melting and/or exhumation. The Ar-Ar isotopic systematics on aliquots of paired stone NWA 4881 are consistent with an impact event at >= 3.5 Ga. This is inferred to record the event that induced granularization of NWA 3163 (and paired rocks). A later event is also recorded at similar to 2 Ga by Ar-Ar isotopes is consistent with an increase in the number of impacts on the lunar surface at this time (Fernandes et al., 2013). Northwest Africa 3163 and its paired stones therefore record a c. 2.4 Gyr record of lunar crustal production, metamorphism, brecciation, impacts and eventual ejection from the lunar surface. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [McLeod, Claire L.; Brandon, Alan D.; Lapen, Thomas; Shafer, John T.] Univ Houston, Dept Earth & Atmospher Sci, 4800 Calhoun Rd, Houston, TX 77004 USA.
[Fernandes, Vera A.] Leibniz Inst Res Evolut & Biodivers, Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany.
[Fernandes, Vera A.] Univ Oslo, Ctr Earth Evolut & Dynam, N-0316 Oslo, Norway.
[Fernandes, Vera A.] Univ Nova Lisboa, Inst Dev New Technol UNINOVA, Lisbon, Portugal.
[Peslier, Anne H.] NASA, Jacobs, Johnson Space Ctr, Mail Code XI3, Houston, TX 77058 USA.
[Fritz, Joerg] Saalbau Weltraum Projekt, Wilhelmstr 38, D-64646 Heppenheim, Germany.
[Butcher, Alan R.] FEI Co, Eindhoven, Netherlands.
[Irving, Anthony J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
RP McLeod, CL (reprint author), Miami Univ, Dept Geol & Environm Earth Sci, 250 S Patterson Ave, Oxford, OH 45056 USA.
EM mcleodcl@miamioh.edu
RI Fernandes, Vera/B-4653-2013
OI Fernandes, Vera/0000-0003-0848-9229
FU Lunar Science Institute; Cosmochemistry program at NASA; Deutsche
Forshungsgeminschaft [FE 1523/3-1]
FX ADB received funding for this project through the Lunar Science
Institute and the Cosmochemistry program at NASA. Gavyn Rollinson at the
Camborne School of Mines, University of Exeter, UK is thanked for his
assistance during acquisition of the QEMSCAN images. VAF acknowledges
research funding from Deutsche Forshungsgeminschaft via grant FE
1523/3-1. Additional thanks are extended to 2 anonymous reviewers who
comments and suggestions improved this manuscript. Further thanks to
Marc Norman whose input significantly improved the discussion and
interpretation of this new data.
NR 144
TC 0
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U1 7
U2 8
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 AUG 15
PY 2016
VL 187
BP 350
EP 374
DI 10.1016/j.gca.2016.04.032
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DR2ME
UT WOS:000379737800018
ER
PT J
AU Cuzzone, JK
Clark, PU
Carlson, AE
Ullman, DJ
Rinterknecht, VR
Milne, GA
Lunkka, JP
Wohlfarth, B
Marcott, SA
Caffee, M
AF Cuzzone, Joshua K.
Clark, Peter U.
Carlson, Anders E.
Ullman, David J.
Rinterknecht, Vincent R.
Milne, Glenn A.
Lunkka, Juha-Pekka
Wohlfarth, Barbara
Marcott, Shaun A.
Caffee, Marc
TI Final deglaciation of the Scandinavian Ice Sheet and implications for
the Holocene global sea-level budget
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE sea level; ice sheets; Holocene
ID LAST GLACIAL MAXIMUM; LATERAL VISCOSITY VARIATIONS; NUCLIDE
PRODUCTION-RATES; BE-10 PRODUCTION-RATE; COSMOGENIC NUCLIDES; MANTLE
VISCOSITY; HUDSON-BAY; BALTIC SEA; AGE EARTH; MODEL
AB The last deglaciation of the Scandinavian Ice Sheet (SIS) from similar to 21,000 to 13,000 yr ago is well constrained by several hundred Be-10 and C-14 ages. The subsequent retreat history, however, is established primarily from minimum-limiting C-14 ages and incomplete Baltic-Sea varve records, leaving a substantial fraction of final SIS retreat history poorly constrained. Here we develop a high-resolution chronology for the final deglaciation of the SIS based on 79 Be-10 cosmogenic exposure dates sampled along three transects spanning southern to northern Sweden and Finland. Combining this new chronology with existing Be-10 ages on deglaciation since the Last Glacial Maximum shows that rates of SIS margin retreat were strongly influenced by deglacial millennial-scale climate variability and its effect on surface mass balance, with regional modulation of retreat associated with dynamical controls. Ice-volume estimates constrained by our new chronology suggest that the SIS contributed 8 m sea-level equivalent to global sea-level rise between similar to 14.5 ka and 10 ka. Final deglaciation was largely complete by similar to 10.5 ka, with highest rates of sea-level rise occurring during the Bolling-Allerod, a 50% decrease during the Younger Dryas, and a rapid increase during the early Holocene. Combining our SIS volume estimates with estimated contributions from other remaining Northern Hemisphere ice sheets suggests that the Antarctic Ice Sheet (AIS) contributed 14.4 +/- 5.9 m to global sea-level rise since 13 ka. This new constraint supports those studies that indicate that an ice volume of 15 m or more of equivalent sea-level rise was lost from the AIS during the last deglaciation. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Cuzzone, Joshua K.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Clark, Peter U.; Carlson, Anders E.; Ullman, David J.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Rinterknecht, Vincent R.] Univ Paris 01, CNRS, Lab Geog Phys, UMR 8591, F-92195 Meudon, France.
[Milne, Glenn A.] Univ Ottawa, Dept Earth & Environm Sci, Ottawa, ON, Canada.
[Lunkka, Juha-Pekka] Univ Oulu, OMS Glacial Sedimentol & Stratig Grp, POB 3000, FI-90014 Oulu, Finland.
[Wohlfarth, Barbara] Univ Stockholm, Dept Geol Sci, Stockholm, Sweden.
[Marcott, Shaun A.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Caffee, Marc] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Caffee, Marc] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
[Rinterknecht, Vincent R.] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AL, Fife, Scotland.
RP Cuzzone, JK (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Joshua.K.Cuzzone@jpl.nasa.gov
FU GSA graduate student research grant; NSF [EAR-0958417, EAR-0958872,
EAR-1343573, EAR-0844151]
FX We thank Jay Alder, Aaron Barth, Andrea Balbas, Nilo Bill, Svante
Bjorck, Akkaneewut Chabangborn, Brent Goehring, Nat Lifton, and
Jukka-Pekka Palmu for help and discussions related to this project,
Jonathan Bamber for the base map used in Fig. 3d, and the two journal
reviewers for their helpful comments. Research was supported by a GSA
graduate student research grant to JKC, NSF grant EAR-0958417 to PUC,
and NSF grants EAR-0958872 and EAR-1343573 to AEC. PRIME Lab is
supported by NSF grant EAR-0844151.
NR 67
TC 7
Z9 7
U1 11
U2 20
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 AUG 15
PY 2016
VL 448
BP 34
EP 41
DI 10.1016/j.epsl.2016.05.019
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DP4HS
UT WOS:000378457600004
ER
PT J
AU Bishop, JL
Rampe, EB
AF Bishop, Janice L.
Rampe, Elizabeth B.
TI Evidence for a changing Martian climate from the mineralogy at Mawrth
Vallis
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; mineralogy; spectroscopy; weathering; climate
ID CLAY MINERALOGY; THEMIS DATA; MARS; ALLOPHANE; TES; ABUNDANCE; REGION;
STRATIGRAPHY; IMOGOLITE; SPECTRA
AB Layered outcrops in the Mawrth Vallis region of Mars contain the greatest diversity of aqueous alteration products on the planet, and these materials are used to infer past aqueous environments. Orbital investigations indicate Al/Si-rich clay-bearing units overly an Fe/Mg-smectite-rich unit. Many different secondary minerals have been identified in the upper Al/Si-rich clay units, but the presence of poorly crystalline phases has not been previously investigated. Identification of similar to 10-30% allophane and imogolite in the clay-bearing units resolves previous mineralogical discrepancies between TES and CRISM of clay-bearing units on Mars. We demonstrate here that the poorly crystalline aluminosilicates allophane and imogolite comprise a significant portion of the uppermost stratum of the Al/Si-clay-rich units. These phases are unique to immature soils derived from volcanic ash in well-drained, mildly acidic environments on Earth, and we hypothesize that the deposits discovered here originate from supervolcanic activity in nearby Arabia Terra. The transition through time from smectite-bearing units to the uppermost allophane/imogolite unit in Mawrth Vallis signifies a change in climate from a warm and wet environment to one where water was sporadic and likely depleted rapidly. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Bishop, Janice L.] Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Rampe, Elizabeth B.] NASA JSC, Aerodyne Ind, Jacobs JETS, Houston, TX 77058 USA.
RP Bishop, JL (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM jbishop@seti.org
FU NASA's Mars Data Analysis Program [NNX12AJ33G]; NASA Astrobiology
Institute [NNX15BB01G]; NASA's Mars Fundamental Research Program; NASA's
Solar System Workings Program [NNX15AH57G]
FX The authors are grateful to the science and operations teams from
MRO/CRISM and MGS/TES for acquiring the data. Funding from NASA's Mars
Data Analysis Program (NNX12AJ33G) and the NASA Astrobiology Institute
(NNX15BB01G) to J. Bishop, funding from NASA's Mars Fundamental Research
Program to E. Rampe, and funding from NASA's Solar System Workings
Program (NNX15AH57G) to both authors are appreciated. Thanks are due to
C. Gross for preparing the MOC/MOLA topographical image. The authors are
grateful to J. Michalski and an anonymous reviewer for helpful comments
that improved the paper.
NR 49
TC 0
Z9 0
U1 10
U2 18
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 AUG 15
PY 2016
VL 448
BP 42
EP 48
DI 10.1016/j.epsl.2016.04.031
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DP4HS
UT WOS:000378457600005
ER
PT J
AU Bednarcyk, BA
Aboudi, J
Arnold, SM
AF Bednarcyk, Brett A.
Aboudi, Jacob
Arnold, Steven M.
TI Enhanced composite damping through engineered interfaces
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE Composites; Damping; Micromechanics; Multiscale modeling; High-fidelity
generalized method of cells; Homogenization
ID POLYMER-MATRIX COMPOSITES; FIBER COMPOSITES; MODELS; MICROMECHANICS;
ENERGY
AB The damping properties of unidirectional, laminated, and woven composites have been predicted using a multiscale implementation of the High-Fidelity Generalized Method of Cells micromechanics theory. This model considers periodic repeating unit cell geometries on both the global and local scales and utilizes the constituent material specific damping coefficients, mechanical properties, and local fields, along with the strain energy approach, to determine effective directional specific damping coefficients of the composite. In addition to comparisons of the HFGMC predictions with results from the literature, the effect of a degraded fiber/matrix interface was examined parametrically. A significant finding was that strong maxima exist in the predicted composite damping coefficients as a function of degree of interfacial mechanical degradation. This suggests that drastic improvements in damping in composites can be achieved by properly engineering the fiber/matrix interface. The multiscale HFGMC simulations presented illustrate that the decrease in composite mechanical properties caused by such an engineered interface can be minimized when implemented within a technologically relevant laminate, while still maintaining an extreme improvement in the laminate damping properties. Published by Elsevier Ltd.
C1 [Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Aboudi, Jacob] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
RP Bednarcyk, BA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
EM Brett.A.Bednarcyk@nasa.gov
NR 23
TC 0
Z9 0
U1 6
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
EI 1879-2146
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD AUG 15
PY 2016
VL 92-93
BP 91
EP 104
DI 10.1016/j.ijsolstr.2016.04.020
PG 14
WC Mechanics
SC Mechanics
GA DP4LY
UT WOS:000378468600009
ER
PT J
AU Reichardt, A
Dillon, RP
Borgonia, JP
Shapiro, AA
McEnerney, BW
Momose, T
Hosemann, P
AF Reichardt, Ashley
Dillon, R. Peter
Borgonia, John Paul
Shapiro, Andrew A.
McEnerney, Bryan W.
Momose, Tatsuki
Hosemann, Peter
TI Development and characterization of Ti-6Al-4V to 304L stainless steel
gradient components fabricated with laser deposition additive
manufacturing
SO MATERIALS & DESIGN
LA English
DT Article
DE Laser deposition; Functionally graded; Ti-alloy; Stainless steel 304L;
Fe-V sigma phase
ID DIRECT METAL-DEPOSITION; MECHANICAL-PROPERTIES; COPPER INTERLAYER;
ALLOY; TITANIUM; 304-STAINLESS-STEEL; MICROSTRUCTURES; EVOLUTION; CR
AB In this study, a multi-hopper laser deposition system is used to additively manufacture functionally graded Ti-6Al-4V to 304L stainless steel components with a vanadium interlayer. Grain morphology, phase, and composition are mapped along the component gradients with electron backscatter diffraction (EBSD) and energy dispersive X-ray spectroscopy (EDS), and mechanical property changes are assessed utilizing Vickers hardness and nanoindentation. Precipitation of brittle intermetallic compounds such as FeTi and the formation of an Fe-V-Cr sigma phase are confirmed to be the causes ofmid-fabrication cracking in the components. Guided by multicomponent phase diagrams, alternate paths in composition space are proposed to strategically avoid unfavorable phase formation along the gradient. Composition-dependent adjustment of process parameters is also proposed to reduce the prevalence of observed powder inclusions, homogenize grain morphology, and improve component mechanical properties. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Reichardt, Ashley; Hosemann, Peter] Univ Calif Berkeley, Dept Nucl Engn, Berkeley, CA 94720 USA.
[Dillon, R. Peter; Borgonia, John Paul; Shapiro, Andrew A.; McEnerney, Bryan W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Momose, Tatsuki] Tohoku Univ, Dept Mat Proc, Sendai, Miyagi 980, Japan.
RP Reichardt, A (reprint author), Univ Calif Berkeley, 4155 Etcheverry Hall,MC 1730, Berkeley, CA 94720 USA.
EM areichar@berkeley.edu
OI Hosemann, Peter/0000-0003-2281-2213
FU NASA [1534814]
FX This paper was developed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA (1534814).
NR 36
TC 0
Z9 0
U1 40
U2 68
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0264-1275
EI 1873-4197
J9 MATER DESIGN
JI Mater. Des.
PD AUG 15
PY 2016
VL 104
BP 404
EP 413
DI 10.1016/j.matdes.2016.05.016
PG 10
WC Materials Science, Multidisciplinary
SC Materials Science
GA DN9FH
UT WOS:000377384400047
ER
PT J
AU Marchione, D
McCoustra, MRS
AF Marchione, Demian
McCoustra, Martin R. S.
TI Non-covalent interaction of benzene with methanol and diethyl ether
solid surfaces
SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS
LA English
DT Article
ID DENSITY-FUNCTIONAL THEORY; IMMISCIBLE LIQUIDS; HYDROGEN-BONDS;
SUPRAMOLECULAR CHEMISTRY; MULTIPHOTON IONIZATION; DESORPTION-KINETICS;
CH/PI INTERACTIONS; PI-INTERACTIONS; DIMETHYL ETHER; GRAIN SURFACES
AB We present laboratory experiments on binary, layered ices comprised of benzene (C6H6) on methanol (CH3OH) and on diethyl ether (CH3CH2OCH2CH3). Temperature programmed desorption (TPD) and reflection-absorption infrared spectroscopy (RAIRS) have been used to investigate the growth mechanisms in these systems. Ab initio quantum chemical calculations on simple gas-phase model clusters are used to aid interpretation of the experimental data by highlighting the key interactions established at the interface. Our observations are consistent with C6H6 forming islands on CH3OH, although evidence of strong hydrogen bonding interactions indicates some degree of surface wetting. In contrast, layer-by-layer growth is proposed for C6H6 on the CH3CH2OCH2CH3 substrate.
C1 [Marchione, Demian; McCoustra, Martin R. S.] Heriot Watt Univ, Inst Chem Sci, Edinburgh EH14 4AS, Midlothian, Scotland.
[Marchione, Demian] CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Marchione, D (reprint author), Heriot Watt Univ, Inst Chem Sci, Edinburgh EH14 4AS, Midlothian, Scotland.; Marchione, D (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM marchionedemian@gmail.com; m.r.s.mccoustra@hw.ac.uk
OI McCoustra, Martin/0000-0002-5716-110X
FU European Community FP7-ITN Marie-Curie Programme (LASSIE project)
[238258]; Heriot-Watt University
FX The authors would like to acknowledge the use of the EPSRC UK National
Service for Computational Chemistry Software (NSCCS) at Imperial College
London and contributions from its staff in carrying out this work. The
authors acknowledge the support of the European Community FP7-ITN
Marie-Curie Programme (LASSIE project, grant agreement #238258).
Financial support from Heriot-Watt University for a number of upgrades
to the UHV system is also acknowledged. DM clarifies that his
contribution to this work has been done as a private venture and not in
the author's capacity as an affiliate of the Jet Propulsion Laboratory,
California Institute of Technology. The authors would like to thank
Prof. Maciej Gutowski (Heriot-Watt University) and Dr Enrico Ronca
(Princeton University) for the very helpful discussions.
NR 90
TC 1
Z9 1
U1 9
U2 9
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 1463-9076
EI 1463-9084
J9 PHYS CHEM CHEM PHYS
JI Phys. Chem. Chem. Phys.
PD AUG 14
PY 2016
VL 18
IS 30
BP 20790
EP 20801
DI 10.1039/c6cp01787h
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DT4CV
UT WOS:000381428600084
PM 27414704
ER
PT J
AU Lefevre, R
Berthebaud, D
Bux, S
Hebert, S
Gascoin, F
AF Lefevre, Robin
Berthebaud, David
Bux, Sabah
Hebert, Sylvie
Gascoin, Franck
TI Magnetic and thermoelectric properties of the ternary pseudo-hollandite
BaxCr5Se8 (0.5 < x < 0.55) solid solution
SO DALTON TRANSACTIONS
LA English
DT Article
ID HIGHER MANGANESE SILICIDES; CHALCOGENIDES; CHROMIUM; PERFORMANCE
AB The structure of Ba0.5Cr5Se8 has been recently resolved, and its thermoelectric and magnetic properties have been studied. A ZT of 0.12 was found at around 800 K. Here, we report a study on the pseudohollandite BaxCr5Se8 solid-solution with 0.5 <= x <= 0.55 and its thermoelectric and magnetic properties. There is no significant impact either on the cell parameters depending on the cation content or on the magnetic properties. However, thermoelectric properties are radically changed depending on x content. While the low thermal conductivity, around 0.8 W m(-1) K-1, remains similar for all samples, a respective increase and decrease of the resistivity and the Seebeck coefficient are observed with increasing Ba content. The maximum Seebeck coefficient is found with Ba0.5Cr5Se8 at around 635 K with 315 mu V K-1, and the Seebeck coefficient then decreases and is correlated with an activation of minority charge carriers confirmed by Hall measurements. A similar but steeper behavior is observed for the Ba0.55Cr5Se8 temperature dependence plot at around 573 K. Finally, the best thermoelectric performances are found using the lowest content of Ba, unlike when x tends to 0.55, ZT approaches a tenth of the initial best value. BaxCr5Se8 compounds are antiferromagnetic with T-N = 58 K. A large peak in thermal conductivity is observed around the antiferromagnetic transition for all stoichiometry.
C1 [Lefevre, Robin; Berthebaud, David; Hebert, Sylvie; Gascoin, Franck] UCBN, ENSICAEN, CNRS, Lab CRISMAT,UMR 6508, 6 Blvd Marechal Juin, F-14050 Caen 04, France.
[Bux, Sabah] Jet Prop Lab, 4800 Oak Grove Dr MS 277-207, Pasadena, CA 91109 USA.
RP Gascoin, F (reprint author), UCBN, ENSICAEN, CNRS, Lab CRISMAT,UMR 6508, 6 Blvd Marechal Juin, F-14050 Caen 04, France.
EM franck.gascoin@ensicaen.fr
FU french Agence Nationale de la Recherche (ANR) [ANR-10-LABX-09-01];
National Aeronautics and Space Administration; NASA Science Missions
Directorate's Radioisotope Power Systems Thermoelectric Technology
Development Project
FX Authors would like to thank Fabien Veillon for PPMS and MPMS SQUID
measurements and Stephanie Gascoin for support concerning the powder
X-ray diffraction experiments. The authors acknowledge the financial
support of the french Agence Nationale de la Recherche (ANR), through
the program "Investissements d'Avenir" (ANR-10-LABX-09-01), LabEx EMC3.
Part of this research was carried out at the Jet Propulsion Laboratory,
the California Institute of Technology, under a contract with the
National Aeronautics and Space Administration. Part of this work
supported by the NASA Science Missions Directorate's Radioisotope Power
Systems Thermoelectric Technology Development Project.
NR 28
TC 0
Z9 0
U1 7
U2 11
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 1477-9226
EI 1477-9234
J9 DALTON T
JI Dalton Trans.
PD AUG 14
PY 2016
VL 45
IS 30
BP 12119
EP 12126
DI 10.1039/c6dt02166b
PG 8
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA DT2RM
UT WOS:000381328100024
PM 27396273
ER
PT J
AU Oetjen, H
Payne, VH
Neu, JL
Kulawik, SS
Edwards, DP
Eldering, A
Worden, HM
Worden, JR
AF Oetjen, Hilke
Payne, Vivienne H.
Neu, Jessica L.
Kulawik, Susan S.
Edwards, David P.
Eldering, Annmarie
Worden, Helen M.
Worden, John R.
TI A joint data record of tropospheric ozone from Aura-TES and MetOp-IASI
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AIR-QUALITY; NORTH-AMERICA; SURFACE OZONE; EMISSION SPECTROMETER; ASIAN
EMISSIONS; ERROR ANALYSIS; SATELLITE; CHEMISTRY; TRANSPORT; RETRIEVALS
AB The Tropospheric Emission Spectrometer (TES) on Aura and Infrared Atmospheric Sounding Interferometer (IASI) on MetOp-A together provide a time series of 10 years of free-tropospheric ozone with an overlap of 3 years. We characterise the differences between TES and IASI ozone measurements and find that IASI's coarser vertical sensitivity leads to a small (<5 ppb) low bias relative to TES for the free troposphere. The TES-IASI differences are not dependent on season or any other factor and hence the measurements from the two instruments can be merged, after correcting for the offset, in order to study decadal-scale changes in tropospheric ozone. We calculate time series of regional monthly mean ozone in the free troposphere over eastern Asia, the western United States (US), and Europe, carefully accounting for differences in spatial sampling between the instruments. We show that free-tropospheric ozone over Europe and the western US has remained relatively constant over the past decade but that, contrary to expectations, ozone over Asia in recent years does not continue the rapid rate of increase observed from 2004 to 2010.
C1 [Oetjen, Hilke; Payne, Vivienne H.; Neu, Jessica L.; Kulawik, Susan S.; Eldering, Annmarie; Worden, John R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Oetjen, Hilke; Eldering, Annmarie] UCLA JPL Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Kulawik, Susan S.] BAER Inst, Mountain View, CA USA.
[Edwards, David P.; Worden, Helen M.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
RP Payne, VH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM vivienne.h.payne@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA [NNX11AE19G]
FX We acknowledge the NOAA/CLASS data centre for the IASI Level 1c spectra
and EUMETSAT for the Level 2 data. IASI is a joint mission of EUMETSAT
and the Centre National d'Etudes Spatiales (CNES, France). 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. We acknowledge NASA support under the grant
NNX11AE19G. The Hilo ozone sonde data were provided by the Global
Monitoring Division of NOAA (www.esrl.noaa.gov/gmd).
NR 47
TC 0
Z9 0
U1 13
U2 13
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 12
PY 2016
VL 16
IS 15
BP 10229
EP 10239
DI 10.5194/acp-16-10229-2016
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV8ZR
UT WOS:000383229600001
ER
PT J
AU Guerreiro, T
Monteiro, F
Martin, A
Brask, JB
Vertesi, T
Korzh, B
Caloz, M
Bussieres, F
Verma, VB
Lita, AE
Mirin, RP
Nam, SW
Marsilli, F
Shaw, MD
Gisin, N
Brunner, N
Zbinden, H
Thew, RT
AF Guerreiro, T.
Monteiro, F.
Martin, A.
Brask, J. B.
Vertesi, T.
Korzh, B.
Caloz, M.
Bussieres, F.
Verma, V. B.
Lita, A. E.
Mirin, R. P.
Nam, S. W.
Marsilli, F.
Shaw, M. D.
Gisin, N.
Brunner, N.
Zbinden, H.
Thew, R. T.
TI Demonstration of Einstein-Podolsky-Rosen Steering Using Single-Photon
Path Entanglement and Displacement-Based Detection
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID QUANTUM; AMPLIFICATION; NONLOCALITY; GENERATION; INEQUALITY; VIOLATION;
OPTICS; STATES; ATOMS
AB We demonstrate the violation of an Einstein-Podolsky-Rosen steering inequality developed for singlephoton path entanglement with displacement-based detection. We use a high-rate source of heralded singlephoton path-entangled states, combinedwith high-efficiency superconducting-based detectors, in a scheme that is free of any postselection and thus immune to the detection loophole. This result conclusively demonstrates single-photon entanglement in a one-sided device-independent scenario, and opens the way towards implementations of device-independent quantum technologies within the paradigm of path entanglement.
C1 [Guerreiro, T.; Monteiro, F.; Martin, A.; Korzh, B.; Caloz, M.; Bussieres, F.; Gisin, N.; Zbinden, H.; Thew, R. T.] Univ Geneva, Appl Phys Grp, CH-1211 Geneva 4, Switzerland.
[Brask, J. B.; Brunner, N.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
[Vertesi, T.] Hungarian Acad Sci, Inst Nucl Res, POB 51, H-4001 Debrecen, Hungary.
[Verma, V. B.; Lita, A. E.; Mirin, R. P.; Nam, S. W.] NIST, 325 Broadway, Boulder, CO 80305 USA.
[Marsilli, F.; Shaw, M. D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Brunner, N (reprint author), Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
EM nicolas.brunner@unige.ch; robert.thew@unige.ch
RI Brask, Jonatan Bohr/A-5931-2017; Vertesi, Tamas/B-3416-2017; Bussieres,
Felix/E-5384-2011;
OI Brask, Jonatan Bohr/0000-0003-3859-0272; Vertesi,
Tamas/0000-0003-4437-9414; Bussieres, Felix/0000-0003-0234-175X;
/0000-0003-0188-6053; Jung, Kyuhyun/0000-0001-8631-610X
FU Swiss national science foundation [200021_159592]; Swiss national
science foundation (starting grant DIAQ); NCCR-QSIT; OTKA Grant
[K111734]; EU project SIQS Grant [600645]; DARPA QUINESS program
FX The authors thank Natalia Bruno for assistance with the HSPS and LO
setups. This work was supported by the Swiss national science foundation
(Grant No. 200021_159592 and starting grant DIAQ), the NCCR-QSIT, the
OTKA Grant No. K111734, as well as the EU project SIQS Grant No. 600645.
NIST acknowledges funding from the DARPA QUINESS program. Part of the
research on the detectors was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 41
TC 3
Z9 3
U1 8
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD AUG 12
PY 2016
VL 117
IS 7
AR 070404
DI 10.1103/PhysRevLett.117.070404
PG 5
WC Physics, Multidisciplinary
SC Physics
GA DT4VH
UT WOS:000381478800001
PM 27563941
ER
PT J
AU Nielsen, J
Hedeholm, RB
Heinemeier, J
Bushnell, PG
Christiansen, JS
Olsen, J
Ramsey, CB
Brill, RW
Simon, M
Steffensen, KF
Steffensen, JF
AF Nielsen, Julius
Hedeholm, Rasmus B.
Heinemeier, Jan
Bushnell, Peter G.
Christiansen, Jorgen S.
Olsen, Jesper
Ramsey, Christopher Bronk
Brill, Richard W.
Simon, Malene
Steffensen, Kirstine F.
Steffensen, John F.
TI Eye lens radiocarbon reveals centuries of longevity in the Greenland
shark (Somniosus microcephalus)
SO SCIENCE
LA English
DT Article
ID POST-BOMB RADIOCARBON; FEEDING ECOLOGY; NORTHWEST ATLANTIC; AGE
VALIDATION; LAMNA-NASUS; PRE-BOMB; FOOD-WEB; CALIBRATION; OTOLITHS;
DELTA-N-15
AB The Greenland shark (Somniosus microcephalus), an iconic species of the Arctic Seas, grows slowly and reaches >500 centimeters (cm) in total length, suggesting a life span well beyond those of other vertebrates. Radiocarbon dating of eye lens nuclei from 28 female Greenland sharks (81 to 502 cm in total length) revealed a life span of at least 272 years. Only the smallest sharks (220 cm or less) showed signs of the radiocarbon bomb pulse, a time marker of the early 1960s. The age ranges of prebomb sharks (reported as midpoint and extent of the 95.4% probability range) revealed the age at sexual maturity to be at least 156 +/- 22 years, and the largest animal (502 cm) to be 392 +/- 120 years old. Our results show that the Greenland shark is the longest-lived vertebrate known, and they raise concerns about species conservation.
C1 [Nielsen, Julius; Steffensen, Kirstine F.; Steffensen, John F.] Univ Copenhagen, Marine Biol Sect, Strandpromenaden 5, DK-3000 Helsingor, Denmark.
[Nielsen, Julius; Hedeholm, Rasmus B.] Greenland Inst Nat Resources, POB 570,Kivioq 2, Nuuk 3900, Greenland.
[Nielsen, Julius] Natl Aquarium Denmark, Den Bla Planet, Jacob Fortlingsvej 1, DK-2770 Kastrup, Denmark.
[Nielsen, Julius; Christiansen, Jorgen S.] UiT Arctic Univ Norway, Dept Arctic & Marine Biol, N-9037 Tromso, Norway.
[Heinemeier, Jan; Olsen, Jesper] Aarhus Univ, Aarhus AMS Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus, Denmark.
[Bushnell, Peter G.] Indiana Univ South Bend, Dept Biol Sci, 1700 Mishawaka Ave, South Bend, IN USA.
[Ramsey, Christopher Bronk] Univ Oxford, Oxford Radiocarbon Accelerator Unit, Dyson Perrins Bldg,South Parks Rd, Oxford OX1 3QY, England.
[Brill, Richard W.] NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, 74 Magruder Rd, Highlands, NJ 07732 USA.
[Brill, Richard W.] Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA.
[Simon, Malene] Greenland Inst Nat Resources, Greenland Climate Res Ctr, POB 570,Kivioq 2, Nuuk 3900, Greenland.
RP Nielsen, J (reprint author), Univ Copenhagen, Marine Biol Sect, Strandpromenaden 5, DK-3000 Helsingor, Denmark.; Nielsen, J (reprint author), Greenland Inst Nat Resources, POB 570,Kivioq 2, Nuuk 3900, Greenland.; Nielsen, J (reprint author), Natl Aquarium Denmark, Den Bla Planet, Jacob Fortlingsvej 1, DK-2770 Kastrup, Denmark.; Nielsen, J (reprint author), UiT Arctic Univ Norway, Dept Arctic & Marine Biol, N-9037 Tromso, Norway.
EM julius.nielsen@bio.ku.dk
RI Olsen, Jesper/F-1656-2013; Steffensen, John/F-6778-2010
OI Olsen, Jesper/0000-0002-4445-5520; Steffensen, John/0000-0002-4477-8039
FU Commission of Scientific Investigations in Greenland (KVUG); Save Our
Seas Foundation; National Geographic Foundation; Carlsberg Foundation;
Danish Centre for Marine Research; Den Bla Planet-National Aquarium of
Denmark; Greenland Institute of Natural Resources (GINR); Danish Council
for Independent Research
FX We are grateful for the contributions from M. B. Backe throughout the
manuscript. We thank the Commission of Scientific Investigations in
Greenland (KVUG), Save Our Seas Foundation, National Geographic
Foundation, Carlsberg Foundation, Danish Centre for Marine Research, Den
Bla Planet-National Aquarium of Denmark, Greenland Institute of Natural
Resources (GINR), and the Danish Council for Independent Research for
financial support. We thank GINR, the University of Copenhagen and the
TUNU Programme (UIT, The Arctic University of Norway) for ship time. We
are grateful for the collaboration with K.P. Lange. We thank the crews
of the RV Pamiut, RV Dana, RV Helmer Hanssen, RV Sanna, and RV Porsild.
Three anonymous reviewers provided helpful comments and discussion that
improved earlier versions of the manuscript.
NR 38
TC 3
Z9 3
U1 44
U2 61
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 12
PY 2016
VL 353
IS 6300
BP 702
EP 704
DI 10.1126/science.aaf1703
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DT5ZC
UT WOS:000381561200041
PM 27516602
ER
PT J
AU Sawyer, AH
David, CH
Famiglietti, JS
AF Sawyer, Audrey H.
David, Cedric H.
Famiglietti, James S.
TI Continental patterns of submarine groundwater discharge reveal coastal
vulnerabilities
SO SCIENCE
LA English
DT Article
ID VOLCANIC ISLANDS; INTRUSION; AQUIFERS; FLUXES; WATERS; INPUTS; OCEAN
AB Submarine groundwater discharge (SGD) delivers water and dissolved chemicals from continents to oceans, and its spatial distribution affects coastal water quality. Unlike rivers, SGD is broadly distributed and relatively difficult to measure, especially at continental scales. We present spatially resolved estimates of fresh (land-derived) SGD for the contiguous United States, based on historical climate records and high-resolution hydrographic data. Climate controls regional patterns in fresh SGD, while coastal drainage geometry imparts strong local variability. Because the recharge zones that contribute fresh SGD are densely populated, the quality and quantity of fresh SGD are both vulnerable to anthropogenic disturbance. Our analysis unveils hot spots for contaminant discharge to marine waters and saltwater intrusion into coastal aquifers.
C1 [Sawyer, Audrey H.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[David, Cedric H.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sawyer, AH (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
EM sawyer.143@osu.edu
FU Jet Propulsion Laboratory, California Institute of Technology; NASA;
NASA SWOT and Sea Level Science Teams; NSF [EAR-1446724]; Ohio State
University School of Earth Sciences
FX We thank three anonymous reviewers for their suggestions, and M. Durand,
H. Michael, C. Russoniello, and J. Heiss for discussions. Supported by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA, and grants from the NASA SWOT and Sea Level
Science Teams (C.H.D. and J.S.F.); NSF grant EAR-1446724; and the Ohio
State University School of Earth Sciences. The authors declare no
competing interests. Fresh SGD rates and associated data are freely
available at http://dx.doi.org/10.5281/zenodo.58871.
NR 29
TC 0
Z9 0
U1 28
U2 28
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 12
PY 2016
VL 353
IS 6300
BP 705
EP 707
DI 10.1126/science.aag1058
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DT5ZC
UT WOS:000381561200042
PM 27492476
ER
PT J
AU Weston, JHS
Sokoloski, JL
Chomiuk, L
Linford, JD
Nelson, T
Mukai, K
Finzell, T
Mioduszewski, A
Rupen, MP
Walter, FM
AF Weston, Jennifer H. S.
Sokoloski, J. L.
Chomiuk, Laura
Linford, Justin D.
Nelson, Thomas
Mukai, Koji
Finzell, Tom
Mioduszewski, Amy
Rupen, Michael P.
Walter, Frederick M.
TI Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; novae; cataclysmic variables; stars: variables:
general; stars: winds; outflows; radio continuum: stars; X-rays: stars
ID X-RAY-EMISSION; RS-OPHIUCHI; CLASSICAL NOVAE; 2006 OUTBURST; BLAST WAVE;
V407 CYG; THERMAL EMISSION; WHITE-DWARF; EJECTA MASS; V1723 AQL
AB Since the Fermi discovery of gamma-rays from novae, one of the biggest questions in the field has been how novae generate such high-energy emission. Shocks must be a fundamental ingredient. Six months of radio observations of the 2012 Nova V5589 Sgr with the VLA and 15 weeks of X-ray observations with Swift/XRT show that the radio emission consisted of: (1) a shock-powered, non-thermal flare; and (2) weak thermal emission from 10(-5) M-aS (TM) of freely expanding, photoionized ejecta. Absorption features in the optical spectrum and the peak optical brightness suggest that V5589 Sgr lies 4 kpc away (3.2-4.6 kpc). The shock-powered flare dominated the radio light curve at low frequencies before day 100. The spectral evolution of the radio flare, its high radio brightness temperature, the presence of unusually hard (kT(x) > 33 keV) X-rays, and the ratio of radio to X-ray flux near radio maximum all support the conclusions that the flare was shock-powered and non-thermal. Unlike most other novae with strong shock-powered radio emission, V5589 Sgr is not embedded in the wind of a red-giant companion. Based on the similar inclinations and optical line profiles of V5589 Sgr and V959 Mon, we propose that shocks in V5589 Sgr formed from collisions between a slow flow with an equatorial density enhancement and a subsequent faster flow. We speculate that the relatively high speed and low mass of the ejecta led to the unusual radio emission from V5589 Sgr, and perhaps also to the non-detection of gamma-rays.
C1 [Weston, Jennifer H. S.; Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Chomiuk, Laura; Linford, Justin D.; Finzell, Tom] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
[Mukai, Koji] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, Koji] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Mioduszewski, Amy] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
[Rupen, Michael P.] Natl Res Council Canada, Herzberg Astron Program, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada.
[Rupen, Michael P.] Natl Res Council Canada, Herzberg Astrophys Program, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada.
[Walter, Frederick M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
RP Weston, JHS (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
EM jennifer@astro.columbia.edu; no@astro.columbia.edu; chomiuk@pa.msu.edu
FU NSF [AST-1211778]; NRAO [NRAO 343777]; NASA [NNH13ZDA001N-FERMI,
NNX13A091G]; Provost of Stony Brook University; VLA [S4322]
FX We thank NRAO for its generous allocation of time which made this work
possible. The National Radio Astronomy Observatory is a facility of the
National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. JW and JLS acknowledge support from NSF
award AST-1211778. JW was supported in part by a Student Observing
Support award from NRAO (NRAO 343777). LC, JL, and TF are supported by
NASA Fermi Guest Investigator grant NNH13ZDA001N-FERMI. TN was supported
in part by NASA award NNX13A091G. FMW thanks the Provost of Stony Brook
University for providing support for continued participation in SMARTS.
We acknowledge with thanks the variable star observations from the AAVSO
International Database contributed by observers worldwide and used as
reference in this work. Thanks to C.C. Cheung for use of data from VLA
programme S4322. Thanks to Glen Petitpas for SMA data reduction. Thanks
to Tim Cunningham, Eric Gotthelf, David Schiminovich, and Slavko
Bogdanov for useful discussion.
NR 67
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 11
PY 2016
VL 460
IS 3
BP 2687
EP 2697
DI 10.1093/mnras/stw1161
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT0WV
UT WOS:000381204600029
ER
PT J
AU Zemko, P
Orio, M
Mukai, K
Bianchini, A
Ciroi, S
Cracco, V
AF Zemko, P.
Orio, M.
Mukai, K.
Bianchini, A.
Ciroi, S.
Cracco, V.
TI V4743 Sgr, a magnetic nova?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: V4743 Sgr; novae; cataclysmic variables
ID X-RAY; INTERMEDIATE POLARS; SPECTRAL-ANALYSIS; LIGHT CURVES; V2491 CYG;
OSCILLATIONS; ATMOSPHERES; SAGITTARII; ACCRETION; EVOLUTION
AB Two XMM-Newton observations of Nova V4743 Sgr (Nova Sgr 2002) were performed shortly after it returned to quiescence, 2 and 3.5 yr after the explosion. The X-ray light curves revealed a modulation with a frequency of a parts per thousand integral 0.75 mHz, indicating that V4743 Sgr is most probably an intermediate polar (IP). The X-ray spectra have characteristics in common with known IPs, with a hard thermal plasma component that can be fitted only assuming a partially covering absorber. In 2004, the X-ray spectrum had also a supersoft blackbody-like component, whose temperature was close to that of the white dwarf (WD) in the supersoft X-ray phase following the outburst, but with flux by at least two orders of magnitude lower. In quiescent IPs, a soft X-ray flux component originates at times in the polar regions irradiated by an accretion column, but the supersoft component of V4743 Sgr disappeared in 2006, indicating a possible origin different from accretion. We suggest that it may have been due to an atmospheric temperature gradient on the WD surface, or to continuing localized thermonuclear burning at the bottom of the envelope, before complete turn-off. An optical spectrum obtained with Southern African Large Telescope (SALT) 11.5 yr after the outburst showed a prominent He ii lambda 4686 line and the Bowen blend, which reveal a very hot region, but with peak temperature shifted to the ultraviolet range. V4743 Sgr is the third post-outburst nova and IP candidate showing a low-luminosity supersoft component in the X-ray flux a few years after the outburst.
C1 [Zemko, P.; Bianchini, A.; Ciroi, S.; Cracco, V.] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Orio, M.; Bianchini, A.] INAF Osservatorio Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Orio, M.] Univ Wisconsin, Dept Astron, 475 N Charter Str, Madison, WI 53704 USA.
[Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
RP Zemko, P (reprint author), Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
EM polina.zemko@studenti.unipd.it
FU CARIPARO foundation at the University of Padova; NASA
FX Some of the observations reported in this paper were obtained with the
Southern African Large Telescope (SALT). Polina Zemko acknowledges a
pre-doctoral grant of the CARIPARO foundation at the University of
Padova. Dr Orio was funded by the NASA XMM-Newton program.
NR 39
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 11
PY 2016
VL 460
IS 3
BP 2744
EP 2751
DI 10.1093/mnras/stw1199
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT0WV
UT WOS:000381204600035
ER
PT J
AU Marino, S
Matra, L
Stark, C
Wyatt, MC
Casassus, S
Kennedy, G
Rodriguez, D
Zuckerman, B
Perez, S
Dent, WRF
Kuchner, M
Hughes, AM
Schneider, G
Steele, A
Roberge, A
Donaldson, J
Nesvold, E
AF Marino, S.
Matra, L.
Stark, C.
Wyatt, M. C.
Casassus, S.
Kennedy, G.
Rodriguez, D.
Zuckerman, B.
Perez, S.
Dent, W. R. F.
Kuchner, M.
Hughes, A. M.
Schneider, G.
Steele, A.
Roberge, A.
Donaldson, J.
Nesvold, E.
TI Exocometary gas in the HD 181327 debris ring
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; stars: individual: HD 181327; planetary systems;
radio continuum: planetary systems
ID ICY KUIPER-BELT; BETA-PICTORIS; ALMA OBSERVATIONS; MOLECULAR GAS;
CIRCUMSTELLAR DISK; PLANETARY EMBRYOS; YOUNG STARS; DUST; SYSTEM;
EVOLUTION
AB An increasing number of observations have shown that gaseous debris discs are not an exception. However, until now, we only knew of cases around A stars. Here we present the first detection of (CO)-C-12 (2-1) disc emission around an F star, HD 181327, obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) observations at 1.3 mm. The continuum and CO emission are resolved into an axisymmetric disc with ring-like morphology. Using a Markov chain Monte Carlo method coupled with radiative transfer calculations, we study the dust and CO mass distribution. We find the dust is distributed in a ring with a radius of 86.0 +/- 0.4 au and a radial width of 23.2 +/- 1.0 au. At this frequency, the ring radius is smaller than in the optical, revealing grain size segregation expected due to radiation pressure. We also report on the detection of low-level continuum emission beyond the main ring out to similar to 200 au. We model the CO emission in the non-local thermodynamic equilibrium regime and we find that the CO is co-located with the dust, with a total CO gas mass ranging between 1.2 x 10(-6) M-aS center dot and 2.9 x 10(-6) M-aS center dot, depending on the gas kinetic temperature and collisional partners densities. The CO densities and location suggest a secondary origin, i.e. released from icy planetesimals in the ring. We derive a CO+CO2 cometary composition that is consistent with Solar system comets. Due to the low gas densities, it is unlikely that the gas is shaping the dust distribution.
C1 [Marino, S.; Matra, L.; Wyatt, M. C.; Kennedy, G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Marino, S.; Casassus, S.; Rodriguez, D.; Perez, S.] Univ Chile, Dept Astron, Casilla 36-D, Santiago 36, Chile.
[Marino, S.; Casassus, S.; Perez, S.] Millennium Nucleus Protoplanetary Disks, Santiago, Chile.
[Stark, C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Rodriguez, D.] Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10034 USA.
[Zuckerman, B.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Dent, W. R. F.] Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Chile.
[Kuchner, M.; Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD USA.
[Hughes, A. M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
[Schneider, G.] Univ Arizona, Dept Astron, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Steele, A.; Donaldson, J.] Univ Maryland, Dept Astron, College Pk, MD USA.
[Nesvold, E.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
RP Marino, S (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Marino, S (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago 36, Chile.; Marino, S (reprint author), Millennium Nucleus Protoplanetary Disks, Santiago, Chile.
EM s.marino@ast.cam.ac.uk
OI Marino, Sebastian/0000-0002-5352-2924; Kennedy,
Grant/0000-0001-6831-7547
FU European Union through ERC [279973]; Millennium Nucleus (Chilean
Ministry of Economy) [RC130007]; FONDECYT [1130949, 3140601]; Royal
Society
FX We thank Pablo Roman for his help developing the tools uvmem and uvsim
used in this work. We also thank the referee for a constructive report.
This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2012.1.00437.S and ADS/JAO.ALMA#2013.1.00523.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) and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work
was supported by the European Union through ERC grant number 279973. SM,
SC, SP acknowledge financial support from Millennium Nucleus RC130007
(Chilean Ministry of Economy), and additionally by FONDECYT grants
1130949 and 3140601. GMK is supported by the Royal Society as a Royal
Society University Research Fellow.
NR 63
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Z9 6
U1 3
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 11
PY 2016
VL 460
IS 3
BP 2933
EP 2944
DI 10.1093/mnras/stw1216
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT0WV
UT WOS:000381204600048
ER
PT J
AU Holmes, TRH
Hain, CR
Anderson, MC
Crow, WT
AF Holmes, Thomas R. H.
Hain, Christopher R.
Anderson, Martha C.
Crow, Wade T.
TI Cloud tolerance of remote-sensing technologies to measure land surface
temperature
SO HYDROLOGY AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID IN-SITU MEASUREMENTS; MICROWAVE OBSERVATIONS; BRIGHTNESS TEMPERATURE;
WATER-VAPOR; VALIDATION; MSG/SEVIRI; CYCLE
AB Conventional methods to estimate land surface temperature (LST) from space rely on the thermal infrared (TIR) spectral window and is limited to cloud-free scenes. To also provide LST estimates during periods with clouds, a new method was developed to estimate LST based on passive-microwave (MW) observations. The MW-LST product is informed by six polar-orbiting satellites to create a global record with up to eight observations per day for each 0.25 degrees resolution grid box. For days with sufficient observations, a continuous diurnal temperature cycle (DTC) was fitted. The main characteristics of the DTC were scaled to match those of a geostationary TIR-LST product.
This paper tests the cloud tolerance of the MW-LST product. In particular, we demonstrate its stable performance with respect to flux tower observation sites (four in Europe and nine in the United States), over a range of cloudiness conditions up to heavily overcast skies. The results show that TIR-based LST has slightly better performance than MW-LST for clear-sky observations but suffers an increasing negative bias as cloud cover increases. This negative bias is caused by incomplete masking of cloud-covered areas within the TIR scene that affects many applications of TIR-LST. In contrast, for MW-LST we find no direct impact of clouds on its accuracy and bias. MW-LST can therefore be used to improve TIR cloud screening. Moreover, the ability to provide LST estimates for cloud-covered surfaces can help expand current clear-sky-only satellite retrieval products to all-weather applications.
C1 [Holmes, Thomas R. H.; Anderson, Martha C.; Crow, Wade T.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Holmes, Thomas R. H.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hain, Christopher R.] Univ Maryland, Earth Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Holmes, TRH (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.; Holmes, TRH (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM thomas.r.holmes@nasa.gov
RI Anderson, Martha/C-1720-2015
OI Anderson, Martha/0000-0003-0748-5525
FU NASA through the research grant "The Science of Terra and Aqua"
[13-TERAQ13-0181]
FX This work was funded by NASA through the research grant "The Science of
Terra and Aqua" (13-TERAQ13-0181). We would further like to thank Li
Fang (NOAA) for preparation and interpretation of GOES LST.
NR 24
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Z9 0
U1 11
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1027-5606
EI 1607-7938
J9 HYDROL EARTH SYST SC
JI Hydrol. Earth Syst. Sci.
PD AUG 11
PY 2016
VL 20
IS 8
BP 3263
EP 3275
DI 10.5194/hess-20-3263-2016
PG 13
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA DV8IY
UT WOS:000383181900001
ER
PT J
AU Jones, LW
Habel, LA
Weltzien, E
Castillo, A
Gupta, D
Kroenke, CH
Kwan, ML
Quesenberry, CP
Scott, J
Sternfeld, B
Yu, A
Kushi, LH
Caan, BJ
AF Jones, Lee W.
Habel, Laurel A.
Weltzien, Erin
Castillo, Adrienne
Gupta, Dipti
Kroenke, Candyce H.
Kwan, Marilyn L.
Quesenberry, Charles P., Jr.
Scott, Jessica
Sternfeld, Barbara
Yu, Anthony
Kushi, Lawrence H.
Caan, Bette J.
TI Exercise and Risk of Cardiovascular Events in Women With Nonmetastatic
Breast Cancer
SO JOURNAL OF CLINICAL ONCOLOGY
LA English
DT Article
ID PHYSICAL-ACTIVITY; VIGOROUS EXERCISE; HEART-FAILURE; UNITED-STATES;
THERAPY; DISEASE; SURVIVORS; MORTALITY; DEATH; REHABILITATION
AB Purpose
Cardiovascular disease (CVD) is a leading cause of death among women with nonmetastatic breast cancer. Whether exercise is associated with reductions in CVD risk in patients with breast cancer with an elevated CVD risk phenotype is not known.
Methods
Using a prospective design, women (n = 2,973; mean age, 57 years) diagnosed with nonmetastatic breast cancer participating in two registry-based, regional cohort studies, completed a questionnaire that assessed leisure-time recreational physical activity (metabolic equivalent task [MET]-h/wk). The primary end point was the first occurrence of any of the following: new diagnosis of coronary artery disease, heart failure, valve abnormality, arrhythmia, stroke, or CVD death, occurring after study enrollment.
Results
Median follow-up was 8.6 years (range, 0.2 to 14.8 years). In multivariable analysis, the incidence of cardiovascular events decreased across increasing total MET-h/wk categories (P-trend < .001). Compared with, < 2 MET-h/wk, the adjusted hazard ratio was 0.91 (95% CI, 0.76 to 1.09) for 2 to 10.9 MET-h/wk, 0.79 (95% CI, 0.66 to 0.96) for 11 to 24.5 MET-h/wk, and 0.65 (95% CI, 0.53 to 0.80) for >= 24.5 MET-h/wk. Similar trends were observed for the incidence of coronary artery disease and heart failure (Pvalues < .05). Adherence to national exercise guidelines for adult patients with cancer (ie, >= 9 MET-h/wk) was associated with an adjusted 23% reduction in the risk of cardiovascular events in comparison with not meeting the guidelines (< 9 MET-h/wk; P < .001). The association with exercise did not differ according to age, CVD risk factors, menopausal status, or anticancer treatment.
Conclusion
Exercise is associated with substantial, graded reductions in the incidence of cardiovascular events in women with nonmetastatic breast cancer. (C) 2016 by American Society of Clinical Oncology
C1 [Jones, Lee W.; Gupta, Dipti; Yu, Anthony] Mem Sloan Kettering Canc Ctr, 1275 York Ave, New York, NY 10021 USA.
[Habel, Laurel A.; Weltzien, Erin; Castillo, Adrienne; Kroenke, Candyce H.; Kwan, Marilyn L.; Quesenberry, Charles P., Jr.; Sternfeld, Barbara; Kushi, Lawrence H.; Caan, Bette J.] Kaiser Permanente, Oakland, CA USA.
[Scott, Jessica] NASA, Johnson Space Ctr, Houston, TX USA.
RP Jones, LW (reprint author), Mem Sloan Kettering Canc Ctr, Dept Med, 1275 York Ave, New York, NY 10065 USA.
EM jonesl3@mskcc.org
FU National Institutes of Health Awards [R01CA129059, R01CA105274];
National Cancer Institute; Memorial Sloan Kettering Cancer Center [P30
CA008748]; National Cancer Institute's SEER Program [HHSN261201000026C];
Utah State Department of Health; University of Utah
FX Supported by the National Institutes of Health Awards R01CA129059
(B.J.C.), R01CA105274 (L.H.K.), and research grants from the National
Cancer Institute and the Memorial Sloan Kettering Cancer Center Support
Grant/Core Grant No. P30 CA008748 (L.W.J.). The Utah Cancer Registry is
funded by Contract No. HHSN261201000026C from the National Cancer
Institute's SEER Program, with additional support from the Utah State
Department of Health and the University of Utah.
NR 42
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U1 10
U2 11
PU AMER SOC CLINICAL ONCOLOGY
PI ALEXANDRIA
PA 2318 MILL ROAD, STE 800, ALEXANDRIA, VA 22314 USA
SN 0732-183X
EI 1527-7755
J9 J CLIN ONCOL
JI J. Clin. Oncol.
PD AUG 10
PY 2016
VL 34
IS 23
BP 2743
EP +
DI 10.1200/JCO.2015.65.6603
PG 8
WC Oncology
SC Oncology
GA DU8MF
UT WOS:000382467000011
PM 27217451
ER
PT J
AU da Costa, FR
Kleint, L
Petrosian, V
Liu, W
Allred, JC
AF da Costa, Fatima Rubio
Kleint, Lucia
Petrosian, Vahe
Liu, Wei
Allred, Joel C.
TI DATA-DRIVEN RADIATIVE HYDRODYNAMIC MODELING OF THE 2014 MARCH 29 X1.0
SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; line: profiles; radiative transfer; Sun: chromosphere;
Sun: flares
ID MG II H; PARTIAL FREQUENCY REDISTRIBUTION; REGION-IMAGING-SPECTROGRAPH;
K LINES; CHROMOSPHERIC EVAPORATION; IRIS OBSERVATIONS; ELECTRON-BEAMS;
EMISSION; IBIS; RECONNECTION
AB Spectroscopic observations of solar flares provide critical diagnostics of the physical conditions in the flaring atmosphere. Some key features in observed spectra have not yet been accounted for in existing flare models. Here we report a data-driven simulation of the well-observed X1.0 flare on 2014 March 29 that can reconcile some well-known spectral discrepancies. We analyzed spectra of the flaring region from the Interface Region Imaging Spectrograph (IRIS) in Mg II h&k, the Interferometric BIdimensional Spectropolarimeter at the Dunn Solar Telescope (DST/IBIS) in H alpha 6563 angstrom and Ca II 8542 angstrom, and the Reuven Ramaty High Energy Solar Spectroscope Imager (RHESSI) in hard X-rays. We constructed a multithreaded flare loop model and used the electron flux inferred from RHESSI data as the input to the radiative hydrodynamic code RADYN to simulate the atmospheric response. We then synthesized various chromospheric emission lines and compared them with the IRIS and IBIS observations. In general, the synthetic intensities agree with the observed ones, especially near the northern footpoint of the flare. The simulated Mg II line profile has narrower wings than the observed one. This discrepancy can be reduced by using a higher microturbulent velocity (27 km s(-1)) in a narrow chromospheric layer. In addition, we found that an increase of electron density in the upper chromosphere within a narrow height range of similar to 800. km below the transition region can turn the simulated Mg II line core into emission and thus reproduce the single peaked profile, which is a common feature in all IRIS flares.
C1 [da Costa, Fatima Rubio; Petrosian, Vahe] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Kleint, Lucia] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland.
[Liu, Wei] Bay Area Environm Res Inst, 625 2nd St,Suite 209, Petaluma, CA 94952 USA.
[Allred, Joel C.] NASA Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RP da Costa, FR (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
EM frubio@stanford.edu
RI Rubio da Costa, Fatima/F-8156-2010
OI Rubio da Costa, Fatima/0000-0002-8322-7141
FU NASA [NNX13AF79G, NNX14AG03G]; Marie Curie Fellowship; ESA; Norwegian
Space Centre
FX Work performed by F.R.dC, V.P. and W.L. is supported by NASA grants
NNX13AF79G and NNX14AG03G. L.K. is supported by a Marie Curie
Fellowship. J.C.A. is supported by NASA LWS and HSR grants. We thank J.
Leenaarts, A. Kowalski, and F. Effenberger for their helpful
discussions. We gratefully acknowledge the use of supercomputer
resources provided by the NASA High-End Computing (HEC) program through
the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
IRIS is a NASA small explorer mission developed and operated by LMSAL
with mission operations executed at NASA Ames Research center and major
contributions to downlink communications funded by ESA and the Norwegian
Space Centre.
NR 42
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
VL 827
IS 1
AR 38
DI 10.3847/0004-637X/827/1/38
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500038
ER
PT J
AU Fukumura, K
Hendry, D
Clark, P
Tombesi, F
Takahashi, M
AF Fukumura, Keigo
Hendry, Douglas
Clark, Peter
Tombesi, Francesco
Takahashi, Masaaki
TI SOFT X-RAY EXCESS FROM SHOCKED ACCRETING PLASMA IN ACTIVE GALACTIC
NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: individual
(Ark. 120); galaxies: Seyfert; magnetohydrodynamics (MHD); methods:
numerical
ID SEYFERT 1 GALAXIES; KERR BLACK-HOLE; LINE REGION SIZES; SPECTRAL
PROPERTIES; STANDING SHOCKS; PARTICLE-ACCELERATION; REFLECTION MODELS;
COMPACT OBJECTS; MAGNETIC-FIELD; CENTRAL MASSES
AB We propose a novel theoretical model to describe the physical identity of the soft X-ray excess that is ubiquitously detected in many Seyfert galaxies, by considering a steady-state, axisymmetric plasma accretion within the innermost stable circular orbit around a black hole (BH) accretion disk. We extend our earlier theoretical investigations on general relativistic magnetohydrodynamic accretion, which implied that the accreting plasma can develop into a standing shock under suitable physical conditions, causing the downstream flow to be sufficiently hot due to shock compression. We perform numerical calculations to examine, for sets of fiducial plasma parameters, the physical nature of fast magnetohydrodynamic shocks under strong gravity for different BH spins. We show that thermal seed photons from the standard accretion disk can be effectively Compton up-scattered by the energized sub-relativistic electrons in the hot downstream plasma to produce the soft excess feature in X-rays. As a case study, we construct a three-parameter Comptonization model of inclination angle theta(obs), disk photon temperature kT(in), and downstream electron energy kT(e) to calculate the predicted spectra in comparison with a 60 ks XMM-Newton/EPIC-pn spectrum of a typical radio-quiet Seyfert 1 active galactic nucleus, Ark. 120. Our Chi(2)-analyses demonstrate that the model is plausible for successfully describing data for both non-spinning and spinning BHs with derived ranges of 61.3 keV less than or similar to kT(e) less than or similar to 144.3 keV, 21.6 eV less than or similar to kT(in) less than or similar to 34.0 eV, and 17 degrees.5 less than or similar to theta(obs) less than or similar to 42 degrees.6, indicating a compact Comptonizing region of three to four gravitational radii that resembles the putative X-ray coronae.
C1 [Fukumura, Keigo; Hendry, Douglas; Clark, Peter] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
[Tombesi, Francesco] 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.
[Takahashi, Masaaki] Aichi Univ Educ, Dept Phys & Astron, Kariya, Aichi 4488542, Japan.
[Fukumura, Keigo] UC Santa Barbara, Santa Barbara, CA 93106 USA.
RP Fukumura, K (reprint author), James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.; Fukumura, K (reprint author), UC Santa Barbara, Santa Barbara, CA 93106 USA.
EM fukumukx@jmu.edu
FU 4-VA Collaborative at James Madison University
FX The authors acknowledge the anonymous referee for useful comments and
questions. K.F. is grateful to Omer Blaes for his insightful suggestions
about the disk simulations and Rozenn Boissay for a number of useful
comments. Part of this work was conducted while at KITP of UCSB and was
also supported in part by the 4-VA Collaborative at James Madison
University.
NR 117
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
VL 827
IS 1
AR 31
DI 10.3847/0004-637X/827/1/31
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500031
ER
PT J
AU Hensley, BS
Draine, BT
Meisner, AM
AF Hensley, Brandon S.
Draine, B. T.
Meisner, Aaron M.
TI A CASE AGAINST SPINNING PAHS AS THE SOURCE OF THE ANOMALOUS MICROWAVE
EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; radiation mechanisms: general; radio continuum: ISM
ID PERSEUS MOLECULAR-COMPLEX; DIFFUSE INTERSTELLAR-MEDIUM; CENTIMETER-WAVE
CONTINUUM; POWER SPECTRUM ESTIMATION; DUST EMISSION; GALACTIC EMISSION;
ANISOTROPY-PROBE; COMPONENT SEPARATION; INFRARED-EMISSION; NGC 6946
AB We employ an all-sky map of the anomalous microwave emission (AME) produced by component separation of the microwave sky to study correlations between the AME and Galactic dust properties. We find that while the AME is highly correlated with all tracers of dust emission, the best predictor of the AME strength is the dust radiance. Fluctuations in the AME intensity per dust radiance are uncorrelated with fluctuations in the emission from polycyclic aromatic hydrocarbons (PAHs), casting doubt on the association between AME and PAHs. The PAH abundance is strongly correlated with the dust optical depth and dust radiance, consistent with PAH destruction in low density regions. We find that the AME intensity increases with increasing radiation field strength, at variance with predictions from the spinning dust hypothesis. Finally, the temperature dependence of the AME per dust radiance disfavors the interpretation of the AME as thermal emission. A reconsideration of other AME carriers, such as ultrasmall silicates, and other emission mechanisms, such as magnetic dipole emission, is warranted.
C1 [Hensley, Brandon S.; Draine, B. T.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hensley, Brandon S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Meisner, Aaron M.] Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Meisner, Aaron M.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Hensley, BS (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.; Hensley, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brandon.s.hensley@jpl.nasa.gov
FU NSF grant [AST-1408723]; National Aeronautics and Space Administration;
Office of Science, Office of High Energy Physics, of the U.S. Department
of Energy [DE-AC02-05CH11231]
FX We thank the anonymous referee for helpful comments that improved the
quality of this work, and Kieran Cleary, Hans Kristian Eriksen, Doug
Finkbeiner, Chelsea Huang, Alex Lazarian, Mike Peel, David Spergel,
Ingunn Wehus, and Chris White for stimulating conversations. B.S.H. and
B.T.D. acknowledge support from NSF grant AST-1408723. The research was
carried out in part at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. This work was supported in part by the
Director, Office of Science, Office of High Energy Physics, of the U.S.
Department of Energy under contract No. DE-AC02-05CH11231.
NR 62
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
VL 827
IS 1
AR 45
DI 10.3847/0004-637X/827/1/45
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500045
ER
PT J
AU Kay, C
Opher, M
Colaninno, RC
Vourlidas, A
AF Kay, C.
Opher, M.
Colaninno, R. C.
Vourlidas, A.
TI USING ForeCAT DEFLECTIONS AND ROTATIONS TO CONSTRAIN THE EARLY EVOLUTION
OF CMEs
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs)
ID CORONAL MASS EJECTIONS; MAGNETIC-FLUX TUBES; 2010 APRIL 8; ARRIVAL
TIMES; 1 AU; PROPAGATION; EARTH; ROPE; ERUPTION; SUN
AB To accurately predict the space weather effects of the impacts of coronal mass ejection (CME) at Earth one must know if and when a CME will impact Earth and the CME parameters upon impact. In 2015 Kay et al. presented. Forecasting a CME's Altered Trajectory (ForeCAT), a model for CME deflections based on the magnetic forces from the background solar magnetic field. Knowing the deflection and rotation of a CME enables prediction of Earth impacts and the orientation of the CME upon impact. We first reconstruct the positions of the 2010 April 8. and the 2012 July 12 CMEs from the observations. The first of these CMEs exhibits significant deflection and rotation (34 degrees deflection and 58 degrees rotation), while the second shows almost no deflection or rotation (< 3 degrees each). Using ForeCAT, we explore a range of initial parameters, such as the CME's location and size, and find parameters that can successfully reproduce the behavior for each CME. Additionally, since the deflection depends strongly on the behavior of a CME in the low corona, we are able to constrain the expansion and propagation of these CMEs in the low corona.
C1 [Kay, C.; Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Colaninno, R. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Vourlidas, A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Kay, C.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kay, C (reprint author), Boston Univ, Dept Astron, Boston, MA 02215 USA.; Kay, C (reprint author), NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM christina.d.kay@nasa.gov
RI Vourlidas, Angelos/C-8231-2009;
OI Vourlidas, Angelos/0000-0002-8164-5948; Colaninno,
Robin/0000-0002-3253-4205
FU JHU/APL; NASA [S-136361-Y]
FX C.K.'s research was supported by an appointment to the NASA Postdoctoral
Program at NASA GSFC, administered by the Universities Space Research
Association under contract with NASA. A.V. acknowledges support from
JHU/APL. R.C.C. acknowledges the support of NASA contract S-136361-Y to
NRL. The SECCHI data are produced by an international consortium of the
NRL, LMSAL, and NASA GSFC (USA), RAL and Univ. of Birmingham (UK), MPS
(Germany), CSL (Belgium), IOTA and IAS (France).
NR 51
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
VL 827
IS 1
AR 70
DI 10.3847/0004-637X/827/1/70
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500070
ER
PT J
AU Kostov, VB
Orosz, JA
Welsh, WF
Doyle, LR
Fabrycky, DC
Haghighipour, N
Quarles, B
Short, DR
Cochran, WD
Endl, M
Ford, EB
Gregorio, J
Hinse, TC
Isaacson, H
Jenkins, JM
Jensen, ELN
Kane, S
Kull, I
Latham, DW
Lissauer, JJ
Marcy, GW
Mazeh, T
Muller, TWA
Pepper, J
Quinn, SN
Ragozzine, D
Shporer, A
Steffen, JH
Torres, G
Windmiller, G
Borucki, WJ
AF Kostov, Veselin B.
Orosz, Jerome A.
Welsh, William F.
Doyle, Laurance R.
Fabrycky, Daniel C.
Haghighipour, Nader
Quarles, Billy
Short, Donald R.
Cochran, William D.
Endl, Michael
Ford, Eric B.
Gregorio, Joao
Hinse, Tobias C.
Isaacson, Howard
Jenkins, Jon M.
Jensen, Eric L. N.
Kane, Stephen
Kull, Ilya
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Mazeh, Tsevi
Mueller, Tobias W. A.
Pepper, Joshua
Quinn, Samuel N.
Ragozzine, Darin
Shporer, Avi
Steffen, Jason H.
Torres, Guillermo
Windmiller, Gur
Borucki, William J.
TI KEPLER-1647B: THE LARGEST AND LONGEST-PERIOD KEPLER TRANSITING
CIRCUMBINARY PLANET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: individual (KIC-5473556,
Kepler-1647); techniques: photometric
ID TERRESTRIAL EXTRASOLAR PLANETS; CLOSE BINARY-SYSTEMS; MAIN-SEQUENCE
STARS; M-CIRCLE-DOT; ECLIPSING BINARIES; CM-DRACONIS; TIDAL-EVOLUTION;
DATA RELEASE; SPECTROSCOPIC BINARIES; ECHELLE-SPECTROMETER
AB We report the discovery of a new Kepler transiting circumbinary planet (CBP). This latest addition to the stillsmall family of CBPs defies the current trend of known short-period planets orbiting near the stability limit of binary stars. Unlike the previous discoveries, the planet revolving around the eclipsing binary system Kepler-1647 has a very long orbital period (similar to 1100 days) and was at conjunction only twice during the Kepler mission lifetime. Due to the singular configuration of the system, Kepler-1647b is not only the longest-period transiting CBP at the time of writing, but also one of the longest-period transiting planets. With a radius of 1.06 +/- 0.01 RJup, it is also the largest CBP to date. The planet produced three transits in the light curve of Kepler-1647 (one of them during an eclipse, creating a syzygy) and measurably perturbed the times of the stellar eclipses, allowing us to measure its mass, 1.52 +/- 0.65M(Jup). The planet revolves around an 11-day period eclipsing binary consisting of two solar-mass stars on a slightly inclined, mildly eccentric (e(bin) = 0.16), spin-synchronized orbit. Despite having an orbital period three times longer than Earth's, Kepler-1647b is in the conservative habitable zone of the binary star throughout its orbit.
C1 [Kostov, Veselin B.] NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA.
[Orosz, Jerome A.; Welsh, William F.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.
[Doyle, Laurance R.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Welsh, William F.] IMoP, Principia Coll, One Maybeck Pl, Elsah, IL 62028 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Quarles, Billy] Univ Nebraska, Dept Phys & Phys Sci, Kearney, NE 68849 USA.
[Quarles, Billy] NASA, Ames Res Ctr, Space Sci Div MS 245 3, Code SST, Moffett Field, CA 94035 USA.
[Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Ford, Eric B.] Penn State Univ, Dept Astron & Astrophys, 428A Davey Lab, University Pk, PA 16802 USA.
[Gregorio, Joao] Atalaia Grp, Portalegre, Portugal.
[Gregorio, Joao] Crow Observ, Portalegre, Portugal.
[Hinse, Tobias C.] Korea Astron & Space Sci Inst KASI, Adv Astron & Space Sci Div, Daejeon 305348, South Korea.
[Hinse, Tobias C.] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.; Lissauer, Jack J.; Borucki, William J.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Kane, Stephen] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
[Kull, Ilya; Mazeh, Tsevi] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel.
[Latham, David W.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Mueller, Tobias W. A.] Univ Tubingen, Inst Astron & Astrophys, Morgenstelle 10, D-72076 Tubingen, Germany.
[Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA.
[Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl NE Suite 600, Atlanta, GA 30303 USA.
[Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Steffen, Jason H.] Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA.
RP Kostov, VB (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA.
EM veselin.b.kostov@nasa.gov
OI Jensen, Eric/0000-0002-4625-7333; /0000-0001-6545-639X; Pepper,
Joshua/0000-0002-3827-8417
FU NASA's Science Mission Directorate; TRES instrument on the Fred L.
Whipple Observatory 1.5 m telescope; Tull Coude Spectrograph on the
McDonald Observatory 2.7 m Harlan J. Smith Telescope; HIRES instrument
on the W. M. Keck Observatory 10 m telescope; HamSpec instrument on the
Lick Observatory 3.5 m Shane telescope; WHIRC instrument on the WIYN 4 m
telescope; Swarthmore College Observatory 0.6 m telescope; Canela's
Robotic Observatory 0.3 m telescope; NASA under the Exoplanet
Exploration Program; NASA Postdoctoral Program at the Goddard Space
Flight Center; NASA Postdoctoral Program at the Ames Research Center;
NASA [NNX13AI76G, NNX14AB91G]; NASA ADAP program [NNX13AF20G]; NASA PAST
program [NNX14AJ38G]; KASI research grant [2015-1-850-04]; NASA through
the Sagan Fellowship Program
FX We thank the referee for the insightful comments that helped us improve
this paper. We thank Gibor Basri and Andrew Collier Cameron for helpful
discussions regarding stellar activity, and Michael Abdul-Masih, Kyle
Conroy, and Andrej Prsa for discussing the photometric centroid shifts
and John Hood for his support. This research used observations from the
Kepler mission, which is funded by NASA's Science Mission Directorate;
the TRES instrument on the Fred L. Whipple Observatory 1.5 m telescope;
the Tull Coude Spectrograph on the McDonald Observatory 2.7 m Harlan J.
Smith Telescope; the HIRES instrument on the W. M. Keck Observatory 10 m
telescope; the HamSpec instrument on the Lick Observatory 3.5 m Shane
telescope; the WHIRC instrument on the WIYN 4 m telescope; the
Swarthmore College Observatory 0.6 m telescope; and the Canela's Robotic
Observatory 0.3 m telescope. This research made use of the SIMBAD
database, operated at CDS, Strasbourg, France; data products from the
Two Micron All Sky Survey (2MASS) and the United Kingdom Infrared
Telescope (UKIRT); and the NASA exoplanet archive NexSci49
and the NASA Community Follow-Up Observation Program (CFOP) website,
operated by the NASA Exoplanet Science Institute and the California
Institute of Technology, under contract with NASA under the Exoplanet
Exploration Program. V.B.K. and B.Q. gratefully acknowledge support by
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center and at the Ames Research Center, administered by Oak Ridge
Associated Universities through a contract with NASA. W.F.W., J.A.O.,
G.W., and B.Q. gratefully acknowledge support from NASA via grants
NNX13AI76G and NNX14AB91G. N.H. acknowledges support from the NASA ADAP
program under grant NNX13AF20G and NASA PAST program grant NNX14AJ38G.
T.C.H. acknowledges support from KASI research grant 2015-1-850-04. Part
of the numerical computations have been carried out using the SFI/HEA
Irish Center for High-End Computing (ICHEC) and the POLARIS computing
cluster at the Korea Astronomy and Space Science Institute (KASI). 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 134
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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 AUG 10
PY 2016
VL 827
IS 1
AR 86
DI 10.3847/0004-637X/827/1/86
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500086
ER
PT J
AU Ngo, H
Knutson, HA
Hinkley, S
Bryan, M
Crepp, JR
Batygin, K
Crossfield, I
Hansen, B
Howard, AW
Johnson, JA
Mawet, D
Morton, TD
Muirhead, PS
Wang, J
AF Ngo, Henry
Knutson, Heather A.
Hinkley, Sasha
Bryan, Marta
Crepp, Justin R.
Batygin, Konstantin
Crossfield, Ian
Hansen, Brad
Howard, Andrew W.
Johnson, John A.
Mawet, Dimitri
Morton, Timothy D.
Muirhead, Philip S.
Wang, Ji
TI FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT
FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE
KOZAI-LIDOV MIGRATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; methods: observational; planetary
systems; planets and satellites: dynamical evolution and stability;
techniques: high angular resolution
ID SPIN-ORBIT MISALIGNMENT; COLOR-MAGNITUDE DIAGRAMS; LUCKY IMAGING SEARCH;
TRANSIT LIGHT-CURVE; IN-SITU FORMATION; SOLAR-TYPE STARS; LOW-MASS
STARS; GAS-GIANT; HOST STARS; KEPLER OBJECTS
AB Stellar companions can influence the formation and evolution of planetary systems, but there are currently few observational constraints on the properties of planet-hosting binary star systems. We search for stellar companions around 77 transiting hot Jupiter systems to explore the statistical properties of this population of companions as compared to field stars of similar spectral type. After correcting for survey incompleteness, we find that 47% +/- 7% of hot Jupiter systems have stellar companions with semimajor axes between 50 and 2000 au. This is 2.9 times larger than the field star companion fraction in this separation range, with a significance of 4.4 sigma. In the 1-50 au range, only 3.9(-2.0)(+4.5)% of hot Jupiters host stellar companions, compared to the field star value of 16.4% +/- 0.7%, which is a 2.7 sigma difference. We find that the distribution of mass ratios for stellar companions to hot Jupiter systems peaks at small values and therefore differs from that of field star binaries which tend to be uniformly distributed across all mass ratios. We conclude that either wide separation stellar binaries are more favorable sites for gas giant planet formation at all separations, or that the presence of stellar companions preferentially causes the inward migration of gas giant planets that formed farther out in the disk via dynamical processes such as Kozai-Lidov oscillations. We determine that less than 20% of hot Jupiters have stellar companions capable of inducing Kozai-Lidov oscillations assuming initial semimajor axes between 1 and 5 au, implying that the enhanced companion occurrence is likely correlated with environments where gas giants can form efficiently.
C1 [Ngo, Henry; Knutson, Heather A.; Batygin, Konstantin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hinkley, Sasha] Univ Exeter, Dept Phys & Astron, Exeter, Devon, England.
[Bryan, Marta; Mawet, Dimitri; Wang, Ji] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Crossfield, Ian] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Hansen, Brad] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Johnson, John A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Mawet, Dimitri] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Morton, Timothy D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Muirhead, Philip S.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
RP Ngo, H (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM hngo@caltech.edu
RI Muirhead, Philip/H-2273-2014;
OI Muirhead, Philip/0000-0002-0638-8822; Ngo, Henry/0000-0001-5172-4859
FU NASA [NNX14AD24G]; Natural Sciences and Engineering Research Council of
Canada; NASA Earth and Space Science Fellowship Program [NNX15AR12H];
California Institute of Technology
FX This work was supported by NASA grant NNX14AD24G. H.N. is grateful for
funding support from the Natural Sciences and Engineering Research
Council of Canada and the NASA Earth and Space Science Fellowship
Program grant NNX15AR12H.; This work was based on observations at the W.
M. Keck Observatory granted by the California Institute of Technology.
We thank the observers who contributed to the measurements reported here
and acknowledge the efforts of the Keck Observatory staff. We extend
special thanks to those of Hawaiian ancestry on whose sacred mountain of
Mauna Kea we are privileged to be guests.
NR 107
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
VL 827
IS 1
AR 8
DI 10.3847/0004-637X/827/1/8
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500008
ER
PT J
AU Nord, B
Buckley-Geer, E
Lin, H
Diehl, HT
Helsby, J
Kuropatkin, N
Amara, A
Collett, T
Allam, S
Caminha, GB
De Bom, C
Desai, S
Dumet-Montoya, H
Pereira, MED
Finley, DA
Flaugher, B
Furlanetto, C
Gaitsch, H
Gill, M
Merritt, KW
More, A
Tucker, D
Saro, A
Rykoff, ES
Rozo, E
Birrer, S
Abdalla, FB
Agnello, A
Auger, M
Brunner, RJ
Kind, MC
Castander, FJ
Cunha, CE
da Costa, LN
Foley, RJ
Gerdes, DW
Glazebrook, K
Gschwend, J
Hartley, W
Kessler, R
Lagattuta, D
Lewis, G
Maia, MAG
Makler, M
Menanteau, E
Niernberg, A
Scolnic, D
Vieira, JD
Gramillano, R
Abbott, TMC
Banerji, M
Benoit-Levy, A
Brooks, D
Burke, DL
Capozzi, D
Rosell, AC
Carretero, J
Andrea, CBD
Dietrich, JP
Doel, P
Evrard, AE
Frieman, J
Gaztanaga, E
Gruen, D
Honscheid, K
James, DJ
Kuehn, K
Li, TS
Lima, M
Marshall, JL
Martini, P
Melchior, P
Miquel, R
Neilsen, E
Nichol, RC
Ogando, R
Plazas, AA
Romer, AK
Sako, M
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, E
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Walker, AR
Wester, W
Zhang, Y
AF Nord, B.
Buckley-Geer, E.
Lin, H.
Diehl, H. T.
Helsby, J.
Kuropatkin, N.
Amara, A.
Collett, T.
Allam, S.
Caminha, G. B.
De Bom, C.
Desai, S.
Dumet-Montoya, H.
Pereira, M. Elidaiana da S.
Finley, D. A.
Flaugher, B.
Furlanetto, C.
Gaitsch, H.
Gill, M.
Merritt, K. W.
More, A.
Tucker, D.
Saro, A.
Rykoff, E. S.
Rozo, E.
Birrer, S.
Abdalla, F. B.
Agnello, A.
Auger, M.
Brunner, R. J.
Kind, M. Carrasco
Castander, F. J.
Cunha, C. E.
da Costa, L. N.
Foley, R. J.
Gerdes, D. W.
Glazebrook, K.
Gschwend, J.
Hartley, W.
Kessler, R.
Lagattuta, D.
Lewis, G.
Maia, M. A. G.
Makler, M.
Menanteau, E.
Niernberg, A.
Scolnic, D.
Vieira, J. D.
Gramillano, R.
Abbott, T. M. C.
Banerji, M.
Benoit-Levy, A.
Brooks, D.
Burke, D. L.
Capozzi, D.
Rosell, A. Carnero
Carretero, J.
Andrea, C. B. D'
Dietrich, J. P.
Doel, P.
Evrard, A. E.
Frieman, J.
Gaztanaga, E.
Gruen, D.
Honscheid, K.
James, D. J.
Kuehn, K.
Li, T. S.
Lima, M.
Marshall, J. L.
Martini, P.
Melchior, P.
Miquel, R.
Neilsen, E.
Nichol, R. C.
Ogando, R.
Plazas, A. A.
Romer, A. K.
Sako, M.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, E.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Walker, A. R.
Wester, W.
Zhang, Y.
CA DES Collaboration
TI OBSERVATION AND CONFIRMATION OF SIX STRONG-LENSING SYSTEMS IN THE DARK
ENERGY SURVEY SCIENCE VERIFICATION DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; galaxies:
distances and redshifts; gravitational lensing: strong; methods:
observational; techniques: spectroscopic
ID ATACAMA COSMOLOGY TELESCOPE; ALL-SKY SURVEY; GRAVITATIONALLY LENSED
QUASARS; OPTICAL IMAGING SURVEYS; SOUTH-POLE TELESCOPE; GALAXY STRONG
LENSES; SPT-SZ SURVEY; MULTIOBJECT SPECTROGRAPH; SUBMILLIMETER GALAXIES;
AUTOMATIC DETECTION
AB We report the observation and confirmation of the first group-and cluster-scale strong gravitational lensing systems found in Dark Energy Survey data. Through visual inspection of data from the Science Verification season, we identified 53 candidate systems. We then obtained spectroscopic follow-up of 21 candidates using the Gemini Multi-object Spectrograph at the Gemini South telescope and the Inamori-Magellan Areal Camera and Spectrograph at the Magellan/Baade telescope. With this follow-up, we confirmed six candidates as gravitational lenses: three of the systems are newly discovered, and the remaining three were previously known. Of the 21 observed candidates, the remaining 15 either were not detected in spectroscopic observations, were observed and did not exhibit continuum emission (or spectral features), or were ruled out as lensing systems. The confirmed sample consists of one group-scale and five galaxy-cluster-scale lenses. The lensed sources range in redshift z similar to 0.80-3.2 and in i-band surface brightness i(SB) similar to 23-25 mag arcsec(-2) (2 '' aperture). For each of the six systems, we estimate the Einstein radius theta(E) and the enclosed mass M-enc, which have ranges theta(E) similar to 5 ''-9 '' and M-enc similar to 8 x 10(12) to 6 x 10(13)M(circle dot), respectively.
C1 [Nord, B.; Buckley-Geer, E.; Lin, H.; Diehl, H. T.; Kuropatkin, N.; Allam, S.; Finley, D. A.; Flaugher, B.; Gaitsch, H.; Merritt, K. W.; Tucker, D.; Frieman, J.; Neilsen, E.; Scarpine, V.; Soares-Santos, M.; Sobreira, E.; Wester, W.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Helsby, J.; Kessler, R.; Scolnic, D.; Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Amara, A.; Birrer, S.; Hartley, W.] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland.
[Collett, T.; Capozzi, D.; Andrea, C. B. D'; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Caminha, G. B.; De Bom, C.; Pereira, M. Elidaiana da S.; Makler, M.] ICRA, Ctr Brasileiro Pesquisas Fis, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Caminha, G. B.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy.
[De Bom, C.] Ctr Fed Educ Tecnol Celso Suckow Fonseca, Rodovia Mario Covas,Lote J2,Quadra J, BR-23810000 Itaguai, RJ, Brazil.
[Desai, S.; Dietrich, J. P.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.; Dietrich, J. P.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Dumet-Montoya, H.] Univ Fed Rio de Janeiro, Campus Macac,Rua Aloisio Gomes da Silva, BR-27930560 Macac, RJ, Brazil.
[Furlanetto, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Gill, M.; Rykoff, E. S.; Burke, D. L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[More, A.] Univ Tokyo, Kavli IPMU WPI, UTIAS, Kashiwa, Chiba 2778583, Japan.
[Saro, A.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Rykoff, E. S.; Cunha, C. E.; Burke, D. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Agnello, A.] PAB, Dept Phys & Astron, 430 Portola Plaza,Box 951547, Los Angeles, CA 90095 USA.
[Auger, M.; Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Brunner, R. J.; Kind, M. Carrasco; Foley, R. J.; Menanteau, E.; Vieira, J. D.; Gramillano, R.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 Green St, Urbana, IL 61801 USA.
[Brunner, R. J.; Kind, M. Carrasco; Menanteau, E.; Vieira, J. D.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[Castander, F. J.; Carretero, J.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Caner Can Magrans,S-N, E-08193 Barcelona, Spain.
[da Costa, L. N.; Gschwend, J.; Maia, M. A. G.; Rosell, A. Carnero; Lima, M.; Ogando, R.; Sobreira, E.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[da Costa, L. N.; Gschwend, J.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RI, Brazil.
[Foley, R. J.; Vieira, J. D.; Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Gerdes, D. W.; Evrard, A. E.; Schubnell, M.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Lagattuta, D.] Univ Lyon 1, Ctr Rech Astrophys Lyon, CNRS, Observ Lyon, 9 Ave Charles Andre, F-69561 St Genis Laval, France.
[Lewis, G.] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia.
[Niernberg, A.; Honscheid, K.; Martini, P.; Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Benoit-Levy, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Benoit-Levy, A.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain.
[Andrea, C. B. D'] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Evrard, A. E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Gruen, D.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Honscheid, K.; Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Lima, M.] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sako, M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, Madrid, Spain.
RP Nord, B (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
EM nord@fnal.gov
RI Lima, Marcos/E-8378-2010; Bartosch Caminha, Gabriel/C-8952-2013; Ogando,
Ricardo/A-1747-2010; Gaztanaga, Enrique/L-4894-2014;
OI Bartosch Caminha, Gabriel/0000-0001-6052-3274; Ogando,
Ricardo/0000-0003-2120-1154; Gaztanaga, Enrique/0000-0001-9632-0815;
Abdalla, Filipe/0000-0003-2063-4345; Sobreira,
Flavia/0000-0002-7822-0658
FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of
Science and Education of Spain; Science and Technology Facilities
Council of the United Kingdom; Higher Education Funding Council for
England; National Center for Supercomputing Applications at the
University of Illinois at Urbana-Champaign; Kavli Institute of
Cosmological Physics at the University of Chicago; Center for Cosmology
and Astro-Particle Physics at the Ohio State University; Mitchell
Institute for Fundamental Physics and Astronomy at Texas AM University;
Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de
Desenvolvimento Cientfico e Tecnologico; Ministerio da Ciencia e
Tecnologia; Deutsche Forschungsgemeinschaft; National Science Foundation
[AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986];
Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERDF funds from the
European Union; Argonne National Laboratory; University of California at
Santa Cruz; University of Cambridge; Centro de Investigaciones
Energeticas; Medioambientales y Tecnologicas-Madrid; University of
Chicago; University College London; DES-Brazil Consortium;
Eidgenoessische 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 and the 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; CAPES [12203-1]; CNPq; Alfred P. Sloan Foundation; United
States Department of Energy [DE-AC02-07CH11359]
FX 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, the Center for Cosmology and
Astro-Particle Physics at the Ohio State University, the Mitchell
Institute for Fundamental Physics and Astronomy at Texas A&M University,
Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de
Desenvolvimento Cientfico e Tecnologico and the Ministerio da Ciencia e
Tecnologia, the Deutsche Forschungsgemeinschaft, and the Collaborating
Institutions in the Dark Energy Survey. The DES data management system
is supported by the National Science Foundation under Grant Number
AST-1138766. The DES participants from Spanish institutions are
partially supported by MINECO under grants AYA2012-39559, ESP2013-48274,
FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some
of which include ERDF funds from the European Union.; The Collaborating
Institutions are Argonne National Laboratory, the University of
California at Santa Cruz, the University of Cambridge, Centro de
Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the
University of Chicago, University College London, the DES-Brazil
Consortium, the Eidgenoessische 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.; C.F.
acknowledges funding from CAPES (proc. 12203-1). This paper has gone
through internal review by the DES collaboration. This research has made
use of NASA's Astrophysics Data System.; C.D.B. would like to thank CNPq
for the financial support.; R.J.F. gratefully acknowledges support from
the Alfred P. Sloan Foundation.; Fermilab is operated by Fermi Research
Alliance, LLC, under Contract No. DE-AC02-07CH11359 with the United
States Department of Energy.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J.
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PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500051
ER
PT J
AU Salmon, B
Papovich, C
Long, J
Willner, SP
Finkelstein, SL
Ferguson, HC
Dickinson, M
Duncan, K
Faber, SM
Hathi, N
Koekemoer, A
Kurczynski, P
Newman, J
Pacifici, C
Perez-Gonzalez, PG
Pforr, J
AF Salmon, Brett
Papovich, Casey
Long, James
Willner, S. P.
Finkelstein, Steven L.
Ferguson, Henry C.
Dickinson, Mark
Duncan, Kenneth
Faber, S. M.
Hathi, Nimish
Koekemoer, Anton
Kurczynski, Peter
Newman, Jeffery
Pacifici, Camilla
Perez-Gonzalez, Pablo G.
Pforr, Janine
TI BREAKING THE CURVE WITH CANDELS: A BAYESIAN APPROACH TO REVEAL THE
NON-UNIVERSALITY OF THE DUST-ATTENUATION LAW AT HIGH REDSHIFT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: high-redshift;
galaxies: statistics
ID STAR-FORMING GALAXIES; SIMILAR-TO 2; SPECTRAL ENERGY-DISTRIBUTION;
ORIGINS DEEP SURVEY; GOODS-SOUTH FIELD; STELLAR POPULATION SYNTHESIS;
EXTRAGALACTIC LEGACY SURVEY; LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC
NUCLEI; SMALL-MAGELLANIC-CLOUD
AB Dust attenuation affects nearly all observational aspects of galaxy evolution, yet very little is known about the form of the dust-attenuation law in the distant universe. Here, we model the spectral energy distributions of galaxies at z similar to 1.5-3 from CANDELS with rest-frame UV to near-IR imaging under different assumptions about the dust law, and compare the amount of inferred attenuated light with the observed infrared (IR) luminosities. Some individual galaxies show strong Bayesian evidence in preference of one dust law over another, and this preference agrees with their observed location on the plane of infrared excess (IRX, L-TIR/L-UV) and UV slope (beta). We generalize the shape of the dust law with an empirical model, A(lambda,delta) = E(B - V)k(lambda) (lambda/lambda(V))(delta) where k(lambda) is the dust law of Calzetti et al., and show that there exists a correlation between the color excess E (B-V) and tilt delta with delta = (0.62 +/- 0.05)log(E(B - V))+(0.26 +/- 0.02). Galaxies with high color excess have a shallower, starburst-like law, and those with low color excess have a steeper, SMC-like law. Surprisingly, the galaxies in our sample show no correlation between the shape of the dust law and stellar mass, star formation rate, or beta. The change in the dust law with color excess is consistent with a model where attenuation is caused by scattering, a mixed star-dust geometry, and/or trends with stellar population age, metallicity, and dust grain size. This rest-frame UV-to-near-IR method shows potential to constrain the dust law at even higher redshifts (z > 3).
C1 [Salmon, Brett; Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA.
[Long, James] Texas A&M Univ, Dept Stat, College Stn, TX 77843 USA.
[Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Ferguson, Henry C.; Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Duncan, Kenneth] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Duncan, Kenneth] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Faber, S. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Hathi, Nimish; Pforr, Janine] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Kurczynski, Peter] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Newman, Jeffery] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Newman, Jeffery] PITT PACC, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Pacifici, Camilla] Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
[Perez-Gonzalez, Pablo G.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
RP Salmon, B (reprint author), Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA.
EM bsalmon@physics.tamu.edu
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Salmon, Brett/0000-0002-7453-7279;
Koekemoer, Anton/0000-0002-6610-2048
FU National Aeronautics and Space Administration (NASA) [NAS5-26555]; HST
program [GO-12060]; NASA grant from Space Telescope Science Institute
[GO-12060]; Spanish MINECO [AYA2012-31277]
FX We thank the referee for thoughtful and constructive feedback on this
work. We acknowledge our colleagues in the CANDELS collaboration for
very useful comments and suggestions. We also thank the great effort of
all the CANDELS team members for their work to provide a robust and
valuable data set. We thank Karl Gordon for insightful discussions on
the physical implications of these results. We also thank Daniela
Calzetti and Veronique Buat for helpful comments and comments. This work
is based in part on observations taken by the CANDELS Multi-Cycle
Treasury Program with the NASA/ESA HST, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. This work is supported by HST program No. GO-12060.
Support for Program No. GO-12060 was provided by NASA through a grant
from the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. We acknowledge the Spanish MINECO grant
AYA2012-31277 for funding the contribution from Pablo Perez-Gonzalez.
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 contract with the National
Aeronautics and Space Administration (NASA). The authors acknowledge the
Texas A&M University Brazos HPC cluster that contributed to the research
reported here. URL: http://brazos.tamu.edu.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500020
ER
PT J
AU Sinukoff, E
Howard, AW
Petigura, EA
Schlieder, JE
Crossfield, IJM
Ciardi, DR
Fulton, BJ
Isaacson, H
Aller, KM
Baranec, C
Beichman, CA
Hansen, BMS
Knutson, HA
Law, NM
Liu, MC
Riddle, R
Dressing, CD
AF Sinukoff, Evan
Howard, Andrew W.
Petigura, Erik A.
Schlieder, Joshua E.
Crossfield, Ian J. M.
Ciardi, David R.
Fulton, Benjamin J.
Isaacson, Howard
Aller, Kimberly M.
Baranec, Christoph
Beichman, Charles A.
Hansen, Brad M. S.
Knutson, Heather A.
Law, Nicholas M.
Liu, Michael C.
Riddle, Reed
Dressing, Courtney D.
TI ELEVEN MULTIPLANET SYSTEMS FROM K2 CAMPAIGNS 1 AND 2 AND THE MASSES OF
TWO HOT SUPER-EARTHS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: late-type; stars: solar-type; techniques:
photometric; techniques: radial velocities; techniques: spectroscopic
ID MAIN-SEQUENCE STARS; INFRARED TELESCOPE FACILITY; LASER ADAPTIVE OPTICS;
PLANETARY CANDIDATES; M-DWARFS; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS;
SOLID EXOPLANETS; RADIAL-VELOCITY; BAND SPECTRA
AB We present a catalog of 11 multiplanet systems from Campaigns 1 and 2 of the K2 mission. We report the sizes and orbits of 26 planets split between seven two-planet systems and four three-planet systems. These planets stem from a systematic search of the K2 photometry for all dwarf stars observed by K2 in these fields. We precisely characterized the host stars with adaptive optics imaging and analysis of high-resolution optical spectra from Keck/HIRES and medium-resolution spectra from IRTF/SpeX. We confirm two planet candidates by mass detection and validate the remaining 24 candidates to >99% confidence. Thirteen planets were previously validated or confirmed by other studies, and 24 were previously identified as planet candidates. The planets are mostly smaller than Neptune (21/26 planets), as in the Kepler mission, and all have short periods (P < 50 days) due to the duration of the K2 photometry. The host stars are relatively bright (most have Kp < 12.5 mag) and are amenable to follow-up characterization. For K2-38, we measured precise radial velocities using Keck/HIRES and provide initial estimates of the planet masses. K2-38b is a short-period super-Earth with a radius of 1.55 +/- 0.16 R-circle plus, a mass of 12.0 +/- 2.9M(circle plus), and a high density consistent with an iron-rich composition. The outer planet K2-38c is a lower-density sub-Neptune-size planet with a radius of 2.42 +/- 0.29 R-circle plus and a mass of 9.9 +/- 4.6M(circle plus) that likely has a substantial envelope. This new planet sample demonstrates the capability of K2 to discover numerous planetary systems around bright stars.
C1 [Sinukoff, Evan; Howard, Andrew W.; Fulton, Benjamin J.; Aller, Kimberly M.; Baranec, Christoph; Liu, Michael C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Petigura, Erik A.; Knutson, Heather A.; Dressing, Courtney D.] CALTECH, Pasadena, CA 91125 USA.
[Schlieder, Joshua E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Crossfield, Ian J. M.] Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA.
[Ciardi, David R.; Beichman, Charles A.] CALTECH, NASA Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA.
[Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hansen, Brad M. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Hansen, Brad M. S.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Riddle, Reed] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP Sinukoff, E (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
OI Ciardi, David/0000-0002-5741-3047; Isaacson, Howard/0000-0002-0531-1073;
Fulton, Benjamin/0000-0003-3504-5316
FU Natural Sciences and Engineering Research Council of Canada (NSERC);
Hubble Fellowship - Space Telescope Science Institute
[HST-HF2-51365.001-A]; NASA [NAS 5-26555]; NASA Astrophysics Data
Analysis Program grant; K2 Guest Observer Program; European Union
Seventh Framework Programme (FP7) [313014]; NASA Postdoctoral Program at
NASA Ames Research Center; National Science Foundation Graduate Research
Fellowship [2014184874]; Office of Science of the U.S. Department of
Energy [DE-AC02-05CH11231]; MAST [NNX09AF08G]; Robert Martin Ayers
Sciences Fund; National Science Foundation [AST-0906060, AST-0960343,
AST-1207891]; Mt. Cuba Astronomical Foundation; Robo-AO; University of
Hawai'i; Alfred P. Sloan Foundation
FX We thank Sam Grunblatt, Matthew Hosek Jr., John Livingston, and Geoff
Marcy for helpful discussions. We thank Lauren Weiss and Lea Hirsch for
their help with observing with Keck-HIRES. E.S. is supported by a
postgraduate scholarship from the Natural Sciences and Engineering
Research Council of Canada (NSERC). E.A.P. acknowledges support from a
Hubble Fellowship grant HST-HF2-51365.001-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA under contract
NAS 5-26555. A.W.H. acknowledges support for our K2 team through a NASA
Astrophysics Data Analysis Program grant. A.W.H. and I.J.M.C.
acknowledge support from the K2 Guest Observer Program. E.D.L. received
funding from the European Union Seventh Framework Programme
(FP7/2007-2013) under grant agreement no. 313014 (ETAEARTH). The
research of J.E.S. was supported by an appointment to the NASA
Postdoctoral Program at NASA Ames Research Center, administered by Oak
Ridge Associated Universities through a contract with NASA. B.J.F.
acknowledges support from a National Science Foundation Graduate
Research Fellowship under grant no. 2014184874. This research used
resources of the National Energy Research Scientific Computing Center, a
DOE Office of Science User Facility supported by the Office of Science
of the U.S. Department of Energy under Contract no. DE-AC02-05CH11231.
This work made use of the SIMBAD database (operated at CDS, Strasbourg,
France), NASA's Astrophysics Data System Bibliographic Services, and
data products from the Two Micron All Sky Survey (2MASS), the APASS
database, the SDSS-III project, and the Digitized Sky Survey. Some of
the data presented in this paper were obtained from the Mikulski Archive
for Space Telescopes (MAST). 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 was made possible through the
use of the AAVSO Photometric All-Sky Survey (APASS), funded by the
Robert Martin Ayers Sciences Fund. This study benefits from use of the
Robo-AO system, which 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 grant nos. 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. 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). 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2016
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SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500078
ER
PT J
AU Stecker, FW
Scully, ST
Malkan, MA
AF Stecker, Floyd W.
Scully, Sean T.
Malkan, Matthew A.
TI AN EMPIRICAL DETERMINATION OF THE INTERGALACTIC BACKGROUND LIGHT FROM UV
TO FIR WAVELENGTHS USING FIR DEEP GALAXY SURVEYS AND THE GAMMA-RAY
OPACITY OF THE UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE diffuse radiation; galaxies: luminosity function, mass function; Sun:
infrared
ID INFRARED LUMINOSITY FUNCTIONS; STAR-FORMING GALAXIES;
AROMATIC-HYDROCARBON EMISSION; EXTRAGALACTIC LEGACY SURVEY; SIMILAR-TO
4; MU-M; OPTICAL DEPTH; SPITZER VIEW; EVOLUTION; SPECTRUM
AB We have previously calculated the intergalactic background light (IBL) as a function of redshift from the Lyman limit in the far-ultraviolet to a wavelength of 5 mu m in the near-infrared range, based purely on data from deep galaxy surveys. Here, we use similar methods to determine the mid-and far-infrared IBL from 5 to 850 mu m. Our approach enables us to constrain the range of photon densities by determining the uncertainties in observationally determined luminosity densities and spectral gradients. By also including the effect of the 2.7 K cosmic background photons, we determine upper and lower limits on the opacity of the universe to gamma-rays up to PeV energies within a 68% confidence band. Our direct results on the IBL are consistent with those from complimentary gamma-ray analyses using observations from the Fermi gamma-ray space telescope and the H.E.S.S. air Cerenkov telescope. Thus, we find no evidence of previously suggested processes for the modification of gamma-ray spectra other than that of absorption by pair production alone.
C1 [Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Stecker, Floyd W.; Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Scully, Sean T.] James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA.
RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.; Stecker, FW (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM Floyd.W.Stecker@nasa.gov; scullyst@jmu.edu; malkan@astro.ucla.edu
OI Malkan, Matthew/0000-0001-6919-1237
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SN 0004-637X
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JI Astrophys. J.
PD AUG 10
PY 2016
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SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500006
ER
PT J
AU Wyper, PF
deVore, CR
Karpen, JT
Lynch, BJ
AF Wyper, P. F.
deVore, C. R.
Karpen, J. T.
Lynch, B. J.
TI THREE-DIMENSIONAL SIMULATIONS OF TEARING AND INTERMITTENCY IN CORONAL
JETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: flares; Sun: magnetic fields; magnetic
reconnection
ID X-RAY JETS; CHROMOSPHERIC ANEMONE JETS; FAST MAGNETIC RECONNECTION;
CURRENT SHEETS; ACTIVE-REGION; FLUX EMERGENCE; SOLAR-FLARE; FILAMENT
ERUPTIONS; ELECTRIC-CURRENTS; MASS EJECTIONS
AB Observations of coronal jets increasingly suggest that local fragmentation and intermittency play an important role in the dynamics of these events. In this work, we investigate this fragmentation in high-resolution simulations of jets in the closed-field corona. We study two realizations of the embedded-bipole model, whereby impulsive helical outflows are driven by reconnection between twisted and untwisted field across the domed fan plane of a magnetic null. We find that the reconnection region fragments following the onset of a tearing-like instability, producing multiple magnetic null points and flux-rope structures within the current layer. The flux ropes formed within the weak-field region in the center of the current layer are associated with "blobs" of density enhancement that become filamentary threads as the flux ropes are ejected from the layer, whereupon new flux ropes form behind them. This repeated formation and ejection of flux ropes provides a natural explanation for the intermittent outflows, bright blobs of emission, and filamentary structure observed in some jets. Additional observational signatures of this process are discussed. Essentially all jet models invoke reconnection between regions of locally closed and locally open field as the jet-generation mechanism. Therefore, we suggest that this repeated tearing process should occur at the separatrix surface between the two flux systems in all jets. A schematic picture of tearing-mediated jet reconnection in three dimensions is outlined.
C1 [Wyper, P. F.] NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[deVore, C. R.; Karpen, J. T.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Lynch, B. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Wyper, PF (reprint author), NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM peter.f.wyper@nasa.gov; c.richard.devore@nasa.gov; judy.karpen@nasa.gov;
blynch@ssl.berkeley.edu
RI Wyper, Peter/H-9166-2013; Lynch, Benjamin/B-1300-2013;
OI Lynch, Benjamin/0000-0001-6886-855X
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DU1ZK
UT WOS:000382009500004
ER
PT J
AU Fragos, T
Lehmer, BD
Naoz, S
Zezas, A
Basu-Zych, A
AF Fragos, T.
Lehmer, B. D.
Naoz, S.
Zezas, A.
Basu-Zych, A.
TI ENERGY FEEDBACK FROM X-RAY BINARIES IN THE EARLY UNIVERSE (vol 776, L31,
2013)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fragos, T.; Naoz, S.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Lehmer, B. D.] Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Basu-Zych, A.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Zezas, A.] Univ Crete, Dept Phys, POB 2208, Iraklion 71003, Crete, Greece.
[Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece.
RP Fragos, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Fragos, T (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
EM tfragos@cfa.harvard.edu
RI Zezas, Andreas/C-7543-2011
OI Zezas, Andreas/0000-0001-8952-676X
NR 2
TC 0
Z9 0
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 AUG 10
PY 2016
VL 827
IS 1
AR L21
DI 10.3847/2041-8205/827/1/L21
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT2TO
UT WOS:000381334900021
ER
PT J
AU Narita, Y
Nakamura, R
Baumjohann, W
Glassmeier, KH
Motschmann, U
Giles, B
Magnes, W
Fischer, D
Torbert, RB
Russell, CT
Strangeway, RJ
Burch, JL
Nariyuki, Y
Saito, S
Gary, SP
AF Narita, Y.
Nakamura, R.
Baumjohann, W.
Glassmeier, K. -H.
Motschmann, U.
Giles, B.
Magnes, W.
Fischer, D.
Torbert, R. B.
Russell, C. T.
Strangeway, R. J.
Burch, J. L.
Nariyuki, Y.
Saito, S.
Gary, S. P.
TI ON ELECTRON-SCALE WHISTLER TURBULENCE IN THE SOLAR WIND
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE plasmas; solar wind; turbulence
ID 1 AU; MULTISCALE; STRENGTH; CLUSTER; WAVES
AB For the first time, the dispersion relation for turbulence magnetic field fluctuations in the solar wind is determined directly on small scales of the order of the electron inertial length, using four-point magnetometer observations from the Magnetospheric Multiscale mission. The data are analyzed using the high-resolution adaptive wave telescope technique. Small-scale solar wind turbulence is primarily composed of highly obliquely propagating waves, with dispersion consistent with that of the whistler mode.
C1 [Narita, Y.; Nakamura, R.; Baumjohann, W.; Magnes, W.; Fischer, D.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
[Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany.
[Motschmann, U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Theoret Phys, Braunschweig, Germany.
[Giles, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA.
[Russell, C. T.; Strangeway, R. J.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
[Nariyuki, Y.] Toyama Univ, Fac Human Dev, Toyama, Japan.
[Saito, S.] Nagoya Univ, Grad Sch Sci, Inst Space Earth Environm Res, Nagoya, Aichi, Japan.
[Gary, S. P.] Space Sci Inst, Los Alamos, NM USA.
[Glassmeier, K. -H.] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany.
[Motschmann, U.] Deutsch Zentrum Luft & Raumfahrt, Inst Planetenforsch, Berlin, Germany.
RP Narita, Y (reprint author), Austrian Acad Sci, Space Res Inst, Graz, Austria.
EM yasuhito.narita@oeaw.ac.at
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA [NNG04EB99C]; Austrian Academy of Sciences; Austrian Space
Applications Programme [FFG/ASAP-844377]; Deutsches Zentrum fur Luft-
und Raumfahrt; German Bundesministerium fur Wirtschaft und Energie [50
OC 1402]; JSPS KAKENHI [26287119]
FX The dedication and expertise of the Magnetospheric Multiscale (MMS)
development and operations teams are greatly appreciated. Work at
JHU/APL, UCLA, UNH, and SwRI was supported by NASA contract number
NNG04EB99C. We acknowledge the use of L2 survey Flux-Gate Magnetometer
data (FGM), Search-Coil Magnetometer (SCM) data, and fast survey mode
data of ion velocity moments from the Dual Ion Spectrometers (DIS) of
Fast Plasma Investigation (FPI) of the MMS spacecraft. Data are stored
at the MMS Science Data Center at https://lasp.colorado.edu/mms/sdc/ and
at Coordinated Data Analysis Web (CDAWeb; http://cdaweb.gsfc.nasa.gov/),
and are available upon request. The Austrian part of the development,
operation, and calibration of the FGM was financially supported by a
rolling grant of the Austrian Academy of Sciences and the Austrian Space
Applications Programme with the contract number FFG/ASAP-844377. K.H.G.
is financially supported by the Deutsches Zentrum fur Luft- und
Raumfahrt and the German Bundesministerium fur Wirtschaft und Energie
under contract 50 OC 1402. This work was supported by JSPS KAKENHI grant
number 26287119. Y. N. is grateful for a discussion with O. Le Contel
and L. Mirioni on the use of search coil magnetometer data on the
analyzed time interval.
NR 34
TC 7
Z9 7
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2016
VL 827
IS 1
AR L8
DI 10.3847/2041-8205/827/1/L8
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT2TO
UT WOS:000381334900008
ER
PT J
AU Tilvi, V
Pirzkal, N
Malhotra, S
Finkelstein, SL
Rhoads, JE
Windhorst, R
Grogin, NA
Koekemoer, A
Zakamska, NL
Ryan, R
Christensen, L
Hathi, N
Pharo, J
Joshi, B
Yang, H
Gronwall, C
Cimatti, A
Walsh, J
O'Connell, R
Straughn, A
Ostlin, G
Rothberg, B
Livermore, RC
Hibon, P
Gardner, JP
AF Tilvi, V.
Pirzkal, N.
Malhotra, S.
Finkelstein, S. L.
Rhoads, J. E.
Windhorst, R.
Grogin, N. A.
Koekemoer, A.
Zakamska, N. L.
Ryan, R.
Christensen, L.
Hathi, N.
Pharo, J.
Joshi, B.
Yang, H.
Gronwall, C.
Cimatti, A.
Walsh, J.
O'Connell, R.
Straughn, A.
Ostlin, G.
Rothberg, B.
Livermore, R. C.
Hibon, P.
Gardner, Jonathan P.
TI FIRST RESULTS FROM THE FAINT INFRARED GRISM SURVEY (FIGS): FIRST
SIMULTANEOUS DETECTION OF Ly alpha EMISSION AND LYMAN BREAK FROM A
GALAXY AT z=7.51
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE dark ages, reionization, first stars; early universe; galaxies:
high-redshift; intergalactic medium
ID ULTRA-DEEP-FIELD; HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC LEGACY SURVEY;
QUASI-STELLAR OBJECTS; LENS-AMPLIFIED SURVEY; SIMILAR-TO 7; LUMINOSITY
FUNCTION; SPECTROSCOPIC CONFIRMATION; COSMIC REIONIZATION; HST
SPECTROSCOPY
AB Galaxies at high redshifts are a valuable tool for studying cosmic dawn, therefore it is crucial to reliably identify these galaxies. Here, we present an unambiguous and first simultaneous detection of both the Ly alpha emission and the Lyman break from a z = 7.512 +/- 0.004 galaxy, observed in the Faint Infrared Grism Survey (FIGS). These spectra, taken with the G102 grism on the Hubble Space Telescope (HST), show a significant emission line detection (6 sigma) in two observational position angles (PAs), with Lya line flux of 1.06 +/- 0.19 x 10(-17) erg s(-1) cm(-2). The line flux is nearly a factor of four higher than that in the archival MOSFIRE spectroscopic observations. This is consistent with other recent observations, implying that ground-based near-infrared spectroscopy underestimates the total emission line fluxes, and if confirmed, can have strong implications for reionization studies that are based on ground-based Ly alpha measurements. A 4 sigma detection of the NV line in one PA also suggests a weak active galactic nucleus (AGN), and if confirmed, would make this source the highest-redshift AGN yet found. These observations from HST thus clearly demonstrate the sensitivity of the FIGS survey, and the capability of grism spectroscopy for studying the epoch of reionization.
C1 [Tilvi, V.; Malhotra, S.; Rhoads, J. E.; Windhorst, R.; Pharo, J.; Joshi, B.; Yang, H.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Pirzkal, N.; Grogin, N. A.; Koekemoer, A.; Ryan, R.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Finkelstein, S. L.; Livermore, R. C.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
[Zakamska, N. L.] Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA.
[Zakamska, N. L.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr, 3400 N Charles St, Baltimore, MD 21218 USA.
[Christensen, L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr 1, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Hathi, N.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Gronwall, C.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Gronwall, C.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Cimatti, A.] Univ Bologna, Dipartimento Fis & Astron, Alma Mater Studiorum, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Walsh, J.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[O'Connell, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Straughn, A.; Gardner, Jonathan P.] Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
[Ostlin, G.] Stockholm Univ, Dept Astron, Oscar Klein Ctr, SE-10691 Stockholm, Sweden.
[Rothberg, B.] Large Binocular Observ, Tucson, AZ 85721 USA.
[Hibon, P.] Gemini South Observ, Casilla 603, La Serena, Chile.
RP Tilvi, V (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RI Hathi, Nimish/J-7092-2014; Christensen, Lise/M-5301-2014
OI Hathi, Nimish/0000-0001-6145-5090; Christensen, Lise/0000-0001-8415-7547
FU FIGS program with the NASA/ESA HST [GO 13779]; NASA [NAS5-26555]; NASA
JWST Interdisciplinary Scientist grant from GSFC [NNX14AN10G]
FX We thank the referee for very useful feedback that improved this
manuscript. This work is based on observations taken by the FIGS program
(GO 13779) with the NASA/ESA HST, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. R.A.W. acknowledges support from NASA JWST Interdisciplinary
Scientist grant NNX14AN10G from GSFC.
NR 45
TC 0
Z9 0
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2016
VL 827
IS 1
AR L14
DI 10.3847/2041-8205/827/1/L14
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT2TO
UT WOS:000381334900014
ER
PT J
AU Walton, DJ
Furst, F
Bachetti, M
Barret, D
Brightman, M
Fabian, AC
Gehrels, N
Harrison, FA
Heida, M
Middleton, MJ
Rana, V
Roberts, TP
Stern, D
Tao, L
Webb, N
AF Walton, D. J.
Furst, F.
Bachetti, M.
Barret, D.
Brightman, M.
Fabian, A. C.
Gehrels, N.
Harrison, F. A.
Heida, M.
Middleton, M. J.
Rana, V.
Roberts, T. P.
Stern, D.
Tao, L.
Webb, N.
TI A 78 DAY X-RAY PERIOD DETECTED FROM NGC 5907 ULX1 BY SWIFT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: individual (NGC 5907 ULX1)
ID XMM-NEWTON; BLACK-HOLE; BROAD-BAND; M82 X-1; BINARIES; MASS;
VARIABILITY; ACCRETION; NUSTAR; PARAMETERS
AB We report the detection of a 78.1 +/- 0.5 day period in the X-ray light curve of the extreme ultraluminous X-ray source NGC 5907 ULX1 (L-X,L-peak similar to 5 x 10(40) erg s(-1)), discovered during an extensive monitoring program with Swift. These periodic variations are strong, with the observed flux changing by a factor of similar to 3-4 between the peaks and the troughs of the cycle; our simulations suggest that the observed periodicity is detected comfortably in excess of 3 sigma significance. We discuss possible origins for this X-ray period, but conclude that at the current time we cannot robustly distinguish between orbital and super-orbital variations.
C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Walton, D. J.; Furst, F.; Brightman, M.; Harrison, F. A.; Heida, M.; Rana, V.; Tao, L.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Bachetti, M.] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy.
[Barret, D.; Webb, N.] Univ Toulouse, IRAP, UPS OMP, Toulouse, France.
[Barret, D.; Webb, N.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Fabian, A. C.; Middleton, M. J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Roberts, T. P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Tao, L.] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China.
RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Walton, DJ (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
OI Bachetti, Matteo/0000-0002-4576-9337
FU ERC [340442]; French Space Agency (CNES); Ernest Rutherford STFC
fellowship; STFC [ST/L00075X/1]
FX The authors would like to thank the reviewer for their timely and
positive feedback, which helped to improve the final manuscript. A.C.F.
acknowledges support from ERC Advanced Grant 340442. The work of
D.J.W./D.S. was performed at JPL/Caltech, under contract with NASA. D.B.
and N.W. acknowledge financial support from the French Space Agency
(CNES), M.J.M. acknowledges support from an Ernest Rutherford STFC
fellowship, and T.P.R. acknowledges support from the STFC consolidated
grant ST/L00075X/1. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester, and also made use of
the XRT Data Analysis Software (XRTDAS) developed under the
responsibility of the ASI Science Data Center (ASDC), Italy. We
acknowledge the use of public data from the Swift data archive. This
research has also made use of a collection of ISIS functions
(ISISscripts) provided by ECAP/Remeis observatory and MIT.
NR 42
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 AUG 10
PY 2016
VL 827
IS 1
AR L13
DI 10.3847/2041-8205/827/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DT2TO
UT WOS:000381334900013
ER
PT J
AU Ern, M
Trinh, QT
Kaufmann, M
Krisch, I
Preusse, P
Ungermann, J
Zhu, YJ
Gille, JC
Mlynczak, MG
Russell, JM
Schwartz, MJ
Riese, M
AF Ern, Manfred
Quang Thai Trinh
Kaufmann, Martin
Krisch, Isabell
Preusse, Peter
Ungermann, Joern
Zhu, Yajun
Gille, John C.
Mlynczak, Martin G.
Russell, James M., III
Schwartz, Michael J.
Riese, Martin
TI Satellite observations of middle atmosphere gravity wave absolute
momentum flux and of its vertical gradient during recent stratospheric
warmings
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; POLAR MLT REGION; SUDDEN WARMINGS;
GENERAL-CIRCULATION; GLOBAL CIRCULATION; SABER EXPERIMENT; NORTHERN
WINTER; CLIMATE MODELS; MOUNTAIN WAVES; MESOSPHERE
AB Sudden stratospheric warmings (SSWs) are circulation anomalies in the polar region during winter. They mostly occur in the Northern Hemisphere and affect also surface weather and climate. Both planetary waves and gravity waves contribute to the onset and evolution of SSWs. While the role of planetary waves for SSW evolution has been recognized, the effect of gravity waves is still not fully understood, and has not been comprehensively analyzed based on global observations. In particular, information on the gravity wave driving of the background winds during SSWs is still missing.
We investigate the boreal winters from 2001/2002 until 2013/2014. Absolute gravity wave momentum fluxes and gravity wave dissipation (potential drag) are estimated from temperature observations of the satellite instruments HIRDLS and SABER. In agreement with previous work, we find that sometimes gravity wave activity is enhanced before or around the central date of major SSWs, particularly during vortex-split events. Often, SSWs are associated with polar-night jet oscillation (PJO) events. For these events, we find that gravity wave activity is strongly suppressed when the wind has reversed from eastward to westward (usually after the central date of a major SSW). In addition, gravity wave potential drag at the bottom of the newly forming eastward-directed jet is remarkably weak, while considerable potential drag at the top of the jet likely contributes to the downward propagation of both the jet and the new elevated stratopause. During PJO events, we also find some indication for poleward propagation of gravity waves. Another striking finding is that obviously localized gravity wave sources, likely mountain waves and jet-generated gravity waves, play an important role during the evolution of SSWs and potentially contribute to the triggering of SSWs by preconditioning the shape of the polar vortex. The distribution of these hot spots is highly variable and strongly depends on the zonal and meridional shape of the background wind field, indicating that a pure zonal average view sometimes is a too strong simplification for the strongly perturbed conditions during the evolution of SSWs.
C1 [Ern, Manfred; Quang Thai Trinh; Kaufmann, Martin; Krisch, Isabell; Preusse, Peter; Ungermann, Joern; Zhu, Yajun; Riese, Martin] Forschungszentrum Julich GmbH, Inst Energie & Klimaforsch, Stratosphare IEK 7, D-52425 Julich, Germany.
[Gille, John C.] Univ Colorado, Ctr Limb Atmospher Sounding, Boulder, CO 80309 USA.
[Gille, John C.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Schwartz, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ern, M (reprint author), Forschungszentrum Julich GmbH, Inst Energie & Klimaforsch, Stratosphare IEK 7, D-52425 Julich, Germany.
EM m.ern@fz-juelich.de
RI Riese, Martin/A-3927-2013; Ern, Manfred/I-8839-2016; Ungermann,
Jorn/K-7776-2012; Preusse, Peter/A-1193-2013
OI Riese, Martin/0000-0001-6398-6493; Ern, Manfred/0000-0002-8565-2125;
Ungermann, Jorn/0000-0001-9095-8332; Preusse, Peter/0000-0002-8997-4965
FU Deutsche Forschungsgemeinschaft (DFG) which is part of the DFG
researchers group MS-GWaves [PR 919/4-1]; DFG which is part of the DFG
priority program SPP1788 "Dynamic Earth" [ER 474/3-1]; Bundesministerium
fur Bildung und Forschung (BMBF) [01LG1206C]; NASA
FX This work was partly supported by the Deutsche Forschungsgemeinschaft
(DFG) project PR 919/4-1 (MS-GWaves/SV) which is part of the DFG
researchers group MS-GWaves, by the DFG project ER 474/3-1 (TigerUC)
which is part of the DFG priority program SPP1788 "Dynamic Earth", as
well as by the Bundesministerium fur Bildung und Forschung (BMBF)
project no. 01LG1206C (ROMIC/GW-LCYCLE). Work at the Jet Propulsion
Laboratory, California Institute of Technology, was done under contract
with NASA.
NR 120
TC 3
Z9 3
U1 14
U2 14
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 9
PY 2016
VL 16
IS 15
BP 9983
EP 10019
DI 10.5194/acp-16-9983-2016
PG 37
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV7UZ
UT WOS:000383144600002
ER
PT J
AU Spang, R
Hoffmann, L
Hopfner, M
Griessbach, S
Muller, R
Pitts, MC
Orr, AMW
Riese, M
AF Spang, Reinhold
Hoffmann, Lars
Hoepfner, Michael
Griessbach, Sabine
Mueller, Rolf
Pitts, Michael C.
Orr, Andrew M. W.
Riese, Martin
TI A multi-wavelength classification method for polar stratospheric cloud
types using infrared limb spectra
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID NITRIC-ACID; OZONE DEPLETION; HETEROGENEOUS FORMATION; ARCTIC
STRATOSPHERE; OPTICAL-CONSTANTS; EMISSION-SPECTRA; GREENHOUSE GASES;
MIPAS; WINTER; ICE
AB The Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) instrument on board the ESA Envisat satellite operated from July 2002 until April 2012. The infrared limb emission measurements represent a unique dataset of daytime and night-time observations of polar stratospheric clouds (PSCs) up to both poles. Cloud detection sensitivity is comparable to space-borne lidars, and it is possible to classify different cloud types from the spectral measurements in different atmospheric windows regions.
Here we present a new infrared PSC classification scheme based on the combination of a well-established two-colour ratio method and multiple 2-D brightness temperature difference probability density functions. The method is a simple probabilistic classifier based on Bayes' theorem with a strong independence assumption. The method has been tested in conjunction with a database of radiative transfer model calculations of realistic PSC particle size distributions, geometries, and composition. The Bayesian classifier distinguishes between solid particles of ice and nitric acid trihydrate (NAT), as well as liquid droplets of super-cooled ternary solution (STS).
The classification results are compared to coincident measurements from the space-borne lidar Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) instrument over the temporal overlap of both satellite missions (June 2006-March 2012). Both datasets show a good agreement for the specific PSC classes, although the viewing geometries and the vertical and horizontal resolution are quite different. Discrepancies are observed between the CALIOP and the MIPAS ice class. The Bayesian classifier for MIPAS identifies substantially more ice clouds in the Southern Hemisphere polar vortex than CALIOP. This disagreement is attributed in part to the difference in the sensitivity on mixed-type clouds. Ice seems to dominate the spectral behaviour in the limb infrared spectra and may cause an overestimation in ice occurrence compared to the real fraction of ice within the PSC area in the polar vortex.
The entire MIPAS measurement period was processed with the new classification approach. Examples like the detection of the Antarctic NAT belt during early winter, and its possible link to mountain wave events over the Antarctic Peninsula, which are observed by the Atmospheric Infrared Sounder (AIRS) instrument, highlight the importance of a climatology of 9 Southern Hemisphere and 10 Northern Hemisphere winters in total. The new dataset is valuable both for detailed process studies, and for comparisons with and improvements of the PSC parameterizations used in chemistry transport and climate models.
C1 [Spang, Reinhold; Mueller, Rolf; Riese, Martin] Forschungszentrum Julich, Inst Energie & Klimaforsch, IEK 7, Julich, Germany.
[Hoffmann, Lars; Griessbach, Sabine] Forschungszentrum Julich, JSC, Julich, Germany.
[Hoepfner, Michael] Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, Karlsruhe, Germany.
[Pitts, Michael C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Orr, Andrew M. W.] British Antarctic Survey, Cambridge, England.
RP Spang, R (reprint author), Forschungszentrum Julich, Inst Energie & Klimaforsch, IEK 7, Julich, Germany.
EM r.spang@fz-juelich.de
RI Hoffmann, Lars/A-5173-2013; Muller, Rolf/A-6669-2013; Riese,
Martin/A-3927-2013; Spang, Reinhold/A-2738-2013
OI Hoffmann, Lars/0000-0003-3773-4377; Muller, Rolf/0000-0002-5024-9977;
Riese, Martin/0000-0001-6398-6493; Spang, Reinhold/0000-0002-2483-5761
FU ESA; International Space Science Institute (ISSI) in Bern, Switzerland
FX The authors would like to thank ESA for providing MIPAS level 1b data
and funding of the MIPclouds study as well as NASA for providing CALIOP
data. Reinhold Spang thanks Ines Tritscher (FZJ) for support with the
visualization of the CALIOP data. Part of this work is inspired by
discussions during the 1st PSC Initiative (PSCi) workshop funded by the
International Space Science Institute (ISSI) in Bern, Switzerland.
NR 73
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U1 7
U2 7
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 9
PY 2016
VL 9
IS 8
BP 3619
EP 3639
DI 10.5194/amt-9-3619-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV7VL
UT WOS:000383146000001
ER
PT J
AU Benedetti, M
Realpe-Gomez, J
Biswas, R
Perdomo-Ortiz, A
AF Benedetti, Marcello
Realpe-Gomez, John
Biswas, Rupak
Perdomo-Ortiz, Alejandro
TI Estimation of effective temperatures in quantum annealers for sampling
applications: A case study with possible applications in deep learning
SO PHYSICAL REVIEW A
LA English
DT Article
ID PROBABILITY-DISTRIBUTIONS; CONTRASTIVE DIVERGENCE; INFERENCE; MODEL
AB An increase in the efficiency of sampling from Boltzmann distributions would have a significant impact on deep learning and other machine-learning applications. Recently, quantum annealers have been proposed as a potential candidate to speed up this task, but several limitations still bar these state-of-the-art technologies from being used effectively. One of the main limitations is that, while the device may indeed sample from a Boltzmann-like distribution, quantum dynamical arguments suggest it will do so with an instance-dependent effective temperature, different from its physical temperature. Unless this unknown temperature can be unveiled, it might not be possible to effectively use a quantum annealer for Boltzmann sampling. In this work, we propose a strategy to overcome this challenge with a simple effective-temperature estimation algorithm. We provide a systematic study assessing the impact of the effective temperatures in the learning of a special class of a restricted Boltzmann machine embedded on quantum hardware, which can serve as a building block for deep-learning architectures. We also provide a comparison to k-step contrastive divergence (CD-k) with k up to 100. Although assuming a suitable fixed effective temperature also allows us to outperform one-step contrastive divergence (CD-1), only when using an instance-dependent effective temperature do we find a performance close to that of CD-100 for the case studied here.
C1 [Benedetti, Marcello; Realpe-Gomez, John; Perdomo-Ortiz, Alejandro] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
[Benedetti, Marcello; Realpe-Gomez, John] SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA.
[Benedetti, Marcello] UCL, Dept Comp Sci, Mortimer St, London WC1E 6BT, England.
[Realpe-Gomez, John] Univ Cartagena, Inst Matemat Aplicadas, Bolivar 130001, Colombia.
[Biswas, Rupak] NASA, Ames Res Ctr, Explorat Technol Directorate, Moffett Field, CA 94035 USA.
[Perdomo-Ortiz, Alejandro] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Perdomo-Ortiz, A (reprint author), NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.; Perdomo-Ortiz, A (reprint author), Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM alejandro.perdomoortiz@nasa.gov
FU NASA Ames Research Center [NNA14AA60C, NAS2-03144]
FX This work was supported by NASA Ames Research Center under Contracts No.
NNA14AA60C and No. NAS2-03144. The authors would like to thank V. M.
Janakiraman, Z. Jiang, T. Lanting, E. Rieffel, N. Wiebe, and B. Jacobs
for useful discussions.
NR 68
TC 1
Z9 1
U1 6
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD AUG 9
PY 2016
VL 94
IS 2
AR 022308
DI 10.1103/PhysRevA.94.022308
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DT2HK
UT WOS:000381301200005
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Andeen, K
Anderson, T
Ansseau, I
Anton, G
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Axani, S
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
Blaufuss, E
Blot, S
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Burgman, A
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Clark, K
Classen, L
Coenders, S
Collin, GH
Conrad, JM
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Rosendo, ED
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
di Lorenzo, V
Dujmovic, H
Dumm, JP
Dunkman, M
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fahey, S
Fazely, AR
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Flis, S
Fosig, CC
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Giang, W
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Griffith, Z
Ismail, AH
Hallgren, A
Halzen, F
Hansen, E
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jeong, M
Jero, K
Jones, BJP
Jurkovic, M
Kappes, A
Karg, T
Karle, A
Katz, U
Kauer, M
Keivani, A
Kelley, JL
Kheirandish, A
Kim, M
Kintscher, T
Kiryluk, J
Kittler, T
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, M
Kruckl, G
Kruger, C
Kunnen, J
Kunwar, S
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lennarz, D
Lesiak-Bzdak, M
Leuermann, M
Lu, L
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Mancina, S
Mandelartz, M
Maruyama, R
Mase, K
Maunu, R
McNally, F
Meagher, K
Medici, M
Meier, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Mohrmann, L
Montaruli, T
Moulai, M
Nahnhauer, R
Naumann, U
Neer, G
Niederhausen, H
Nowicki, SC
Nygren, DR
Pollmann, AO
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Pankova, DV
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Quinnan, M
Raab, C
Rameez, M
Rawlins, K
Relich, M
Resconi, E
Rhode, W
Richman, M
Riedel, B
Robertson, S
Rott, C
Ruhe, T
Ryckbosch, D
Rysewyk, D
Sabbatini, L
Salvado, J
Herrera, SES
Sandrock, A
Sandroos, J
Sarkar, S
Satalecka, K
Schlunder, P
Schmidt, T
Schoneberg, S
Schonwald, A
Seckel, D
Seunarine, S
Soldin, D
Song, M
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Steuer, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Tatar, J
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Rossem, M
van Santen, J
Veenkamp, J
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Wiebe, K
Wille, L
Williams, DR
Wills, L
Wissing, H
Wolf, M
Wood, TR
Woolsey, E
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Andeen, K.
Anderson, T.
Ansseau, I.
Anton, G.
Archinger, M.
Argueelles, C.
Arlen, T. C.
Auffenberg, J.
Axani, S.
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.
Blaufuss, E.
Blot, S.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Burgman, A.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Clark, K.
Classen, L.
Coenders, S.
Collin, G. H.
Conrad, J. M.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Rosendo, E. del Pino
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
di Lorenzo, V.
Dujmovic, H.
Dumm, J. P.
Dunkman, M.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fahey, S.
Fazely, A. R.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Flis, S.
Foesig, C. -C.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Giang, W.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Griffith, Z.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansen, E.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jeong, M.
Jero, K.
Jones, B. J. P.
Jurkovic, M.
Kappes, A.
Karg, T.
Karle, A.
Katz, U.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kheirandish, A.
Kim, M.
Kintscher, T.
Kiryluk, J.
Kittler, T.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, M.
Krueckl, G.
Krueger, C.
Kunnen, J.
Kunwar, S.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lennarz, D.
Lesiak-Bzdak, M.
Leuermann, M.
Lu, L.
Luenemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Mancina, S.
Mandelartz, M.
Maruyama, R.
Mase, K.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meier, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Mohrmann, L.
Montaruli, T.
Moulai, M.
Nahnhauer, R.
Naumann, U.
Neer, G.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Pollmann, A. Obertacke
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Pankova, D. V.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Quinnan, M.
Raab, C.
Rameez, M.
Rawlins, K.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Riedel, B.
Robertson, S.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Rysewyk, D.
Sabbatini, L.
Salvado, J.
Herrera, S. E. Sanchez
Sandrock, A.
Sandroos, J.
Sarkar, S.
Satalecka, K.
Schlunder, P.
Schmidt, T.
Schoeneberg, S.
Schoenwald, A.
Seckel, D.
Seunarine, S.
Soldin, D.
Song, M.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Steuer, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Stroem, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Tatar, J.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Rossem, M.
van Santen, J.
Veenkamp, J.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Wiebe, K.
Wille, L.
Williams, D. R.
Wills, L.
Wissing, H.
Wolf, M.
Wood, T. R.
Woolsey, E.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zoll, M.
CA IceCube Collaboration
TI Searches for Sterile Neutrinos with the IceCube Detector
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID OSCILLATIONS; SYSTEM; MODEL
AB The IceCube neutrino telescope at the South Pole has measured the atmospheric muon neutrino spectrum as a function of zenith angle and energy in the approximate 320 GeV to 20 TeV range, to search for the oscillation signatures of light sterile neutrinos. No evidence for anomalous nu(mu) or (nu) over bar (mu) disappearance is observed in either of two independently developed analyses, each using one year of atmospheric neutrino data. New exclusion limits are placed on the parameter space of the 3 + 1 model, in which muon antineutrinos experience a strong Mikheyev-Smirnov-Wolfenstein-resonant oscillation. The exclusion limits extend to sin(2)2 theta(24) <= 0.02 at Delta m(2) similar to 0.3 eV(2) at the 90% confidence level. The allowed region from global analysis of appearance experiments, including LSND and MiniBooNE, is excluded at approximately the 99% confidence level for the global best-fit value of vertical bar U-e4 vertical bar(2).
C1 [Auffenberg, J.; Leuermann, M.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Providence Dr, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Klein, S. R.; Miarecki, S.; Price, P. B.; Tatar, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Klein, S. R.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Tatar, J.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Kroll, M.; Mandelartz, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Homeier, A.; Voge, M.] Univ Bonn, Inst Phys, Nussallee 12, D-53115 Bonn, Germany.
[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Luenemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Argueelles, C.; Axani, S.; Collin, G. H.; Conrad, J. M.; Jones, B. J. P.; Moulai, M.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Lu, L.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Hansen, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Boerner, M.; Fuchs, T.; Meier, M.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Schlunder, P.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Lennarz, D.; Mahn, K. B. M.; Neer, G.; Rysewyk, D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Giang, W.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Herrera, S. E. Sanchez; Weaver, Ch.; Wood, T. R.; Woolsey, E.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Anton, G.; Katz, U.; Kittler, T.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Ahlers, M.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Krueger, C.; Mancina, S.; McNally, F.; Merino, G.; Sabbatini, L.; Salvado, J.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Rossem, M.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ahlers, M.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Krueger, C.; Mancina, S.; McNally, F.; Merino, G.; Sabbatini, L.; Salvado, J.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Rossem, M.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C. -C.; Koepke, L.; Krueckl, G.; Sandroos, J.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Andeen, K.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Berghaus, P.] Natl Res Nucl Univ, MEPhI Moscow Engn Phys Inst, Moscow 115409, Russia.
[Abraham, K.; Bernhard, A.; Coenders, S.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany.
[Classen, L.; Kappes, A.] Univ Munster, Inst Kernphys, D-48149 Munster, Germany.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England.
[Kurahashi, N.; Richman, M.; Wills, L.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; Dujmovic, H.; In, S.; Jeong, M.; Kim, M.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[BenZvi, S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Boersma, D. J.; Botner, O.; Burgman, A.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Helbing, K.; Hickford, S.; Hoffmann, R.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Bernardini, E.; Blot, S.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kintscher, T.; Kowalski, M.; Kunwar, S.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Satalecka, K.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Salvado, J.] Univ Valencia, CSIC, Inst Fis Corpuscular, Valencia 46071, Spain.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aartsen, MG (reprint author), Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
RI Anton, Gisela/C-4840-2013; Beatty, James/D-9310-2011; Sarkar,
Subir/G-5978-2011; Tjus, Julia/G-8145-2012; Katz, Uli/E-1925-2013;
Maruyama, Reina/A-1064-2013; Koskinen, David/G-3236-2014
OI Anton, Gisela/0000-0003-2039-4724; Beatty, James/0000-0003-0481-4952;
Sarkar, Subir/0000-0002-3542-858X; Katz, Uli/0000-0002-7063-4418;
Maruyama, Reina/0000-0003-2794-512X; Koskinen, David/0000-0002-0514-5917
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, 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, Sweden; Swedish Polar Research
Secretariat, Sweden; Swedish National Infrastructure for Computing
(SNIC), Sweden; Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Germany; Deutsche
Forschungsgemeinschaft (DFG), Germany; Helmholtz Alliance for
Astroparticle Physics (HAP), Germany; Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO Odysseus program; Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland; National Research Foundation of Korea
(NRF); Villum Fonden, Danish National Research Foundation (DNRF),
Denmark
FX We acknowledge support from the following agencies: U.S. National
Science Foundation Office of Polar Programs, U.S. National Science
Foundation Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin, Madison, the Open Science Grid (OSG)
grid infrastructure, U.S. Department of Energy, 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 program, Flanders Institute to
encourage scientific and technological research in industry (IWT),
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); the Swiss National
Science Foundation (SNSF), Switzerland; National Research Foundation of
Korea (NRF); and Villum Fonden, Danish National Research Foundation
(DNRF), Denmark.
NR 66
TC 20
Z9 20
U1 7
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD AUG 8
PY 2016
VL 117
IS 7
AR 071801
DI 10.1103/PhysRevLett.117.071801
PG 9
WC Physics, Multidisciplinary
SC Physics
GA DT4US
UT WOS:000381477200004
PM 27563950
ER
PT J
AU Gorham, PW
Nam, J
Romero-Wolf, A
Hoover, S
Allison, P
Banerjee, O
Beatty, JJ
Belov, K
Besson, DZ
Binns, WR
Bugaev, V
Cao, P
Chen, C
Chen, P
Clem, JM
Connolly, A
Dailey, B
Deaconu, C
Cremonesi, L
Dowkontt, PF
DuVernois, MA
Field, RC
Fox, BD
Goldstein, D
Gordon, J
Hast, C
Hebert, CL
Hill, B
Hughes, K
Hupe, R
Israel, MH
Javaid, A
Kowalski, J
Lam, J
Learned, JG
Liewer, KM
Liu, TC
Link, JT
Lusczek, E
Matsuno, S
Mercurio, BC
Miki, C
Miocinovic, P
Mottram, M
Mulrey, K
Naudet, CJ
Ng, J
Nichol, RJ
Palladino, K
Rauch, BF
Reil, K
Roberts, J
Rosen, M
Rotter, B
Russell, J
Ruckman, L
Saltzberg, D
Seckel, D
Schoorlemmer, H
Stafford, S
Stockham, J
Stockham, M
Strutt, B
Tatem, K
Varner, GS
Vieregg, AG
Walz, D
Wissel, SA
Wu, F
AF Gorham, P. W.
Nam, J.
Romero-Wolf, A.
Hoover, S.
Allison, P.
Banerjee, O.
Beatty, J. J.
Belov, K.
Besson, D. Z.
Binns, W. R.
Bugaev, V.
Cao, P.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
Dailey, B.
Deaconu, C.
Cremonesi, L.
Dowkontt, P. F.
DuVernois, M. A.
Field, R. C.
Fox, B. D.
Goldstein, D.
Gordon, J.
Hast, C.
Hebert, C. L.
Hill, B.
Hughes, K.
Hupe, R.
Israel, M. H.
Javaid, A.
Kowalski, J.
Lam, J.
Learned, J. G.
Liewer, K. M.
Liu, T. C.
Link, J. T.
Lusczek, E.
Matsuno, S.
Mercurio, B. C.
Miki, C.
Miocinovic, P.
Mottram, M.
Mulrey, K.
Naudet, C. J.
Ng, J.
Nichol, R. J.
Palladino, K.
Rauch, B. F.
Reil, K.
Roberts, J.
Rosen, M.
Rotter, B.
Russell, J.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Schoorlemmer, H.
Stafford, S.
Stockham, J.
Stockham, M.
Strutt, B.
Tatem, K.
Varner, G. S.
Vieregg, A. G.
Walz, D.
Wissel, S. A.
Wu, F.
CA ANITA Collaboration
TI Characteristics of Four Upward-Pointing Cosmic-Ray-like Events Observed
with ANITA
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID RADIO-EMISSION; AIR-SHOWERS; ENERGY
AB We report on four radio-detected cosmic-ray (CR) or CR-like events observed with the Antarctic Impulsive Transient Antenna (ANITA), a NASA-sponsored long-duration balloon payload. Two of the four were previously identified as stratospheric CR air showers during the ANITA-I flight. A third stratospheric CR was detected during the ANITA-II flight. Here, we report on characteristics of these three unusual CR events, which develop nearly horizontally, 20-30 km above the surface of Earth. In addition, we report on a fourth steeply upward-pointing ANITA-I CR-like radio event which has characteristics consistent with a primary that emerged from the surface of the ice. This suggests a possible tau-lepton decay as the origin of this event, but such an interpretation would require significant suppression of the standard model tau-neutrino cross section.
C1 [Gorham, P. W.; DuVernois, M. A.; Fox, B. D.; Hebert, C. L.; Hill, B.; Kowalski, J.; Learned, J. G.; Link, J. T.; Matsuno, S.; Miki, C.; Miocinovic, P.; Roberts, J.; Rosen, M.; Rotter, B.; Russell, J.; Ruckman, L.; Schoorlemmer, H.; Tatem, K.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Nam, J.; Chen, C.; Chen, P.; Liu, T. C.] Natl Taiwan Univ, Grad Inst Astrophys, Dept Phys, Taipei 10617, Taiwan.
[Nam, J.; Chen, C.; Chen, P.; Liu, T. C.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan.
[Romero-Wolf, A.; Belov, K.; Liewer, K. M.; Naudet, C. J.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Hoover, S.; Dowkontt, P. F.; Lam, J.; Saltzberg, D.; Wu, F.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Allison, P.; Banerjee, O.; Beatty, J. J.; Connolly, A.; Dailey, B.; Gordon, J.; Hughes, K.; Hupe, R.; Mercurio, B. C.; Palladino, K.; Stafford, S.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Allison, P.; Beatty, J. J.; Connolly, A.] Ohio State Univ, Ctr Cosmol & Particle Astrophys, Columbus, OH 43210 USA.
[Besson, D. Z.; Stockham, J.; Stockham, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Binns, W. R.; Bugaev, V.; Israel, M. H.; Rauch, B. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Cao, P.; Clem, J. M.; Javaid, A.; Mulrey, K.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA.
[Deaconu, C.; Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Dept Phys, Chicago, IL 60637 USA.
[Cremonesi, L.; Mottram, M.; Nichol, R. J.; Strutt, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Field, R. C.; Hast, C.; Ng, J.; Reil, K.; Walz, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Goldstein, D.] Univ Calif Irvine, Dept Phys, Irvine, CA 92697 USA.
[Lusczek, E.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Wissel, S. A.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
RP Gorham, PW (reprint author), Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
RI Beatty, James/D-9310-2011;
OI Beatty, James/0000-0003-0481-4952; Lusczek,
Elizabeth/0000-0003-4680-965X
FU NASA; U.S. Department of Energy, High Energy Physics Division
FX We thank NASA for their generous support of ANITA, the Columbia
Scientific Balloon Facility for their excellent field support, and the
National Science Foundation for their Antarctic operations support. This
work was also supported by the U.S. Department of Energy, High Energy
Physics Division.
NR 18
TC 2
Z9 2
U1 3
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD AUG 8
PY 2016
VL 117
IS 7
AR 071101
DI 10.1103/PhysRevLett.117.071101
PG 5
WC Physics, Multidisciplinary
SC Physics
GA DT4US
UT WOS:000381477200002
PM 27563945
ER
PT J
AU Silva, RA
West, JJ
Lamarque, JF
Shindell, DT
Collins, WJ
Dalsoren, S
Faluvegi, G
Folberth, G
Horowitz, LW
Nagashima, T
Naik, V
Rumbold, ST
Sudo, K
Takemura, T
Bergmann, D
Cameron-Smith, P
Cionni, I
Doherty, RM
Eyring, V
Josse, B
MacKenzie, IA
Plummer, D
Righi, M
Stevenson, DS
Strode, S
Szopa, S
Zengast, G
AF Silva, Raquel A.
West, J. Jason
Lamarque, Jean-Francois
Shindell, Drew T.
Collins, William J.
Dalsoren, Stig
Faluvegi, Greg
Folberth, Gerd
Horowitz, Larry W.
Nagashima, Tatsuya
Naik, Vaishali
Rumbold, Steven T.
Sudo, Kengo
Takemura, Toshihiko
Bergmann, Daniel
Cameron-Smith, Philip
Cionni, Irene
Doherty, Ruth M.
Eyring, Veronika
Josse, Beatrice
MacKenzie, Ian A.
Plummer, David
Righi, Mattia
Stevenson, David S.
Strode, Sarah
Szopa, Sophie
Zengast, Guang
TI The effect of future ambient air pollution on human premature mortality
to 2100 using output from the ACCMIP model ensemble
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID INTERCOMPARISON PROJECT ACCMIP; FINE PARTICULATE MATTER; GREENHOUSE-GAS
EMISSIONS; OZONE-RELATED MORTALITY; CLIMATE-CHANGE; HEALTH IMPACTS;
ATMOSPHERIC CHEMISTRY; TROPOSPHERIC OZONE; GLOBAL BURDEN; CHANGING
CLIMATE
AB Ambient air pollution from ground-level ozone and fine particulate matter (PM2.5) is associated with premature mortality. Future concentrations of these air pollutants will be driven by natural and anthropogenic emissions and by climate change. Using anthropogenic and biomass burning emissions projected in the four Representative Concentration Pathway scenarios (RCPs), the ACCMIP ensemble of chemistry-climate models simulated future concentrations of ozone and PM2.5 at selected decades between 2000 and 2100. We use output from the ACCMIP ensemble, together with projections of future population and baseline mortality rates, to quantify the human premature mortality impacts of future ambient air pollution. Future air-pollution-related premature mortality in 2030, 2050 and 2100 is estimated for each scenario and for each model using a health impact function based on changes in concentrations of ozone and PM2.5 relative to 2000 and projected future population and baseline mortality rates. Additionally, the global mortality burden of ozone and PM2.5 in 2000 and each future period is estimated relative to 1850 concentrations, using present-day and future population and baseline mortality rates. The change in future ozone concentrations relative to 2000 is associated with excess global premature mortality in some scenarios/periods, particularly in RCP8.5 in 2100 (316 thousand deaths year(-1)), likely driven by the large increase in methane emissions and by the net effect of climate change projected in this scenario, but it leads to considerable avoided premature mortality for the three other RCPs. However, the global mortality burden of ozone markedly increases from 382 000 (121 000 to 728 000) deaths year(-1) in 2000 to between 1.09 and 2.36 million deaths year(-1) in 2100, across RCPs, mostly due to the effect of increases in population and baseline mortality rates. PM2.5 concentrations decrease relative to 2000 in all scenarios, due to projected reductions in emissions, and are associated with avoided premature mortality, particularly in 2100: between -2.39 and -1.31 million deaths year(-1) for the four RCPs. The global mortality burden of PM2.5 is estimated to decrease from 1.70 (1.30 to 2.10) million deaths year 1 in 2000 to between 0.95 and 1.55 million deaths year 1 in 2100 for the four RCPs due to the combined effect of decreases in PM2.5 concentrations and changes in population and baseline mortality rates. Trends in future air-pollution-related mortality vary regionally across scenarios, reflecting assumptions for economic growth and air pollution control specific to each RCP and region. Mortality estimates differ among chemistry-climate models due to differences in simulated pollutant concentrations, which is the greatest contributor to overall mortality uncertainty for most cases assessed here, supporting the use of model ensembles to characterize uncertainty. Increases in exposed population and baseline mortality rates of respiratory diseases magnify the impact on premature mortality of changes in future air pollutant concentrations and explain why the future global mortality burden of air pollution can exceed the current burden, even where air pollutant concentrations decrease.
C1 [Silva, Raquel A.; West, J. Jason] Univ N Carolina, Environm Sci & Engn, Chapel Hill, NC 27599 USA.
[Lamarque, Jean-Francois] Natl Ctr Atmospher Res, NCAR Earth Syst Lab, POB 3000, Boulder, CO 80307 USA.
[Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Collins, William J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Dalsoren, Stig] CICERO, Oslo, Norway.
[Faluvegi, Greg] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Faluvegi, Greg] Columbia Earth Inst, New York, NY USA.
[Folberth, Gerd; Rumbold, Steven T.] Met Off Hadley Ctr, Exeter, Devon, England.
[Horowitz, Larry W.; Naik, Vaishali] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Nagashima, Tatsuya] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Earth & Environm Sci, Nagoya, Aichi, Japan.
[Takemura, Toshihiko] Kyushu Univ, Res Inst Appl Mech, Fukuoka, Japan.
[Bergmann, Daniel; Cameron-Smith, Philip] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Cionni, Irene] Agenzia Nazl Nuove Tecnol Energia & Sviluppo Econ, Bologna, Italy.
[Doherty, Ruth M.; MacKenzie, Ian A.; Stevenson, David S.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland.
[Eyring, Veronika; Righi, Mattia] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
[Josse, Beatrice] CNRS Ctr Natl Rech Meteorol, GAME CNRM, Meteo France, Toulouse, France.
[Plummer, David] Environm Canada, Canadian Ctr Climate Modeling & Anal, Victoria, BC, Canada.
[Strode, Sarah] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Strode, Sarah] Univ Space Res Assoc, Columbia, MD USA.
[Szopa, Sophie] LSCE CEA CNRS UVSQ, Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Zengast, Guang] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Rumbold, Steven T.] Univ Reading, NCAS, Reading, Berks, England.
[Zengast, Guang] NIWA, Wellington, New Zealand.
RP West, JJ (reprint author), Univ N Carolina, Environm Sci & Engn, Chapel Hill, NC 27599 USA.
EM jjwest@email.unc.edu
RI Righi, Mattia/I-5120-2013; Takemura, Toshihiko/C-2822-2009; Eyring,
Veronika/O-9999-2016; Szopa, Sophie/F-8984-2010; Kyushu,
RIAM/F-4018-2015; Collins, William/A-5895-2010; Naik,
Vaishali/A-4938-2013; West, Jason/J-2322-2015; Strode,
Sarah/H-2248-2012; Stevenson, David/C-8089-2012; Cameron-Smith,
Philip/E-2468-2011
OI Takemura, Toshihiko/0000-0002-2859-6067; Eyring,
Veronika/0000-0002-6887-4885; Szopa, Sophie/0000-0002-8641-1737;
Collins, William/0000-0002-7419-0850; Naik,
Vaishali/0000-0002-2254-1700; West, Jason/0000-0001-5652-4987; Strode,
Sarah/0000-0002-8103-1663; Stevenson, David/0000-0002-4745-5673;
Cameron-Smith, Philip/0000-0002-8802-8627
FU Portuguese Foundation for Science and Technology; Graduate School (UNC -
Chapel Hill); NIEHS [1 R21 ES022600-01]; US Dept. of Energy (BER) under
LLNL [DE-AC52-07NA27344]; NERSC [DE-AC02-05CH11231]; UK Natural
Environment Research Council [NE/I008063/1]
FX The research here described was funded by a fellowship from the
Portuguese Foundation for Science and Technology, by a Dissertation
Completion Fellowship from The Graduate School (UNC - Chapel Hill) and
by NIEHS grant no. 1 R21 ES022600-01. We thank Karin Yeatts (Department
of Epidemiology, UNC - Chapel Hill) for her help in researching
projections of future population and baseline mortality rates, Colin
Mathers (WHO) for advising us on the IFs, Peter Speyer (IHME, University
of Washington) for providing us access to GBD2010 cause-specific
mortality data at the country-level, and Amanda Henley (Davis Library
Research & Instructional Services, UNC - Chapel Hill) for facilitating
our access to LandScan 2011 Global Population Dataset. The work of
Daniel Bergmann and Philip Cameron-Smith was funded by the US Dept. of
Energy (BER), performed under the auspices of LLNL under Contract
DE-AC52-07NA27344 and used the supercomputing resources of NERSC under
contract no. DE-AC02-05CH11231. Ruth Doherty, Ian MacKenzie and David
Stevenson acknowledge ARCHER supercomputing resources and funding under
the UK Natural Environment Research Council grant NE/I008063/1. Guang
Zeng acknowledges the NZ eScience Infrastructure, which is funded
jointly by NeSI's collaborator institutions and through the MBIE's
Research Infrastructure programme.
NR 64
TC 1
Z9 1
U1 14
U2 14
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 5
PY 2016
VL 16
IS 15
BP 9847
EP 9862
DI 10.5194/acp-16-9847-2016
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV7EY
UT WOS:000383100300001
ER
PT J
AU Cyr-Racine, FY
Moustakas, LA
Keeton, CR
Sigurdson, K
Gilman, DA
AF Cyr-Racine, Francis-Yan
Moustakas, Leonidas A.
Keeton, Charles R.
Sigurdson, Kris
Gilman, Daniel A.
TI Dark census: Statistically detecting the satellite populations of
distant galaxies
SO PHYSICAL REVIEW D
LA English
DT Article
ID STRONG GRAVITATIONAL LENSES; SMALL-SCALE STRUCTURE; MICROLENSING LIGHT
CURVES; FLUX-RATIO ANOMALIES; MATTER SUBSTRUCTURE; MASS SUBSTRUCTURE;
LAMBDA-CDM; COSMOLOGICAL MODEL; MILKY-WAY; IDENTIFYING LENSES
AB In the standard structure formation scenario based on the cold dark matter paradigm, galactic halos are predicted to contain a large population of dark matter subhalos. While the most massive members of the subhalo population can appear as luminous satellites and be detected in optical surveys, establishing the existence of the low mass and mostly dark subhalos has proven to be a daunting task. Galaxy-scale strong gravitational lenses have been successfully used to study mass substructures lying close to lensed images of bright background sources. However, in typical galaxy-scale lenses, the strong lensing region only covers a small projected area of the lens's dark matter halo, implying that the vast majority of subhalos cannot be directly detected in lensing observations. In this paper, we point out that this large population of dark satellites can collectively affect gravitational lensing observables, hence possibly allowing their statistical detection. Focusing on the region of the galactic halo outside the strong lensing area, we compute from first principles the statistical properties of perturbations to the gravitational time delay and position of lensed images in the presence of a mass substructure population. We find that in the standard cosmological scenario, the statistics of these lensing observables are well approximated by Gaussian distributions. The formalism developed as part of this calculation is very general and can be applied to any halo geometry and choice of subhalo mass function. Our results significantly reduce the computational cost of including a large substructure population in lens models and enable the use of Bayesian inference techniques to detect and characterize the distributed satellite population of distant lens galaxies.
C1 [Cyr-Racine, Francis-Yan] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Cyr-Racine, Francis-Yan; Moustakas, Leonidas A.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Cyr-Racine, Francis-Yan; Moustakas, Leonidas A.] CALTECH, Pasadena, CA 91125 USA.
[Keeton, Charles R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Sigurdson, Kris] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Gilman, Daniel A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Cyr-Racine, FY (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.; Cyr-Racine, FY (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.; Cyr-Racine, FY (reprint author), CALTECH, Pasadena, CA 91125 USA.
OI Moustakas, Leonidas/0000-0003-3030-2360
FU W. M. Keck Foundation; National Science Foundation [1066293,
AST-0747311]; National Aeronautics and Space Administration (NASA); NASA
ATFP program [399131.02.02.02.98]; Natural Science and Engineering
Research Council (NSERC) of Canada Discovery Grant; NASA Undergraduate
Internship and Student Internship programs
FX We thank Geoffrey Bryden, James Bullock, Curt Cutler, Olivier Dore,
David Hogg, Jeffrey Jewel, James Taylor, and Michele Vallisneri for
useful conversations. The work of F.-Y.C.-R. was performed in part at
the California Institute of Technology for the Keck Institute for Space
Studies, which is funded by the W. M. Keck Foundation. F.-Y.C.-R. thanks
the Aspen Center for Physics, where some of this work was performed. The
Aspen Center for Physics is supported by the National Science Foundation
under Grant No. 1066293. Part of the research described in this paper
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration (NASA). L.A.M. gratefully acknowledges support by the
NASA ATFP program through Award No. 399131.02.02.02.98. C. R. K.
acknowledges support from the National Science Foundation under Grant
No. AST-0747311. The research of K. S. is supported in part by a Natural
Science and Engineering Research Council (NSERC) of Canada Discovery
Grant. D. A. G. acknowledges the support of the NASA Undergraduate
Internship and Student Internship programs.
NR 126
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U1 1
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 5
PY 2016
VL 94
IS 4
AR 043505
DI 10.1103/PhysRevD.94.043505
PG 27
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DS7KV
UT WOS:000380963300004
ER
PT J
AU Ruangsri, U
Vigeland, SJ
Hughes, SA
AF Ruangsri, Uchupol
Vigeland, Sarah J.
Hughes, Scott A.
TI Gyroscopes orbiting black holes: A frequency-domain approach to
precession and spin-curvature coupling for spinning bodies on generic
Kerr orbits
SO PHYSICAL REVIEW D
LA English
DT Article
ID TEST PARTICLES; GRAVITATIONAL-WAVES; SPACETIME; MOTION; RELATIVITY;
RADIATION; FIELD
AB A small body orbiting a black hole follows a trajectory that, at leading order, is a geodesic of the black hole spacetime. Much effort has gone into computing "self-force" corrections to this motion, arising from the small body's own contributions to the system's spacetime. Another correction to the motion arises from coupling of the small body's spin to the black hole's spacetime curvature. Spin-curvature coupling drives a precession of the small body, and introduces a "force" (relative to the geodesic) which shifts the small body's worldline. These effects scale with the small body's spin at leading order. In this paper, we show that the equations which govern spin-curvature coupling can be analyzed with a frequency-domain decomposition, at least to leading order in the small body's spin. We show how to compute the frequency of precession along generic orbits, and how to describe the small body's precession and motion in the frequency domain. We illustrate this approach with a number of examples. This approach is likely to be useful for understanding spin coupling effects in the extreme mass ratio limit, and may provide insight into modeling spin effects in the strong field for nonextreme mass ratios.
C1 [Ruangsri, Uchupol; Hughes, Scott A.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Ruangsri, Uchupol; Hughes, Scott A.] MIT, Kavli Inst, Cambridge, MA 02139 USA.
[Vigeland, Sarah J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Vigeland, Sarah J.] Univ Wisconsin, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53211 USA.
RP Ruangsri, U (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Ruangsri, U (reprint author), MIT, Kavli Inst, Cambridge, MA 02139 USA.
FU NSF [PHY-1403261]; NASA [NNX08AL42G]
FX This work was supported at MIT by NSF Grant No. PHY-1403261, and at the
Jet Propulsion Laboratory by an appointment to the NASA Postdoctoral
Program, administered by Oak Ridge Associated Universities through a
contract with NASA. We are very grateful for feedback and helpful
comments on an earlier draft of this paper from Niels Warburton and
Georgios Loukes-Gerakopoulos, to feedback from L. Filipe O. Costa and
Jose Natario on our original arXiv.org posting, and to the paper's
anonymous referee from an extremely thorough and helpful report. Many of
our calculations were done using the package MATHEMATICA. A very early
version of this work was supported at MIT by NASA Grant No. NNX08AL42G,
and was published as a chapter in S. J. V.'s Ph.D. thesis [98].
NR 98
TC 5
Z9 5
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 5
PY 2016
VL 94
IS 4
AR 044008
DI 10.1103/PhysRevD.94.044008
PG 29
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DS7KV
UT WOS:000380963300005
ER
PT J
AU Benjamin, CL
Stowe, RP
St John, L
Sams, CF
Mehta, SK
Crucian, BE
Pierson, DL
Komanduri, KV
AF Benjamin, Cara L.
Stowe, Raymond P.
St John, Lisa
Sams, Clarence F.
Mehta, Satish K.
Crucian, Brian E.
Pierson, Duane L.
Komanduri, Krishna V.
TI Decreases in thymopoiesis of astronauts returning from space flight
SO JCI INSIGHT
LA English
DT Article
ID CORD BLOOD TRANSPLANTATION; LONG-DURATION SPACEFLIGHT; THYMIC FUNCTION;
T-CELLS; IMMUNE RECONSTITUTION; CYTOKINE PRODUCTION; THYMOCYTES;
APOPTOSIS; MICE; SYSTEM
AB Following the advent of molecular assays that measure T cell receptor excision circles (TRECs) present in recent thymic emigrants, it has been conclusively shown that thymopoiesis persists in most adults, but that functional output decreases with age, influencing the maintenance of a diverse and functional T cell receptor (TCR) repertoire. Space flight has been shown to result in a variety of phenotypic and functional changes in human T cells and in the reactivation of latent viruses. While space flight has been shown to influence thymic architecture in rodents, thymopoiesis has not previously been assessed in astronauts. Here, we assessed thymopoiesis longitudinally over a 1-year period prior to and after long-term space flight (median duration, 184 days) in 16 astronauts. While preflight assessments of thymopoiesis remained quite stable in individual astronauts, we detected significant suppression of thymopoiesis in all subjects upon return from space flight. We also found significant increases in urine and plasma levels of endogenous glucocorticoids coincident with the suppression of thymopoiesis. The glucocorticoid induction and thymopoiesis suppression were transient, and they normalized shortly after return to Earth. This is the first report to our knowledge to prospectively demonstrate a significant change in thymopoiesis in healthy individuals in association with a defined physiologic emotional and physical stress event. These results suggest that suppression of thymopoiesis has the potential to influence the maintenance of the TCR repertoire during extended space travel. Further studies of thymopoiesis and endogenous glucocorticoids in other stress states, including illness, are warranted.
C1 [Benjamin, Cara L.; Komanduri, Krishna V.] Univ Miami, Sylvester Canc Ctr, Adult Stem Cell Transplant Program, Miami, FL USA.
[Stowe, Raymond P.] Microgen Labs, La Marque, TX USA.
[St John, Lisa] Univ Texas MD Anderson Canc Ctr, Houston, TX 77030 USA.
[Sams, Clarence F.; Crucian, Brian E.; Pierson, Duane L.] NASA Johnson Space Ctr, Houston, TX USA.
[Mehta, Satish K.] Jestech, Houston, TX USA.
RP Komanduri, KV (reprint author), Univ Miami, 1501 NW 10th Ave,BRB Room 916, Miami, FL 33136 USA.
EM kkomanduri@med.miami.edu
NR 41
TC 0
Z9 0
U1 1
U2 1
PU AMER SOC CLINICAL INVESTIGATION INC
PI ANN ARBOR
PA 35 RESEARCH DR, STE 300, ANN ARBOR, MI 48103 USA
SN 2379-3708
J9 JCI INSIGHT
JI JCI Insight
PD AUG 4
PY 2016
VL 1
IS 12
AR e88787
DI 10.1172/jci.insight.88787
PG 8
WC Medicine, Research & Experimental
SC Research & Experimental Medicine
GA EB1NH
UT WOS:000387118800011
PM 27699228
ER
PT J
AU De Sanctis, MC
Raponi, A
Ammannito, E
Ciarniello, M
Toplis, MJ
McSween, HY
Castillo-Rogez, JC
Ehlmann, BL
Carrozzo, FG
Marchi, S
Tosi, F
Zambon, F
Capaccioni, F
Capria, MT
Fonte, S
Formisano, M
Frigeri, A
Giardino, M
Longobardo, A
Magni, G
Palomba, E
McFadden, LA
Pieters, CM
Jaumann, R
Schenk, P
Mugnuolo, R
Raymond, CA
Russell, CT
AF De Sanctis, M. C.
Raponi, A.
Ammannito, E.
Ciarniello, M.
Toplis, M. J.
McSween, H. Y.
Castillo-Rogez, J. C.
Ehlmann, B. L.
Carrozzo, F. G.
Marchi, S.
Tosi, F.
Zambon, F.
Capaccioni, F.
Capria, M. T.
Fonte, S.
Formisano, M.
Frigeri, A.
Giardino, M.
Longobardo, A.
Magni, G.
Palomba, E.
McFadden, L. A.
Pieters, C. M.
Jaumann, R.
Schenk, P.
Mugnuolo, R.
Raymond, C. A.
Russell, C. T.
TI Bright carbonate deposits as evidence of aqueous alteration on (1) Ceres
SO NATURE
LA English
DT Article
ID AMMONIUM-BEARING MINERALS; OPTICAL-CONSTANTS; WATER ICE; MU-M; COMET
67P/CHURYUMOV-GERASIMENKO; CRYSTALLINE H2O-ICE; SURFACE-COMPOSITION; CI
CHONDRITES; SPECTROSCOPY; ENCELADUS
AB The typically dark surface of the dwarf planet Ceres is punctuated by areas of much higher albedo, most prominently in the Occator crater(1). These small bright areas have been tentatively interpreted as containing a large amount of hydrated magnesium sulfate(1), in contrast to the average surface, which is a mixture of lowalbedo materials and magnesium phyllosilicates, ammoniated phyllosilicates and carbonates(2-4). Here we report high spatial and spectral resolution near-infrared observations of the bright areas in the Occator crater on Ceres. Spectra of these bright areas are consistent with a large amount of sodium carbonate, constituting the most concentrated known extraterrestrial occurrence of carbonate on kilometre-wide scales in the Solar System. The carbonates are mixed with a dark component and small amounts of phyllosilicates, as well as ammonium carbonate or ammonium chloride. Some of these compounds have also been detected in the plume of Saturn's sixth-largest moon Enceladus(5). The compounds are endogenous and we propose that they are the solid residue of crystallization of brines and entrained altered solids that reached the surface from below. The heat source may have been transient (triggered by impact heating). Alternatively, internal temperatures may be above the eutectic temperature of subsurface brines, in which case fluids may exist at depth on Ceres today.
C1 [De Sanctis, M. C.; Raponi, A.; Ammannito, E.; Ciarniello, M.; Carrozzo, F. G.; Marchi, S.; Tosi, F.; Zambon, F.; Capaccioni, F.; Capria, M. T.; Fonte, S.; Formisano, M.; Frigeri, A.; Giardino, M.; Longobardo, A.; Magni, G.; Palomba, E.] Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA USA.
[Toplis, M. J.] Univ Toulouse 3, Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Castillo-Rogez, J. C.; Ehlmann, B. L.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ehlmann, B. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Marchi, S.] SRI, Solar Syst Explorat Res Virtual Inst, 1050 Walnut St, Boulder, CO 80302 USA.
[McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Jaumann, R.] German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
[Schenk, P.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Mugnuolo, R.] Agenzia Spaziale Italiana, Via Politecn, I-00133 Rome, Italy.
RP De Sanctis, MC (reprint author), Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM mariacristina.desanctis@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; McFadden,
Lucy/0000-0002-0537-9975; Palomba, Ernesto/0000-0002-9101-6774; Tosi,
Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU Italian Space Agency; National Aeronautics and Space Administration
(NASA, USA); Deutsches Zentrum fur Luft- und Raumfahrt (DLR, Germany)
FX We thank the following institutions and agencies which supported this
work: the Italian Space Agency, the National Aeronautics and Space
Administration (NASA, USA) and the Deutsches Zentrum fur Luft- und
Raumfahrt (DLR, Germany). The VIR was funded and coordinated by the
Italian Space Agency and built by SELEX ES, with the scientific
leadership of the Institute for Space Astrophysics and Planetology and
the Italian National Institute for Astrophysics, and is operated by the
Institute for Space Astrophysics and Planetology, Italy. A portion of
this work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, USA, under contract to NASA. We also thank the
Dawn Mission Operations team and the Framing Camera team.
NR 38
TC 19
Z9 19
U1 14
U2 14
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD AUG 4
PY 2016
VL 536
IS 7614
BP 54
EP +
DI 10.1038/nature18290
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DS7YM
UT WOS:000380999200028
PM 27362221
ER
PT J
AU Daskalakis, N
Tsigaridis, K
Myriokefalitakis, S
Fanourgakis, GS
Kanakidou, M
AF Daskalakis, Nikos
Tsigaridis, Kostas
Myriokefalitakis, Stelios
Fanourgakis, George S.
Kanakidou, Maria
TI Large gain in air quality compared to an alternative anthropogenic
emissions scenario
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID TROPOSPHERIC OZONE; CARBON-MONOXIDE; AEROSOL TRENDS; MODEL; SIMULATIONS;
VARIABILITY; AEROCOM; REANALYSIS; TRANSPORT; CHEMISTRY
AB During the last 30 years, significant effort has been made to improve air quality through legislation for emissions reduction. Global three-dimensional chemistry-transport simulations of atmospheric composition over the past 3 decades have been performed to estimate what the air quality levels would have been under a scenario of stagnation of anthropogenic emissions per capita as in 1980, accounting for the population increase (BA1980) or using the standard practice of neglecting it (AE1980), and how they compare to the historical changes in air quality levels. The simulations are based on assimilated meteorology to account for the year-to- year observed climate variability and on different scenarios of anthropogenic emissions of pollutants. The ACCMIP historical emissions dataset is used as the starting point. Our sensitivity simulations provide clear indications that air quality legislation and technology developments have limited the rapid increase of air pollutants. The achieved reductions in concentrations of nitrogen oxides, carbon monoxide, black carbon, and sulfate aerosols are found to be significant when comparing to both BA1980 and AE1980 simulations that neglect any measures applied for the protection of the environment. We also show the potentially large tropospheric air quality benefit from the development of cleaner technology used by the growing global population. These 30-year hindcast sensitivity simulations demonstrate that the actual benefit in air quality due to air pollution legislation and technological advances is higher than the gain calculated by a simple comparison against a constant anthropogenic emissions simulation, as is usually done. Our results also indicate that over China and India the beneficial technological advances for the air quality may have been masked by the explosive increase in local population and the disproportional increase in energy demand partially due to the globalization of the economy.
C1 [Daskalakis, Nikos; Myriokefalitakis, Stelios; Fanourgakis, George S.; Kanakidou, Maria] Univ Crete, Dept Chem, Environm Chem Proc Lab, POB 2208, Iraklion 70013, Greece.
[Daskalakis, Nikos] Fdn Res & Technol Hellas FORTH ICE HT, Inst Chem Engn, Patras 26504, Greece.
[Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Daskalakis, Nikos] UPMC UVSQ CNRS, Observat Spatiales, Milieux, LATMOS,Lab Atmospheres, Paris, France.
RP Daskalakis, N; Kanakidou, M (reprint author), Univ Crete, Dept Chem, Environm Chem Proc Lab, POB 2208, Iraklion 70013, Greece.; Daskalakis, N (reprint author), Fdn Res & Technol Hellas FORTH ICE HT, Inst Chem Engn, Patras 26504, Greece.; Daskalakis, N (reprint author), UPMC UVSQ CNRS, Observat Spatiales, Milieux, LATMOS,Lab Atmospheres, Paris, France.
EM nick@chemistry.uoc.gr; mariak@chemistry.uoc.gr
RI Kanakidou, Maria/D-7882-2012; Myriokefalitakis, Stylianos/J-3701-2014
OI Kanakidou, Maria/0000-0002-1724-9692; Myriokefalitakis,
Stylianos/0000-0002-1541-7680
FU EU-FP7 project PEGASOS [FP7-ENV-2010-265148]; EU-FP7 project ECLIPSE
[FP7-ENV-2011-282688]; EU-FP7 project BACCHUS [603445]
FX This work has been supported by the EU-FP7 project PEGASOS
(FP7-ENV-2010-265148), the EU-FP7 project ECLIPSE (FP7-ENV-2011-282688),
and the EU-FP7 project BACCHUS (project number 603445). We thank Frank
Dentener and Michael Gauss for pertinent comments during early stages of
this work.
NR 58
TC 1
Z9 1
U1 5
U2 5
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 4
PY 2016
VL 16
IS 15
BP 9771
EP 9784
DI 10.5194/acp-16-9771-2016
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV6MD
UT WOS:000383049300001
ER
PT J
AU Kasoar, M
Voulgarakis, A
Lamarque, JF
Shindell, DT
Bellouin, N
Collins, WJ
Faluvegi, G
Tsigaridis, K
AF Kasoar, Matthew
Voulgarakis, Apostolos
Lamarque, Jean-Francois
Shindell, Drew T.
Bellouin, Nicolas
Collins, William J.
Faluvegi, Greg
Tsigaridis, Kostas
TI Regional and global temperature response to anthropogenic SO2 emissions
from China in three climate models
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AEROSOL MICROPHYSICS MODEL; SULFUR-DIOXIDE EMISSIONS; SULFATE AEROSOL;
GISS MODELE2; SEA-SALT; SIMULATIONS; PRECIPITATION; CHEMISTRY; AEROCOM;
20TH-CENTURY
AB We use the HadGEM3-GA4, CESM1, and GISS ModelE2 climate models to investigate the global and regional aerosol burden, radiative flux, and surface temperature responses to removing anthropogenic sulfur dioxide (SO2) emissions from China. We find that the models differ by up to a factor of 6 in the simulated change in aerosol optical depth (AOD) and shortwave radiative flux over China that results from reduced sulfate aerosol, leading to a large range of magnitudes in the regional and global temperature responses. Two of the three models simulate a near-ubiquitous hemispheric warming due to the regional SO2 removal, with similarities in the local and remote pattern of response, but overall with a substantially different magnitude. The third model simulates almost no significant temperature response. We attribute the discrepancies in the response to a combination of substantial differences in the chemical conversion of SO2 to sulfate, translation of sulfate mass into AOD, cloud radiative interactions, and differences in the radiative forcing efficiency of sulfate aerosol in the models. The model with the strongest response (HadGEM3-GA4) compares best with observations of AOD regionally, however the other two models compare similarly (albeit poorly) and still disagree substantially in their simulated climate response, indicating that total AOD observations are far from sufficient to determine which model response is more plausible. Our results highlight that there remains a large uncertainty in the representation of both aerosol chemistry as well as direct and indirect aerosol radiative effects in current climate models, and reinforces that caution must be applied when interpreting the results of modelling studies of aerosol influences on climate. Model studies that implicate aerosols in climate responses should ideally explore a range of radiative forcing strengths representative of this uncertainty, in addition to thoroughly evaluating the models used against observations.
C1 [Kasoar, Matthew; Voulgarakis, Apostolos] Imperial Coll London, Dept Phys, London, England.
[Lamarque, Jean-Francois] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling & Climate & Gl, POB 3000, Boulder, CO 80307 USA.
[Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Bellouin, Nicolas; Collins, William J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Faluvegi, Greg; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Faluvegi, Greg; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Kasoar, M (reprint author), Imperial Coll London, Dept Phys, London, England.
EM m.kasoar12@imperial.ac.uk
RI Collins, William/A-5895-2010
OI Collins, William/0000-0002-7419-0850
FU Natural Environment Research Council [NE/K500872/1]; European
Commission's Marie Curie Actions International Research Staff Exchange
Scheme (IRSES)
FX Matthew Kasoar and Apostolos Voulgarakis are supported by the Natural
Environment Research Council under grant no. NE/K500872/1. Also, we wish
to thank the European Commission's Marie Curie Actions International
Research Staff Exchange Scheme (IRSES) for funding MK's placement at
NASA GISS and Columbia University and facilitating interactions on this
work with the US colleagues, as part of the Regional Climate-Air Quality
Interactions (REQUA) project. Simulations with GISS-E2 used resources
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center.
Simulations with HadGEM3-GA4 were performed using the MONSooN system, a
collaborative facility supplied under the Joint Weather and Climate
Research Programme, which is a strategic partnership between the Met
Office and the Natural Environment Research Council. We specifically
thank Fiona O'Connor, Jeremy Walton, and Mohit Dalvi from the Met Office
for their support with using the HadGEM3-GA4 model.
NR 75
TC 5
Z9 5
U1 13
U2 13
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 4
PY 2016
VL 16
IS 15
BP 9785
EP 9804
DI 10.5194/acp-16-9785-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV6MD
UT WOS:000383049300002
ER
PT J
AU Bauder, JM
Breininger, DR
Bolt, MR
Legare, ML
Jenkins, CL
Rothermel, BB
McGarigal, K
AF Bauder, Javan M.
Breininger, David R.
Bolt, M. Rebecca
Legare, Michael L.
Jenkins, Christopher L.
Rothermel, Betsie B.
McGarigal, Kevin
TI The Influence of Sex and Season on Conspecific Spatial Overlap in a
Large, Actively-Foraging Colubrid Snake
SO PLOS ONE
LA English
DT Article
ID EASTERN INDIGO SNAKE; RATTLESNAKES CROTALUS-VIRIDIS; KERNEL
DENSITY-ESTIMATION; HOME-RANGE OVERLAP; DRYMARCHON-COUPERI; BODY-SIZE;
SPACE-USE; MASTICOPHIS-FLAGELLUM; POPULATION REGULATION; TERRITORIAL
BEHAVIOR
AB Understanding the factors influencing the degree of spatial overlap among conspecifics is important for understanding multiple ecological processes. Compared to terrestrial carnivores, relatively little is known about the factors influencing conspecific spatial overlap in snakes, although across snake taxa there appears to be substantial variation in conspecific spatial overlap. In this study, we described conspecific spatial overlap of eastern indigo snakes (Drymarchon couperi) in peninsular Florida and examined how conspecific spatial overlap varied by sex and season (breeding season vs. non-breeding season). We calculated multiple indices of spatial overlap using 6-and 3-month utilization distributions (UD) of dyads of simultaneously adjacent telemetered snakes. We also measured conspecific UD density values at each telemetry fix and modeled the distribution of those values as a function of overlap type, sex, and season using generalized Pareto distributions. Home range overlap between males and females was significantly greater than overlap between individuals of the same sex and male home ranges often completely contained female home ranges. Male home ranges overlapped little during both seasons, whereas females had higher levels of overlap during the non-breeding season. The spatial patterns observed in our study are consistent with those seen in many mammalian carnivores, in which low male-male overlap and high inter-sexual overlap provides males with greater access to females. We encourage additional research on the influence of prey availability on conspecific spatial overlap in snakes as well as the behavioral mechanisms responsible for maintaining the low levels of overlap we observed.
C1 [Bauder, Javan M.; McGarigal, Kevin] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA.
[Breininger, David R.; Bolt, M. Rebecca] NASA, Ecol Programs, Integrated Miss Support Serv, Kennedy Space Ctr, Titusville, FL USA.
[Legare, Michael L.] Merritt Isl Natl Wildlife Refuge, Titusville, FL USA.
[Jenkins, Christopher L.] Orianne Soc, Athens, GA USA.
[Rothermel, Betsie B.] Archbold Biol Stn, Venus, FL USA.
RP Bauder, JM (reprint author), Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA.
EM javanvonherp@gmail.com
FU United States Fish and Wildlife Service; Orianne Society; NASA; Bailey
Wildlife Foundation
FX Funding for this project was provided by the United States Fish and
Wildlife Service (www.fws.gov) and The Orianne Society
(www.oriannesociety.org) to JMB and CLJ and by the United States Fish
and Wildlife Service, NASA, and the Bailey Wildlife Foundation to DRB,
MRB, and MLL. The funders had no role in the study design, data
collection and analysis, decision to publish, or preparation of this
manuscript.
NR 101
TC 1
Z9 1
U1 14
U2 15
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD AUG 4
PY 2016
VL 11
IS 8
AR e0160033
DI 10.1371/journal.pone.0160033
PG 19
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DT3GL
UT WOS:000381368900027
PM 27490346
ER
PT J
AU Yan, XL
Wright, JS
Zheng, XD
Livesey, NJ
Vomel, H
Zhou, XJ
AF Yan, Xiaolu
Wright, Jonathon S.
Zheng, Xiangdong
Livesey, Nathaniel J.
Vomel, Holger
Zhou, Xiuji
TI Validation of Aura MLS retrievals of temperature, water vapour and ozone
in the upper troposphere and lower-middle stratosphere over the Tibetan
Plateau during boreal summer
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID EOS MLS; SATELLITE; TRANSPORT; HUMIDITY
AB We validate Aura Microwave Limb Sounder (MLS) version 3 (v3) and version 4 (v4) retrievals of summertime temperature, water vapour and ozone in the upper troposphere and lower-middle stratosphere (UTLS; 10-316 hPa) against balloon soundings collected during the Study of Ozone, Aerosols and Radiation over the Tibetan Plateau (SOAR-TP). Mean v3 and v4 profiles of temperature, water vapour and ozone in this region during the measurement campaigns are almost identical through most of the stratosphere (10-68 hPa), but differ in several respects in the upper troposphere and tropopause layer. Differences in v4 relative to v3 include slightly colder mean temperatures from 100 to 316 hPa, smaller mean water vapour mixing ratios in the upper troposphere (215-316 hPa) and a more vertically homogeneous profile of mean ozone mixing ratios below the climatological tropopause (100-316 hPa). These changes substantially improve agreement between ozonesondes and MLS ozone retrievals in the upper troposphere, but slightly worsen existing cold and dry biases at these levels.
Aura MLS temperature profiles contain significant cold biases relative to collocated temperature measurements in several layers of the lower-middle stratosphere and in the upper troposphere. MLS retrievals of water vapour volume mixing ratio generally compare well with collocated measurements, excepting a substantial dry bias (-32 +/- 11% in v4) that extends through most of the upper troposphere (121-261 hPa). MLS retrievals of ozone volume mixing ratio are biased high relative to collocated ozonesondes in the stratosphere (18-83 hPa), but are biased low at 100 hPa. The largest relative biases in ozone retrievals (approximately +70 %) are located at 83 hPa. MLS v4 offers substantial benefits relative to v3, particularly with respect to water vapour and ozone. Key improvements include larger data yields, reduced noise in the upper troposphere and smaller fluctuations in the bias profile at pressures larger than 100 hPa. The situation for temperature is less clear, with cold biases and noise levels in the upper troposphere, both larger in v4 than in v3. Several aspects of our results differ from those of validations conducted in other locations. These differences are often amplified by monsoon onset, indicating that the Asian monsoon anticyclone poses unique challenges for remote sensing that impact the quality of MLS retrievals in this region.
C1 [Yan, Xiaolu; Zheng, Xiangdong; Zhou, Xiuji] Chinese Acad Meteorol Sci, Beijing, Peoples R China.
[Wright, Jonathon S.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing, Peoples R China.
[Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Vomel, Holger] Natl Ctr Atmospher Res, Earth Observing Lab, POB 3000, Boulder, CO 80307 USA.
[Yan, Xiaolu] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China.
[Yan, Xiaolu] Forschungszentrum Julich, Inst Energy & Climate Res Stratosphere IEK 7, Julich, Germany.
RP Zheng, XD (reprint author), Chinese Acad Meteorol Sci, Beijing, Peoples R China.; Wright, JS (reprint author), Tsinghua Univ, Ctr Earth Syst Sci, Beijing, Peoples R China.
EM jswright@tsinghua.edu.cn; zhengxd@cams.cma.gov.cn
FU National Natural Science Foundation of China [40875014]; Special Fund
for Meteorological Research in the Public Interest [GYHY201106023];
Science and Technological Innovation Team Project of Chinese Academy of
Meteorological Science [2011Z003, 2013Z005]; Young Thousand Talents
fellowship at Tsinghua University; Tengchong Meteorological Bureau in
Yunnan; Naqu Meteorological Bureau; Lhasa Meteorological Bureau; Linzhi
Meteorological Bureau in Tibet
FX Support for the balloon soundings at Tengchong was provided by the
National Natural Science Foundation of China under grant 40875014.
Support for the balloon soundings at Naqu, Lhasa and Linzhi was provided
the Special Fund for Meteorological Research in the Public Interest
under grant GYHY201106023 and the Science and Technological Innovation
Team Project of Chinese Academy of Meteorological Science under grants
2011Z003 and 2013Z005. The validation analysis was supported by a Young
Thousand Talents fellowship at Tsinghua University. The measurement
campaigns were supported by the Tengchong Meteorological Bureau in
Yunnan and the Naqu Meteorological Bureau, Lhasa Meteorological Bureau
and Linzhi Meteorological Bureau in Tibet. Work at the Jet Propulsion
Laboratory, California Institute of Technology was performed under a
contract with the National Aeronautics and Space Administration. We
thank Michelle Santee, Irina Gerasimov and James E. Johnson for
facilitating early access to the MLS version 4 data; Yonghong Ma and
Yong Zhang from the Tibet Meteorological Bureau; Weiguo Wang from Yunnan
University and the staff members of Kunming Observatory; Kejia Jia at
the Linzhi Meteorological Bureau; and Wei Li, Jianyang Song, Jin Ma and
Shumeng Sun from the Chinese Academy of Meteorological Sciences.
NR 39
TC 0
Z9 0
U1 3
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 3
PY 2016
VL 9
IS 8
BP 3547
EP 3566
DI 10.5194/amt-9-3547-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV6MG
UT WOS:000383049600001
ER
PT J
AU Hedelius, JK
Viatte, C
Wunch, D
Roehl, CM
Toon, GC
Chen, J
Jones, T
Wofsy, SC
Franklin, JE
Parker, H
Dubey, MK
Wennberg, PO
AF Hedelius, Jacob K.
Viatte, Camille
Wunch, Debra
Roehl, Coleen M.
Toon, Geoffrey C.
Chen, Jia
Jones, Taylor
Wofsy, Steven C.
Franklin, Jonathan E.
Parker, Harrison
Dubey, Manvendra K.
Wennberg, Paul O.
TI Assessment of errors and biases in retrievals of X-CO2, X-CH4, X-CO, and
X-N2O from a 0.5 cm(-1) resolution solar-viewing spectrometer
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID FOURIER-TRANSFORM SPECTROMETRY; GREENHOUSE-GAS EMISSIONS; INSTRUMENTAL
LINE-SHAPE; PORTABLE FTIR SPECTROMETERS; COLUMN OBSERVING NETWORK; FTS;
CH4; SPECTROSCOPY; VERIFICATION; CALIBRATION
AB Bruker (TM) EM27/SUN instruments are commercial mobile solar-viewing near-IR spectrometers. They show promise for expanding the global density of atmospheric column measurements of greenhouse gases and are being marketed for such applications. They have been shown to measure the same variations of atmospheric gases within a day as the high-resolution spectrometers of the Total Carbon Column Observing Network (TCCON). However, there is little known about the long-term precision and uncertainty budgets of EM27/SUN measurements. In this study, which includes a comparison of 186 measurement days spanning 11 months, we note that atmospheric variations of X-gas within a single day are well captured by these low-resolution instruments, but over several months, the measurements drift noticeably. We present comparisons between EM27/SUN instruments and the TCCON using GGG as the retrieval algorithm. In addition, we perform several tests to evaluate the robustness of the performance and determine the largest sources of errors from these spectrometers. We include comparisons of X-CO2, X-CH4, X-CO, and X-N2O. Specifically we note EM27/SUN biases for January 2015 of 0.03, 0.75, -0.12, and 2.43% for X-CO2, X-CH4, X-CO, and X-N2O respectively, with 1 sigma running precisions of 0.08 and 0.06% for X-CO2 and X-CH4 from measurements in Pasadena. We also identify significant error caused by nonlinear sensitivity when using an extended spectral range detector used to measure CO and N2O.
C1 [Hedelius, Jacob K.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Viatte, Camille; Wunch, Debra; Roehl, Coleen M.; Toon, Geoffrey C.; Wennberg, Paul O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Chen, Jia; Jones, Taylor; Wofsy, Steven C.; Franklin, Jonathan E.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Chen, Jia; Jones, Taylor; Wofsy, Steven C.; Franklin, Jonathan E.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
[Franklin, Jonathan E.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Parker, Harrison; Dubey, Manvendra K.] Los Alamos Natl Lab, Earth & Environm Sci, Los Alamos, NM USA.
[Wunch, Debra] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Chen, Jia] Tech Univ Munich, Elect & Comp Engn, Munich, Germany.
RP Hedelius, JK (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
EM jhedeliu@caltech.edu
RI Dubey, Manvendra/E-3949-2010;
OI Dubey, Manvendra/0000-0002-3492-790X; Hedelius,
Jacob/0000-0003-2025-7519
FU W. M. Keck Institute for Space Studies; Caltech Chemistry and Chemical
Engineering Division Fellowship - Dow Chemical Graduate Fellowship; NASA
Carbon Cycle Science program [NNX14AI60G]; Jet Propulsion Laboratory;
NASA-CMS; NSF MRI Award [1337512]
FX We thank Frank Hase and Michael Gisi for helpful discussions on ghost
reduction, detector nonlinearity, and ILS measurements. We further thank
Michael Gisi and Bruker Optics (TM) for loaning us a standard InGaAs
detector for testing and for instructions on realigning the EM27/SUN. We
thank Dietrich Feist for discussions on mirror degradation. We also
thank Nicholas Jones, David Giffith, Frank Hase, and Sabrina Arnold for
sharing their experience with mirror degradation. This work is supported
in part by the W. M. Keck Institute for Space Studies. Jacob Hedelius
was also partially supported by a Caltech Chemistry and Chemical
Engineering Division Fellowship funded by the Dow Chemical Graduate
Fellowship, and expresses thanks to them. The authors gratefully
acknowledge funding from the NASA Carbon Cycle Science program (grant
number NNX14AI60G) and the Jet Propulsion Laboratory. Manvendra K. Dubey
acknowledges funding from the NASA-CMS program for field observations
and from the LANL-LDRD for the acquisition of the LANL EM27/SUN. Jia
Chen, Taylor Jones, Jonathan E. Franklin, and Steven C. Wofsy
acknowledge funding provided by NSF MRI Award 1337512.
NR 43
TC 0
Z9 0
U1 4
U2 4
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 3
PY 2016
VL 9
IS 8
BP 3527
EP 3546
DI 10.5194/amt-9-3527-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3MT
UT WOS:000382827300001
ER
PT J
AU Bell, JR
Molthan, AL
AF Bell, Jordan R.
Molthan, Andrew L.
TI Evaluation of Approaches to Identifying Hail Damage to Crop Vegetation
Using Satellite Imagery
SO JOURNAL OF OPERATIONAL METEOROLOGY
LA English
DT Article
ID INDEX; STORM
AB During the growing season in the central United States, severe thunderstorms frequently occur and produce large hail that damages the underlying vegetation, often in agricultural areas. Satellite remote sensing provides a tool for identifying these damaged areas. Previous studies have used changes in the normalized difference vegetation index (NDVI) to identify and examine these areas of damage, but have done so in a manual, time-consuming manner. This study examines an automated approach to detecting areas of hail damage in satellite imagery. Two techniques are evaluated: (i) use of an NDVI change threshold and (ii) detection of anomalies that occur in both daily NDVI and land surface temperature imagery. The two techniques are scored against one another using three different case studies. Two of the case studies occurred late in the growing season in August, and the third occurred in the growing season in early June. The NDVI threshold performed well in the two August case studies with a final probability of detection (POD) ranging from 0.497 to 0.647, whereas the anomaly detection for these two case studies had a lower POD of 0.317 to 0.587. The early June case study highlighted the limitations of using an NDVI threshold and the strengths of using anomaly detection. The POD for the NDVI threshold technique was 0.07-0.08 with a false alarm ratio (FAR) of 0.661-0.758, whereas the anomaly detection had a POD of 0.399-0.418 and a FAR of 0.540-0.681 for this third case study.
C1 [Bell, Jordan R.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
[Molthan, Andrew L.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA.
RP Bell, JR (reprint author), 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM jordan.r.bell@nasa.gov
NR 23
TC 0
Z9 0
U1 0
U2 0
PU NATL WEATHER ASSOC
PI NORMAN
PA 350 DAVID L BOREN BLVD, STE 2750, NORMAN, OK USA
SN 2325-6184
J9 J OPER METEOROL
JI J. Oper. Meteorol.
PD AUG 2
PY 2016
VL 4
IS 11
BP 142
EP 159
DI 10.15191/nwajom.2016.0411
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EC9VM
UT WOS:000388492400001
ER
PT J
AU Petersen, N
Jaekel, P
Rosenberger, A
Weber, T
Scott, J
Castrucci, F
Lambrecht, G
Ploutz-Snyder, L
Damann, V
Kozlovskaya, I
Mester, J
AF Petersen, Nora
Jaekel, Patrick
Rosenberger, Andre
Weber, Tobias
Scott, Jonathan
Castrucci, Filippo
Lambrecht, Gunda
Ploutz-Snyder, Lori
Damann, Volker
Kozlovskaya, Inessa
Mester, Joachim
TI Exercise in space: the European Space Agency approach to in-flight
exercise countermeasures for long-duration missions on ISS
SO EXTREME PHYSIOLOGY & MEDICINE
LA English
DT Article
DE Exercise countermeasures; Microgravity; European Space Agency;
International Space Station; Astronaut training; Space flight; Physical
performance
ID SPACEFLIGHT; MICROGRAVITY; WEIGHT; MUSCLE; BONE
AB Background: To counteract microgravity (mu G)-induced adaptation, European Space Agency (ESA) astronauts on long-duration missions (LDMs) to the International Space Station (ISS) perform a daily physical exercise countermeasure program. Since the first ESA crewmember completed an LDM in 2006, the ESA countermeasure program has strived to provide efficient protection against decreases in body mass, muscle strength, bone mass, and aerobic capacity within the operational constraints of the ISS environment and the changing availability of on-board exercise devices. The purpose of this paper is to provide a description of ESA's individualised approach to in-flight exercise countermeasures and an up-to-date picture of how exercise is used to counteract physiological changes resulting from mu G-induced adaptation. Changes in the absolute workload for resistive exercise, treadmill running and cycle ergometry throughout ESA's eight LDMs are also presented, and aspects of pre-flight physical preparation and post-flight reconditioning outlined.
Results: With the introduction of the advanced resistive exercise device (ARED) in 2009, the relative contribution of resistance exercise to total in-flight exercise increased (33-46 %), whilst treadmill running (42-33 %) and cycle ergometry (26-20 %) decreased. All eight ESA crewmembers increased their in-flight absolute workload during their LDMs for resistance exercise and treadmill running (running speed and vertical loading through the harness), while cycle ergometer workload was unchanged across missions.
Conclusion: Increased or unchanged absolute exercise workloads in-flight would appear contradictory to typical post-flight reductions in muscle mass and strength, and cardiovascular capacity following LDMs. However, increased absolute in-flight workloads are not directly linked to changes in exercise capacity as they likely also reflect the planned, conservative loading early in the mission to allow adaption to mu G exercise, including personal comfort issues with novel exercise hardware (e.g. the treadmill harness). Inconsistency in hardware and individualised support concepts across time limit the comparability of results from different crewmembers, and questions regarding the difference between cycling and running in mu G versus identical exercise here on Earth, and other factors that might influence in-flight exercise performance, still require further investigation.
C1 [Petersen, Nora; Jaekel, Patrick; Rosenberger, Andre; Scott, Jonathan; Lambrecht, Gunda] Wyle GmbH, Cologne, Germany.
[Petersen, Nora; Jaekel, Patrick; Rosenberger, Andre; Weber, Tobias; Scott, Jonathan; Castrucci, Filippo; Damann, Volker] ESA, Space Med Off HSO AM, European Astronaut Ctr Dept, D HSO, Geb 12,POB 906096, D-51147 Cologne, Germany.
[Castrucci, Filippo] Deutsch Zentrum Luft & Raumfahrt, Cologne, Germany.
[Ploutz-Snyder, Lori] NASA, Univ Space Res Assoc, Johnson Space Ctr, B261,SK3, Houston, TX 77058 USA.
[Kozlovskaya, Inessa] Russian Space Federat Roscosmos, Inst Biomed Problems IBMP, Khoroshevskoe Shosse 76A, Moscow 123007, Russia.
[Petersen, Nora; Mester, Joachim] German Sport Univ Cologne DSHS, Inst Training Sci & Sport Informat, Sportpk Muengersdorf 6, D-50933 Cologne, Germany.
[Damann, Volker] ISU, Parc Innovat,1 Rue Jean Domin Cassini, F-67400 Illkirch Graffenstaden, France.
RP Petersen, N (reprint author), ESA, Space Med Off HSO AM, European Astronaut Ctr Dept, D HSO, Geb 12,POB 906096, D-51147 Cologne, Germany.
EM Nora.Petersen@esa.int
RI Kozlovskaya, Inesa/R-9729-2016
NR 24
TC 0
Z9 0
U1 2
U2 2
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 2046-7648
J9 EXTREME PHYSIOL MED
JI Extreme Physiol. Med.
PD AUG 2
PY 2016
VL 5
AR 9
DI 10.1186/s13728-016-0050-4
PG 13
WC Physiology
SC Physiology
GA EB9XT
UT WOS:000387751900001
PM 27489615
ER
PT J
AU Vitello, EA
Quek, SI
Kincaid, H
Fuchs, T
Crichton, DJ
Troisch, P
Liu, AY
AF Vitello, Elizabeth A.
Quek, Sue-Ing
Kincaid, Heather
Fuchs, Thomas
Crichton, Daniel J.
Troisch, Pamela
Liu, Alvin Y.
TI Cancer-secreted AGR2 induces programmed cell death in normal cells
SO ONCOTARGET
LA English
DT Article
DE AGR2; prostate cancer cell types; prostate stromal cells; programmed
cell death; SAT1
ID PROSTATE-CANCER; ANTERIOR GRADIENT-2; PANCREATIC-CANCER;
DOWN-REGULATION; STROMAL CELLS; VOIDED URINE; GENE; EXPRESSION;
APOPTOSIS; PROMOTES
AB Anterior Gradient 2 (AGR2) is a protein expressed in many solid tumor types including prostate, pancreatic, breast and lung. AGR2 functions as a protein disulfide isomerase in the endoplasmic reticulum. However, AGR2 is secreted by cancer cells that overexpress this molecule. Secretion of AGR2 was also found in salamander limb regeneration. Due to its ubiquity, tumor secretion of AGR2 must serve an important role in cancer, yet its molecular function is largely unknown. This study examined the effect of cancer-secreted AGR2 on normal cells. Prostate stromal cells were cultured, and tissue digestion media containing AGR2 prepared from prostate primary cancer 10-076 CP and adenocarcinoma LuCaP 70CR xenograft were added. The control were tissue digestion media containing no AGR2 prepared from benign prostate 10076 NP and small cell carcinoma LuCaP 145.1 xenograft. In the presence of tumor-secreted AGR2, the stromal cells were found to undergo programmed cell death (PCD) characterized by formation of cellular blebs, cell shrinkage, and DNA fragmentation as seen when the stromal cells were UV irradiated or treated by a pro-apoptotic drug. PCD could be prevented with the addition of the monoclonal AGR2-neutralizing antibody P3A5. DNA microarray analysis of LuCaP 70CR media-treated vs. LuCaP 145.1 media-treated cells showed downregulation of the gene SAT1 as a major change in cells exposed to AGR2. RT-PCR analysis confirmed the array result. SAT1 encodes spermidine/spermine N-1-acetyltransferase, which maintains intracellular polyamine levels. Abnormal polyamine metabolism as a result of altered SAT1 activity has an adverse effect on cells through the induction of PCD.
C1 [Vitello, Elizabeth A.; Quek, Sue-Ing; Liu, Alvin Y.] Univ Washington, Dept Urol, Seattle, WA 98195 USA.
[Vitello, Elizabeth A.; Quek, Sue-Ing; Liu, Alvin Y.] Univ Washington, Inst Stem Cell & Regenerat Med, Seattle, WA 98195 USA.
[Kincaid, Heather; Fuchs, Thomas; Crichton, Daniel J.] EDRN Informat Ctr, Pasadena, CA USA.
[Kincaid, Heather; Fuchs, Thomas; Crichton, Daniel J.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Troisch, Pamela] Inst Syst Biol, Seattle, WA USA.
[Quek, Sue-Ing] Singapore Polytech, Ctr Biomed & Life Sci T11A 412, Level 4, Singapore, Singapore.
RP Vitello, EA (reprint author), Univ Washington, Dept Urol, Seattle, WA 98195 USA.; Vitello, EA (reprint author), Univ Washington, Inst Stem Cell & Regenerat Med, Seattle, WA 98195 USA.
EM evitello@uw.edu
FU NCI [CA111244, NNN13R204T]
FX This work was supported by NCI grant CA111244, an interagency agreement
between NASA and JPL Task Order Number NNN13R204T.
NR 45
TC 0
Z9 0
U1 1
U2 1
PU IMPACT JOURNALS LLC
PI ALBANY
PA 6211 TIPTON HOUSE, STE 6, ALBANY, NY 12203 USA
SN 1949-2553
J9 ONCOTARGET
JI Oncotarget
PD AUG 2
PY 2016
VL 7
IS 31
BP 49425
EP 49434
DI 10.18632/oncotarget.9921
PG 10
WC Oncology; Cell Biology
SC Oncology; Cell Biology
GA DY8ZS
UT WOS:000385422000047
PM 27283903
ER
PT J
AU Snider, G
Weagle, CL
Murdymootoo, KK
Ring, A
Ritchie, Y
Stone, E
Walsh, A
Akoshile, C
Anh, NX
Balasubramanian, R
Brook, J
Qonitan, FD
Dong, JL
Griffith, D
He, KB
Holben, BN
Kahn, R
Lagrosas, N
Lestari, P
Ma, ZW
Misra, A
Norford, LK
Quel, EJ
Salam, A
Schichtel, B
Segev, L
Tripathi, S
Wang, C
Yu, C
Zhang, Q
Zhang, YX
Brauer, M
Cohen, A
Gibson, MD
Liu, Y
Martins, JV
Rudich, Y
Martin, RV
AF Snider, Graydon
Weagle, Crystal L.
Murdymootoo, Kalaivani K.
Ring, Amanda
Ritchie, Yvonne
Stone, Emily
Walsh, Ainsley
Akoshile, Clement
Nguyen Xuan Anh
Balasubramanian, Rajasekhar
Brook, Jeff
Qonitan, Fatimah D.
Dong, Jinlu
Griffith, Derek
He, Kebin
Holben, Brent N.
Kahn, Ralph
Lagrosas, Nofel
Lestari, Puji
Ma, Zongwei
Misra, Amit
Norford, Leslie K.
Quel, Eduardo J.
Salam, Abdus
Schichtel, Bret
Segev, Lior
Tripathi, Sachchida
Wang, Chien
Yu, Chao
Zhang, Qiang
Zhang, Yuxuan
Brauer, Michael
Cohen, Aaron
Gibson, Mark D.
Liu, Yang
Martins, J. Vanderlei
Rudich, Yinon
Martin, Randall V.
TI Variation in global chemical composition of PM2.5: emerging results from
SPARTAN
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID FINE PARTICULATE MATTER; SINGLE-PARAMETER REPRESENTATION; CONDENSATION
NUCLEUS ACTIVITY; BIOMASS BURNING AEROSOL; SOUTHEASTERN UNITED-STATES;
EXTENDED FOLLOW-UP; LONG-TERM EXPOSURE; HARVARD 6 CITIES; HYGROSCOPIC
GROWTH; AIR-POLLUTION
AB The Surface PARTiculate mAtter Network (SPARTAN) is a long-term project that includes characterization of chemical and physical attributes of aerosols from filter samples collected worldwide. This paper discusses the ongoing efforts of SPARTAN to define and quantify major ions and trace metals found in fine particulate matter (PM2.5). Our methods infer the spatial and temporal variability of PM2.5 in a cost-effective manner. Gravimetrically weighed filters represent multi-day averages of PM2.5, with a collocated nephelometer sampling air continuously. SPARTAN instruments are paired with AErosol RObotic NETwork (AERONET) sun photometers to better understand the relationship between ground-level PM2.5 and columnar aerosol optical depth (AOD).
We have examined the chemical composition of PM2.5 at 12 globally dispersed, densely populated urban locations and a site at Mammoth Cave (US) National Park used as a background comparison. So far, each SPARTAN location has been active between the years 2013 and 2016 over periods of 2-26 months, with an average period of 12 months per site. These sites have collectively gathered over 10 years of quality aerosol data. The major PM2.5 constituents across all sites (relative contribution +/- SD) are ammoniated sulfate (20% +/- 11 %), crustal material (13.4% +/- 9.9 %), equivalent black carbon (11.9% +/- 8.4 %), ammonium nitrate (4.7% +/- 3.0 %), sea salt (2.3% +/- 1.6 %), trace element oxides (1.0% +/- 1.1 %), water (7.2% +/- 3.3 %) at 35% RH, and residual matter (40% +/- 24 %).
Analysis of filter samples reveals that several PM2.5 chemical components varied by more than an order of magnitude between sites. Ammoniated sulfate ranges from 1.1 mu g m(-3) (Buenos Aires, Argentina) to 17 mu g m(-3) (Kanpur, India in the dry season). Ammonium nitrate ranged from 0.2 mu g m(-3) (Mammoth Cave, in summer) to 6.8 mu g m(-3) (Kanpur, dry season). Equivalent black carbon ranged from 0.7 mu g m(-3) (Mammoth Cave) to over 8 mu g m(-3) (Dhaka, Bangladesh and Kanpur, India). Comparison of SPARTAN vs. coincident measurements from the Interagency Monitoring of Protected Visual Environments (IMPROVE) network at Mammoth Cave yielded a high degree of consistency for daily PM2.5 (r(2) = 0.76, slope = 1.12), daily sulfate (r(2) = 0.86, slope = 1.03), and mean fractions of all major PM2.5 components (within 6 %). Major ions generally agree well with previous studies at the same urban locations (e.g. sulfate fractions agree within 4% for 8 out of 11 collocation comparisons). Enhanced anthropogenic dust fractions in large urban areas (e.g. Singapore, Kanpur, Hanoi, and Dhaka) are apparent from high Zn : Al ratios.
The expected water contribution to aerosols is calculated via the hygroscopicity parameter kappa(v) for each filter. Mean aggregate values ranged from 0.15 (Ilorin) to 0.28 (Rehovot). The all-site parameter mean is 0.20 +/- 0.04. Chemical composition and water retention in each filter measurement allows inference of hourly PM2.5 at 35% relative humidity by merging with nephelometer measurements. These hourly PM2.5 estimates compare favourably with a beta attenuation monitor (MetOne) at the nearby US embassy in Beijing, with a coefficient of variation r(2) = 0.67 (n = 3167), compared to r(2) = 0.62 when kappa(v) was not considered. SPARTAN continues to provide an open-access database of PM2.5 compositional filter information and hourly mass collected from a global federation of instruments.
C1 [Snider, Graydon; Murdymootoo, Kalaivani K.; Ring, Amanda; Ritchie, Yvonne; Stone, Emily; Walsh, Ainsley; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Weagle, Crystal L.; Martin, Randall V.] Dalhousie Univ, Dept Chem, Halifax, NS, Canada.
[Akoshile, Clement] Univ Ilorin, Dept Phys, Ilorin, Nigeria.
[Nguyen Xuan Anh] Vietnam Acad Sci & Technol, Inst Geophys, Hanoi, Vietnam.
[Balasubramanian, Rajasekhar] Natl Univ Singapore, Dept Civil & Environm Engn, Singapore, Singapore.
[Brook, Jeff] Univ Toronto, Dept Publ Hlth Sci, Toronto, ON, Canada.
[Qonitan, Fatimah D.; Lestari, Puji] ITB, Fac Civil & Environm Engn, JL Ganesha 10, Bandung, Indonesia.
[Dong, Jinlu; He, Kebin; Zhang, Qiang; Zhang, Yuxuan] Tsinghua Univ, Ctr Earth Syst Sci, Beijing, Peoples R China.
[Griffith, Derek] Council Sci & Ind Res CSIR, Pretoria, South Africa.
[Holben, Brent N.; Kahn, Ralph] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lagrosas, Nofel] Ateneo Manila Univ, Manila Observ, Quezon City, Philippines.
[Ma, Zongwei] Nanjing Univ, Sch Environm, Nanjing, Jiangsu, Peoples R China.
[Misra, Amit; Tripathi, Sachchida] Indian Inst Technol Kanpur, Ctr Environm Sci & Engn, Kanpur, Uttar Pradesh, India.
[Norford, Leslie K.] MIT, Dept Architecture, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Quel, Eduardo J.] UNIDEF CITEDEF CONICET, Juan B de la Salle 4397 B1603ALO Villa Martelli, Buenos Aires, DF, Argentina.
[Salam, Abdus] Univ Dhaka, Dept Chem, Dhaka, Bangladesh.
[Schichtel, Bret] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Segev, Lior; Rudich, Yinon] Weizmann Inst Sci, Dept Earth & Planetary Sci, Rehovot, Israel.
[Wang, Chien] MIT, Ctr Global Change Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Yu, Chao; Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, 1518 Clifton Rd NE, Atlanta, GA 30322 USA.
[Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC, Canada.
[Cohen, Aaron] Hlth Effects Inst, 101 Fed St Suite 500, Boston, MA USA.
[Gibson, Mark D.] Dalhousie Univ, Dept Proc Engn & Appl Sci, Halifax, NS, Canada.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MA USA.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MA USA.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Snider, G; Martin, RV (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.; Martin, RV (reprint author), Dalhousie Univ, Dept Chem, Halifax, NS, Canada.; Martin, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM graydon.snider@dal.ca; randall.martin@dal.ca
RI Zhang, Qiang/D-9034-2012; Tripathi, Sachchida/J-4840-2016;
Balasubramanian, Rajasekhar/C-2243-2011
OI Balasubramanian, Rajasekhar/0000-0002-5627-3628
FU Natural Sciences and Engineering Research Council (NSERC) of Canada;
grant HIBAH WCU-ITB; National Academy of Sciences; USAID; Singapore
National Research Foundation (NRF) through the Singapore-MIT Alliance
for Research and Technology (SMART), Center for Environmental Sensing
and Modeling
FX SPARTAN is an IGAC-endorsed activity (www.igacproject.org). The Natural
Sciences and Engineering Research Council (NSERC) of Canada supported
this work. We are grateful to many who have offered helpful comments and
advice on the creation of this network including Jay Al-Saadi, Ross
Anderson, Kalpana Balakrishnan, Len Barrie, Sundar Christopher, Matthew
Cooper, Jim Crawford, Doug Dockery, Jill Engel-Cox, Greg Evans, Markus
Fiebig, Allan Goldstein, Judy Guernsey, Ray Hoff, Rudy Husar, Mike
Jerrett, Michaela Kendall, Rich Kleidman, Petros Koutrakis, Glynis
Lough, Doreen Neil, John Ogren, Norm O'Neil, Jeff Pierce, Thomas
Holzer-Popp, Ana Prados, Lorraine Remer, Sylvia Richardson, and Frank
Speizer. Data collection in Rehovot was supported in part by the
Environmental Health Fund (Israel) and the Weizmann Institute. Partial
support for the ITB site was under the grant HIBAH WCU-ITB. The site at
IIT Kanpur is supported in part by National Academy of Sciences and
USAID. The views expressed here are of authors and do not necessarily
reflect those of NAS or USAID. The Singapore site is supported by the
Singapore National Research Foundation (NRF) through the Singapore-MIT
Alliance for Research and Technology (SMART), Center for Environmental
Sensing and Modeling.
NR 110
TC 0
Z9 0
U1 25
U2 25
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 2
PY 2016
VL 16
IS 15
BP 9629
EP 9653
DI 10.5194/acp-16-9629-2016
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3MG
UT WOS:000382825800004
ER
PT J
AU Connor, BJ
Sherlock, V
Toon, G
Wunch, D
Wennberg, PO
AF Connor, Brian J.
Sherlock, Vanessa
Toon, Geoff
Wunch, Debra
Wennberg, Paul O.
TI GFIT2: an experimental algorithm for vertical profile retrieval from
near-IR spectra
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID OZONE; CO2; STRATOSPHERE
AB An algorithm for retrieval of vertical profiles from ground-based spectra in the near IR is described and tested. Known as GFIT2, the algorithm is primarily intended for CO2, and is used exclusively for CO2 in this paper. Retrieval of CO2 vertical profiles from ground-based spectra is theoretically possible, would be very beneficial for carbon cycle studies and the validation of satellite measurements, and has been the focus of much research in recent years. GFIT2 is tested by application both to synthetic spectra and to measurements at two Total Carbon Column Observing Network (TCCON) sites. We demonstrate that there are approximately 3 degrees of freedom for the CO2 profile, and the algorithm performs as expected on synthetic spectra. We show that the accuracy of retrievals of CO2 from measurements in the 1.61 mu (6220 cm(-1)) spectral band is limited by small uncertainties in calculation of the atmospheric spectrum. We investigate several techniques to minimize the effect of these uncertainties in calculation of the spectrum. These techniques are somewhat effective but to date have not been demonstrated to produce CO2 profile retrievals with sufficient precision for applications to carbon dynamics. We finish by discussing ongoing research which may allow CO2 profile retrievals with sufficient accuracy to significantly improve the scientific value of the measurements from that achieved with column retrievals.
C1 [Connor, Brian J.] BC Consulting Ltd, Martinborough, New Zealand.
[Sherlock, Vanessa] Natl Inst Water & Atmospher Res, Wellington, New Zealand.
[Toon, Geoff] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wunch, Debra; Wennberg, Paul O.] CALTECH, Pasadena, CA 91125 USA.
RP Connor, BJ (reprint author), BC Consulting Ltd, Martinborough, New Zealand.
EM bcconsulting@xtra.co.nz
FU NASA [OCO-2]; NASA's Carbon Cycle Science Investigation Program
[NNX14AI60G]
FX Part of this research was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. We thank
NASA's Carbon Cycle Science Investigation Program for supporting the
development of GFIT2 (NNX14AI60G). Operations of TCCON at Lamont,
Oklahoma, are made possible by NASA's OCO-2 project in collaboration
with the DOE ARM program. Cessna data from the SGP are available through
the ARM archive (www.archive.arm.gov). We thank Sebastien Biraud for his
assistance in interpreting the aircraft data.
NR 20
TC 0
Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 2
PY 2016
VL 9
IS 8
BP 3513
EP 3525
DI 10.5194/amt-9-3513-2016
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3MP
UT WOS:000382826900001
ER
PT J
AU Plainaki, C
Lilensten, J
Radioti, A
Andriopoulou, M
Milillo, A
Nordheim, TA
Dandouras, I
Coustenis, A
Grassi, D
Mangano, V
Massetti, S
Orsini, S
Lucchetti, A
AF Plainaki, Christina
Lilensten, Jean
Radioti, Aikaterini
Andriopoulou, Maria
Milillo, Anna
Nordheim, Tom A.
Dandouras, Iannis
Coustenis, Athena
Grassi, Davide
Mangano, Valeria
Massetti, Stefano
Orsini, Stefano
Lucchetti, Alice
TI Planetary space weather: scientific aspects and future perspectives
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Review
DE Space weather; Planetary atmospheres; Planetary magnetospheres;
Exospheres; Interactions; Comparative planetology; Future missions;
JUICE; BEPI COLOMBO
ID INTERPLANETARY MAGNETIC-FIELD; NEUTRAL MASS-SPECTROMETER; MAIN AURORAL
OVAL; SOLAR-WIND CONDITIONS; ICE GIANT PLANETS; MAGNETOSPHERE-IONOSPHERE
SYSTEM; MESSENGER ORBITAL OBSERVATIONS; MAGNETOPAUSE RECONNECTION RATE;
CARBON-DIOXIDE ATMOSPHERE; CASSINI UVIS OBSERVATIONS
AB In this paper, we review the scientific aspects of planetary space weather at different regions of our Solar System, performing a comparative planetology analysis that includes a direct reference to the circum-terrestrial case. Through an interdisciplinary analysis of existing results based both on observational data and theoretical models, we review the nature of the interactions between the environment of a Solar System body other than the Earth and the impinging plasma/radiation, and we offer some considerations related to the planning of future space observations. We highlight the importance of such comparative studies for data interpretations in the context of future space missions (e.g. ESA JUICE; ESA/JAXA BEPI COLOMBO). Moreover, we discuss how the study of planetary space weather can provide feedback for better understanding the traditional circum-terrestrial space weather. Finally, a strategy for future global investigations related to this thematic is proposed.
C1 [Plainaki, Christina; Milillo, Anna; Grassi, Davide; Mangano, Valeria; Massetti, Stefano; Orsini, Stefano] INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
[Plainaki, Christina] Univ Athens, Nucl & Particle Phys Dept, Fac Phys, Athens 15784, Greece.
[Lilensten, Jean] CNRS UGA, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France.
[Radioti, Aikaterini] Univ Liege, Inst Astrophys & Geophys, Lab Phys Atmospher & Planetaire, B-4000 Liege, Belgium.
[Andriopoulou, Maria] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Nordheim, Tom A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Dandouras, Iannis] Univ Toulouse, CNRS, IRAP, F-31028 Toulouse, France.
[Coustenis, Athena] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris Meudon, F-92195 Meudon, France.
[Lucchetti, Alice] Univ Padua, CISAS, Via Venezia 15, I-35131 Padua, Italy.
RP Plainaki, C (reprint author), INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.; Plainaki, C (reprint author), Univ Athens, Nucl & Particle Phys Dept, Fac Phys, Athens 15784, Greece.
EM christina.plainaki@iaps.inaf.it
FU Italian Space Agency (ASI) under contract "SERENA" [I/090/06/0];
European contract EUROPLANET Horizon research and innovation programme
[654208]; French Programme National de Planetologie; PRODEX Programme;
Belgian Federal Science Policy Office
FX The authors would like to thank the referee for valuable comments that
helped to improve the quality of the paper. This paper is financially
supported by the Italian Space Agency (ASI) under contract "SERENA", No.
I/090/06/0. The idea for writing this article came out after a series of
discussions in the context of the 11th European Space Weather Week
(2014). JL's contribution is under the European contract EUROPLANET
Horizon 2020 research and innovation programme under Grant Agreement No.
654208, Task 4, package 7: VA1-PSWD (Planetary Space Weather and Diary)
and under grant by the French Programme National de Planetologie. AR is
supported by the PRODEX Programme managed by the European Space Agency
in collaboration with the Belgian Federal Science Policy Office.
Discussions in this paper have been partially performed in the context
of the activities of the 2014 ISSI International Team #322, Towards a
global unified model of Europa's exosphere in view of the JUICE mission,
http://www.issibern.ch/teams/exospherejuice/. Simulation results based
on the WSA-ENLIL+Cone model have been provided by the Community
Coordinated Modeling Center at Goddard Space Flight Center through their
public Runs on Request system (http://ccmc.gsfc.nasa.gov; run number:
Alexey_-Isavnin_011316_SH_1). The WSA model was developed by N. Arge at
AFRL and the ENLIL Model was developed by D. Odstrcil at GMU. The
authors thank G. Gronoff (LARC - NASA) and David Pawlowski (East
Michigan University) for their help in getting the data for the Mars
upper atmosphere, Mathieu Barthelemy (Grenoble University Space Center,
France) for helpful discussions concerning space weather applications,
Sergio Fabiani (INFN, Italy) and Alda Rubini (INAF-IAPS, Italy) for
discussions on technological issues regarding future space missions, and
Leila Mays (NASA) for providing material based on the WSA-ENLIL+Cone
simulations. The authors also thank Chris Arridge (Lancaster University,
UK) and Fran Bagenal (University of Colorado, USA) for useful feedback
considering the magnetosphere of Uranus, Alessandro Mura (INAF-IAPS,
Italy) and Helen Mavromichalaki (National and Kapodistrian University of
Athens, Greece) for fruitful discussions on interplanetary physics and
circum-terrestrial space weather, and Panayiotis Lavvas (CNRS, France)
for providing feedback related to Titan atmospheric science. The editor
thanks an anonymous referee for the assistance in evaluating this paper.
NR 566
TC 1
Z9 1
U1 17
U2 18
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 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD AUG 2
PY 2016
VL 6
AR A31
DI 10.1051/swsc/2016024
PG 56
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DS4RT
UT WOS:000380769500001
ER
PT J
AU Battaglia, N
Leauthaud, A
Miyatake, H
Hasselfield, M
Grallad, MB
Allison, R
Bond, JR
Calabrese, E
Crichton, D
Devlin, MJ
Dunkley, J
Dunner, R
Erben, T
Ferrara, S
Halpern, M
Hilton, M
Hill, JC
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, JP
Kneib, JP
Kosowsky, A
Makler, M
Marriage, TA
Menanteaus, F
Miller, L
Moodley, K
Moraesv, B
Niemack, MD
Page, L
Shan, H
Sehgal, N
Sherwin, BD
Sievers, JL
Sifon, C
Spergel, DN
Staggs, ST
Taylor, JE
Thornton, R
van Waerbekek, L
Wollackag, EJ
AF Battaglia, N.
Leauthaud, A.
Miyatake, H.
Hasselfield, M.
Grallad, M. B.
Allison, R.
Bond, J. R.
Calabrese, E.
Crichton, D.
Devlin, M. J.
Dunkley, J.
Duenner, R.
Erben, T.
Ferrara, S.
Halpern, M.
Hilton, M.
Hill, J. C.
Hincks, A. D.
Hlozek, R.
Huffenberger, K. M.
Hughes, J. P.
Kneib, J. P.
Kosowsky, A.
Makler, M.
Marriage, T. A.
Menanteaus, F.
Miller, L.
Moodley, K.
Moraesv, B.
Niemack, M. D.
Page, L.
Shan, H.
Sehgal, N.
Sherwin, B. D.
Sievers, J. L.
Sifon, C.
Spergel, D. N.
Staggs, S. T.
Taylor, J. E.
Thornton, R.
van Waerbekek, L.
Wollackag, E. J.
TI Weak-lensing mass calibration of the Atacama Cosmology Telescope
equatorial Sunyaev-Zeldovich cluster sample with the
Canada-France-Hawaii telescope stripe 82 survey
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE galaxy clusters; gravitational lensing; Sunyaev-Zeldovich effect
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; GALAXY SHAPE MEASUREMENT; SZ
SCALING RELATIONS; DARK-MATTER HALOES; II. X-RAY; INTRINSIC ALIGNMENTS;
CROSS-CORRELATION; POWER SPECTRUM; COSMIC SHEAR
AB Mass calibration uncertainty is the largest systematic effect for using clusters of galaxies to constrain cosmological parameters. We present weak lensing mass measurements from the Canada-France-Hawaii Telescope Stripe 82 Survey for galaxy clusters selected through their high signal-to-noise thermal Sunyaev-Zeldovich (tSZ) signal measured with the Atacama Cosmology Telescope (ACT). For a sample of 9 ACT clusters with a tSZ signal-to-noise greater than five the average weak lensing mass is (4.8 +/- 0.8) x 10(14) M-circle dot, consistent with the tSZ mass estimate of (4.70 +/- 1.0) x 10(14) M-circle dot which assumes a universal pressure profile for the cluster gas. Our results are consistent with previous weak-lensing measurements of tSZ-detected clusters from the Planck satellite. When comparing our results, we estimate the Eddington bias correction for the sample intersection of Planck and weak-lensing clusters which was previously excluded.
C1 [Battaglia, N.; Miyatake, H.; Hasselfield, M.; Calabrese, E.; Ferrara, S.; Hlozek, R.; Sherwin, B. D.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Leauthaud, A.; Miyatake, H.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Miyatake, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grallad, M. B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Grallad, M. B.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Allison, R.; Calabrese, E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Bond, J. R.] Canadian Inst Theoret Astrophys, Toronto, ON M55 3H8, Canada.
[Devlin, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Duenner, R.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago, Chile.
[Erben, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Halpern, M.; Hincks, A. D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Hilton, M.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hill, J. C.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kneib, J. P.] EPFL, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, France.
[Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Makler, M.] Ctr Brasileiro Pesquisas Fsicas, Rio De Janeiro, RJ, Brazil.
[Menanteaus, F.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Menanteaus, F.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Moraesv, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Moraesv, B.] Minist Educ Brazil, CAPES Fdn, BR-70040020 Brasilia, DF, Brazil.
[Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Shan, H.] Ecole Polytech Fed Lausanne, Observ Sauverny, Lab Astrophys LASTRO, CH-1290 Versoix, Switzerland.
[Sehgal, N.] Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Sherwin, B. D.] Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Sherwin, B. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Sievers, J. L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Staggs, S. T.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Taylor, J. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[van Waerbekek, L.] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Wollackag, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Battaglia, N (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM nbatta@astro.princeton.edu
OI Huffenberger, Kevin/0000-0001-7109-0099; Sifon,
Cristobal/0000-0002-8149-1352
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; U.S. National Science Foundation [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI); Comision Nacional
de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI;
NSERC, Ontario; ORF-RE; U of T deans; Laboratorio Interinstitucional de
e-Astronomia (LIneA); Lyman Spitzer Fellowship; Japan Society for the
Promotion of Science (JSPS); Jet Propulsion Laboratory, California
Institute of Technology; Simons Foundation; NSF [AST-1311756,
AST-1312380]; NASA [NNX12AG72G]; Deutsche Forschungsgemeinschaft
[Transregional Collaborative Research Centre TR33]; Marie-Curie
International Incoming Fellowship [FP7-PEOPLE-2012-IIF/327561]; NSFC of
China [11103011]; CAPES Foundation [12174-13-0]
FX This work is supported by World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan. The ACT project is supported
by the U.S. National Science Foundation through awards AST-0408698 and
AST-0965625, as well as awards PHY-0855887 and PHY-1214379. ACT funding
was also provided by Princeton University, the University of
Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC.
ACT operates in the Parque Astronomico Atacama in northern Chile under
the auspices of the Comision Nacional de Investigacion Cientifica y
Tecnologica de Chile (CONICYT). Simulations were performed on the GPC
supercomputer at the SciNet HPC Consortium and CITA's Sunnyvale
high-performance computing clusters. SCINET is funded and supported by
CFI, NSERC, Ontario, ORF-RE and U of T deans. We thank the CFHTLenS team
for their pipeline development and verification upon which much of the
CS82 survey pipeline was built. This work was based on observations
obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,
at the Canada-France-Hawaii Telescope (CFHT), which is operated by the
National Research Council (NRC) of Canada, the Institut National des
Science de l'Univers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. The Brazilian
partnership on CFHT is managed by the Laboratorio Nacional de
Astrofisica (LNA). We thank the support of the Laboratorio
Interinstitucional de e-Astronomia (LIneA). NB and RH acknowledge
support from the Lyman Spitzer Fellowship. HM is supported in part by
Japan Society for the Promotion of Science (JSPS) Research Fellowships
for Young Scientists and by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. JCH is partially supported by a Junior Fellow
award from the Simons Foundation. JCH and DNS acknowledge support from
NSF AST-1311756. DNS acknowledges the support of NASA grant NNX12AG72G.
AK acknowledges the support of NSF AST-1312380. TE is supported by the
Deutsche Forschungsgemeinschaft through the Transregional Collaborative
Research Centre TR33 - The Dark Universe. HS acknowledges the support
from Marie-Curie International Incoming Fellowship
(FP7-PEOPLE-2012-IIF/327561) and NSFC of China under grants 11103011. BM
acknowledges financial support from the CAPES Foundation grant
12174-13-0. We thank J. G. Bartlett and G. Rocha for their helpful
discussions on the Planck SZ source catalog and B. Partridge for helpful
comments on the paper. We thank M. Simet, E. Rozo, and R. Mandelbaum for
access to their data that assisted us in responding to the referee
report and our anonymous referee for their insightful comments.
NR 105
TC 0
Z9 0
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD AUG
PY 2016
IS 8
AR 013
DI 10.1088/1475-7516/2016/08/013
PG 24
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EE8EW
UT WOS:000389859100005
ER
PT J
AU Dev, PSB
Kazanas, D
Mohapatra, RN
Teplitz, VL
Zhang, YC
AF Dev, P. S. Bhupal
Kazanas, D.
Mohapatra, R. N.
Teplitz, V. L.
Zhang, Yongchao
TI Heavy right-handed neutrino dark matter and PeV neutrinos at IceCube
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter theory; gamma ray theory; neutrino theory; ultra high energy
photons and neutrinos
ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; STRONG CP PROBLEM;
GAUGE-MODELS; B-L; MASSES; PARITY; QUARK; PHENOMENOLOGY; OSCILLATIONS
AB We discuss a simple non-supersymmetric model based on the electroweak gauge group SU(2)(L) x SU(2)' x U(1)(B-L) where the lightest of the right-handed neutrinos, which are part of the leptonic doublet of SU(2)', play the role of a long-lived unstable dark matter with mass in the multi-PeV range. We use a resonant s-channel annihilation to obtain the correct thermal relic density and relax the unitarity bound on dark matter mass. In this model, there exists a 3-body dark matter decay mode producing tau leptons and neutrinos, which could be the source for the PeV cascade events observed in the IceCube experiment. The model can be tested with more precise flavor information of the highest-energy neutrino events in future data.
C1 [Dev, P. S. Bhupal] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
[Kazanas, D.; Teplitz, V. L.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mohapatra, R. N.] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Teplitz, V. L.] Southern Methodist Univ, Dept Phys, Dallas, TX 75205 USA.
[Zhang, Yongchao] Univ Libre Bruxelles, Serv Phys Theor, Blvd Triomphe,CP225, B-1050 Brussels, Belgium.
[Zhang, Yongchao] Sun Yat Sen Univ, Sch Phys, Guangzhou 510275, Guangdong, Peoples R China.
RP Dev, PSB (reprint author), Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
EM bhupal.dev@mpi-hd.mpg.de; demos.kazanas-1@nasa.gov; rmohapat@umd.edu;
vigdor.l.teplitz@nasa.gov; yongchao.zhang@ulb.ac.be
OI Dev, Bhupal/0000-0003-4655-2866
FU DFG [RO 2516/5-1]; US National Science Foundation [PHY-1315155]; HSN;
Belgian Science Policy [IAP VII/37]; National Natural Science Foundation
of China (NSFC) [11375277]; Mainz Institute for Theoretical Physics
(MITP); Munich Institute for Astro- and Particle Physics (MIAPP)
FX B.D. is grateful to Pasquale Di Bari and Stefano Morisi for useful
discussions on PeV DM at IceCube, and to the Mainz Institute for
Theoretical Physics (MITP) and Munich Institute for Astro- and Particle
Physics (MIAPP) for their hospitality and partial support during the
completion of this work. Y.Z. would like to thank Julian Heeck for the
enlightening discussions, and also Hong-Hao Zhang for his gracious
hospitality during the visit at Sun Yat-Sen University where part of the
work was done. The work of B.D. is supported by the DFG grant RO
2516/5-1. The work of R.N.M. is supported by the US National Science
Foundation Grant No. PHY-1315155. Y.Z. would like to thank the HSN and
Belgian Science Policy (IAP VII/37) for support. Y.Z. is also grateful
to the National Natural Science Foundation of China (NSFC) under Grant
No. 11375277 for financial support.
NR 104
TC 3
Z9 3
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD AUG
PY 2016
IS 8
AR 034
DI 10.1088/1475-7516/2016/08/034
PG 22
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EE8EW
UT WOS:000389859100021
ER
PT J
AU Macdonald, RL
Munafo, A
Johnston, CO
Panesi, M
AF Macdonald, R. L.
Munafo, A.
Johnston, C. O.
Panesi, M.
TI Nonequilibrium radiation and dissociation of CO molecules in
shock-heated flows
SO PHYSICAL REVIEW FLUIDS
LA English
DT Article
ID CHEMICAL-KINETIC PROBLEMS; FUTURE NASA MISSIONS; II FLIGHT EXPERIMENT;
RATE CONSTANTS; GAS-DYNAMICS; MARS ENTRY; MODEL; MIXTURE; WAVE; AIR
AB This work addresses the study of the behavior of the excited electronic states of CO molecules in the nonequilibrium relaxation zone behind a normal shock for a CO2-N-2 mixture representative of the Mars atmosphere. The hybrid state-to-state (StS) model developed accounts for thermal nonequilibrium between the translational energy mode of the gas and the vibrational energy mode of individual molecules. The electronic states of CO molecules are treated as separate species, allowing for non-Boltzmann distributions of their populations. The StS model is coupled with a nonequilibrium radiation solver, HPC-RAD, allowing for the calculation of the radiation signature from the molecular and atomic species in the gas. This study focuses on the radiation from the fourth positive system of CO, which dominates the radiation heating on the forebody for higher speed Mars entry applications. In the rapidly dissociating regime behind strong shock waves, the population of the ground electronic state of CO [CO(X-1 Sigma)], departs from Maxwell-Boltzmann distributions, owing to the efficient collisional excitation to the electronically excited CO(A(1) Pi) state. In general the assumption of the equilibrium between electronic and vibration fails when the excitation of electronic states is driven by heavy particles. The comparison of the radiation heating predictions obtained using the conventional quasi-steady-state (QSS) approach and the physics-based StS approach revealed differences in radiative heating predictions of up to 50%. These results demonstrate that the choice of nonequilibrium model can have a significant impact on radiative heating simulations, and more importantly, they cast serious doubts on the validity of the QSS assumption for the condition of interest to this work.
C1 [Macdonald, R. L.; Munafo, A.; Panesi, M.] Univ Illinois, Urbana, IL 61801 USA.
[Johnston, C. O.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Panesi, M (reprint author), Univ Illinois, Urbana, IL 61801 USA.
EM mpanesi@illinois.edu
FU NASA Entry System Modeling Project in the Space Technology Mission
Directory; NASA Ames Research Center [NNX14AB67A]
FX Support from the NASA Entry System Modeling Project in the Space
Technology Mission Directory is gratefully acknowledged. Program
Managers are Dr. M. Wright and Dr. M. Barnhardt at NASA Ames Research
Center, under Grant No. NNX14AB67A. The authors would like to thank the
NASA Ames quantum computational chemistry group (in particular Dr. D. W.
Schwenke and Dr. R. L. Jaffe) for sharing the Hyper-rad database.
NR 68
TC 0
Z9 0
U1 2
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-990X
J9 PHYS REV FLUIDS
JI Phys. Rev. Fluids
PD AUG 1
PY 2016
VL 1
IS 4
AR 043401
DI 10.1103/PhysRevFluids.1.043401
PG 20
WC Physics, Fluids & Plasmas
SC Physics
GA EF3FB
UT WOS:000390209000001
ER
PT J
AU Bryson, KL
Ostrowski, DR
AF Bryson, K. L.
Ostrowski, D. R.
TI METEORITE FRACTURES AND SCALING FOR ASTEROID ATMOSPHERIC ENTRY.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Bryson, K. L.; Ostrowski, D. R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bryson, K. L.; Ostrowski, D. R.] Ames Res Ctr, BAER Inst, Moffett Field, CA USA.
EM kathryn.bryson@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A185
EP A185
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400043
ER
PT J
AU Buchner, E
Schmieder, M
AF Buchner, E.
Schmieder, M.
TI DISCOVERY OF POSSIBLE METEORITIC MATTER ON SHATTER CONES AND
SLICKENSIDES-1. RIES CRATER, SOUTHERN GERMANY.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Buchner, E.] Neu Ulm Univ Appl Sci, HNU, Wileystr 1, D-89231 Neu Ulm, Germany.
[Buchner, E.] Univ Stuttgart, Inst Mineral & Kristallchem, Azenberstr 18, D-70174 Stuttgart, Germany.
[Schmieder, M.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Schmieder, M.] NASA, SSERVI, Washington, DC 20546 USA.
EM elmar.buchner@hs-neu-ulm.de
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A187
EP A187
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400045
ER
PT J
AU Buchner, E
Schmieder, M
AF Buchner, E.
Schmieder, M.
TI DISCOVERY OF POSSIBLE METEORITIC MATTER ON SHATTER CONES-2. CLEARWATER
EAST IMPACT STRUCTURE, QUEBEC, CANADA.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID MELT
C1 [Buchner, E.] Neu Ulm Univ Appl Sci, HNU, Wileystr 1, D-89231 Neu Ulm, Germany.
[Buchner, E.] Univ Stuttgart, Inst Mineral & Kristallchem, Azenberstr 18, D-70174 Stuttgart, Germany.
[Schmieder, M.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Schmieder, M.] NASA, SSERVI, Washington, DC 20546 USA.
EM elmar.buchner@hs-neu-ulm.de
NR 11
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A186
EP A186
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400044
ER
PT J
AU Bussey, DBJ
Worms, JC
Schlutz, J
Spiero, F
AF Bussey, D. B. J.
Worms, J. C.
Schlutz, J.
Spiero, F.
TI THE ISECG SCIENCE WHITE PAPER: SCIENCE ENABLED BY HUMAN EXPLORATION
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Bussey, D. B. J.] NASA, Washington, DC 20546 USA.
[Worms, J. C.] European Sci Fdn, Strasbourg, France.
[Schlutz, J.] DLR, Cologne, Germany.
[Spiero, F.] CNES, Paris, France.
EM ben.bussey@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A191
EP A191
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400049
ER
PT J
AU Chan, QHS
Nakato, A
Zolensky, ME
Nakamura, T
Kebukawa, Y
AF Chan, Q. H. S.
Nakato, A.
Zolensky, M. E.
Nakamura, T.
Kebukawa, Y.
TI EFFECTS OF SHORT-TERM THERMAL ALTERATION ON ORGANIC MATTER IN
EXPERIMENTALLY-HEATED TAGISH LAKE OBSERVED BY RAMAN SPECTROSCOPY
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID CARBONACEOUS CHONDRITES; CM-CHONDRITES; METAMORPHISM
C1 [Chan, Q. H. S.; Zolensky, M. E.] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Nakato, A.] JAXA, Sagamihara, Kanagawa 2525210, Japan.
[Nakamura, T.] Tohoku Univ, Sendai, Miyagi 9808578, Japan.
[Kebukawa, Y.] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa, Japan.
EM hschan@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A200
EP A200
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400058
ER
PT J
AU Demasi, M
Britt, DT
Kring, DA
AF Demasi, M.
Britt, D. T.
Kring, D. A.
TI WHAT DO METEORITE FALLS TELL US ABOUT THE STRENGTH OF ASTEROID BOULDERS?
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Demasi, M.; Britt, D. T.] Univ Cent Florida, Dept Phys, 4111 Libra Dr, Orlando, FL 32816 USA.
[Demasi, M.; Britt, D. T.] Ctr Lunar & Asteroid Surface Sci, 12354 Res Pkwy Suite 214, Orlando, FL 32826 USA.
[Demasi, M.; Britt, D. T.; Kring, D. A.] NASA, SSERVI, Orlando, FL USA.
[Kring, D. A.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM hovtej@knights.ucf.edu
NR 5
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A225
EP A225
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400083
ER
PT J
AU Flynn, GJ
Keller, LP
Wirick, S
Hu, W
Li, L
Yan, H
Huang, X
Nazaretski, E
Lauer, K
Chu, YS
AF Flynn, G. J.
Keller, L. P.
Wirick, S.
Hu, W.
Li, L.
Yan, H.
Huang, X.
Nazaretski, E.
Lauer, K.
Chu, Y. S.
TI HIGH-NICKEL IRON-SULFIDES IN ANHYDROUS, GEMS-RICH CP IDPs.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, 101 Broad St, Plattsburgh, NY 12901 USA.
[Keller, L. P.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Wirick, S.] Focused Beam Enterprises, Westhampton, NY 11977 USA.
[Hu, W.; Li, L.; Yan, H.; Huang, X.; Nazaretski, E.; Lauer, K.; Chu, Y. S.] Brookhaven Natl Lab, NSLS 2, Upton, NY 11973 USA.
EM george.flynn@plattsburgh.edu
NR 7
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A258
EP A258
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400116
ER
PT J
AU Fries, M
Abell, P
Brisset, J
Britt, D
Colwell, J
Durda, D
Dove, A
Graham, L
Hartzell, C
John, K
Leonard, M
Love, S
Sdfnchez, DP
Scheeres, DJ
AF Fries, M.
Abell, P.
Brisset, J.
Britt, D.
Colwell, J.
Durda, D.
Dove, A.
Graham, L.
Hartzell, C.
John, K.
Leonard, M.
Love, S.
Sdfnchez, D. P.
Scheeres, D. J.
TI THE STRATA-1 EXPERIMENT ON MICROGRAVITY REGOLITH SEGREGATION.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Fries, M.; Abell, P.; Graham, L.; John, K.] NASA, ARES, Johnson Space Ctr, Houston, TX USA.
[Brisset, J.; Britt, D.; Colwell, J.; Dove, A.] Univ Cent Florida, Orlando, FL 32816 USA.
[Brisset, J.; Britt, D.; Colwell, J.; Dove, A.] NASA, SSERVI, Orlando, FL USA.
[Durda, D.] Southwest Res Inst, Boulder, CO USA.
[Hartzell, C.] Univ Maryland, College Pk, MD 20742 USA.
[Leonard, M.] T STAR, Bryan, TX USA.
[Love, S.] NASA, Johnson Space Ctr, Houston, TX USA.
[Sdfnchez, D. P.; Scheeres, D. J.] Univ Colorado Boulder, Boulder, CO USA.
EM marc.d.fries@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A265
EP A265
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400123
ER
PT J
AU Fries, M
Fries, J
Hankey, M
Matson, R
AF Fries, Marc
Fries, Jeffrey
Hankey, Mike
Matson, Robert
TI METEORITE FALLS OBSERVED IN US WEATHER RADAR DATA IN 2015 AND 2016 (TO
DATE)
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Fries, Marc] NASA, ARES, Johnson Space Ctr, Houston, TX USA.
[Fries, Jeffrey] USAF Weather Agcy, Weather Grp 1, Offutt AFB, NE 68113 USA.
[Hankey, Mike] Amer Meteor Soc, Geneseo, NY 14454 USA.
[Matson, Robert] Leidos Inc, 3030 Old Ranch Pkwy,Ste 200, Seal Beach, CA 90740 USA.
EM marc.d.fries@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A266
EP A266
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400124
ER
PT J
AU Fu, RR
Ermakov, AI
Marchi, S
Castillo-Rogez, JC
Raymond, CA
King, SD
Bland, MT
Russell, CT
AF Fu, R. R.
Ermakov, A. I.
Marchi, S.
Castillo-Rogez, J. C.
Raymond, Carol A.
King, Scott D.
Bland, Michael T.
Russell, Christopher T.
TI THERMAL EVOLUTION AND FLUID FLOW IN PLANETESIMALS INFERRED FROM DAWN
MISSION OBSERVATIONS OF CERES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID CHONDRITE PARENT BODIES; WATER
C1 [Fu, R. R.] Columbia Univ, 61 Route 9W, Palisades, NY 10964 USA.
[Fu, R. R.; Ermakov, A. I.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Marchi, S.] Southwest Res Ins, 1050 Walnut St, Boulder, CO 80302 USA.
[Castillo-Rogez, J. C.; Raymond, Carol A.; Russell, Christopher T.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[King, Scott D.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24060 USA.
[Bland, Michael T.] USGS Astrogeol Sci Ctr, 2255 N Gemini Rd, Flagstaff, AZ 86001 USA.
EM rf2006@ldeo.columbia.edu
NR 9
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A268
EP A268
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400126
ER
PT J
AU Funk, RC
Peslier, AH
Brandon, AD
Humayun, M
AF Funk, R. C.
Peslier, A. H.
Brandon, A. D.
Humayun, M.
TI PETROLOGY AND GEOCHEMISTRY OF NEW PAIRED MARTIAN METEORITES LARKMAN
NUNATAK 12240 AND LARKMAN NUNATAK 12095.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID OXYGEN FUGACITY; UPPER-MANTLE; SHERGOTTITES; BASALTS; MARS;
PETROGENESIS; ELEMENT; STATE; CRUST
C1 [Funk, R. C.] NASA, GeoControl JETS, Johnson Space Ctr, Mail Code X12, Houston, TX 77058 USA.
[Peslier, A. H.] NASA, Jacobs, JSC, Mail Code X13, Houston, TX 77058 USA.
[Brandon, A. D.] Univ Houston, 4800 Calhoun Rd, Houston, TX 77004 USA.
[Humayun, M.] Florida State Univ, 1800 E Paul Dirac Dr, Tallahassee, FL 32310 USA.
EM rachel.c.funk@nasa.gov; anne.h.peslier@nasa.gov; abrandon@uh.edu;
humavun@magnet.fsu.edu
NR 10
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A274
EP A274
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400132
ER
PT J
AU Gellert, R
Arvidson, RE
Clark, BC
Ming, DW
Mittlefehldt, DW
Morris, RW
Squyres, SW
VanBommel, S
Yen, AS
AF Gellert, R.
Arvidson, R. E.
Clark, B. C.
Ming, D. W.
Mittlefehldt, D. W.
Morris, R. W.
Squyres, S. W.
VanBommel, S.
Yen, A. S.
TI Igneous and sedimentary compositions from four landing sites on Mars
from the Alpha Particle X-ray Spectrometer (APXS)
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Gellert, R.; VanBommel, S.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Arvidson, R. E.] Washington Univ, St Louis, MO USA.
[Clark, B. C.] Space Sci Inst, Bolder, CA USA.
[Ming, D. W.; Mittlefehldt, D. W.; Morris, R. W.] JSC, ARES, Houston, TX USA.
[Squyres, S. W.] Cornell, Ithaca, NY USA.
[Yen, A. S.] JPL, Pasadena, CA USA.
EM rgellert@uoguelph.ca
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A280
EP A280
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400138
ER
PT J
AU Hagiya, K
Ohsumi, K
Komatsu, M
Mikouchi, T
Zolensky, ME
Hirata, A
Yamaguchi, S
Kurokawa, A
AF Hagiya, K.
Ohsumi, K.
Komatsu, M.
Mikouchi, T.
Zolensky, M. E.
Hirata, A.
Yamaguchi, S.
Kurokawa, A.
TI CRYSTALLOGRAPHIC STUDY OF ITOKAWA PARTICLE, RA-QD02-0127 BY USING
ENERGY-SCANNING X-RAY DIFFRACTION METHOD WITH SYNCHROTRON RADIATION.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Hagiya, K.; Hirata, A.; Yamaguchi, S.; Kurokawa, A.] Univ Hyogo, Sch Sci, Kamigori, Hyogo 6781297, Japan.
[Ohsumi, K.] JASRI, Japan Synchrotron Radiat Res Inst, Sayo, Hyogo 6795198, Japan.
[Komatsu, M.] Graduate Univ Adv Studies, SOKENDAI, Hayama, Kanagawa 2400193, Japan.
[Komatsu, M.] Waseda Univ, Dept Earth Sci, Shinjuku Ku, Tokyo 1698050, Japan.
[Mikouchi, T.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Zolensky, M. E.] NASA, XI2, Johnson Space Ctr, Houston, TX 77058 USA.
EM hagiya@sci.u-hyogo.ac.jp
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A307
EP A307
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400165
ER
PT J
AU Han, J
Keller, LP
Danielson, LR
AF Han, J.
Keller, L. P.
Danielson, L. R.
TI EXPERIMENTAL INSIGHTS INTO THE ORIGIN OF DEFECT-STRUCTURED HIBONITES
FOUND IN METEORITES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Han, J.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Han, J.; Keller, L. P.] NASA JSC, ARES, Code X13, Houston, TX 77058 USA.
[Danielson, L. R.] NASA JSC, Jacobs JETS, Houston, TX 77058 USA.
EM jangmi.han@nasa.gov
NR 11
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A311
EP A311
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400169
ER
PT J
AU Hartmann, WK
Daubar, I
AF Hartmann, W. K.
Daubar, I.
TI UTILIZING SMALL IMPACT CRATERS TO CLARIFY THE HISTORY OF MARTIAN
SURFACES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Hartmann, W. K.] Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
[Daubar, I.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hartmann@psi.edu; Ingrid.Daubar@jpl.nasa.gov
NR 4
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A315
EP A315
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400173
ER
PT J
AU Kebukawa, Y
Ito, M
Zolensky, ME
Rahman, Z
Kilcoyne, ALD
Nakato, A
Takeichi, Y
Suga, H
Miyamoto, C
Mase, K
Takahashi, Y
Chan, Q
Fries, M
AF Kebukawa, Y.
Ito, M.
Zolensky, M. E.
Rahman, Z.
Kilcoyne, A. L. D.
Nakato, A.
Takeichi, Y.
Suga, H.
Miyamoto, C.
Mase, K.
Takahashi, Y.
Chan, Q.
Fries, M.
TI ORGANIC AGGREGATES WITH delta D AND delta N-15 ANOMALIES IN THE ZAG
CLAST REVEALED BY STXM AND NANOSIMS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Kebukawa, Y.] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa, Japan.
[Ito, M.] JAMSTEC, Kochi Inst Core Sample Res, Yokosuka, Kanagawa, Japan.
[Rahman, Z.] NASA Johnson Space Ctr, Jacobs, Houston, TX USA.
[Kilcoyne, A. L. D.] Lawrence Berkeley Natl Lab, Adv Light Source, Lawrence, KS USA.
[Nakato, A.] Kyoto Univ, Grad Sch Sci, Kyoto 6068501, Japan.
[Takeichi, Y.; Mase, K.] High Energy Accelerator Res Org KEK, Inst Mat Struct Sci, Tsukuba, Ibaraki, Japan.
[Suga, H.] Hiroshima Univ, Dept Earth & Planetary Syst Sci, Hiroshima 730, Japan.
[Miyamoto, C.; Takahashi, Y.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1138654, Japan.
EM kebukawa@ynu.ac.jp
RI Kilcoyne, David/I-1465-2013
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A366
EP A366
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400224
ER
PT J
AU Keller, LP
Snead, C
McKeegan, KD
AF Keller, L. P.
Snead, C.
McKeegan, K. D.
TI COORDINATED ANALYSES OF HYDRATED INTERPLANETARY DUST PARTICLES: SAMPLES
OF PRIMITIVE SOLAR SYSTEM BODIES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID CHONDRITES; SILICATE
C1 [Keller, L. P.] NASA JSC, ARES, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA.
[Snead, C.; McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
EM Lindsay.P.Keller@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A367
EP A367
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400225
ER
PT J
AU Kohnert, F
Otto, KA
Jaumann, R
Krohn, K
Kersten, E
Preusker, F
Roatsch, T
Raymond, CA
Russell, CT
AF Kohnert, Frauke
Otto, Katharina A.
Jaumann, Ralf
Krohn, Katrin
Kersten, E.
Preusker, F.
Roatsch, T.
Raymond, C. A.
Russell, C. T.
TI Mobility of Landslides on Asteroid Vesta
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Kohnert, Frauke; Otto, Katharina A.; Jaumann, Ralf; Krohn, Katrin; Kersten, E.; Preusker, F.; Roatsch, T.] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany.
[Kohnert, Frauke] Martin Luther Univ Halle Wittenberg, Halle, Germany.
[Jaumann, Ralf] Free Univ Berlin, Planetary Sci & Remote Sensing, Berlin, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys, Los Angeles, CA USA.
EM frauke.kohnert@dlr.de
NR 9
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A379
EP A379
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400237
ER
PT J
AU Krohn, K
Jaumann, R
Otto, KA
von der Gathen, I
Matz, KD
Buczkowski, DL
Williams, DA
Pieters, CM
Preusker, F
Roatsch, T
Stephan, K
Wagner, RJ
Russell, CT
Raymond, CA
AF Krohn, K.
Jaumann, R.
Otto, K. A.
von der Gathen, I.
Matz, K. -D.
Buczkowski, D. L.
Williams, D. A.
Pieters, C. M.
Preusker, F.
Roatsch, T.
Stephan, K.
Wagner, R. J.
Russell, C. T.
Raymond, C. A.
TI Cryogenic Flows on Ceres
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Krohn, K.; Jaumann, R.; Otto, K. A.; von der Gathen, I.; Matz, K. -D.; Preusker, F.; Roatsch, T.; Stephan, K.; Wagner, R. J.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[Buczkowski, D. L.] JHU APL, Laurel, MD USA.
[Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Raymond, C. A.] CALTECH, NASA JPL, Pasadena, CA 91125 USA.
EM Katrin.Krohn@dlr.de
NR 4
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A391
EP A391
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400249
ER
PT J
AU Liu, MC
Keller, LP
McKeegan, KD
AF Liu, M. -C.
Keller, L. P.
McKeegan, K. D.
TI MAGNESIUM AND TITANIUM ISOTOPIC COMPOSITIONS OF AN UNUSUAL
HIBONITE-PEROVSKITE REFRACTORY INCLUSION FROM ALLENDE: IT IS FUN.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Liu, M. -C.; McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA.
[Keller, L. P.] NASA, JSC, ARES, Robert M Walker Lab Space Sci, Washington, DC 20546 USA.
EM mcliu@ucla.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A417
EP A417
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400275
ER
PT J
AU Marhas, KK
Messenger, S
Amari, S
AF Marhas, K. K.
Messenger, S.
Amari, S.
TI Cr ISOTOPIC COMPOSITION FROM MAINSTREAM AND X TYPE PRESOLAR SiC GRAINS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID SOLAR-SYSTEM; CHROMIUM; ORGUEIL
C1 [Marhas, K. K.] Phys Res Lab, Planetary Sci Div, Ahmadabad 380009, Gujarat, India.
[Messenger, S.] NASA, Johnson Space Ctr, ARES Div, Ctr Isotope Cosmochem & Geochronol, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Amari, S.] Washington Univ, Lab Space Sci, St Louis, MO 63130 USA.
[Amari, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
EM kkmarhas@prl.res.in
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A445
EP A445
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400303
ER
PT J
AU McCubbin, FM
Mccoy, TJ
AF McCubbin, F. M.
Mccoy, T. J.
TI EXPECTED GEOCHEMICAL AND MINERALOGICAL PROPERTIES OF METEORITES FROM
MERCURY: INFERENCES FROM MESSENGER DATA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID RAY SPECTROMETER; SURFACE
C1 [McCubbin, F. M.] NASA, Johnson Space Ctr, Mail Code X12,2101 NASA Pkwy, Houston, TX 77058 USA.
[Mccoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
NR 15
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A451
EP A451
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400309
ER
PT J
AU Miller, KE
Lauretta, DS
Berger, EL
Thompson, MS
Zega, TJ
AF Miller, K. E.
Lauretta, D. S.
Berger, E. L.
Thompson, M. S.
Zega, T. J.
TI COPPER SULFIDES IN THE R CHONDRITES: EVIDENCE OF HYDROTHERMAL ALTERATION
IN LOW PETROLOGIC TYPES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID TEMPERATURES; CUBANITE
C1 [Miller, K. E.; Lauretta, D. S.; Thompson, M. S.; Zega, T. J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Berger, E. L.] NASA, GeoControl Syst Inc, Jacobs JETS, Johnson Space Ctr, Houston, TX 77058 USA.
EM kemiller@lpl.arizona.edu
NR 17
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A463
EP A463
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400321
ER
PT J
AU Mittlefehldt, DW
Peng, ZX
Mertzman, SA
AF Mittlefehldt, D. W.
Peng, Z. X.
Mertzman, S. A.
TI COMPOSITIONS OF NORMAL AND ANOMALOUS EUCRITE-TYPE MAFIC ACHONDRITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX USA.
[Peng, Z. X.] NASA, Jacobs Technol, Johnson Space Ctr, Houston, TX USA.
[Mertzman, S. A.] Franklin & Marshall Coll, Earth & Environm Dept, Lancaster, PA 17604 USA.
EM david.w.mittlefehldt@nasa.gov
NR 7
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A465
EP A465
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400323
ER
PT J
AU Nuth, JA
Johnson, NM
Ferguson, FT
AF Nuth, Joseph A., III
Johnson, Natasha M.
Ferguson, Frank T.
TI CAN SURFACE MEDIATED REACTIONS OF CO AND HYDROGEN ENHANCE COAGULATION IN
THE INNERMOST REGIONS OF THE SOLAR NEBULA?
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID SPHERES
C1 [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 690, Greenbelt, MD 20771 USA.
[Johnson, Natasha M.; Ferguson, Frank T.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
[Ferguson, Frank T.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA.
EM joseph.a.nuth@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A490
EP A490
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400348
ER
PT J
AU Ostrowski, DR
Bryson, KL
AF Ostrowski, D. R.
Bryson, K. L.
TI PHYSICAL PROPERTY COMPARISON OF ORDINARY CHONDRITE CLASSES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Ostrowski, D. R.; Bryson, K. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ostrowski, D. R.; Bryson, K. L.] BAER Inst, Ames Res Ctr, Moffett Field, CA USA.
EM daniel.r.ostrowski@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A499
EP A499
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400357
ER
PT J
AU Ott, U
Baecker, B
Trieloff, M
Cordier, C
Folco, L
AF Ott, U.
Baecker, B.
Trieloff, M.
Cordier, C.
Folco, L.
TI NOBLE GAS INVENTORY OF TRANSANTARCTIC MOUNTAIN MICROMETEORITES: INSIGHTS
INTO THEIR PROVENANCE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID INTERPLANETARY DUST PARTICLES; NITROGEN; EARTH; WATER
C1 [Ott, U.] Univ West Hungary, Szombathely, Hungary.
[Ott, U.; Baecker, B.] Max Planck Inst Chem, Mainz, Germany.
[Ott, U.; Baecker, B.; Trieloff, M.] Heidelberg Univ, Heidelberg, Germany.
[Baecker, B.] NASA, Marshall SFC, Huntsville, AL USA.
[Cordier, C.; Folco, L.] Univ Pisa, Pisa, Italy.
[Cordier, C.] Univ Grenoble Alpes, Grenoble, France.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A500
EP A500
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400358
ER
PT J
AU Otto, KA
Jaumann, R
Krohn, K
Buczkowski, DL
von der Gathen, I
Kersten, E
Mest, SC
Nass, A
Neesemann, A
Preusker, F
Roatsch, T
Schroder, SE
Schulzeck, F
Scully, JEC
Stephan, K
Wagner, R
Williams, DA
Raymond, CA
Russell, CT
AF Otto, K. A.
Jaumann, R.
Krohn, K.
Buczkowski, D. L.
von der Gathen, I.
Kersten, E.
Mest, S. C.
Nass, A.
Neesemann, A.
Preusker, F.
Roatsch, T.
Schroder, S. E.
Schulzeck, F.
Scully, J. E. C.
Stephan, K.
Wagner, R.
Williams, D. A.
Raymond, C. A.
Russell, C. T.
TI Polygonal Impact Craters on Ceres: Morphology and Distribution.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Otto, K. A.; Jaumann, R.; Krohn, K.; von der Gathen, I.; Kersten, E.; Nass, A.; Preusker, F.; Roatsch, T.; Schroder, S. E.; Schulzeck, F.; Stephan, K.; Wagner, R.] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany.
[Jaumann, R.; Neesemann, A.] Free Univ Berlin, Planetary Sci & Remote Sensing, Berlin, Germany.
[Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Mest, S. C.] Planetary Sci Inst, Tucson, AZ USA.
[Scully, J. E. C.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Williams, D. A.] Arizona State Univ, Tempe, AZ USA.
[Russell, C. T.] Univ Calif LA, Inst Geophys, Los Angeles, CA USA.
EM katharina.otto@dlr.de
NR 8
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A501
EP A501
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400359
ER
PT J
AU Pantazidis, A
Baziotis, I
Manoutsoglou, E
Solomonidou, A
Schwandner, F
Economou, G
Palles, D
Kamitsos, E
Koukouzas, N
Keklikoglou, N
Arvanitidis, C
Martinez-Frias, J
Asimow, PD
AF Pantazidis, A.
Baziotis, I.
Manoutsoglou, E.
Solomonidou, A.
Schwandner, F.
Economou, G.
Palles, D.
Kamitsos, E.
Koukouzas, N.
Keklikoglou, N.
Arvanitidis, C.
Martinez-Frias, J.
Asimow, P. D.
TI BASALTS FROM SANTORINI VOLCANO: A NEW CANDIDATE MARTIAN ANALOGUE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Pantazidis, A.; Baziotis, I.] Agr Univ Athens, GR-11855 Athens, Greece.
[Pantazidis, A.; Manoutsoglou, E.] Tech Univ Crete, Khania, Greece.
[Solomonidou, A.; Schwandner, F.] Jet Prop Lab, La Canada Flintridge, CA USA.
[Economou, G.] Inst Geol & Mineral Explorat, Athens, Greece.
[Palles, D.; Kamitsos, E.] Natl Hellen Res Fdn, Athens, Greece.
[Koukouzas, N.] Natl Ctr Res & Technol, Athens, Greece.
[Keklikoglou, N.; Arvanitidis, C.] Hellen Ctr Marine Res, Iraklion, NE, Greece.
[Martinez-Frias, J.] Inst Geociencias CSIC UCM, Madrid, Spain.
[Asimow, P. D.] Calif Intitute Technol, Pasadena, CA USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A506
EP A506
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400364
ER
PT J
AU Rao, MN
Sutton, SR
Hoppe, P
Nyquist, LE
Ross, DK
Shih, C
AF Rao, M. N.
Sutton, S. R.
Hoppe, P.
Nyquist, L. E.
Ross, D. K.
Shih, C.
TI EVIDENCE FOR PRECURSOR SULFATES, CHROMATES AND VANADATES OF MARTIAN
REGOLITH LINEAGE IN IMPACT GLASSES IN SHERGOTTITES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID OXYGEN FUGACITY
C1 [Rao, M. N.] Johnson Space Ctr, SCI, Houston, TX 77058 USA.
[Sutton, S. R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60439 USA.
[Hoppe, P.] Max Planck Inst Chem, Mainz, Germany.
[Nyquist, L. E.] XI NASA Johnson Space Ctr, Houston, TX USA.
[Ross, D. K.; Shih, C.] Johnson Space Ctr, Jacobs JETS, Houston, TX 77058 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A531
EP A531
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400389
ER
PT J
AU Rios, AC
Cooper, G
AF Rios, A. C.
Cooper, G.
TI ON THE LONG TERM SURVIVAL OF METABOLIC COMPOUNDS DETECTED IN
CARBONACEOUS METEORITES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Rios, A. C.] Univ Space Res Assoc, NASA Postdoctoral Program, MS 239-4, Moffett Field, CA 94035 USA.
[Rios, A. C.; Cooper, G.] NASA, Ames Res Ctr, Exobiol Branch, MS 239-4, Moffett Field, CA 94035 USA.
EM Andro.c.rios@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A538
EP A538
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400396
ER
PT J
AU Sandford, SA
Materese, CK
Nuevo, M
AF Sandford, S. A.
Materese, C. K.
Nuevo, M.
TI THE FORMATION OF NUCLEOBASES FROM THE UV IRRADIATION OF PURINE IN
ASTROPHYSICAL ICES AND COMPARISONS WITH METEORITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID ULTRAVIOLET PHOTOIRRADIATION; EXTRATERRESTRIAL NUCLEOBASES; CARBONACEOUS
METEORITES; MURCHISON METEORITE; PYRIMIDINE; URACIL
C1 [Sandford, S. A.; Materese, C. K.; Nuevo, M.] NASA, Ames Res Ctr, Washington, DC 20546 USA.
[Materese, C. K.; Nuevo, M.] Bay Area Environm Res Inst, Petaluma, CA USA.
EM Scott.A.Sandford@nasa.gov
NR 8
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A551
EP A551
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400409
ER
PT J
AU Satterwhite, CE
Funk, RC
Righter, K
Harrington, RH
AF Satterwhite, C. E.
Funk, R. C.
Righter, K.
Harrington, R. H.
TI Years of Processing Pieces of Space
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Satterwhite, C. E.] NASA, Jacobs, JSC, Mailcode XI2,2101 Nasa Pkwy, Houston, TX 77058 USA.
[Funk, R. C.] NASA, GeoControl Jacobs JETS Contract, JSC, Mailcode XI2,2101 Nasa Pkwy, Houston, TX 77058 USA.
[Righter, K.] NASA, JSC, Mailcode XI2,2101 Nasa Pkwy, Houston, TX 77058 USA.
[Harrington, R. H.] NASA, UTC Jacobs JETS Contract, JSC, Mailcode XI2,2101 Nasa Pkwy, Houston, TX 77058 USA.
EM cecilia.e.satterwhite@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A554
EP A554
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400412
ER
PT J
AU Schmieder, M
Buchner, E
AF Schmieder, M.
Buchner, E.
TI DISCOVERY OF POSSIBLE METEORITIC MATTER ON SHATTER CONES-3. MARQUEZ
DOME, TEXAS, USA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Schmieder, M.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Schmieder, M.] NASA, SSERVI, Washington, DC USA.
[Buchner, E.] HNU Neu Ulm Univ Appl Sci, Wileystr 1, D-89231 Neu Ulm, Germany.
[Buchner, E.] Univ Stuttgart, Inst Mineral, Azenberstr 18, D-70174 Stuttgart, Germany.
EM schmieder@lpi.usra.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A556
EP A556
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400414
ER
PT J
AU Schroder, C
Bland, PA
Golombek, MP
Ashley, JW
Warner, NH
Grant, JA
AF Schroeder, C.
Bland, P. A.
Golombek, M. P.
Ashley, J. W.
Warner, N. H.
Grant, J. A.
TI AMAZONIAN CHEMICAL WEATHERNG RATE DERIVED FROM STONY METEORITE FINDS AT
MERIDIANI PLANUM ON MARS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID CLIMATE; CRATER
C1 [Schroeder, C.] Univ Stirling, Fac Nat Sci, Biol & Environm Sci, Stirling FK9 4LA, Scotland.
[Bland, P. A.] Curtin Univ, Dept Appl Geol, Perth, WA 6845, Australia.
[Golombek, M. P.; Ashley, J. W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Warner, N. H.] SUNY Coll Geneseo, Dept Geol Sci, Geneseo, NY 14454 USA.
[Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
EM chris-tian.schroeder@stir.ac.uk
NR 13
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A558
EP A558
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400416
ER
PT J
AU Schwarz, WH
Breutmann, G
Schmitt, AK
Trieloff, M
Ludwig, T
Hanel, M
Buchner, E
Schmieder, M
Pesonen, LJ
Moilanen, J
AF Schwarz, W. H.
Breutmann, G.
Schmitt, A. K.
Trieloff, M.
Ludwig, T.
Hanel, M.
Buchner, E.
Schmieder, M.
Pesonen, L. J.
Moilanen, J.
TI U/PB DATING OF ZIRCON FROM THE SUVASVESI IMPACT STRUCTURES, FINLAND
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Schwarz, W. H.; Breutmann, G.; Schmitt, A. K.; Trieloff, M.; Ludwig, T.; Hanel, M.] Heidelberg Univ, Inst Geowissensch, Neuenheimer Feld 234-236, D-69120 Heidelberg, Germany.
[Schwarz, W. H.; Trieloff, M.] Klaus Tschira Lab Kosmochem, Neuenheimer Feld 234-236, D-69120 Heidelberg, Germany.
[Buchner, E.] HNU Neu Ulm Univ Appl Sci, Wileystr 1, D-89231 Neu Ulm, Germany.
[Buchner, E.] Univ Stuttgart, Inst Mineral & Kristallchem, Azenbergstr 18, D-70174 Stuttgart, Germany.
[Schmieder, M.] LPI, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Schmieder, M.] NASA, SSERVI, Washington, DC 20546 USA.
[Pesonen, L. J.] Univ Helsinki, Dept Phys, POB 64, Helsinki 00014, Finland.
[Moilanen, J.] Katajarinteentie 1 As 1, Vuolijoki 88270, Finland.
EM Winfried.Schwarz@geow.uni-heidelberg.de
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A561
EP A561
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400419
ER
PT J
AU Schwenzer, SP
Barnes, G
Bridges, JC
Bullock, MA
Chavez, CL
Filiberto, J
Herrmann, S
Hicks, LJ
Kelley, SP
Miller, MA
Moore, JM
Ott, U
Smith, HD
Steer, ED
Swindle, TD
Treiman, AH
AF Schwenzer, S. P.
Barnes, G.
Bridges, J. C.
Bullock, M. A.
Chavez, C. L.
Filiberto, J.
Herrmann, S.
Hicks, L. J.
Kelley, S. P.
Miller, M. A.
Moore, J. M.
Ott, U.
Smith, H. D.
Steer, E. D.
Swindle, T. D.
Treiman, A. H.
TI FRACTIONATED (MARTIAN) NOBLE GASES - EFA, EXPERIMENTS AND METEORITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID ADSORPTION; SIGNATURES; NAKHLA
C1 [Schwenzer, S. P.; Kelley, S. P.; Steer, E. D.] Open Univ, Dept Environm Earth & Ecosyst, Walton Hall, Milton Keynes MK7 5AA, Bucks, England.
[Schwenzer, S. P.; Herrmann, S.; Ott, U.] Max Planck Inst Chem, Mainz, Germany.
[Ott, U.] Univ West Hungary, Szomabthely, Hungary.
[Schwenzer, S. P.; Treiman, A. H.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Barnes, G.] Univ Idaho, Moscow, ID 83843 USA.
[Barnes, G.; Swindle, T. D.] Univ Arizona, Tucson, AZ 85721 USA.
[Bridges, J. C.; Hicks, L. J.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Bullock, M. A.] Southwest Res Inst, Boulder, CO USA.
[Chavez, C. L.; Moore, J. M.; Smith, H. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Filiberto, J.] Southern Illinois Univ, Carbondale, IL 62901 USA.
[Miller, M. A.] Southwest Res Inst, San Antonio, TX 78228 USA.
[Steer, E. D.] Univ Nottingham, Nanoscale & Microscale Res Ctr NMRC, Nottingham NG7 2RD, England.
EM susanne.schwenzer@open.ac.uk
NR 17
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A562
EP A562
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400420
ER
PT J
AU Simkus, DN
Aponte, JC
Hilts, RW
Elsila, JE
Herd, CDK
AF Simkus, D. N.
Aponte, J. C.
Hilts, R. W.
Elsila, J. E.
Herd, C. D. K.
TI COMPOUND-SPECIFIC CARBON ISOTOPE COMPOSITIONS OF ALDEHYDES AND KETONES
IN THE TAGISH LAKE METEORITE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Simkus, D. N.; Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB, Canada.
[Aponte, J. C.; Elsila, J. E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 691, Greenbelt, MD USA.
[Aponte, J. C.] Catholic Univ Amer, Washington, DC 20064 USA.
[Hilts, R. W.] MacEwan Univ, Dept Phys Sci, Edmonton, AB, Canada.
EM simkus@ualberta.ca
NR 9
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A575
EP A575
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400433
ER
PT J
AU Spohn, T
Breuer, D
Plesa, AC
Grott, M
Tosi, N
Banerdt, B
Lognonne, P
Smrekar, S
AF Spohn, T.
Breuer, D.
Plesa, A. -C.
Grott, M.
Tosi, N.
Banerdt, B.
Lognonne, P.
Smrekar, S.
TI HEINRICH WANKE, MARTIAN GEOCHEMISTRY AND THE INSIGHT MISSION
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID MARS
C1 [Spohn, T.; Breuer, D.; Plesa, A. -C.; Grott, M.; Tosi, N.] DLR Inst Planetary Res, Rutherfordestr 2, D-12489 Berlin, Germany.
[Banerdt, B.; Smrekar, S.] Jet Prop Lab, 4800 Oak Wood Dr, Pasadena, CA 91109 USA.
[Lognonne, P.] Inst Phys Globe Paris, 35 Rue Helene Brion, F-75205 Paris 13, France.
EM tilman.spohn@dlr.de; bruce.banerdt@jpl.nasa.gov; lognonne@ipgp.fr
NR 10
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A588
EP A588
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400446
ER
PT J
AU Srinivasan, P
McCubbin, FM
Rahman, Z
Keller, LP
Agee, CB
AF Srinivasan, P.
McCubbin, F. M.
Rahman, Z.
Keller, L. P.
Agee, C. B.
TI NOBLE METAL ARSENIDES AND GOLD INCLUSIONS IN NORTHWEST AFRICA 8186.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID CARBONACEOUS CHONDRITES; ASSEMBLAGES
C1 [Srinivasan, P.; Agee, C. B.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Srinivasan, P.; Agee, C. B.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Srinivasan, P.; McCubbin, F. M.] NASA, Johnson Space Ctr, Mail Code XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
[Rahman, Z.; Keller, L. P.] NASA, Johnson Space Ctr, Mail Code XI3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM psrinivasan@unm.edu
NR 11
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A592
EP A592
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400450
ER
PT J
AU Taylor, S
Lever, JH
Alexander, CMO
Brownlee, DE
Messenger, S
Nittler, LR
Stroud, RM
Wozniakiewicz, P
Clemett, S
AF Taylor, S.
Lever, J. H.
Alexander, C. M. O'D
Brownlee, D. E.
Messenger, S.
Nittler, L. R.
Stroud, R. M.
Wozniakiewicz, P.
Clemett, S.
TI SAMPLING INTERPLANETARY DUST PARTICLES FROM ANTARCTIC AIR.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
ID MICROMETEORITES; GRAINS; SNOW
C1 [Taylor, S.; Lever, J. H.] CRREL, 72 Lyme Rd, Hanover, NH 03755 USA.
[Alexander, C. M. O'D; Nittler, L. R.] Carnegie Inst Sci, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 91195 USA.
[Messenger, S.; Clemett, S.] NASA, Johnson Space Ctr, ARES, Code SR, Houston, TX 77058 USA.
[Stroud, R. M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA.
[Wozniakiewicz, P.] Univ Kent, Sch Phys Sci, Ingram Bldg, Canterbury CT2 7NH, Kent, England.
EM Susan.Taylor@erdc.dren.mil; James.Lever@erdc.dren.mil;
alexande@dtm.ciw.edu; browlee@astro.washington.edu;
scott.messenger@nasa.gov; lnit-tler@ciw.edu; stroud@nrl.navy.mil;
pjw@kent.ac.uk; simon.j.clemett@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A618
EP A618
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400476
ER
PT J
AU Warren, PH
Kohl, I
Young, ED
Isa, J
Morgan, M
Liu, Y
AF Warren, P. H.
Kohl, I.
Young, E. D.
Isa, J.
Morgan, M.
Liu, Y.
TI ENIGMATIC ENCLAVES OF SILICA AND AUGITE, WITHOUT FELDSPAR, IN EUCRITE
NWA 10553.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Warren, P. H.; Kohl, I.; Young, E. D.; Isa, J.] Univ Calif Los Angeles, Earth Space Sci Dept, Los Angeles, CA 90095 USA.
[Morgan, M.] Colorado Sch Mines, Golden, CO 80401 USA.
[Liu, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pwarren@ucla.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A651
EP A651
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400509
ER
PT J
AU Zeigler, RA
Korotev, RL
AF Zeigler, R. A.
Korotev, R. L.
TI PETROGRAPHY, GEOCHEMISTRY, AND PAIRING RELATIONSHIPS OF BASALTIC LUNAR
METEORITE MILLER RANGE 13317.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Zeigler, R. A.] NASA, Johnson Space Ctr, 2101 NASA Rd 1,Mail Code XI2, Houston, TX 77058 USA.
[Korotev, R. L.] Washington Univ St Louis, 1 Brookings Dr Campus Box 1169, St Louis, MO USA.
EM ryan.a.zeigler@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A686
EP A686
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400544
ER
PT J
AU Zolensky, ME
Fries, M
Utas, J
Chan, QHS
Kebukawa, Y
Steele, A
Bodnar, RJ
Ito, M
Nakashima, D
Nakamura, T
Greenwood, R
Rahman, Z
Le, L
Ross, DK
AF Zolensky, M. E.
Fries, M.
Utas, J.
Chan, Q. H. -S.
Kebukawa, Y.
Steele, A.
Bodnar, R. J.
Ito, M.
Nakashima, D.
Nakamura, T.
Greenwood, R.
Rahman, Z.
Le, L.
Ross, D. K.
TI C CHONDRITE CLASTS IN H CHONDRITE REGOLITH BRECCIAS: SOMETHING DIFFERENT
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 79th Annual Meeting of the Meteoritical-Society
CY AUG 07-12, 2016
CL Berlin, GERMANY
SP Meteorit Soc
C1 [Zolensky, M. E.; Fries, M.; Chan, Q. H. -S.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Utas, J.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Kebukawa, Y.] Yokohama Natl Univ, Yokohama, Kanagawa 2408501, Japan.
[Steele, A.] Carnegie Geophys Lab, Washington, DC 20015 USA.
[Bodnar, R. J.] Virginia Tech, Blacksburg, VA 24061 USA.
[Ito, M.] JAMSTEC, Kochi 7838502, Japan.
[Nakashima, D.; Nakamura, T.] Tohoku Univ, Sendai, Miyagi 9808577, Japan.
[Greenwood, R.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Rahman, Z.; Le, L.; Ross, D. K.] Jacobs ESCG, Houston, TX 77058 USA.
EM Michael.e.zolensky@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2016
VL 51
SU 1
SI SI
BP A691
EP A691
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA ED2GQ
UT WOS:000388662400549
ER
PT J
AU Nimmo, F
Pappalardo, RT
AF Nimmo, F.
Pappalardo, R. T.
TI Ocean worlds in the outer solar system
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Review
ID EUROPAS ICE SHELL; STRONG TIDAL DISSIPATION; HYDRATED SALT MINERALS;
LATE HEAVY BOMBARDMENT; KUIPER-BELT OBJECTS; GALILEAN SATELLITES;
THERMAL EVOLUTION; SUBSURFACE OCEAN; LIQUID WATER; HYDROTHERMAL SYSTEMS
AB Many outer solar system bodies are thought to harbor liquid water oceans beneath their ice shells. This article first reviews how such oceans are detected. We then discuss how they are maintained, when they formed, and what the oceans' likely characteristics are. We focus in particular on Europa, Ganymede, Callisto, Titan, and Enceladus, bodies for which there is direct evidence of subsurface oceans. We also consider candidate ocean worlds such as Pluto and Triton.
C1 [Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Pappalardo, R. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nimmo, F (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
EM fnimmo@es.ucsc.edu
FU NASA [NNX13AG02G, NNX15AQ88G]
FX We thank Hauke Hussmann and an anonymous reviewer for careful comments
on the MS. The portion of this work performed by R.T.P. was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Parts of F.N.'s work were supported by NASA grants NNX13AG02G and
NNX15AQ88G. This is a review article. It contains no novel data.
NR 192
TC 0
Z9 0
U1 12
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG
PY 2016
VL 121
IS 8
BP 1378
EP 1399
DI 10.1002/2016JE005081
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MI
UT WOS:000387794800001
ER
PT J
AU Wilson, EH
Atreya, SK
Kaiser, RI
Mahaffy, PR
AF Wilson, Eric H.
Atreya, Sushil K.
Kaiser, Ralf I.
Mahaffy, Paul R.
TI Perchlorate formation on Mars through surface radiolysis-initiated
atmospheric chemistry: A potential mechanism
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID EVALUATED KINETIC-DATA; GAS-PHASE REACTIONS; PHOTOIONIZATION QUANTUM
EFFICIENCY; ROCKNEST AEOLIAN DEPOSIT; CROSS-SECTIONS;
ABSORPTION-COEFFICIENTS; TEMPERATURE-DEPENDENCE; PHOTOCHEMICAL DATA;
MARTIAN SOIL; GALE CRATER
AB Recent observations of the Martian surface by the Phoenix lander and the Sample Analysis at Mars indicate the presence of perchlorate (ClO4-). The abundance and isotopic composition of these perchlorates suggest that the mechanisms responsible for their formation in the Martian environment may be unique in our solar system. With this in mind, we propose a potential mechanism for the production of Martian perchlorate: the radiolysis of the Martian surface by galactic cosmic rays, followed by the sublimation of chlorine oxides into the atmosphere and their subsequent synthesis to form perchloric acid (HClO4) in the atmosphere, and the surface deposition and subsequent mineralization of HClO4 in the regolith to form surface perchlorates. To evaluate the viability of this mechanism, we employ a one-dimensional chemical model, examining chlorine chemistry in the context of Martian atmospheric chemistry. Considering the chlorine oxide, OCIO, we find that an OCIO flux as low as 3.2 x 10(7) molecules cm(-2) s(-1) sublimated into the atmosphere from the surface could produce sufficient HClO4 to explain the perchlorate concentration on Mars, assuming an accumulation depth of 30 cm and integrated over the Amazonian period. Radiolysis provides an efficient pathway for the oxidation of chlorine, bypassing the efficient Cl/HCl recycling mechanism that characterizes HClO4 formation mechanisms proposed for the Earth but not Mars.
C1 [Wilson, Eric H.; Atreya, Sushil K.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Wilson, EH (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM wilson@umich.edu
FU National Aeronautics and Space Administration [NNX14AG39G]; NASA Mars
Science Laboratory Project
FX We thank R. Navarro-Gonzalez, A. A. Pavlov, B. Sutter, and M.H. Wong for
their useful comments on the manuscript and the MSL team for the
successful operation of the mission. R.I.K. acknowledges support from
the National Aeronautics and Space Administration under grant
NNX14AG39G. This paper is a modeling paper that uses model inputs that
are referenced accordingly throughout. We note that there are no
data-sharing issues since all of the numerical information is provided
in the figures and tables produced by solving the equations in the
paper. This research was supported by the NASA Mars Science Laboratory
Project.
NR 114
TC 0
Z9 0
U1 6
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 AUG
PY 2016
VL 121
IS 8
BP 1472
EP 1487
DI 10.1002/2016JE005078
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MI
UT WOS:000387794800006
PM 27774369
ER
PT J
AU Doyle, R
Chien, S
Kortenkamp, D
Woods, M
AF Doyle, Richard
Chien, Steve
Kortenkamp, David
Woods, Mark
TI Introduction to the Special Issue on Intelligent Systems for Space
Exploration
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Editorial Material
C1 [Doyle, Richard; Chien, Steve] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kortenkamp, David] TRACLabs, Webster, TX 77598 USA.
[Woods, Mark] SCISYS UK Ltd, Bristol BS4 5SS, Avon, England.
RP Doyle, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 1940-3151
EI 2327-3097
J9 J AEROSP INFORM SYST
JI J. Aerosp. Inf. Syst.
PD AUG
PY 2016
VL 13
IS 8
BP 279
EP 279
DI 10.2514/1.I010487
PG 1
WC Engineering, Aerospace
SC Engineering
GA EC5YC
UT WOS:000388212200001
ER
PT J
AU Burl, MC
Thompson, DR
deGranville, C
Bornstein, BJ
AF Burl, Michael C.
Thompson, David R.
deGranville, Charles
Bornstein, Benjamin J.
TI ROCKSTER: Onboard Rock Segmentation Through Edge Regrouping
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Article
ID REAL-TIME; MARS; EXPLORATION; TRACKING; SCIENCE; VISION; FIELDS; SHAPE
AB To perform more complex space exploration activities with limited human intervention, an intelligent system must be able not only to sense its environment, but also to interpret the sensory data it acquires. Rock Segmentation Through Edge Regrouping is an autonomous perception algorithm for scientific analysis that is deployed on Mars. It conducts onboard analysis of images collected by the Mars Exploration Rover Opportunity and provides a list of closed rock contours to the Autonomous Exploration for Gathering Increased Science software module, which then prioritizes the identified rocks for subsequent targeting based on preferences expressed by scientists. Rock Segmentation Through Edge Regrouping processes 1 Kx1 K images in 600-900 s on the MER RAD6000 flight processor, clocked to operate at 20 million instructions per second, with a guaranteed high-water memory footprint of less than 4 megabytes of RAM. In all runs on Mars with rocks or outcrop present, the top 10 returned targets have been valid rocks or outcrop with one exception, which was a dark patch of soil. In several runs in which there were no rocks present, the algorithm correctly returned no detections. A nearly integer-only parallel version of the algorithm has been demonstrated on a Tilera TILE64 multicore processor.
C1 [Burl, Michael C.; Thompson, David R.; deGranville, Charles] Jet Prop Lab, Machine Learning & Instrument Auton Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bornstein, Benjamin J.] Jet Prop Lab, Syst Architecture & Engn Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Burl, MC (reprint author), Jet Prop Lab, Machine Learning & Instrument Auton Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Michael.C.Burl@jpl.nasa.gov; David.R.Thompson@jpl.nasa.gov;
Charles.K.deGranville@jpl.nasa.gov; Benjamin.J.Bornstein@jpl.nasa.gov
NR 60
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 1940-3151
EI 2327-3097
J9 J AEROSP INFORM SYST
JI J. Aerosp. Inf. Syst.
PD AUG
PY 2016
VL 13
IS 8
BP 329
EP 342
DI 10.2514/1.I010381
PG 14
WC Engineering, Aerospace
SC Engineering
GA EC5YC
UT WOS:000388212200005
ER
PT J
AU Ehresmann, B
Hassler, DM
Zeitlin, C
Guo, JN
Kohler, J
Wimmer-Schweingruber, RF
Appel, JK
Brinza, DE
Rafkin, SCR
Bottcher, SI
Burmeister, S
Lohf, H
Martin, C
Bohm, E
Matthia, D
Reitz, G
AF Ehresmann, Bent
Hassler, Donald M.
Zeitlin, Cary
Guo, Jingnan
Koehler, Jan
Wimmer-Schweingruber, Robert F.
Appel, Jan K.
Brinza, David E.
Rafkin, Scot C. R.
Boettcher, Stephan I.
Burmeister, Soenke
Lohf, Henning
Martin, Cesar
Boehm, Eckart
Matthiae, Daniel
Reitz, Guenther
TI Charged particle spectra measured during the transit to Mars with the
Mars Science Laboratory Radiation Assessment Detector (MSL/RAD)
SO LIFE SCIENCES IN SPACE RESEARCH
LA English
DT Article
DE RAD; MSL; Radiation; GCR; Transit Earth-Mars
ID GALACTIC COSMIC-RAYS; SOLAR MODULATION; MARTIAN SURFACE; ENVIRONMENT;
MODELS; RAD
AB The Mars Science Laboratory (MSL) started its 253-day cruise to Mars on November 26, 2011. During cruise the Radiation Assessment Detector (RAD), situated on board the Curiosity rover, conducted measurements of the energetic-particle radiation environment inside the spacecraft. This environment consists mainly of galactic cosmic rays (GCRs), as well as secondary particles created by interactions of these GCRs with the spacecraft. The RAD measurements can serve as a proxy for the radiation environment a human crew would encounter during a transit to Mars, for a given part of the solar cycle, assuming that a crewed vehicle would have comparable shielding. The measurements of radiological quantities made by RAD are important in themselves, and, the same data set allow for detailed analysis of GCR-induced particle spectra inside the spacecraft. This provides important inputs for the evaluation of current transport models used to model the free-space (and spacecraft) radiation environment for different spacecraft shielding and different times in the solar cycle. Changes in these conditions can lead to significantly different radiation fields and, thus, potential health risks, emphasizing the need for validated transport codes. Here, we present the first measurements of charged particle fluxes inside a spacecraft during the transit from Earth to Mars. Using data obtained during the last two month of the cruise to Mars (June 11-July 14, 2012), we have derived detailed energy spectra for low-Z particles stopping in the instrument's detectors, as well as integral fluxes for penetrating particles with higher energies. Furthermore, we analyze the temporal changes in measured proton fluxes during quiet solar periods (i.e., when no solar energetic particle events occurred) over the duration of the transit (December 9, 2011-July 14, 2012) and correlate them with changing heliospheric conditions. (C) 2016 The Committee on Space Research (COSPAR). Published by Elsevier Ltd. All rights reserved.
C1 [Ehresmann, Bent; Hassler, Donald M.; Rafkin, Scot C. R.] Southwest Res Inst, Space Sci & Engn Div, 1050 Walnut St, Boulder, CO 80302 USA.
[Zeitlin, Cary] Southwest Res Inst, Earth Oceans & Space Dept, Durham, NH USA.
[Guo, Jingnan; Koehler, Jan; Wimmer-Schweingruber, Robert F.; Appel, Jan K.; Boettcher, Stephan I.; Burmeister, Soenke; Lohf, Henning; Martin, Cesar; Boehm, Eckart] Univ Kiel, Kiel, Germany.
[Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Matthiae, Daniel; Reitz, Guenther] Deutsch Zentrum Luft & Raumfahrt, Cologne, Germany.
RP Ehresmann, B (reprint author), Southwest Res Inst, Space Sci & Engn Div, 1050 Walnut St, Boulder, CO 80302 USA.
EM ehresmann@boulder.swri.edu
NR 35
TC 0
Z9 0
U1 2
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2214-5524
EI 2214-5532
J9 LIFE SCI SPACE RES
JI Life Sci. Space Res.
PD AUG
PY 2016
VL 10
BP 29
EP 37
DI 10.1016/j.lssr.2016.07.001
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EC3GU
UT WOS:000388015100004
PM 27662785
ER
PT J
AU Knipp, DJ
Giles, BL
AF Knipp, Delores J.
Giles, Barbara L.
TI Global Positioning System Energetic Particle Data: The Next Space
Weather Data Revolution
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Knipp, Delores J.] Univ Colorado, Boulder, CO 80309 USA.
[Knipp, Delores J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80305 USA.
[Giles, Barbara L.] Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Giles, Barbara L.] Goddard Space Flight Ctr, MMS Fast Plasma Invest, Greenbelt, MD USA.
RP Knipp, DJ (reprint author), Univ Colorado, Boulder, CO 80309 USA.; Knipp, DJ (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80305 USA.
EM dknipp@agu.org
NR 3
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD AUG
PY 2016
VL 14
IS 8
BP 526
EP 527
DI 10.1002/2016SW001483
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EC0OV
UT WOS:000387801400001
ER
PT J
AU Nunez, M
Nieves-Chinchilla, T
Pulkkinen, A
AF Nunez, Marlon
Nieves-Chinchilla, Teresa
Pulkkinen, Antti
TI Prediction of shock arrival times from CME and flare data
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID CORONAL MASS EJECTIONS; INTERPLANETARY SHOCKS; SOLAR-WIND; OUTER
HELIOSPHERE; INNER HELIOSPHERE; MAGNETIC CLOUD; 2 SPACECRAFT; 1 AU;
MODEL; EVOLUTION
AB This paper presents the Shock Arrival Model (SARM) for predicting shock arrival times for distances from 0.72 AU to 8.7 AU by using coronal mass ejections (CME) and flare data. SARM is an aerodynamic drag model described by a differential equation that has been calibrated with a data set of 120 shocks observed from 1997 to 2010 by minimizing the mean absolute error (MAE), normalized to 1 AU. SARM should be used with CME data (radial, earthward, or plane-of-sky speeds) and flare data (peak flux, duration, and location). In the case of 1 AU, the MAE and the median of absolute errors were 7.0 h and 5.0 h, respectively, using the available CME/flare data. The best results for 1 AU (an MAE of 5.8 h) were obtained using both CME data, either radial or cone model-estimated speeds, and flare data. For the prediction of shock arrivals at distances from 0.72 AU to 8.7 AU, the normalized MAE and the median were 7.1 h and 5.1 h, respectively, using the available CME/flare data. SARM was also calibrated to be used with CME data alone or flare data alone, obtaining normalized MAE errors of 8.9 h and 8.6 h, respectively, for all shock events. The model verification was carried out with an additional data set of 20 shocks observed from 2010 to 2012 with radial CME speeds to compare SARM with the empirical ESA model and the numerical MHD-based ENLIL model. The results show that the ENLIL's MAE was lower than the SARM's MAE, which was lower than the ESA's MAE. The SARM's best results were obtained when both flare and true CME speeds were used.
C1 [Nunez, Marlon] Univ Malaga, Dept Languages & Comp Sci, Malaga, Spain.
[Nieves-Chinchilla, Teresa; Pulkkinen, Antti] NASA, GSFC, Heliophys Sci Div, Greenbelt, MD USA.
RP Nunez, M (reprint author), Univ Malaga, Dept Languages & Comp Sci, Malaga, Spain.
EM mnunez@uma.es
OI Nunez, Marlon/0000-0001-5374-5231
FU Plan Propio de Investigacion of Universidad de Malaga / Campus de
Excelencia Internacional Andalucia Tech; European Space Agency's
Technology Research Programme (project SEPsFLAREs) [4000109626/13/NL/AK]
FX The SARM model was funded by the Plan Propio de Investigacion of
Universidad de Malaga / Campus de Excelencia Internacional Andalucia
Tech, and by the European Space Agency's Technology Research Programme
(project SEPsFLAREs; Contract No. 4000109626/13/NL/AK). As mentioned in
the text, the shock arrival predictions presented in this paper are
available by processing the SARM model at
http://spaceweather.uma.es/sarm/index.html with data in Table 1 and
Table 3.
NR 62
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD AUG
PY 2016
VL 14
IS 8
BP 544
EP 562
DI 10.1002/2016SW001361
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EC0OV
UT WOS:000387801400004
ER
PT J
AU Jian, LK
MacNeice, PJ
Mays, ML
Taktakishvili, A
Odstrcil, D
Jackson, B
Yu, HS
Riley, P
Sokolov, IV
AF Jian, L. K.
MacNeice, P. J.
Mays, M. L.
Taktakishvili, A.
Odstrcil, D.
Jackson, B.
Yu, H. -S.
Riley, P.
Sokolov, I. V.
TI Validation for global solar wind prediction using Ulysses comparison:
Multiple coronal and heliospheric models installed at the Community
Coordinated Modeling Center
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID MASS EJECTIONS CMES; MAGNETIC-FIELDS; 3-DIMENSIONAL PROPAGATION; INNER
HELIOSPHERE; FLUX TRANSPORT; ALFVEN WAVES; MHD MODEL; INTERPLANETARY;
EVOLUTION; DRIVEN
AB The prediction of the background global solar wind is a necessary part of space weather forecasting. Several coronal and heliospheric models have been installed and/or recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang-Sheely-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling Framework (SWMF), and heliospheric tomography using interplanetary scintillation data. Ulysses recorded the last fast latitudinal scan from southern to northern poles in 2007. By comparing the modeling results with Ulysses observations over seven Carrington rotations, we have extended our third-party validation from the previous near-Earth solar wind to middle to high latitudes, in the same late declining phase of solar cycle 23. Besides visual comparison, we have quantitatively assessed the models' capabilities in reproducing the time series, statistics, and latitudinal variations of solar wind parameters for a specific range of model parameter settings, inputs, and grid configurations available at CCMC. The WSA-Enlil model results vary with three different magnetogram inputs. The MAS-Enlil model captures the solar wind parameters well, despite its underestimation of the speed at middle to high latitudes. The new version of SWMF misses many solar wind variations probably because it uses lower grid resolution than other models. The interplanetary scintillation-tomography cannot capture the latitudinal variations of solar wind well yet. Because the model performance varies with parameter settings which are optimized for different epochs or flow states, the performance metric study provided here can serve as a template that researchers can use to validate the models for the time periods and conditions of interest to them.
C1 [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jian, L. K.; MacNeice, P. J.; Mays, M. L.; Taktakishvili, A.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Mays, M. L.; Taktakishvili, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Odstrcil, D.] 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, La Jolla, CA 92093 USA.
[Riley, P.] Predict 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.; Jian, LK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM lan.jian@nasa.gov
RI Sokolov, Igor/H-9860-2013
OI Sokolov, Igor/0000-0002-6118-0469
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 the
University of California, San Diego. 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, MWO, and
NSO/SOLIS teams for providing the photospheric magnetograms. We
appreciate all the modeling teams for providing their models at the CCMC
and for their consultation. We are grateful to Ward Manchester for
verifying the current version of SWMF/AWSoM at the University of
Michigan performs the same as reported here at Ulysses orbit. L.K.J.
thanks Rebekah M. Evans for running the SWMF v8.03 model in 2012. We
acknowledge the Space Physics Data Facility at NASA/GSFC for providing
Ulysses data (see http://omniweb.gsfc.nasa.gov/coho/).
NR 62
TC 0
Z9 0
U1 7
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD AUG
PY 2016
VL 14
IS 8
BP 592
EP 611
DI 10.1002/2016SW001435
PG 20
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EC0OV
UT WOS:000387801400007
ER
PT J
AU Teng, W
Rui, HL
Strub, R
Vollmer, B
AF Teng, William
Rui, Hualan
Strub, Richard
Vollmer, Bruce
TI OPTIMAL REORGANIZATION OF NASA EARTH SCIENCE DATA FOR ENHANCED
ACCESSIBILITY AND USABILITY FOR THE HYDROLOGY COMMUNITY
SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION
LA English
DT Article
DE data management; remote sensing; time series analysis; data access; data
rods; hydrology; digital divide
ID DATA ASSIMILATION SYSTEM; GIOVANNI
AB A long-standing "Digital Divide" in data representation exists between the preferred way of data access by the hydrology community and the common way of data archival by earth science data centers. Typically, in hydrology, earth surface features are expressed as discrete spatial objects (e.g., watersheds), and time-varying data are contained in associated time series. Data in earth science archives, although stored as discrete values (of satellite swath pixels or geographical grids), represent continuous spatial fields, one file per time step. This Divide has been an obstacle, specifically, between the Consortium of Universities for the Advancement of Hydrologic Science, Inc. and NASA earth science data systems. In essence, the way data are archived is conceptually orthogonal to the desired method of access. Our recent work has shown an optimal method of bridging the Divide, by enabling operational access to long-time series (e.g., 36 years of hourly data) of selected NASA datasets. These time series, which we have termed "data rods," are pre-generated or generated on-the-fly. This optimal solution was arrived at after extensive investigations of various approaches, including one based on "data curtains." The on-the-fly generation of data rods uses "data cubes," NASA Giovanni, and parallel processing. The optimal reorganization of NASA earth science data has significantly enhanced the access to and use of the data for the hydrology user community.
C1 [Teng, William; Rui, Hualan; Strub, Richard] NASA, ADNET Syst Inc, Goddard Earth Sci Data & Informat Serv Ctr, Code 610-2, Greenbelt, MD 20771 USA.
[Vollmer, Bruce] NASA, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD 20771 USA.
RP Teng, W (reprint author), NASA, ADNET Syst Inc, Goddard Earth Sci Data & Informat Serv Ctr, Code 610-2, Greenbelt, MD 20771 USA.
EM william.l.teng@nasa.gov
FU NASA's Advancing Collaborative Connections for Earth System Science
(ACCESS) Program; GES DISC
FX We are grateful for the support of this "data rods" project by NASA's
Advancing Collaborative Connections for Earth System Science (ACCESS)
Program and by the GES DISC. We thank the other members of the "data
rods" project team for contributing their parts of the project, to which
the data rods are connected: David Maidment, Tim Whiteaker, David
Arctur, and Gonzalo Espinoza Davalos of the University of Texas at
Austin; and Christa Peters-Lidard, David Mocko, and Dalia Kirschbaum of
NASA GSFC Hydrological Sciences Laboratory. We also thank the three
anonymous reviewers and the associate editor for their comments and
suggestions. Their efforts have greatly improved the article.
NR 25
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1093-474X
EI 1752-1688
J9 J AM WATER RESOUR AS
JI J. Am. Water Resour. Assoc.
PD AUG
PY 2016
VL 52
IS 4
BP 825
EP 835
DI 10.1111/1752-1688.12405
PG 11
WC Engineering, Environmental; Geosciences, Multidisciplinary; Water
Resources
SC Engineering; Geology; Water Resources
GA EB2DW
UT WOS:000387168800003
ER
PT J
AU Snow, AD
Christensen, SD
Swain, NR
Nelson, EJ
Ames, DP
Jones, NL
Ding, D
Noman, NS
David, CH
Pappenberger, F
Zsoter, E
AF Snow, Alan D.
Christensen, Scott D.
Swain, Nathan R.
Nelson, E. James
Ames, Daniel P.
Jones, Norman L.
Ding, Deng
Noman, Nawajish S.
David, Cedric H.
Pappenberger, Florian
Zsoter, Ervin
TI A HIGH-RESOLUTION NATIONAL-SCALE HYDROLOGIC FORECAST SYSTEM FROM A
GLOBAL ENSEMBLE LAND SURFACE MODEL
SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION
LA English
DT Article
DE ECMWF; RAPID; Tethys Platform; CondorPy; HTCondor; CI-WATER; GloFAS;
NFIE; flood prediction; streamflow prediction; forecast
ID PREDICTION; UNCERTAINTY; IGNORANCE; ECMWF
AB Warning systems with the ability to predict floods several days in advance have the potential to benefit tens of millions of people. Accordingly, large-scale streamflow prediction systems such as the Advanced Hydrologic Prediction Service or the Global Flood Awareness System are limited to coarse resolutions. This article presents a method for routing global runoff ensemble forecasts and global historical runoff generated by the European Centre for Medium-Range Weather Forecasts model using the Routing Application for Parallel computation of Discharge to produce high spatial resolution 15-day stream forecasts, approximate recurrence intervals, and warning points at locations where streamflow is predicted to exceed the recurrence interval thresholds. The processing method involves distributing the computations using computer clusters to facilitate processing of large watersheds with high-density stream networks. In addition, the Streamflow Prediction Tool web application was developed for visualizing analyzed results at both the regional level and at the reach level of high-density stream networks. The application formed part of the base hydrologic forecasting service available to the National Flood Interoperability Experiment and can potentially transform the nation's forecast ability by incorporating ensemble predictions at the nearly 2.7 million reaches of the National Hydrography Plus Version 2 Dataset into the national forecasting system.
C1 [Snow, Alan D.] US Army Engineer Res & Dev Ctr, Coastal & Hydraul Lab, 3909 Halls Ferry Rd, Vicksburg, MS 39180 USA.
[Christensen, Scott D.; Swain, Nathan R.; Nelson, E. James; Ames, Daniel P.; Jones, Norman L.] Brigham Young Univ, Dept Civil & Environm Engn, Provo, UT 84602 USA.
[Ding, Deng; Noman, Nawajish S.] Esri, Redlands, CA 92373 USA.
[David, Cedric H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Pappenberger, Florian; Zsoter, Ervin] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading, Berks, England.
RP Snow, AD (reprint author), US Army Engineer Res & Dev Ctr, Coastal & Hydraul Lab, 3909 Halls Ferry Rd, Vicksburg, MS 39180 USA.
EM alan.d.snow@usace.army.mil
RI Pappenberger, Florian/A-2839-2009;
OI Pappenberger, Florian/0000-0003-1766-2898; Snow,
Alan/0000-0002-7333-3100
FU National Science Foundation [1135483]; Jet Propulsion Laboratory;
California Institute of Technology; National Aeronautics and Space
Administration
FX This research is based upon work supported by the National Science
Foundation under Grant No. 1135483. Cedric H. David was supported by the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. We
would also like to express appreciation to Curtis Rae for his assistance
in the GIS preprocessing of the NFIE regions.
NR 29
TC 2
Z9 2
U1 4
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1093-474X
EI 1752-1688
J9 J AM WATER RESOUR AS
JI J. Am. Water Resour. Assoc.
PD AUG
PY 2016
VL 52
IS 4
BP 950
EP 964
DI 10.1111/1752-1688.12434
PG 15
WC Engineering, Environmental; Geosciences, Multidisciplinary; Water
Resources
SC Engineering; Geology; Water Resources
GA EB2DW
UT WOS:000387168800013
ER
PT J
AU Wagstaff, KL
Tang, BY
Thompson, DR
Khudikyan, S
Wyngaard, J
Deller, AT
Palaniswamy, D
Tingay, SJ
Wayth, RB
AF Wagstaff, Kiri L.
Tang, Benyang
Thompson, David R.
Khudikyan, Shakeh
Wyngaard, Jane
Deller, Adam T.
Palaniswamy, Divya
Tingay, Steven J.
Wayth, Randall B.
TI A Machine Learning Classifier for Fast Radio Burst Detection at the VLBA
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE methods: data analysis
ID V-FASTR; TRANSIENTS; TELESCOPE; ARRAY; FRAMEWORK; MERGERS; SEARCH;
ORIGIN
AB Time domain radio astronomy observing campaigns frequently generate large volumes of data. Our goal is to develop automated methods that can identify events of interest buried within the larger data stream. The V-FASTR fast transient system was designed to detect rare fast radio bursts within data collected by the Very Long Baseline Array. The resulting event candidates constitute a significant burden in terms of subsequent human reviewing time. We have trained and deployed a machine learning classifier that marks each candidate detection as a pulse from a known pulsar, an artifact due to radio frequency interference, or a potential new discovery. The classifier maintains high reliability by restricting its predictions to those with at least 90% confidence. We have also implemented several efficiency and usability improvements to the V-FASTR web-based candidate review system. Overall, we found that time spent reviewing decreased and the fraction of interesting candidates increased. The classifier now classifies (and therefore filters) 80%-90% of the candidates, with an accuracy greater than 98%, leaving only the 10%-20% most promising candidates to be reviewed by humans.
C1 [Wagstaff, Kiri L.; Tang, Benyang; Thompson, David R.; Khudikyan, Shakeh; Wyngaard, Jane] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Deller, Adam T.] ASTRON, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands.
[Palaniswamy, Divya; Tingay, Steven J.; Wayth, Randall B.] Curtin Univ, ICRAR, Bentley, WA 6845, Australia.
[Palaniswamy, Divya] Univ Nevada, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA.
[Tingay, Steven J.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia.
RP Wagstaff, KL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kiri.l.wagstaff@jpl.nasa.gov
RI Wayth, Randall/B-2444-2013;
OI Wayth, Randall/0000-0002-6995-4131; Deller, Adam/0000-0001-9434-3837
FU State Government of Western Australia; joint venture partners; Jet
Propulsion Laboratory under a Research and Technology Development Grant;
National Aeronautics and Space Administration
FX The International Center 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. Steven J. Tingay is a Western Australian Premiers
Research Fellow.; This work was done in part at the Jet Propulsion
Laboratory under a Research and Technology Development Grant, under
contract with the National Aeronautics and Space Administration.
Copyright 2015. All Rights Reserved. US Government Support Acknowledged.
NR 30
TC 0
Z9 0
U1 5
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2016
VL 128
IS 966
AR 084503
DI 10.1088/1538-3873/128/966/084503
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LI
UT WOS:000387112900004
ER
PT J
AU Cappi, M
De Marco, B
Ponti, G
Ursini, F
Petrucci, PO
Bianchi, S
Kaastra, JS
Kriss, GA
Mehdipour, M
Whewell, M
Arav, N
Behar, E
Boissay, R
Branduardi-Raymont, G
Costantini, E
Ebrero, J
Di Gesu, L
Harrison, FA
Kaspi, S
Matt, G
Paltani, S
Peterson, BM
Steenbrugge, KC
Walton, DJ
AF Cappi, M.
De Marco, B.
Ponti, G.
Ursini, F.
Petrucci, P. -O.
Bianchi, S.
Kaastra, J. S.
Kriss, G. A.
Mehdipour, M.
Whewell, M.
Arav, N.
Behar, E.
Boissay, R.
Branduardi-Raymont, G.
Costantini, E.
Ebrero, J.
Di Gesu, L.
Harrison, F. A.
Kaspi, S.
Matt, G.
Paltani, S.
Peterson, B. M.
Steenbrugge, K. C.
Walton, D. J.
TI Anatomy of the AGN in NGC 5548 VIII. XMM-Newton's EPIC detailed view of
an unexpected variable multilayer absorber
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; X-rays: galaxies; galaxies: individual: NGC 5548
ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; BROAD-LINE REGION; SEYFERT-1
GALAXY NGC-5548; ACCRETION-DISK WINDS; ULTRA-FAST OUTFLOWS; QUASAR PDS
456; EMISSION-LINE; SPECTRAL VARIABILITY; ASCA OBSERVATIONS
AB In 2013, we conducted a large multi-wavelength campaign on the archetypical Seyfert 1 galaxy NGC 5548. Unexpectedly, this usually unobscured source appeared strongly absorbed in the soft X-rays during the entire campaign, and signatures of new and strong outflows were present in the almost simultaneous UV HST/COS data. Here we carry out a comprehensive spectral analysis of all available XMM-Newton observations of NGC 5548 (precisely 14 observations from our campaign plus three from the archive, for a total of similar to 763 ks) in combination with three simultaneous NuSTAR observations. We obtain a best-fit underlying continuum model composed by i) a weakly varying flat (Gamma similar to 1.5-1.7) power-law component; ii) a constant, cold reflection (FeK + continuum) component; iii) a soft excess, possibly owing to thermal Comptonization; and iv) a constant, ionized scattered emission-line dominated component. Our main findings are that, during the 2013 campaign, the first three of these components appear to be partially covered by a heavy and variable obscurer that is located along the line of sight (LOS), which is consistent with a multilayer of cold and mildly ionized gas. We characterize in detail the short timescale (mostly similar to ks-to-days) spectral variability of this new obscurer, and find it is mostly due to a combination of column density and covering factor variations, on top of intrinsic power-law (flux and slope) variations. In addition, our best-fit spectrum is left with several (but marginal) absorption features at rest-frame energies similar to 6.7-6.9 keV and similar to 8 keV, as well as a weak broad emission line feature redwards of the 6.4 keV emission line. These could indicate a more complex underlying model, e.g. a P-Cygni-type emission profile if we allow for a large velocity and wide-angle outflow. These findings are consistent with a picture where the obscurer represents the manifestation along the LOS of a multilayer of gas, which is also in multiphase, and which is likely outflowing at high speed, and simultaneously producing heavy obscuration and scattering in the X-rays, as well as broad absorption features in the UV.
C1 [Cappi, M.; Ponti, G.] IASF Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy.
[De Marco, B.; Ponti, G.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Ursini, F.; Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
[Ursini, F.; Petrucci, P. -O.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Petrucci, P. -O.] CNRS, IPAG, F-38000 Grenoble, France.
[Kaastra, J. S.; Mehdipour, M.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J. S.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 TA Utrecht, Netherlands.
[Kaastra, J. S.; Costantini, E.; Di Gesu, L.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Kriss, G. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Mehdipour, M.; Whewell, M.; Branduardi-Raymont, G.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Arav, N.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Behar, E.; Kaspi, S.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Boissay, R.; Paltani, S.] Univ Geneva, Dept Astron, 16 Chemin Ecogia, CH-1290 Versoix, Switzerland.
[Ebrero, J.] European Space Astron Ctr, POB 78, Madrid 28691, Spain.
[Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Peterson, B. M.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Peterson, B. M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA.
[Steenbrugge, K. C.] Univ Catolica Norte, Inst Astron, Avenida Angamos 0610,1280 Casilla, Antofagasta, Casilla, Chile.
[Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Cappi, M (reprint author), IASF Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy.
EM massimo.appi@inaf.it
RI Bianchi, Stefano/B-4804-2010
OI Bianchi, Stefano/0000-0002-4622-4240
FU ESA; Italian Space Agency [ASI-INAF I/037/12/P1]; EU Marie Curie
Intra-European fellowship [FP-PEOPLE-2012-IEF-331095]; ESA Member
States; USA (NASA); NASA [NAS5-26555]; International Space Science
Institute (ISSI) in Bern; NWO, the Netherlands Organization for
Scientific Research; NWO; UK STFC; NASA through from the Space Telescope
Science Institute [13184]; ASI/INAF [I/037/12/0]; PRIN INAF; CNES;
CNRS/PICS; Fondo Fortalecimiento de la Productividad Cientifica VRIDT;
EU Horizon 2020 research and innovation programme under the Marie
Sklodowska-Curie grant [655324]; iCORE program of the Planning and
Budgeting Committee [1937/12]; INAF/PICS; US NSF [AST-1008882];
Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luft- und Raumfahrt [FKZ 50 OR 1408]; VINCI program of the
French-Italian University
FX This paper is based on observations obtained with the XMM-Newton
satellite, an ESA funded mission with contributions by ESA Member States
and USA. M.C. and S.B. acknowledges financial support from the Italian
Space Agency under grant ASI-INAF I/037/12/P1. G.P. acknowledges support
via an EU Marie Curie Intra-European fellowship under contract no.
FP-PEOPLE-2012-IEF-331095. This work is based on observations obtained
with XMM-Newton, an ESA science mission with instruments and
contributions directly funded by ESA Member States and the USA (NASA).
This research has made use of data obtained with the NuSTAR mission, a
project led by the California Institute of Technology (Caltech), managed
by the Jet Propulsion Laboratory (JPL) and funded by NASA. We thank the
International Space Science Institute (ISSI) in Bern for their support
and hospitality. SRON is supported financially by NWO, the Netherlands
Organization for Scientific Research. M.M. acknowledges support from NWO
and the UK STFC. This work was supported by NASA through grants for HST
program number 13184 from the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, incorporated under NASA contract NAS5-26555. M.C.
acknowledges financial support from contracts ASI/INAF n.I/037/12/0 and
PRIN INAF 2011 and 2012. P.-O.P. acknowledges financial support from the
CNES and from the CNRS/PICS. K.C.S. acknowledges financial support from
the Fondo Fortalecimiento de la Productividad Cientifica VRIDT 2013.
E.B. received funding from the EU Horizon 2020 research and innovation
programme under the Marie Sklodowska-Curie grant agreement No. 655324,
and from the iCORE program of the Planning and Budgeting Committee
(grant No. 1937/12). S.B., G.M., and A.D.R. acknowledge INAF/PICS
financial support. G.M. and F.U. acknowledge financial support from the
Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. B.M.P.
acknowledges support from the US NSF through grant AST-1008882. G.P.
acknowledges support via an EU Marie Curie Intra-European fellowship
under contract No. FP-PEOPLE-2012-IEF-331095 and Bundesministerium fur
Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt
(BMWI/DLR, FKZ 50 OR 1408). F.U. acknowledges Ph.D. funding from the
VINCI program of the French-Italian University. M.W. acknowledges the
support of a Ph.D. studentship awarded by the UK STFC.
NR 113
TC 2
Z9 2
U1 2
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A27
DI 10.1051/0004-6361/201628464
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600122
ER
PT J
AU Comparat, J
Delubac, T
Jouvel, S
Raichoor, A
Kneib, JP
Yeche, C
Abdalla, FB
Le Cras, C
Maraston, C
Wilkinson, DM
Zhu, G
Jullo, E
Prada, F
Schlegel, D
Xu, Z
Zou, H
Bautista, J
Bizyaev, D
Bolton, A
Brownstein, JR
Dawson, KS
Escoffier, S
Gaulme, P
Kinemuchi, K
Malanushenko, E
Malanushenko, V
Mariappan, V
Newman, JA
Oravetz, D
Pan, K
Percival, WJ
Prakash, A
Schneider, DP
Simmons, A
Abbott, TMC
Allam, S
Banerji, M
Benoit-Levy, A
Bertin, E
Brooks, D
Capozzi, D
Rosell, AC
Kind, MC
Carretero, J
Castander, FJ
Cunha, CE
da Costa, LN
Desai, S
Doel, P
Eifler, TF
Estrada, J
Flaugher, B
Fosalba, P
Frieman, J
Gaztanaga, E
Gerdes, DW
Gruen, D
Gruendl, RA
Gutierrez, G
Honscheid, K
James, DJ
Kuehn, K
Kuropatkin, N
Lahav, O
Lima, M
Maia, MAG
March, M
Marshall, JL
Miquel, R
Plazas, AA
Reil, K
Roe, N
Romer, AK
Roodman, A
Rykoff, ES
Sako, M
Sanchez, E
Scarpine, V
Sevilla-Noarbe, I
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Walker, AR
Zhang, Y
AF Comparat, J.
Delubac, T.
Jouvel, S.
Raichoor, A.
Kneib, J-P.
Yeche, C.
Abdalla, F. B.
Le Cras, C.
Maraston, C.
Wilkinson, D. M.
Zhu, G.
Jullo, E.
Prada, F.
Schlegel, D.
Xu, Z.
Zou, H.
Bautista, J.
Bizyaev, D.
Bolton, A.
Brownstein, J. R.
Dawson, K. S.
Escoffier, S.
Gaulme, P.
Kinemuchi, K.
Malanushenko, E.
Malanushenko, V.
Mariappan, V.
Newman, J. A.
Oravetz, D.
Pan, K.
Percival, W. J.
Prakash, A.
Schneider, D. P.
Simmons, A.
Abbott, T. M. C.
Allam, S.
Banerji, M.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Capozzi, D.
Rosell, A. Carnero
Kind, M. Carrasco
Carretero, J.
Castander, F. J.
Cunha, C. E.
da Costa, L. N.
Desai, S.
Doel, P.
Eifler, T. F.
Estrada, J.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gaztanaga, E.
Gerdes, D. W.
Gruen, D.
Gruendl, R. A.
Gutierrez, G.
Honscheid, K.
James, D. J.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Lima, M.
Maia, M. A. G.
March, M.
Marshall, J. L.
Miquel, R.
Plazas, A. A.
Reil, K.
Roe, N.
Romer, A. K.
Roodman, A.
Rykoff, E. S.
Sako, M.
Sanchez, E.
Scarpine, V.
Sevilla-Noarbe, I.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Walker, A. R.
Zhang, Y.
TI SDSS-IV eBOSS emission-line galaxy pilot survey
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE large-scale structure of Universe; galaxies: general; methods:
observational
ID OSCILLATION SPECTROSCOPIC SURVEY; DIGITAL SKY SURVEY; BARYON
ACOUSTIC-OSCILLATIONS; 1ST DATA RELEASE; DARK ENERGY; LUMINOSITY
FUNCTION; TARGET SELECTION; DATA REDUCTION; SURVEY DESIGN; SURVEY VIPERS
AB The Sloan Digital Sky Survey IV extended Baryonic Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) will observe 195 000 emission-line galaxies (ELGs) to measure the baryonic acoustic oscillation (BAO) standard ruler at redshift 0.9. To test different ELG selection algorithms, 9000 spectra were observed with the SDSS spectrograph as a pilot survey based on data from several imaging surveys. First, using visual inspection and redshift quality flags, we show that the automated spectroscopic redshifts assigned by the pipeline meet the quality requirements for a reliable BAO measurement. We also show the correlations between sky emission, signal-to-noise ratio in the emission lines, and redshift error. Then we provide a detailed description of each target selection algorithm we tested and compare them with the requirements of the eBOSS experiment. As a result, we provide reliable redshift distributions for the different target selection schemes we tested. Finally, we determine an target selection algorithms that is best suited to be applied on DECam photometry because they fulfill the eBOSS survey efficiency requirements.
C1 [Comparat, J.; Prada, F.] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain.
[Comparat, J.; Prada, F.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Delubac, T.; Kneib, J-P.] Ecole Polytech Fed Lausanne, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, Switzerland.
[Jouvel, S.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Raichoor, A.; Yeche, C.] CEA, Ctr Saclay, IRFU SPP, F-91191 Gif Sur Yvette, France.
[Kneib, J-P.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Le Cras, C.; Maraston, C.; Wilkinson, D. M.; Percival, W. J.; Capozzi, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Zhu, G.; Thomas, D.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Prada, F.] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18080 Granada, Spain.
[Schlegel, D.; Roe, N.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Xu, Z.; Zou, H.] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China.
[Bautista, J.; Bolton, A.; Brownstein, J. R.; Dawson, K. S.; Mariappan, V.] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA.
[Bizyaev, D.; Gaulme, P.; Kinemuchi, K.; Malanushenko, E.; Malanushenko, V.; Oravetz, D.; Pan, K.; Simmons, A.] Apache Point Observ, POB 59, Sunspot, NM 88349 USA.
[Bizyaev, D.; Gaulme, P.; Kinemuchi, K.; Malanushenko, E.; Malanushenko, V.; Oravetz, D.; Pan, K.; Simmons, A.] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA.
[Bizyaev, D.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia.
[Escoffier, S.] Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13388 Marseille, France.
[Newman, J. A.; Prakash, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, J. A.; Prakash, A.] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA.
[Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Abbott, T. M. C.; James, D. J.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, Casilla 603, La Serena, Chile.
[Allam, S.; Estrada, J.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Rosell, A. Carnero; da Costa, L. N.; Lima, M.; Maia, M. A. G.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Rosell, A. Carnero; da Costa, L. N.; Maia, M. A. G.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[Carretero, J.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain.
[Carretero, J.; Castander, F. J.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Cunha, C. E.; Roodman, A.; Rykoff, E. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Desai, S.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Eifler, T. F.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Gerdes, D. W.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Gruen, D.] Univ Munich, Univ Sternwarte, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Honscheid, K.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, Barcelona 08010, Spain.
[Reil, K.; Roodman, A.; Rykoff, E. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, Madrid, Spain.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
RP Comparat, J (reprint author), Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain.; Comparat, J (reprint author), Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
EM j.comparat@csic.es
RI Lima, Marcos/E-8378-2010; Gaztanaga, Enrique/L-4894-2014;
OI Gaztanaga, Enrique/0000-0001-9632-0815; Abdalla,
Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658
FU Spanish MICINNs Consolider-Ingenio Programme [MultiDark CSD2009-00064];
MINECO Centro de Excelencia Severo Ochoa Programme [SEV-2012-0249,
FPA2012-34694, AYA2014-60641-C2-1-P, AYA2012-31101]; spanish MEC
Salvador de Madariaga program [PRX14/00444]; LIDA ERC advanced grant;
P2IO LabEx in the framework Investissements d'Avenir [ANR-10-LABX-0038,
ANR-11-IDEX-0003-01]; CNRS; Labex OCEVU; Alfred P. Sloan Foundation; US
Department of Energy Office of Science; Center for High-Performance
Computing at the University of Utah; US 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; Center for Cosmology and Astro-Particle Physics
at the Ohio State University; Mitchell Institute for Fundamental Physics
and Astronomy at Texas AM University; Financiadora de Estudos e
Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do
Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche
Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy
Survey; National Science Foundation [AST-1138766]; MINECO
[AYA2012-39559, ESP-2013-48274, FPA2013-47986]; Centro de Excelencia
Severo Ochoa [SEV-2012-0234]; European Research Council under the
European Union's Seventh Framework Programme (FP7) including ERC grant
[240672, 291329, 306478]; National Aeronautics and Space Administration;
National Science Foundation; Carnegie Institution for Science, Carnegie
Mellon University; Chilean Participation Group; French Participation
Group; Harvard-Smithsonian Center for Astrophysics; Instituto de
Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for
the Physics and Mathematics of the Universe (IPMU)/University of Tokyo;
Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik
Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg);
Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut
fur Extraterrestrische Physik (MPE); National Astronomical Observatory
of China; New Mexico State University; New York University; University
of Notre Dame; Observatario Nacional/MCTI; Ohio State University;
Pennsylvania State University; Shanghai Astronomical Observatory; United
Kingdom Participation Group; Universidad Nacional Autonoma de Mexico;
University of Arizona; University of Colorado Boulder; University of
Portsmouth; University of Utah; University of Virginia; University of
Washington; University of Wisconsin; Vanderbilt University; Yale
University; Brazilian Participation Group
FX J.C. and F.P. acknowledge support from the Spanish MICINNs
Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064,
MINECO Centro de Excelencia Severo Ochoa Programme under the grants
SEV-2012-0249, FPA2012-34694, and the projects AYA2014-60641-C2-1-P and
AYA2012-31101. We also thank the Lawrence Berkeley National Laboratory
for its hospitality. F.P. acknowledges the spanish MEC Salvador de
Madariaga program, Ref. PRX14/00444. T.D. and J.P.K. acknowledge support
from the LIDA ERC advanced grant. AR acknowledges funding from the P2IO
LabEx (ANR-10-LABX-0038) in the framework Investissements d'Avenir
(ANR-11-IDEX-0003-01) managed by the French National Research Agency
(ANR). E.J. acknowledges the support of CNRS and the Labex OCEVU. This
paper represents an effort by the SDSS-III, SDSS-IV and DES
collaborations. Funding for SDSS-III was 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
web site is www.sdss.org. SDSS-IV acknowledges support and resources
from the Center for High-Performance Computing at the University of
Utah. SDSS-IV is managed by the Astrophysical Research Consortium for
the Participating Institutions of the SDSS Collaboration including the
Brazilian Participation Group, the Carnegie Institution for Science,
Carnegie Mellon University, the Chilean Participation Group, the French
Participation Group, Harvard-Smithsonian Center for Astrophysics,
Instituto de Astrofisica de Canarias, The Johns Hopkins University,
Kavli Institute for the Physics and Mathematics of the Universe
(IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory,
Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur
Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA
Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE),
National Astronomical Observatory of China, New Mexico State University,
New York University, University of Notre Dame, Observatario
Nacional/MCTI, The Ohio State University, Pennsylvania State University,
Shanghai Astronomical Observatory, United Kingdom Participation Group,
Universidad Nacional Autonoma de Mexico, University of Arizona,
University of Colorado Boulder, University of Portsmouth, University of
Utah, University of Virginia, University of Washington, University of
Wisconsin, Vanderbilt University, Yale University and the french
participation group. Funding for the DES Projects has been provided by
the US 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, the Center for
Cosmology and Astro-Particle Physics at the Ohio State University, the
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M
University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas
Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho
Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio
da Ciencia, Tecnologia e Inovacao, 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 University of Edinburgh, the
Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National
Accelerator Laboratory, 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 Munchen 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. The DES data
management system is supported by the National Science Foundation under
Grant Number AST-1138766. The DES participants from Spanish institutions
are partially supported by MINECO under grants AYA2012-39559,
ESP-2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa
SEV-2012-0234. Research leading to these results has received funding
from the European Research Council under the European Union's Seventh
Framework Programme (FP7/2007-2013) including ERC grant agreements
240672, 291329, and 306478. We are grateful for the extraordinary
contributions of our CTIO colleagues and the DECam Construction,
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 group. This paper includes targets
derived from the images of 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 paper
has gone through internal review by the DES collaboration.
NR 60
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U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A121
DI 10.1051/0004-6361/201527377
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600039
ER
PT J
AU Cruz-Diaz, GA
Martin-Domenech, R
Caro, GMM
Chen, YJ
AF Cruz-Diaz, G. A.
Martin-Domenech, R.
Munoz Caro, G. M.
Chen, Y. -J.
TI Negligible photodesorption of methanol ice and active photon-induced
desorption of its irradiation products
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ultraviolet: ISM; astrochemistry; ISM: molecules; methods: laboratory:
molecular; molecular processes
ID ABSORPTION CROSS-SECTIONS; VACUUM-UV SPECTROSCOPY; CO ICE;
MOLECULAR-DYNAMICS; SOLID METHANOL; INFRARED-SPECTROSCOPY;
THERMAL-DESORPTION; INTERSTELLAR DUST; ORGANIC-MOLECULES;
ELECTRON-IMPACT
AB Context. Methanol is a common component of interstellar and circumstellar ice mantles and is often used as an evolution indicator in star-forming regions. The observations of gas-phase methanol in the interiors of dense molecular clouds at temperatures as low as 10 K suggest that non-thermal ice desorption must be active. Ice photodesorption has been proposed to explain the abundances of gas-phase molecules toward the coldest regions.
Aims. Laboratory experiments were performed to investigate the potential photodesorption of methanol toward the coldest regions.
Methods. Solid methanol was deposited at 8 K and UV-irradiated at various temperatures starting from 8 K. The irradiation of the ice was monitored by means of infrared spectroscopy and the molecules in the gas phase were detected using quadrupole mass spectroscopy. Fully deuterated methanol was used for confirmation of the results.
Results. The photodesorption of methanol to the gas phase was not observed in the mass spectra at different irradiation temperatures. We estimate an upper limit of 3 x 10(-5) molecules per incident photon. On the other hand, photon-induced desorption of the main photoproducts was clearly observed.
Conclusions. The negligible photodesorption of methanol could be explained by the ability of UV-photons in the 114-180 nm (10.87-6.88 eV) range to dissociate this molecule efficiently. Therefore, the presence of gas-phase methanol in the absence of thermal desorption remains unexplained. On the other hand, we find CH4 to desorb from irradiated methanol ice, which was not found to desorb in the pure CH4 ice irradiation experiments.
C1 [Cruz-Diaz, G. A.; Martin-Domenech, R.; Munoz Caro, G. M.] INTA CSIC, Ctr Astrobiol, Carretera Ajalvir Km 4, Madrid 28850, Spain.
[Cruz-Diaz, G. A.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Cruz-Diaz, G. A.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Chen, Y. -J.] Natl Cent Univ, Dept Phys, Jhongli 32054, Taoyuan County, Taiwan.
RP Cruz-Diaz, GA (reprint author), INTA CSIC, Ctr Astrobiol, Carretera Ajalvir Km 4, Madrid 28850, Spain.; Cruz-Diaz, GA (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.; Cruz-Diaz, GA (reprint author), Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
EM gustavo.a.cruzdiaz@nasa.gov; munozcg@cab.inta-csic.es
RI Munoz Caro, Guillermo /L-6370-2014;
OI Munoz Caro, Guillermo /0000-0001-7003-7368; Cruz-Diaz, Gustavo
Adolfo/0000-0003-2270-6103
FU Spanish MINECO [AYA2011-29375, AYA2014-60585-P]; CONSOLIDER grant
[CSD2009-00038]; NSC [NSC99-2112-M-008-011-MY3,
NSC99-2923-M-008-011-MY3]; NSF Planetary Astronomy Program [AST-1108898]
FX This research was financed by the Spanish MINECO under project
AYA2011-29375, AYA2014-60585-P, and CONSOLIDER grant CSD2009-00038. This
work was partially supported by NSC grants NSC99-2112-M-008-011-MY3 and
NSC99-2923-M-008-011-MY3, and the NSF Planetary Astronomy Program under
Grant AST-1108898.
NR 76
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A68
DI 10.1051/0004-6361/201526761
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600010
ER
PT J
AU Davidsson, BJR
Sierks, H
Guttler, C
Marzari, F
Pajola, M
Rickman, H
A'Hearn, MF
Auger, AT
El-Maarry, MR
Fornasier, S
Gutierrez, PJ
Keller, HU
Massironi, M
Snodgrass, C
Vincent, JB
Barbieri, C
Lamy, PL
Rodrigo, R
Koschny, D
Barucci, MA
Bertaux, JL
Bertini, I
Cremonese, G
Da Deppo, V
Debei, S
De Cecco, M
Feller, C
Fulle, M
Groussin, O
Hviid, SF
Hofner, S
Ip, WH
Jorda, L
Knollenberg, J
Kovacs, G
Kramm, JR
Kuhrt, E
Kuppers, M
La Forgia, F
Lara, LM
Lazzarin, M
Lopez Moreno, JJ
Moissl-Fraund, R
Mottola, S
Naletto, G
Oklay, N
Thomas, N
Tubiana, C
AF Davidsson, B. J. R.
Sierks, H.
Guettler, C.
Marzari, F.
Pajola, M.
Rickman, H.
A'Hearn, M. F.
Auger, A. -T.
El-Maarry, M. R.
Fornasier, S.
Gutierrez, P. J.
Keller, H. U.
Massironi, M.
Snodgrass, C.
Vincent, J. -B.
Barbieri, C.
Lamy, P. L.
Rodrigo, R.
Koschny, D.
Barucci, M. A.
Bertaux, J. -L.
Bertini, I.
Cremonese, G.
Da Deppo, V.
Debei, S.
De Cecco, M.
Feller, C.
Fulle, M.
Groussin, O.
Hviid, S. F.
Hoefner, S.
Ip, W. -H.
Jorda, L.
Knollenberg, J.
Kovacs, G.
Kramm, J. -R.
Kuehrt, E.
Kueppers, M.
La Forgia, F.
Lara, L. M.
Lazzarin, M.
Lopez Moreno, J. J.
Moissl-Fraund, R.
Mottola, S.
Naletto, G.
Oklay, N.
Thomas, N.
Tubiana, C.
TI The primordial nucleus of comet 67P/Churyumov-Gerasimenko
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: individual: 67P/Churyumov-Gerasimenko; Kuiper belt: general;
protoplanetary disks
ID JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; EARLY SOLAR-SYSTEM;
TRANS-NEPTUNIAN REGION; SPITZER-SPACE-TELESCOPE; SHORT-PERIOD COMETS;
GASEOUS PROTOPLANETARY DISK; SIZE-FREQUENCY DISTRIBUTION; SHORT-LIVED
RADIOISOTOPES; NON-GRAVITATIONAL FORCES
AB Context. We investigate the formation and evolution of comet nuclei and other trans-Neptunian objects (TNOs) in the solar nebula and primordial disk prior to the giant planet orbit instability foreseen by the Nice model.
Aims. Our goal is to determine whether most observed comet nuclei are primordial rubble-pile survivors that formed in the solar nebula and young primordial disk or collisional rubble piles formed later in the aftermath of catastrophic disruptions of larger parent bodies. We also propose a concurrent comet and TNO formation scenario that is consistent with observations.
Methods. We used observations of comet 67P/Churyumov-Gerasimenko by the ESA Rosetta spacecraft, particularly by the OSIRIS camera system, combined with data from the NASA Stardust sample-return mission to comet 81P/Wild 2 and from meteoritics; we also used existing observations from ground or from spacecraft of irregular satellites of the giant planets, Centaurs, and TNOs. We performed modeling of thermophysics, hydrostatics, orbit evolution, and collision physics.
Results. We find that thermal processing due to short-lived radionuclides, combined with collisional processing during accretion in the primordial disk, creates a population of medium-sized bodies that are comparably dense, compacted, strong, heavily depleted in supervolatiles like CO and CO2; they contain little to no amorphous water ice, and have experienced extensive metasomatism and aqueous alteration due to liquid water. Irregular satellites Phoebe and Himalia are potential representatives of this population. Collisional rubble piles inherit these properties from their parents. Contrarily, comet nuclei have low density, high porosity, weak strength, are rich in supervolatiles, may contain amorphous water ice, and do not display convincing evidence of in situ metasomatism or aqueous alteration. We outline a comet formation scenario that starts in the solar nebula and ends in the primordial disk, that reproduces these observed properties, and additionally explains the presence of extensive layering on 67P/Churyumov-Gerasimenko (and on 9P/Tempel 1 observed by Deep Impact), its bi-lobed shape, the extremely slow growth of comet nuclei as evidenced by recent radiometric dating, and the low collision probability that allows primordial nuclei to survive the age of the solar system.
Conclusions. We conclude that observed comet nuclei are primordial rubble piles, and not collisional rubble piles. We argue that TNOs formed as a result of streaming instabilities at sizes below similar to 400 km and that similar to 350 of these grew slowly in a low-mass primordial disk to the size of Triton, Pluto, and Eris, causing little viscous stirring during growth. We thus propose a dynamically cold primordial disk, which prevented medium-sized TNOs from breaking into collisional rubble piles and allowed the survival of primordial rubble-pile comets. We argue that comets formed by hierarchical agglomeration out of material that remained after TNO formation, and that this slow growth was a necessity to avoid thermal processing by short-lived radionuclides that would lead to loss of supervolatiles, and that allowed comet nuclei to incorporate similar to 3 Myr old material from the inner solar system.
C1 [Davidsson, B. J. R.; Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Davidsson, B. J. R.] Jet Prop Lab, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Sierks, H.; Guettler, C.; A'Hearn, M. F.; Vincent, J. -B.; Hoefner, S.; Kovacs, G.; Kramm, J. -R.; Oklay, N.; Tubiana, C.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Marzari, F.] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy.
[Pajola, M.; Massironi, M.; Bertini, I.] Univ Padua, Ctr Ateneo Studi & Attivita Spaziali Giuseppe Col, Via Venezia 15, I-35131 Padua, Italy.
[Rickman, H.] PAN Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[A'Hearn, M. F.] Akad Wissensch Gottingen, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Auger, A. -T.; Groussin, O.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[El-Maarry, M. R.; Thomas, N.] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Fornasier, S.; Barucci, M. A.; Feller, C.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France.
[Gutierrez, P. J.; Lara, L. M.; Lopez Moreno, J. J.] CSIC, Inst Astrofis Andalucia, C Glorieta Astron S-N, E-18008 Granada, Spain.
[Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, Mendelssohnstr 3, D-38106 Braunschweig, Germany.
[Massironi, M.] Univ Padua, Dipartimento Geosci, I-35131 Padua, Italy.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Barbieri, C.] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Lamy, P. L.; Jorda, L.] CNRS, Lab Astrophys Marseille, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Lamy, P. L.; Jorda, L.] Aix Marseille Univ, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Rodrigo, R.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Rodrigo, R.] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Koschny, D.] ESA, European Space Res & Technol Ctr, Sci Support Off, Keplerlaan 1,Postbus 299, NL-2201 AZ Noordwijk, Netherlands.
[Bertaux, J. -L.] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Cremonese, G.] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Da Deppo, V.] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[Debei, S.] Univ Padua, Dept Ind Engn, Via Venezia 1, I-35131 Padua, Italy.
[De Cecco, M.] Univ Trento, Via Mesiano 77, I-38100 Trento, Italy.
[Feller, C.] Univ Paris Diderot, Sorbonne Paris Cite, 4 Rue Elsa Morante, F-75205 Paris 13, France.
[Fulle, M.] INAF, Osservatorio Astron, I-34014 Trieste, Italy.
[Hviid, S. F.; Knollenberg, J.; Kuehrt, E.; Mottola, S.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, Rutherfordstr 2, D-12489 Berlin, Germany.
[Ip, W. -H.] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan.
[Kueppers, M.; Mottola, S.] ESA, European Space Astron Ctr, Operat Dept, POB 78, Madrid 28691, Spain.
[Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
RP Davidsson, BJR (reprint author), Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.; Davidsson, BJR (reprint author), Jet Prop Lab, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bjorn.davidsson@jp1.nasa.gov
RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014;
OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez,
Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi,
Matteo/0000-0002-7757-8818
FU national funding agency of Germany (DLR); national funding agency of
France (CNES); national funding agency of Italy (ASI); national funding
agency of Spain (MEC); national funding agency of Sweden (SNSB);
national funding agency of ESA Technical Directorate
FX We are grateful to Paul Weissman and an anonymous referee for their
comments that substantially improved our paper. We thank Bastian
Gundlach and Jurgen Blum for sharing unpublished results from their
laboratory measurements. OSIRIS was built by a consortium led by the
Max-Planck-Institut fur Sonnensystemforschung, Gottingen, Germany, in
collaboration with CISAS, University of Padova, Italy, the Laboratoire
d'Astrophysique de Marseille, France, the Instituto de Astrofisica de
Andalucia, CSIC, Granada, Spain, the Scientific Support Office of the
European Space Agency, Noordwijk, The Netherlands, the Instituto
Nacional de Tecnica Aeroespacial, Madrid, Spain, the Universidad
Politechnica de Madrid, Spain, the Department of Physics and Astronomy
of Uppsala University, Sweden, and the Institut fur Datentechnik und
Kommunikationsnetze der Technischen Universitat Braunschweig, Germany.
The support of the national funding agencies of Germany (DLR), France
(CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical
Directorate is gratefully acknowledged. We thank the Rosetta Science
Ground Segment at ESAC, the Rosetta Mission Operations Centre at ESOC,
and the Rosetta Project at ESTEC for their outstanding work enabling the
science return of the Rosetta Mission.
NR 341
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A63
DI 10.1051/0004-6361/201526968
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600023
ER
PT J
AU Ferretti, R
Amanullah, R
Goobar, A
Johansson, J
Vreeswijk, PM
Butler, RP
Cao, Y
Cenko, SB
Doran, G
Filippenko, AV
Freeland, E
Hosseinzadeh, G
Howell, DA
Lundqvist, P
Mattila, S
Nordin, J
Nugent, PE
Petrushevska, T
Valenti, S
Vogt, S
Wozniak, P
AF Ferretti, R.
Amanullah, R.
Goobar, A.
Johansson, J.
Vreeswijk, P. M.
Butler, R. P.
Cao, Y.
Cenko, S. B.
Doran, G.
Filippenko, A. V.
Freeland, E.
Hosseinzadeh, G.
Howell, D. A.
Lundqvist, P.
Mattila, S.
Nordin, J.
Nugent, P. E.
Petrushevska, T.
Valenti, S.
Vogt, S.
Wozniak, P.
TI Time-varying sodium absorption in the Type Ia supernova 2013gh
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE supernovae: general; supernovae: individual: SN 2013gh; dust;
extinction; circumstellar matter; supernovae: individual: iPTF 13dge
ID SN 2014J; CIRCUMSTELLAR MATERIAL; INFRARED-EMISSION; DUST EXTINCTION;
RADIO-EMISSION; LIGHT CURVES; ULTRAVIOLET; TELESCOPE; M82; SPECTRA
AB Context. Temporal variability of narrow absorption lines in high-resolution spectra of Type Ia supernovae (SNe Ia) is studied to search for circumstellar matter. Time series which resolve the profiles of absorption lines such as Na I D or Ca II H&K are expected to reveal variations due to photoionisation and subsequent recombination of the gases. The presence, composition, and geometry of circumstellar matter may hint at the elusive progenitor system of SNe Ia and could also affect the observed reddening law.
Aims. To date, there are few known cases of time-varying Na I D absorption in SNe Ia, all of which occurred during relatively late phases of the supernova (SN) evolution. Photoionisation, however, is predicted to occur during the early phases of SNe Ia, when the supernovae peak in the ultraviolet. We attempt, therefore, to observe early-time absorption-line variations by obtaining high-resolution spectra of SNe before maximum light.
Methods. We have obtained photometry and high-resolution spectroscopy of SNe Ia 2013gh and iPTF 13dge, to search for absorption-line variations. Furthermore, we study interstellar absorption features in relation to the observed photometric colours of the SNe.
Results. Both SNe display deep Na I D and Ca II H&K absorption features. Furthermore, small but significant variations are detected in a feature of the Na I D profile of SN 2013gh. The variations are consistent with either geometric effects of rapidly moving or patchy gas clouds or photoionisation of Na I gas at R approximate to 10(19) cm from the explosion.
Conclusions. Our analysis indicates that it is necessary to focus on early phases to detect photoionisation effects of gases in the circumstellar medium of SNe Ia. Different absorbers such as Na I and Ca II can be used to probe for matter at different distances from the SNe. The nondetection of variations during early phases makes it possible to put limits on the abundance of the species at those distances.
C1 [Ferretti, R.; Amanullah, R.; Goobar, A.; Petrushevska, T.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, S-10692 Stockholm, Sweden.
[Johansson, J.; Vreeswijk, P. M.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel.
[Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Cao, Y.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Cenko, S. B.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
[Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Doran, G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Freeland, E.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Hosseinzadeh, G.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Hosseinzadeh, G.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Mattila, S.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaisalantie 20, Piikkio 21500, Finland.
[Mattila, S.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, Piikkio 21500, Finland.
[Mattila, S.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Nordin, J.] Humboldt Univ, Inst Phys, Newtonstr 15, D-12589 Berlin, Germany.
[Nugent, P. E.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd,MS 50B-4206, Berkeley, CA 94720 USA.
[Valenti, S.] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA.
[Vogt, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Wozniak, P.] Los Alamos Natl Lab, MS D436, Los Alamos, NM 87545 USA.
RP Ferretti, R (reprint author), Stockholm Univ, Dept Phys, Oskar Klein Ctr, S-10692 Stockholm, Sweden.
EM raphael.ferretti@fysik.su.se
RI Butler, Robert/B-1125-2009;
OI Hosseinzadeh, Griffin/0000-0002-0832-2974; Wozniak,
Przemyslaw/0000-0002-9919-3310
FU Swedish Research Council; Swedish Space Board; US NSF [AST-1211916];
TABASGO Foundation; Christopher R. Redlich Fund; European Organisation
for Astronomical Research in the Southern Hemisphere under ESO programme
[091.D-0352(A)]; NASA's Astrophysics Data Analysis Program [NNX13AF35G];
W. M. Keck 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 program
FX We would like to thank Alexis Brandeker for assisting us with the UVES
data, Jesper Sollerman for his helpful comments, and Daniela Vergani for
sharing graphs of the VLA H I data. R.A. and A.G. acknowledge support
from the Swedish Research Council and the Swedish Space Board. The Oskar
Klein Centre is funded by the Swedish Research Council. A.V.F.'s
research was funded by US NSF grant AST-1211916, the TABASGO Foundation,
and the Christopher R. Redlich Fund. This work is based on observations
collected at the European Organisation for Astronomical Research in the
Southern Hemisphere under ESO programme 091.D-0352(A). We made use of
Swift/UVOT data reduced by P. J. Brown and released in the Swift
Optical/Ultraviolet Supernova Archive (SOUSA). SOUSA is supported by
NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. This
work is based on observations made with the Nordic Optical Telescope,
operated by the Nordic Optical Telescope Scientific Association at the
Observatorio del Roque de los Muchachos, La Palma, Spain, of the
Instituto de Astrofisica de Canarias. The data presented here were
obtained in part with ALFOSC, which is provided by the Instituto de
Astrofisica de Andalucia (IAA) under a joint agreement with the
University of Copenhagen and NOTSA. This work makes use of observations
from the LCOGT network. 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 recognise 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 research
used resources of the National Energy Research Scientific Computing
Center, a DOE Office of Science User Facility supported by the Office of
Science of the US Department of Energy under Contract No.
DE-AC02-05CH11231. LANL participation in iPTF was funded by the US
Department of Energy as part of the Laboratory Directed Research and
Development program. A portion of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 69
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A40
DI 10.1051/0004-6361/201628351
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600108
ER
PT J
AU Iwasawa, K
Fabian, AC
Kara, E
Reynolds, CS
Miniutti, G
Tombesi, F
AF Iwasawa, K.
Fabian, A. C.
Kara, E.
Reynolds, C. S.
Miniutti, G.
Tombesi, F.
TI Highly ionized disc and transient outflows in the Seyfert galaxy IRAS
18325-5926
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; SUPERMASSIVE BLACK-HOLES;
SHELL ABSORPTION-LINES; ULTRA-FAST OUTFLOWS; IRON K EMISSION; OPTICAL
CLASSIFICATION; ACCRETION DISKS; QUASAR; PHOTOIONIZATION
AB We report on strong X-ray variability and the Fe K-band spectrum of the Seyfert galaxy IRAS 18325-5926 obtained from the 2001 XMM-Newton EPIC pn observation with a duration of similar to 120 ks. While the X-ray source is highly variable, the 8-10 keV band shows larger variability than that of the lower energies. Amplified 8-10 keV flux variations are associated with two prominent flares of the X-ray source during the observation. The Fe K emission is peaked at 6.6 keV with moderate broadening. It is likely to originate from a highly ionized disc with an ionization parameter of log xi similar or equal to 3. The Fe K line flux responds to the main flare, which supports its disc origin. A short burst of the Fe line flux has no relation to the continuum brightness, for which we have no clear explanation. We also find transient, blueshifted Fe K absorption features that can be identified with high-velocity (similar to 0.2 c) outflows of highly ionized gas, as found in other active galaxies. The deepest absorption feature appears only briefly (similar to 1 h) at the onset of the main flare and disappears when the flare declines. The rapid evolution of the absorption spectrum makes this source peculiar among the active galaxies with high-velocity outflows. Another detection of the absorption feature also precedes the other flare. The variability of the absorption feature partly accounts for the excess variability in the 8-10 keV band where the absorption feature appears. Although no reverberation measurement is available, the black hole mass of similar to 2 x 10(6) M-circle dot is inferred from the X-ray variability. When this mass is assumed, the black hole is accreting at around the Eddington limit, which may fit the highly ionized disc and strong outflows observed in this galaxy.
C1 [Iwasawa, K.] Univ Barcelona, IEEC, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain.
[Iwasawa, K.] ICREA, Pg Lluis Companys 23, Barcelona 08010, Spain.
[Fabian, A. C.; Kara, E.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Kara, E.; Reynolds, C. S.; Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Miniutti, G.] CSIC, INTA, ESAC, Ctr Astrobiol,Dept Astrofis, POB 78, Madrid 28691, Spain.
[Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RP Iwasawa, K (reprint author), Univ Barcelona, IEEC, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain.; Iwasawa, K (reprint author), ICREA, Pg Lluis Companys 23, Barcelona 08010, Spain.
EM kazushi.iwasawa@icc.ub.edu
RI Miniutti, Giovanni/L-2721-2014
OI Miniutti, Giovanni/0000-0003-0707-4531
FU Spanish MINECO [AYA2013-47447-C3-2-P]; ICCUB (Unidad de Excelencia
"Maria de Maeztu") [MDM-2014-0369]
FX KI acknowledges support by the Spanish MINECO under grant
AYA2013-47447-C3-2-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia
"Maria de Maeztu").
NR 47
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A98
DI 10.1051/0004-6361/201528030
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600076
ER
PT J
AU Jaimes, RF
Bramich, DM
Kains, N
Skottfelt, J
Jorgensen, UG
Horne, K
Dominik, M
Alsubai, KA
Bozza, V
Burgdorf, MJ
Novati, SC
Ciceri, S
D'Ago, G
Evans, DF
Galianni, P
Gu, SH
Harpsoe, KBW
Haugbolle, T
Hinse, TC
Hundertmark, M
Juncher, D
Kerins, E
Korhonen, H
Kuffmeier, M
Mancini, L
Peixinho, N
Popovas, A
Rabus, M
Rahvar, S
Scarpetta, G
Schmidt, RW
Snodgrass, C
Southworth, J
Starkey, D
Street, RA
Surdej, J
Tronsgaar, R
Unda-Sanzana, E
von Essen, C
Wang, XB
Wertz, O
AF Jaimes, R. Figuera
Bramich, D. M.
Kains, N.
Skottfelt, J.
Jorgensen, U. G.
Horne, K.
Dominik, M.
Alsubai, K. A.
Bozza, V.
Burgdorf, M. J.
Novati, S. Calchi
Ciceri, S.
D'Ago, G.
Evans, D. F.
Galianni, P.
Gu, S. -H.
Harpsoe, K. B. W.
Haugbolle, T.
Hinse, T. C.
Hundertmark, M.
Juncher, D.
Kerins, E.
Korhonen, H.
Kuffmeier, M.
Mancini, L.
Peixinho, N.
Popovas, A.
Rabus, M.
Rahvar, S.
Scarpetta, G.
Schmidt, R. W.
Snodgrass, C.
Southworth, J.
Starkey, D.
Street, R. A.
Surdej, J.
Tronsgaar, R.
Unda-Sanzana, E.
von Essen, C.
Wang, X. -B.
Wertz, O.
CA MiNDSTEp Consortium
TI Many new variable stars discovered in the core of the globular cluster
NGC 6715 (M54) with EMCCD observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atmospheric effects; instrumentation: high angular resolution; globular
clusters: individual: NGC 6715 (M54); methods: observational; stars:
variables: general; stars: variables: RR Lyrae
ID SAGITTARIUS DWARF GALAXY; RR-LYRAE VARIABLES; DIFFERENCE IMAGE-ANALYSIS;
CROWDED CENTRAL REGION; SPHEROIDAL GALAXY; ACS SURVEY; OOSTERHOFF
DICHOTOMY; DYNAMICAL MODELS; GALACTIC BULGE; BLACK-HOLE
AB Context. We show the benefits of using electron-multiplying CCDs and the shift-and-add technique as a tool to minimise the effects of atmospheric turbulence, such as blending between stars in crowded fields, and to avoid saturated stars in the fields observed. We intend to complete, or improve on, the census of the variable star population in globular cluster NGC 6715.
Aims. Our aim is to obtain high-precision time-series photometry of the very crowded central region of this stellar system via the collection of better angular resolution images than has been previously achieved with conventional CCDs on ground-based telescopes.
Methods. Observations were carried out using the Danish 1.54-m telescope at the ESO La Silla observatory in Chile. The telescope is equipped with an electron-multiplying CCD that enables short-exposure-time images to be obtained (ten images per second) that were stacked using the shift-and-add technique to produce the normal-exposure-time images (minutes). The high precision photometry was performed via difference image analysis employing the DanDIA pipeline. We attempted automatic detection of variable stars in the field.
Results. We statistically analysed the light curves of 1405 stars in the crowded central region of NGC 6715 to automatically identify the variable stars present in this cluster. We found light curves for 17 previously known variable stars near the edges of our reference image (16 RR Lyrae and 1 semi-regular) and we discovered 67 new variables (30 RR Lyrae, 21 irregular (long-period type), 3 semi-regular, 1 W Virginis, 1 eclipsing binary, and 11 unclassified). Photometric measurements for these stars are available in electronic form through the Strasbourg Astronomical Data Centre.
C1 [Jaimes, R. Figuera; Horne, K.; Dominik, M.; Galianni, P.; Hundertmark, M.; Starkey, D.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Jaimes, R. Figuera] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Bramich, D. M.; Alsubai, K. A.] HBKU, Qatar Fdn, QEERI, Doha, Qatar.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Skottfelt, J.; Jorgensen, U. G.; Harpsoe, K. B. W.; Haugbolle, T.; Hundertmark, M.; Juncher, D.; Korhonen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Skottfelt, J.; Jorgensen, U. G.; Haugbolle, T.; Hundertmark, M.; Juncher, D.; Korhonen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Kains, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2 132, I-84084 Fisciano, Italy.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Novati, S. Calchi] CALTECH, NASA, Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
[Novati, S. Calchi; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, Italy.
[Mancini, L.; Rabus, M.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Gu, S. -H.; Wang, X. -B.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
[Gu, S. -H.; Wang, X. -B.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
[Hinse, T. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, Piikkio 21500, Finland.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Schmidt, R. W.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Snodgrass, C.] Max Planck Inst Solar Syst, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Street, R. A.] Global Telescope Network, Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 9c, B-4000 Liege, Belgium.
[Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Manes Vej 30, DK-2100 Copenhagen O, Denmark.
[Ciceri, S.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Burgdorf, M. J.] Univ Hamburg, Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany.
[Peixinho, N.; Unda-Sanzana, E.] Univ Antofagasta, Fac Cs Bas, Unidad Astron, Av U Antofagasta, Antofagasta 02800, Chile.
[Peixinho, N.] Univ Coimbra, Astron Observ, Ctr Earth & Space Sci Res, CITEUC 20, P-3040004 Coimbra, Portugal.
[Kerins, E.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Tronsgaar, R.; von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
RP Jaimes, RF (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
EM robertofiguera@gmail.com
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016
OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago, Giuseppe/0000-0001-9697-7331
FU Danish Natural Science Foundation (FNU); NPRP from the Qatar National
Research Fund (a member of Qatar Foundation) [X-019-1-006]; STFC
[ST/M001296/1]; POR-FSE Campania; UK Science and Technology Facilities
Council; Sapere Aude Starting Grant from the Danish Council for
Independent Research; Danish National Research Foundation; Korea
Research Council of Fundamental Science & Technology (KRCF) via the KRCF
Young Scientist Research Fellowship; KASI [2013-9-400-00, 2014-1-400-06,
2015-1-850-04]; Gemini-Conicyt Fund [32120036]; Portuguese FCT -
Foundation for Science and Technology; European Social Fund
[SFRH/BGCT/113686/2015]; National Funds through FCT - Foundation for
Science and Technology [UID/Multi/00611/2013]; FEDER - European Regional
Development Fund through COMPETE - Operational Programme Competitiveness
and Internationalisation [POCI-01-0145-FEDER-006922]; Communaute
francaise de Belgique - Actions de recherche concertees - Academie
Wallonie-Europe
FX Our thanks go to Christine Clement for clarifying the known variable
star content in NGC 6715 and the numbering systems of the variable stars
while we were working on these clusters. This support to the
astronomical community is very much appreciated. The Danish 1.54 m
telescope is operated based on a grant from the Danish Natural Science
Foundation (FNU). This publication was made possible by NPRP grant #
X-019-1-006 from the Qatar National Research Fund (a member of Qatar
Foundation). The statements made herein are solely the responsibility of
the authors. K.H. acknowledges support from STFC grant ST/M001296/1.
G.D. acknowledges Regione Campania for support from POR-FSE Campania
2014-2020. D.F.E. is funded by the UK Science and Technology Facilities
Council. T.H. is supported by a Sapere Aude Starting Grant from the
Danish Council for Independent Research. Research at Centre for Star and
Planet Formation is funded by the Danish National Research Foundation.
T.C.H. acknowledges support from the Korea Research Council of
Fundamental Science & Technology (KRCF) via the KRCF Young Scientist
Research Fellowship. Programme and for financial support from KASI
travel grant number 2013-9-400-00, 2014-1-400-06 & 2015-1-850-04. N.P.
acknowledges funding by the Gemini-Conicyt Fund, allocated to project
No. 32120036 and by the Portuguese FCT - Foundation for Science and
Technology and the European Social Fund (ref: SFRH/BGCT/113686/2015).
CITEUC is funded by National Funds through FCT - Foundation for Science
and Technology (project: UID/Multi/00611/2013) and FEDER - European
Regional Development Fund through COMPETE 2020 - Operational Programme
Competitiveness and Internationalisation (project:
POCI-01-0145-FEDER-006922). OW and J. Surdej acknowledge support from
the Communaute francaise de Belgique - Actions de recherche concertees -
Academie Wallonie-Europe. This work has made extensive use of the ADS
and SIMBAD services, for which we are thankful.
NR 65
TC 0
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U1 4
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A120
DI 10.1051/0004-6361/201628864
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600165
ER
PT J
AU Pajola, M
Lucchetti, A
Vincent, JB
Oklay, N
El-Maarry, MR
Bertini, I
Naletto, G
Lazzarin, M
Massironi, M
Sierks, H
Barbieri, C
Lamy, P
Rodrigo, R
Koschny, D
Rickman, H
Keller, HU
Agarwal, J
A'Hearn, MF
Barucci, MA
Bertaux, JL
Boudreault, S
Cremonese, G
Da Deppo, V
Davidsson, B
Debei, S
De Cecco, M
Deller, J
Fornasier, S
Fulle, M
Gicquel, A
Groussin, O
Gutierrez, PJ
Guttler, C
Hofmann, M
Hofner, S
Hviid, SF
Ip, WH
Jorda, L
Knollenberg, J
Kramm, JR
Kuhrt, E
Kuppers, M
La Forgia, F
Lara, LM
Lee, JC
Lin, ZY
Moreno, JJL
Marzari, F
Michalik, H
Mottola, S
Preusker, F
Scholten, F
Thomas, N
Toth, I
Tubiana, C
AF Pajola, Maurizio
Lucchetti, Alice
Vincent, Jean-Baptiste
Oklay, Nilda
El-Maarry, Mohamed R.
Bertini, Ivano
Naletto, Giampiero
Lazzarin, Monica
Massironi, Matteo
Sierks, Holger
Barbieri, Cesare
Lamy, Philippe
Rodrigo, Rafael
Koschny, Detlef
Rickman, Hans
Keller, Horst U.
Agarwal, Jessica
A'Hearn, Michael F.
Barucci, Maria A.
Bertaux, Jean-Loup
Boudreault, Steve
Cremonese, Gabriele
Da Deppo, Vania
Davidsson, Bjorn
Debei, Stefano
De Cecco, Mariolino
Deller, Jakob
Fornasier, Sonia
Fulle, Marco
Gicquel, Adeline
Groussin, Olivier
Gutierrez, Pedro J.
Guetler, Carsten
Hofmann, Marc
Hoefner, Sebastian
Hviid, Stubbe F.
Ip, Wing-Huen
Jorda, Laurent
Knollenberg, Joerg
Kramm, J. -Rainer
Kuehrt, Ekkehard
Kuppers, Michael
La Forgia, Fiorangela
Lara, Luisa M.
Lee, Jui-Chi
Lin, Zhong-Yi
Lopez Moreno, Jose J.
Marzari, Francesco
Michalik, Harald
Mottola, Stefano
Preusker, Frank
Scholten, Frank
Thomas, Nicholas
Toth, Imre
Tubiana, Cecilia
TI The southern hemisphere of 67P/Churyumov-Gerasimenko: Analysis of the
preperihelion size-frequency distribution of boulders >= 7m
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods:
data analysis
ID COMET 67P/CHURYUMOV-GERASIMENKO; EJECTA BLOCKS; OSIRIS; EROSION;
SURFACE; CRATER; MOON
AB Aims. We calculate the size-frequency distribution of the boulders on the southern hemisphere of comet 67P Churyumov-Gerasimenko (67P), which was in shadow before the end of April 2015. We compare the new results with those derived from the northern hemisphere and equatorial regions of 67P, highlighting the possible physical processes that lead to these boulder size distributions.
Methods. We used images acquired by the OSIRIS Narrow Angle Camera (NAC) on 2 May 2015 at a distance of 125 km from the nucleus. The scale of this dataset is 2.3 m/px; the high resolution of the images, coupled with the favorable observation phase angle of 62 degrees, provided the possibility to unambiguously identify boulders >= 7 m on the surface of 67P and to manually extract them with the software ArcGIS. We derived the size-frequency distribution of the illuminated southern hemisphere.
Results. We found a power-law index of -3.6 +/- 0.2 for the boulders on the southern hemisphere with a diameter range of 7-35 m. The power-law index is equal to the one previously found on northern and equatorial regions of 67P, suggesting that similar boulder formation processes occur in both hemispheres. The power-law index is related to gravitational events triggered by sublimation and/or thermal fracturing causing regressive erosion. In addition, the presence of a larger number of boulders per km(2) in the southern hemisphere, which is a factor of 3 higher with respect to the northern hemisphere, suggests that the southernmost terrains of 67P are affected by a stronger thermal fracturing and sublimating activity, hence possibly causing larger regressive erosion and gravitational events.
C1 [Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pajola, Maurizio; Bertini, Ivano; Naletto, Giampiero; Barbieri, Cesare] Univ Padua, CISAS, Ctr Studies & Act Space, Via Venezia 15, I-35131 Padua, Italy.
[Lucchetti, Alice; Cremonese, Gabriele] INAF, Osservatorio Astron Padova, Vic Osservatorio 5, I-35122 Padua, Italy.
[Vincent, Jean-Baptiste; Oklay, Nilda; Sierks, Holger; Agarwal, Jessica; Boudreault, Steve; Deller, Jakob; Gicquel, Adeline; Guetler, Carsten; Hofmann, Marc; Hoefner, Sebastian; Kramm, J. -Rainer; Tubiana, Cecilia] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[El-Maarry, Mohamed R.; Thomas, Nicholas] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Naletto, Giampiero] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
[Naletto, Giampiero; Da Deppo, Vania] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[Lazzarin, Monica; Barbieri, Cesare; La Forgia, Fiorangela; Marzari, Francesco] Univ Padua, Dept Phys & Astron G Galilei, Vic Osservatorio 3, I-35122 Padua, Italy.
[Massironi, Matteo] Univ Padua, Dept Geosci, Via G Gradenigo 6, I-35131 Padua, Italy.
[Lamy, Philippe; Jorda, Laurent; Toth, Imre] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Rodrigo, Rafael] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Rodrigo, Rafael] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Koschny, Detlef] European Space Res & Technol Ctr ESA, Sci Support Off, Keplerlaan 1,Postbus 299, NL-2201 AZ Noordwijk ZH, Netherlands.
[Rickman, Hans] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Rickman, Hans] PAS Space Reserch Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[Keller, Horst U.] TU Braunschweig, Inst Geophys & Extraterrestrial Phys, D-38106 Braunschweig, Germany.
[A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Barucci, Maria A.; Fornasier, Sonia] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France.
[Barucci, Maria A.; Fornasier, Sonia] Univ Paris Diderot, Sorbonne Paris Cite, 4 Rue Elsa Morante, F-75205 Paris 13, France.
[Bertaux, Jean-Loup] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Davidsson, Bjorn] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Debei, Stefano] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy.
[De Cecco, Mariolino] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy.
[Fulle, Marco] INAF, Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy.
[Gutierrez, Pedro J.; Lara, Luisa M.; Lopez Moreno, Jose J.] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18008 Granada, Spain.
[Hviid, Stubbe F.; Knollenberg, Joerg; Kuehrt, Ekkehard; Mottola, Stefano; Preusker, Frank; Scholten, Frank] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, Rutherfordstr 2, D-12489 Berlin, Germany.
[Ip, Wing-Huen; Lee, Jui-Chi; Lin, Zhong-Yi] Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan.
[Kuppers, Michael] ESA, European Space Astron Ctr, Operat Dept, POB 78, Madrid 28691, Spain.
[Michalik, Harald] TU Braunschweig, Inst Datentech & Kommunikat Snetze, Hans Sommer Str 66, D-38106 Braunschweig, Germany.
[Toth, Imre] Hungarian Acad Sci, Observ, POB 67, H-1525 Budapest, Hungary.
RP Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Pajola, M (reprint author), Univ Padua, CISAS, Ctr Studies & Act Space, Via Venezia 15, I-35131 Padua, Italy.
EM maurizio.pajola@nasa.gov
RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014;
OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez,
Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi,
Matteo/0000-0002-7757-8818
FU Germany (DLR); Italy (ASI); France (CNES); Spain (MEC); Sweden (SNSB);
ESA Technical Directorate; NASA Postdoctoral Program at the Ames
Research Center
FX We would like to thank the anonymous referee for constructive comments,
suggestions, and corrections that led to an important improvement of the
paper. OSIRIS was built by a consortium of the Max-Planck-Institut fur
Sonnensystemforschung, in Gottingen, Germany, CISAS-University of
Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the
Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the
Research and Scientific Support Department of the European Space Agency,
Noordwijk, The Netherlands, the Instituto Nacional de Tecnica
Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid,
Spain, the Department of Physics and Astronomy of Uppsala University,
Sweden, and the Institut fur Datentechnik and Kommunikationsnetze der
Technischen Universitat Braunschweig, Germany. The support of the
national funding agencies of Germany (DLR), Italy (ASI), France (CNES),
Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is
gratefully acknowledged. We thank the ESA teams at ESAC, ESOC and ESTEC
for their work in support of the Rosetta mission. M. Pajola was
supported for this research in part by an appointment to the NASA
Postdoctoral Program at the Ames Research Center administered by
Universities Space Research Association (USRA) through a contract with
NASA.
NR 24
TC 0
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U1 4
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR L2
DI 10.1051/0004-6361/201628887
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600168
ER
PT J
AU Pajola, M
Oklay, N
La Forgia, F
Giacomini, L
Massironi, M
Bertini, I
El-Maarry, MR
Marzari, F
Preusker, F
Scholten, F
Hofner, S
Lee, JC
Vincent, JB
Groussin, O
Naletto, G
Lazzarin, M
Barbieri, C
Sierks, H
Lamy, P
Rodrigo, R
Koschny, D
Rickman, H
Keller, HU
Agarwal, J
A'Hearn, MF
Barucci, MA
Bertaux, JL
Cremonese, G
Da Deppoll, V
Davidsson, B
De Cecco, M
Debei, S
Ferri, F
Fornasier, S
Fulle, M
Guttler, C
Gutierrez, PJ
Hviid, SF
Ip, WH
Jorda, L
Knollenberg, J
Kramm, JR
Kuppers, M
Kurt, E
Lara, LM
Lin, ZY
Lopez Moreno, JJ
Magrin, S
Michalik, H
Mottola, S
Thomas, N
Tubiana, C
AF Pajola, Maurizio
Oklay, Nilda
La Forgia, Fiorangela
Giacomini, Lorenza
Massironi, Matteo
Bertini, Ivano
El-Maarry, M. R.
Marzari, Francesco
Preusker, Frank
Scholten, Frank
Hoefner, Sebastian
Lee, Jui-Chi
Vincent, Jean-Baptiste
Groussin, Olivier
Naletto, Giampiero
Lazzarin, Monica
Barbieri, Cesare
Sierks, Holger
Lamy, Philippe
Rodrigo, Rafael
Koschny, Detlef
Rickman, Hans
Keller, Horst U.
Agarwal, Jessica
A'Hearn, Michael F.
Barucci, Maria A.
Bertaux, Jean-Loup
Cremonese, Gabriele
Da Deppoll, Vania
Davidsson, Bjoern
De Cecco, Mariolino
Debei, Stefano
Ferri, Francesca
Fornasier, Sonia
Fulle, Marco
Guettler, Carsten
Gutierrez, Pedro J.
Hviid, Stubbe F.
Ip, Wing-Huen
Jorda, Laurent
Knollenberg, Joerg
Kramm, J. -Rainer
Kueppers, Michael
Kuert, Ekkehard
Lara, Luisa M.
Lin, Zhong-Yi
Lopez Moreno, Jose J.
Magrin, Sara
Michalik, Harald
Mottola, Stefano
Thomas, Nicholas
Tubiana, Cecilia
TI Aswan site on comet 67P/Churyumov-Gerasimenko: Morphology, boulder
evolution, and spectrophotometry
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods:
data analysis
ID OSIRIS OBSERVATIONS; LANDING SITE; ROSETTA; GEOMORPHOLOGY; NUCLEUS;
SURFACE; REGION; SHAPE; ICE; 67P
AB Aims. We provide a detailed morphological analysis of the Aswan site on comet 67P/Churyumov-Gerasimenko (67P). We derive the size-frequency distribution of boulders >= 2 m and correlate this distribution with the gravitational slopes for the first time on a comet. We perform the spectral analysis of this region to understand if possible surface variegation is related to the different surface textures observable on the different units. Methods. We used two OSIRIS Narrow Angle Camera (NAC) image data sets acquired on September 19 and 22, 2014, with a scale of 0.5 m/px. Gravitational slopes derived from the 3D shape model of 67P were used to identify and interpret the different units of the site. By means of the high-resolution NAC data sets, boulders >= 2.0 m can be unambiguously identified and extracted using the software ArcGIS. Coregistered and photometrically corrected color cubes were used to perform the spectral analyses, and we retrieved the spectral properties of the Aswan units. Results. The high-resolution morphological map of the Aswan site (0.68 km(2)) shows that this site is characterized by four different units: fine-particle deposits located on layered terrains, gravitational accumulation deposits, taluses, and the outcropping layered terrain. Multiple lineaments are identified on the Aswan cliff, such as fractures, exposed layered outcrops, niches, and terraces. Close to the terrace margin, several arched features observed in plan view suggest that the margin progressively retreats as a result of erosion. The size-frequency of boulders >= 2 m in the entire study area has a power-law index of -3.9 +0.2/-0.3 (1499 boulders >= 2 m/km(2)), suggesting that the Aswan site is mainly dominated by gravitational events triggered by sublimation and/or thermal insolation weathering causing regressive erosion. The boulder size-frequency distribution versus gravitational slopes indicates that when higher gravitational slope terrains are considered, only boulders <= 10 m are identified, as well as steeper power-slope indices. In addition, no boulders >= 2 m are observed on slopes >= 50 degrees. This may indicate that larger blocks detached from a sublimating cliff cannot rest at these slopes and consequently fall down. The spectral analysis performed on the site shows that despite different morphologic units, no spectral differences appear in the multiple textures. This may confirm a redistribution of particles across the nucleus as a consequence of airfall, whether coming from Hapi or from the southern hemisphere when it is active during perihelion.
C1 [Pajola, Maurizio; Bertini, Ivano; Ferri, Francesca] G Colombo Univ Padova, CISAS, Ctr Studies & Act Space, Via Venezia 15, I-35131 Padua, Italy.
[Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Oklay, Nilda; Vincent, Jean-Baptiste; Sierks, Holger; Agarwal, Jessica; Guettler, Carsten; Kramm, J. -Rainer; Tubiana, Cecilia] Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany.
[La Forgia, Fiorangela; Marzari, Francesco; Lazzarin, Monica; Barbieri, Cesare; Magrin, Sara] G Galilei Univ Padova, Dept Phys & Astron, Vic Osservatorio 3, I-35122 Padua, Italy.
[Giacomini, Lorenza; Massironi, Matteo] Univ Padua, Geosci Dept, Via G Gradenigo 6, I-35131 Padua, Italy.
[El-Maarry, M. R.; Thomas, Nicholas] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Preusker, Frank; Scholten, Frank; Knollenberg, Joerg] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, Rutherfordstr 2, D-12489 Berlin, Germany.
[Lee, Jui-Chi; Lin, Zhong-Yi] Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan.
[Groussin, Olivier; Lamy, Philippe; Jorda, Laurent] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Naletto, Giampiero] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
[Naletto, Giampiero; Da Deppoll, Vania] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[Rodrigo, Rafael] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Rodrigo, Rafael] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Koschny, Detlef] European Space Res & Technol Ctr ESA, Sci Support Off, Keplerlaan 1,Postbus 299, NL-2201 AZ Noordwijk, Netherlands.
[Rickman, Hans] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Rickman, Hans] PAS Space Reserch Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[Keller, Horst U.] TU Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Barucci, Maria A.] Univ Paris 06, Univ Paris Diderot, CNRS, LESIA Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France.
[Barucci, Maria A.] Univ Paris Diderot, Sorbonne Paris Cite, 4 Rue Elsa Morante, F-75205 Paris 13, France.
[Bertaux, Jean-Loup] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Cremonese, Gabriele] INAF Osservatorio Astron Padova, Vic Osservatorio 5, I-35122 Padua, Italy.
[Davidsson, Bjoern] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[De Cecco, Mariolino] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy.
[Debei, Stefano] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy.
[Fulle, Marco] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy.
[Gutierrez, Pedro J.; Lara, Luisa M.; Lopez Moreno, Jose J.] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18008 Granada, Spain.
[Kueppers, Michael] ESA, European Space Astron Ctr, Operat Dept, POB 78, Madrid 28691, Spain.
[Michalik, Harald] TU Braunschweig, Inst Datentech & Kommunikationsnetze, Hans Sommer Str 66, D-38106 Braunschweig, Germany.
RP Pajola, M (reprint author), G Colombo Univ Padova, CISAS, Ctr Studies & Act Space, Via Venezia 15, I-35131 Padua, Italy.; Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014;
OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez,
Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi,
Matteo/0000-0002-7757-8818
FU Germany (DLR); Italy (ASI); France (CNES); Spain (MEC); Sweden (SNSB);
ESA Technical Directorate; Rosetta mission; NASA
FX We would like to thank the referee R. Aileen Yingst for important and
constructive comments, suggestions, and corrections that led to a
substantial improvement of the paper. OSIRIS was built by a consortium
of the Max-Planck-Institut fur Sonnensystemforschung, in Gottingen,
Germany, CISAS-University of Padova, Italy, the Laboratoire
d'Astrophysique de Marseille, France, the Instituto de Astrofisica de
Andalucia, CSIC, Granada, Spain, the Research and Scientific Support
Department of the European Space Agency, Noordwijk, The Netherlands, the
Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, the
Universidad Politechnica de Madrid, Spain, the Department of Physics and
Astronomy of Uppsala University, Sweden, and the Institut fur
Datentechnik und Kommunikationsnetze der Technischen Universitat
Braunschweig, Germany. The support of the national funding agencies of
Germany (DLR), Italy (ASI), France (CNES), Spain (MEC), Sweden (SNSB),
and the ESA Technical Directorate is gratefully acknowledged. We thank
the ESA teams at ESAC, ESOC and ESTEC for their work in support of the
Rosetta mission. We made use of the software Arcgis 10.2 together with
the softwares IDL, Matlab, and R to perform our analysis. This research
has made use of the USGS Integrated Software for Imagers and
Spectrometers (ISIS). We gratefully acknowledge the developers of SPICE
and NAIF/PDS resources. M. Pajola was supported for this research in
part by an appointment to the NASA Postdoctoral Program at the Ames
Research Center administered by Universities Space Research Association
(USRA) through a contract with NASA.
NR 40
TC 2
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U1 7
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A69
DI 10.1051/0004-6361/201527865
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600063
ER
PT J
AU Pierre, M
Pacaud, F
Adami, C
Alis, S
Altieri, B
Baran, N
Benoist, C
Birkinshaw, M
Bongiorno, A
Bremer, MN
Brusa, M
Butler, A
Ciliegi, P
Chiappetti, L
Clerc, N
Corasaniti, PS
Coupon, J
De Breuck, C
Democles, J
Desai, S
Delhaize, J
Devriendt, J
Dubois, Y
Eckert, D
Elyiv, A
Ettori, S
Evrard, A
Faccioli, L
Farahi, A
Ferrari, C
Finet, E
Fotopoulou, S
Fourmanoit, N
Gandhi, P
Gastaldello, E
Gastaud, R
Georgantopoulos, I
Giles, P
Guennou, L
Guglielmo, V
Horellou, C
Husband, K
Huynh, M
Lovino, A
Kilbinger, M
Koulouridis, E
Lavoie, S
Le Brun, AMC
Le Fevre, JP
Lidman, C
Lieu, M
Lin, CA
Mantz, A
Maughan, BJ
Maurogordato, S
McCarthy, IG
McGee, S
Melin, JB
Melnyk, O
Menanteau, F
Novak, M
Paltani, S
Plionis, M
Poggianti, BM
Pomarede, D
Pompei, E
Ponman, TJ
Ramos-Ceja, ME
Ranalli, P
Rapetti, D
Raychaudury, S
Reiprich, TH
Rottgering, H
Rozo, E
Rykoff, E
Sadibekova, T
Santos, J
Sauvageot, JL
Schimd, C
Sereno, M
Smith, GP
Smolcic, V
Snowden, S
Spergel, D
Stanford, S
Surdej, J
Valageas, P
Valotti, A
Valtchanov, I
Vignali, C
Willis, J
Ziparo, F
AF Pierre, M.
Pacaud, F.
Adami, C.
Alis, S.
Altieri, B.
Baran, N.
Benoist, C.
Birkinshaw, M.
Bongiorno, A.
Bremer, M. N.
Brusa, M.
Butler, A.
Ciliegi, P.
Chiappetti, L.
Clerc, N.
Corasaniti, P. S.
Coupon, J.
De Breuck, C.
Democles, J.
Desai, S.
Delhaize, J.
Devriendt, J.
Dubois, Y.
Eckert, D.
Elyiv, A.
Ettori, S.
Evrard, A.
Faccioli, L.
Farahi, A.
Ferrari, C.
Finet, E.
Fotopoulou, S.
Fourmanoit, N.
Gandhi, P.
Gastaldello, E.
Gastaud, R.
Georgantopoulos, I.
Giles, P.
Guennou, L.
Guglielmo, V.
Horellou, C.
Husband, K.
Huynh, M.
Lovino, A.
Kilbinger, M.
Koulouridis, E.
Lavoie, S.
Le Brun, A. M. C.
Le Fevre, J. P.
Lidman, C.
Lieu, M.
Lin, C. A.
Mantz, A.
Maughan, B. J.
Maurogordato, S.
McCarthy, I. G.
McGee, S.
Melin, J. B.
Melnyk, O.
Menanteau, F.
Novak, M.
Paltani, S.
Plionis, M.
Poggianti, B. M.
Pomarede, D.
Pompei, E.
Ponman, T. J.
Ramos-Ceja, M. E.
Ranalli, P.
Rapetti, D.
Raychaudury, S.
Reiprich, T. H.
Rottgering, H.
Rozo, E.
Rykoff, E.
Sadibekova, T.
Santos, J.
Sauvageot, J. L.
Schimd, C.
Sereno, M.
Smith, G. P.
Smolcic, V.
Snowden, S.
Spergel, D.
Stanford, S.
Surdej, J.
Valageas, P.
Valotti, A.
Valtchanov, I.
Vignali, C.
Willis, J.
Ziparo, F.
TI The XXL Survey I. Scientific motivations - XMM-Newton observing plan -
Follow-up observations and simulation programme
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: general; large-scale structure of Universe; X-rays: galaxies:
clusters; surveys
ID ACTIVE GALACTIC NUCLEI; SCALE STRUCTURE SURVEY; X-RAY SOURCES;
CHARGE-EXCHANGE EMISSION; POINT-LIKE SOURCES; WIDE-FIELD SURVEY; DEEP
SURVEY; LUMINOSITY FUNCTION; GALAXY CLUSTERS; POWER SPECTRUM
AB Context. The quest for the cosmological parameters that describe our universe continues to motivate the scientific community to undertake very large survey initiatives across the electromagnetic spectrum. Over the past two decades, the Chandra and XMM-Newton observatories have supported numerous studies of X-ray-selected clusters of galaxies, active galactic nuclei (AGNs), and the X-ray background. The present paper is the first in a series reporting results of the XXL-XMM survey; it comes at a time when the Planck mission results are being finalised.
Aims. We present the XXL Survey, the largest XMM programme totaling some 6.9 Ms to date and involving an international consortium of roughly 100 members. The XXL Survey covers two extragalactic areas of 25 deg(2) each at a point-source sensitivity of similar to 5 x 10(-15) erg s(-1) cm(-2) in the [0.5-2] keV band (completeness limit). The survey's main goals are to provide constraints on the dark energy equation of state from the space-time distribution of clusters of galaxies and to serve as a pathfinder for future, wide-area X-ray missions. We review science objectives, including cluster studies, AGN evolution, and large-scale structure, that are being conducted with the support of approximately 30 follow-up programmes.
Methods. We describe the 542 XMM observations along with the associated multi-lambda and numerical simulation programmes. We give a detailed account of the X-ray processing steps and describe innovative tools being developed for the cosmological analysis.
Results. The paper provides a thorough evaluation of the X-ray data, including quality controls, photon statistics, exposure and background maps, and sky coverage. Source catalogue construction and multi-lambda associations are briefly described. This material will be the basis for the calculation of the cluster and AGN selection functions, critical elements of the cosmological and science analyses.
Conclusions. The XXL multi-lambda data set will have a unique lasting legacy value for cosmological and extragalactic studies and will serve as a calibration resource for future dark energy studies with clusters and other X-ray selected sources. With the present article, we release the XMM XXL photon and smoothed images along with the corresponding exposure maps.
C1 [Pierre, M.; Lin, C. A.; Sadibekova, T.; Valageas, P.] CEA Saclay, DSM IRFU SAp, Serv Astrophys AIM, F-91191 Gif Sur Yvette, France.
[Pacaud, F.; Ramos-Ceja, M. E.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Adami, C.; Schimd, C.] Univ Aix Marseille, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Alis, S.; Benoist, C.; Ferrari, C.; Maurogordato, S.] Univ Nice Sophia Antipolis, Observ Cote Azur, Lab Lagrange, UMR 7293, F-06304 Nice, France.
[Alis, S.] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey.
[Altieri, B.] European Space Astron Ctr ESA ESAC, Operat Dept, Madrid, Spain.
[Birkinshaw, M.; Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England.
[Bongiorno, A.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Rome, Italy.
[Brusa, M.; Sereno, M.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Clerc, N.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Ciliegi, P.; Elyiv, A.; Ettori, S.; Sereno, M.] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Chiappetti, L.] IASF Milano, INAF, Via Bassini 15, I-20133 Milan, Italy.
[Corasaniti, P. S.] Univ Paris Diderot, CNRS, LUTh, Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France.
[De Breuck, C.] European Southern Observ, D-85748 Garching, Germany.
[Democles, J.; Lieu, M.; Ziparo, F.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Desai, S.] Univ Munich, D-80539 Munich, Germany.
[Devriendt, J.] Univ Oxford, Astrophys, Oxford OX1 3RH, England.
[Dubois, Y.] UPMC, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75005 Paris, France.
[Dubois, Y.] CNRS, Inst Astrophys Paris, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France.
[Eckert, D.; Fotopoulou, S.; Fourmanoit, N.] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland.
[Evrard, A.; Farahi, A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Evrard, A.; Farahi, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Evrard, A.; Farahi, A.] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA.
[Finet, E.] Univ Liege, Extragalact Astrophys & Space Observat AEOS, Allee 6 Aout,17 Sart Tilman,Bat B5c, B-4000 Liege, Belgium.
[Gandhi, P.] Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England.
[Georgantopoulos, I.] IAASARS, Natl Observ Athens, Penteli 15236, Greece.
[Guennou, L.] Univ Kwazulu Natal, Pretoria, South Africa.
[Horellou, C.] Chalmers, Dept Earth & Space Sci, Technol Onsala Space Observ, S-43992 Onsala, Sweden.
[Huynh, M.] Univ Western Australia, Int Ctr Radio Astron Res, M468, Crawley, WA 6009, Australia.
[Lovino, A.] INAF OAB, Brera, Italy.
[Lavoie, S.] Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC, Canada.
[Le Brun, A. M. C.] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
[Le Fevre, J. P.] CEA Saclay, DSM IRFU SEDI, F-91191 Gif Sur Yvette, France.
[Lidman, C.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Mantz, A.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Melin, J. B.] CEA Saclay, DSM IRFU SPP, F-91191 Gif Sur Yvette, France.
[Melnyk, O.] Tares Shevshenko Natl Univ, Astron Observ, Kiev, Ukraine.
[Menanteau, F.] Univ Illinois, Chicago, IL 60680 USA.
[Plionis, M.] Aristotle Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece.
[Poggianti, B. M.] INAF Astron Observ, Padua, Italy.
[Pompei, E.] European Southern Observ, Alonso Cordova 3107, Santiago, Chile.
[Rapetti, D.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Raychaudury, S.] Presidency Univ, Fac Nat & Math Sci, Dept Phys, 86-1 Coll St, Kolkata 700073, India.
[Rottgering, H.] Leiden Observ, Leiden, Netherlands.
[Rozo, E.; Rykoff, E.] SLAC Natl Accelerator Lab, Menlo Pk, CA USA.
[Novak, M.; Smolcic, V.] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, Zagreb 10000, Croatia.
[Snowden, S.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Spergel, D.] Princeton Univ, Princeton, NJ 08544 USA.
[Stanford, S.] Univ Calif Davis, Davis, CA 95616 USA.
[Valageas, P.] CEA, Inst Phys Theor, Saclay, France.
[Finet, E.] Aryabhatta Res Inst Observat Sci ARIES, Nainita 263129, Uttarakhand, India.
[Ettori, S.] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Plionis, M.] Inst Nacl Astrofis Ospt & Elect, AP 51 216, Puebla 72000, Mexico.
[Santos, J.] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy.
[Guennou, L.] Univ Paris 11, IAS, F-91405 Orsay, France.
RP Pierre, M (reprint author), CEA Saclay, DSM IRFU SAp, Serv Astrophys AIM, F-91191 Gif Sur Yvette, France.
EM mpierre@cea.fr
RI Koulouridis, Elias/C-4731-2014; Ranalli, Piero/K-6363-2013;
OI Menanteau, Felipe/0000-0002-1372-2534; De Breuck,
Carlos/0000-0002-6637-3315; Ranalli, Piero/0000-0003-3956-755X; Ramos
Ceja, Miriam Elizabeth/0000-0002-9117-3251; Gastaldello,
Fabio/0000-0002-9112-0184; Eckert, Dominique/0000-0001-7917-3892
FU BMBF/DLR [50 OR 1117]; DfG [Transregio Programme TR33]; European Union
[333654, 337595, 321913]; ASI-INAF [I/009/10/0]; International Programme
for Scientific Cooperation CNRS-INAF PICS; German Research Association
(DFG) [RE 1462/5, RE 1462/6]
FX XXL is an international project based around an XMM Very Large Programme
surveying two 25 deg2 extragalactic fields at a depth of
similar to 5 x 10-15 erg s-1 cm-2 in
[0.5-2] keV. The XXL website is http://irfu.cea.fr/xxl. Multiband
information and spectroscopic follow-up of the X-ray sources are
obtained through a number of survey programmes, summarised at
http://xxlmultiwave.pbworks.com/. The Saclay group thanks the Centre
National d'Etudes Spatiales (CNES) for long-term support. F.P. thanks
BMBF/DLR for grant 50 OR 1117. F.P. and M.E. R.-C. thank the DfG for
Transregio Programme TR33. V.S acknowledges support from the European
Union's Seventh Frame-work program under grant agreement 333654 (CIG,
"AGN feedback") and grant agreement 337595 (ERC Starting Grant,
"CoSMass"). S.E. acknowledges a contribution from contracts ASI-INAF
I/009/10/0 and PRIN-INAF 2012. The French and Italian groups acknowledge
support from the International Programme for Scientific Cooperation
CNRS-INAF PICS 2012. T.H.R. thanks the German Research Association (DFG)
for Heisenberg grant RE 1462/5 and grant RE 1462/6. D.R. thanks the
Danish National Research Foundation. M.B. thanks the European Union's
FP7 for grant agreement 321913 (CIG, "SMBH evolution through cosmic
time"). A.E. thanks the US DOE and acknowledges sabbatical support from
Institut d'Astrophysique, Paris. M.E. R.-C. is a member of the
International Max Planck Research School (IMPRS) for Astronomy and
Astrophysics at the Universities of Bonn and Cologne. The authors thank
A. K. Romer, the referee, for useful comments on the manuscript.
NR 100
TC 19
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U1 6
U2 6
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A1
DI 10.1051/0004-6361/201526766
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600011
ER
PT J
AU Roth, M
Doerr, HP
Hartlep, T
AF Roth, M.
Doerr, H. -P.
Hartlep, T.
TI Verification of the helioseismic Fourier-Legendre analysis for
meridional flow measurements
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: helioseismology; methods: data analysis; Sun: oscillations; Sun:
interior
ID TIME-DISTANCE HELIOSEISMOLOGY; RING-DIAGRAM ANALYSIS; UPPER CONVECTION
ZONE; TORSIONAL OSCILLATION; CIRCULATION; SUN; INVERSION; CELLS; STATE
AB Context. Measuring the Sun's internal meridional flow is one of the key issues of helioseismology. Using the Fourier-Legendre analysis is a technique for addressing this problem.
Aims. We validate this technique with the help of artificial helioseismic data.
Methods. The analysed data set was obtained by numerically simulating the e ff ect of the meridional flow on the seismic wave field in the full volume of the Sun. In this way, a 51.2-h long time series was generated. The resulting surface velocity field is then analyzed in various settings: Two 360 degrees x 90 degrees halfspheres, two 120 degrees x 60 degrees patches on the front and farside of the Sun (North and South, respectively) and two 120 degrees x 60 degrees patches on the northern and southern frontside only. We compare two possible measurement setups: observations from Earth and from an additional spacecraft on the solar farside, and observations from Earth only, in which case the full information of the global solar oscillation wave field was available.
Results. We find that, with decreasing observing area, the accessible depth range decreases: the 360 degrees x 90 degrees view allows us to probe the meridional flow almost to the bottom of the convection zone, while the 120 degrees x 60 degrees view means only the outer layers can be probed.
Conclusions. These results confirm the validity of the Fourier-Legendre analysis technique for helioseismology of the meridional flow. Furthermore these flows are of special interest for missions like Solar Orbiter that promises to complement standard helioseismic measurements from the solar nearside with farside observations.
C1 [Roth, M.; Doerr, H. -P.] Kiepenheuer Inst Sonnenphys, Schoneckstr 6, D-79104 Freiburg, Germany.
[Hartlep, T.] Stanford Univ, Hansen Expt Phys Lab, Standord, CA 94305 USA.
[Doerr, H. -P.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Hartlep, T.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Roth, M (reprint author), Kiepenheuer Inst Sonnenphys, Schoneckstr 6, D-79104 Freiburg, Germany.
EM mroth@kis.uni-freiburg.de; thomas.hartlep@nasa.gov
OI Hartlep, Thomas/0000-0002-5062-9507; Doerr,
Hans-Peter/0000-0002-7608-631X
FU European Research Council under the European Union's Seventh Framework
Program (FP)/ERC Grant [307117]
FX M.R. thanks D. Braun for useful discussions. The authors thank the
unknown referee for valuable comments on the manuscript. The research
leading to these results has received funding from the European Research
Council under the European Union's Seventh Framework Program
(FP/2007-2013)/ERC Grant Agreement No. 307117.
NR 30
TC 0
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U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A106
DI 10.1051/0004-6361/201526971
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600024
ER
PT J
AU Ryan, DF
Dominique, M
Seaton, D
Stegen, K
White, A
AF Ryan, D. F.
Dominique, M.
Seaton, D.
Stegen, K.
White, A.
TI Effects of flare definitions on the statistics of derived flare
distributions
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: statistical; methods: data analysis; Sun: flares; Sun: X-rays,
gamma rays; Sun: corona
ID SELF-ORGANIZED CRITICALITY; 3 SOLAR-CYCLES; X-RAY FLARES; ACTIVE-REGION;
QUIET SUN; FREQUENCY-DISTRIBUTIONS; TRANSIENT BRIGHTENINGS;
ENERGY-DISTRIBUTION; GLOBAL ENERGETICS; CORONAL LOOPS
AB The statistical examination of solar flares is crucial to revealing their global characteristics and behaviour. Such examinations can tackle large-scale science questions or give context to detailed single-event studies. However, they are often performed using standard but basic flare detection algorithms relying on arbitrary thresholds. This arbitrariness may lead to important scientific conclusions being drawn from results caused by subjective choices in algorithms rather than the true nature of the Sun. In this paper, we explore the effect of the arbitrary thresholds used in the Geostationary Operational Environmental Satellite (GOES) event list and Large Yield RAdiometer (LYRA) Flare Finder algorithms. We find that there is a small but significant relationship between the power law exponent of the GOES flare peak flux frequency distribution and the flare start thresholds of the algorithms. We also find that the power law exponents of these distributions are not stable, but appear to steepen with increasing peak flux. This implies that the observed flare size distribution may not be a power law at all. We show that depending on the true value of the exponent of the flare size distribution, this deviation from a power law may be due to flares missed by the flare detection algorithms. However, it is not possible determine the true exponent from GOES/XRS observations. Additionally we find that the PROBA2/LYRA flare size distributions are artificially steep and clearly non-power law. We show that this is consistent with an insufficient degradation correction. This means that PROBA2/LYRA should not be used for flare statistics or energetics unless degradation is adequately accounted for. However, it can be used to study variations over shorter timescales and for space weather monitoring.
C1 [Ryan, D. F.; Dominique, M.; Seaton, D.; Stegen, K.] Royal Observ Belgium, SIDC, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium.
[Ryan, D. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Seaton, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Seaton, D.] NOAA, Natl Ctr Environm Informat, Boulder, CO USA.
[White, A.] Trinity Coll Dublin, OReilly Inst, Sch Comp Sci & Stat, Dublin 2, Ireland.
RP Ryan, DF (reprint author), Royal Observ Belgium, SIDC, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium.; Ryan, DF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ryand5@tcd.ie
OI White, Arthur/0000-0002-7268-5163
FU Solar-Terrestrial Centre of Excellence; SIDC Data Exploitation project;
Interuniversity Attraction Poles Programme; Belgian Science Policy
Office [IAP P7/08 CHARM]; PRODEX [4000103240]; European Union [284461];
STATICA project - Principal Investigator programme of Science Foundation
Ireland [08/IN.1/I1879]; Belgian Federal Science Policy Office (BELSPO);
Swiss Bundesamt fur Bildung and Wissenschaft
FX The authors would like to thank Ingolf Dammasch for his helpful
discussions. D. Ryan wishes to thank the Solar-Terrestrial Centre of
Excellence and the SIDC Data Exploitation project for their financial
support. M. Dominique's work has been funded by the Interuniversity
Attraction Poles Programme initiated by the Belgian Science Policy
Office (IAP P7/08 CHARM). Support for D. Seaton was provided by PRODEX
grant No. 4000103240 managed by the European Space Agency in
collaboration with the Belgian Federal Science Policy Office (BELSPO) in
support of the PROBA2/SWAP mission and by the European Union's Seventh
Framework Programme for Research, Technological Development and
Demonstration under grant agreement No. 284461 (Project eHeroes,
www.eheroes.eu). A. White has been supported by the STATICA project,
funded by the Principal Investigator programme of Science Foundation
Ireland, contract number 08/IN.1/I1879. LYRA is a project of the Centre
Spatial de Liege, the Physikalisch-Meteorologisches Observatorium Davos
and the Royal Observatory of Belgium funded by the Belgian Federal
Science Policy Office (BELSPO) and by the Swiss Bundesamt fur Bildung
and Wissenschaft. This research has made use of SunPy, an open-source
and free community-developed solar data analysis package written in
Python (SunPy Community et al. 2015).
NR 44
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A133
DI 10.1051/0004-6361/201628130
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600082
ER
PT J
AU Taddia, F
Fremling, C
Sollerman, J
Corsi, A
Gal-Yam, A
Karamehmetoglu, E
Lunnan, R
Bue, B
Ergon, M
Kasliwal, M
Vreeswijk, PM
Wozniak, PR
AF Taddia, F.
Fremling, C.
Sollerman, J.
Corsi, A.
Gal-Yam, A.
Karamehmetoglu, E.
Lunnan, R.
Bue, B.
Ergon, M.
Kasliwal, M.
Vreeswijk, P. M.
Wozniak, P. R.
TI iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; BOLOMETRIC LIGHT CURVES;
SHOCK BREAKOUT; IB/C SUPERNOVAE; LOW-LUMINOSITY; HOST GALAXIES;
SUPERLUMINOUS SUPERNOVAE; EXTENDED PROGENITOR; UBVRI PHOTOMETRY
AB Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H-(and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (similar to 10-15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D).
Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (similar to 30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star.
Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission.
Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (similar to 10 M-circle dot) and strong Ni-56 mixing. The luminous early emission can be reproduced if we account for the presence of an extended (greater than or similar to 500 R-circle dot), low-mass (greater than or similar to 0.045 M-circle dot) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored.
Conclusions. The large ejecta mass and the presence of H-and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive (greater than or similar to 35 M-circle dot) WR star that experienced strong mass loss.
C1 [Taddia, F.; Fremling, C.; Sollerman, J.; Karamehmetoglu, E.; Ergon, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, Alballova, S-10691 Stockholm, Sweden.
[Corsi, A.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA.
[Gal-Yam, A.; Vreeswijk, P. M.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Lunnan, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Bue, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kasliwal, M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Wozniak, P. R.] Los Alamos Natl Lab, MS D436, Los Alamos, NM 87545 USA.
RP Taddia, F (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, Alballova, S-10691 Stockholm, Sweden.
EM francesco.taddia@astro.su.se
OI Wozniak, Przemyslaw/0000-0002-9919-3310
FU Knut and Alice Wallenberg Foundation; National Science Foundation
[AST-1005313]; US Department of Energy as part of the Laboratory
Directed Research and Development program; NSF [1455090]
FX We gratefully acknowledge the support from the Knut and Alice Wallenberg
Foundation. This work is partly based on observations made with the
Nordic Optical Telescope, operated by the Nordic Optical Telescope
Scientific Association at the Observatorio del Roque de los Muchachos,
La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data
presented here were obtained [in part] with ALFOSC, which is provided by
the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement
with the University of Copenhagen and NOTSA. This work is partly based
on observations made with DOLoRes@TNG. This paper made use of Lowell
Observatory's Discovery Channel Telescope (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. The Large Monolithic
Imager (LMI) on DCT was built by Lowell Observatory using funds from the
National Science Foundation (AST-1005313). LANL participation in iPTF
was funded by the US Department of Energy as part of the Laboratory
Directed Research and Development program. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. We thank N. Blagorodnova, E. Bellm, Y. Cao, G. Duggan,
S. Kulkarni, J. Jencson, P. Nugent, for their precious help with the
observations of iPTF15dtg and contribution to iPTF. We thank L. Yan for
her comments on the paper. Based on observations obtained with the
Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar
Observatory as part of the intermediate Palomar Transient Factory (iPTF)
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. A. Corsi
acknowledges support from NSF CAREER Award #1455090.
NR 97
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U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2016
VL 592
AR A89
DI 10.1051/0004-6361/201628703
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600152
ER
PT J
AU Teague, R
Guilloteau, S
Semenov, D
Henning, T
Dutrey, A
Pietu, V
Birnstiel, T
Chapillon, E
Hollenbach, D
Gorti, U
AF Teague, R.
Guilloteau, S.
Semenov, D.
Henning, Th.
Dutrey, A.
Pietu, V.
Birnstiel, T.
Chapillon, E.
Hollenbach, D.
Gorti, U.
TI Measuring turbulence in TW Hydrae with ALMA: methods and limitations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: interferometric; turbulence; methods: observational; ISM:
kinematics and dynamics; submillimeter: ISM
ID PROTOPLANETARY DISKS; TEMPERATURE-GRADIENT; ACCRETION DISKS; DM-TAU;
LINE; SPECTROSCOPY; MILLIMETER; CHEMISTRY
AB Aims. We aim to obtain a spatially resolved measurement of velocity dispersions in the disk of TW Hya.
Methods. We obtained images with high spatial and spectral resolution of the CO J = 2-1, CN N = 2-1 and CS J = 5-4 emission with ALMA in Cycle 2. The radial distribution of the turbulent broadening was derived with two direct methods and one modelling approach. The first method requires a single transition and derives Tex directly from the line profile, yielding a v turb. The second method assumes that two different molecules are co-spatial, which allows using their relative line widths for calculating T-kin and v(turb). Finally we fitted a parametric disk model in which the physical properties of the disk are described by power laws, to compare our direct methods with previous values.
Results. The two direct methods were limited to the outer r > 40 au disk because of beam smear. The direct method found v turb to range from approximate to 130 ms(-1) at 40 au, and to drop to approximate to 50 ms(-1) in the outer disk, which is qualitatively recovered with the parametric model fitting. This corresponds to roughly 0 : 2 0 : 4 c(s). CN was found to exhibit strong non-local thermal equilibrium effects outside r approximate to 140 au, so that v turb was limited to within this radius. The assumption that CN and CS are co-spatial is consistent with observed line widths only within r less than or similar to 100 au, within which v turb was found to drop from 100 ms 1 (approximate to 0.4 c(s)) to zero at 100 au. The parametric model yielded a nearly constant 50 ms(-1) for CS (0.2-0.4 cs). We demonstrate that absolute flux calibration is and will be the limiting factor in all studies of turbulence using a single molecule.
Conclusions. The magnitude of the dispersion is comparable with or below that predicted by the magneto-rotational instability theory. A more precise comparison would require reaching an absolute calibration precision of about 3%, or finding a suitable combination of light and heavy molecules that are co-located in the disk.
C1 [Teague, R.; Semenov, D.; Henning, Th.; Birnstiel, T.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Guilloteau, S.; Dutrey, A.; Chapillon, E.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France.
[Guilloteau, S.; Dutrey, A.; Chapillon, E.] CNRS, LAB, UMR 5804, F-33270 Floirac, France.
[Pietu, V.; Birnstiel, T.] Domaine Univ, IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France.
[Hollenbach, D.; Gorti, U.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Teague, R (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM teague@mpia.de
OI Semenov, Dmitry/0000-0002-3913-7114
FU Deutsche Forschungsgemeinschaft [SPP 1385, SE 1962/1-3, SPP 1833, KL
1469/13-1]; National Program PCMI from INSU-CNRS; National Program PNPS
from INSU-CNRS
FX We thank the referee, whose helpful comments have improved this
manuscript. R.T. is a member of the International Max Planck Research
School for Astronomy and Cosmic Physics at the University of Heidelberg,
Germany. D.S. and T.B. acknowledge support by the Deutsche
Forschungsgemeinschaft through SPP 1385: "The first ten million years of
the solar system a planetary materials approach" (SE 1962/1-3) and SPP
1833 "Building a Habitable Earth" (KL 1469/13-1), respectively. This
research made use of System. This paper makes use of the following ALMA
data: ADS/JAO. ALMA#2013.1.00387. S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ. This work was supported by the
National Programs PCMI and PNPS from INSU-CNRS.
NR 24
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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 AUG
PY 2016
VL 592
AR A49
DI 10.1051/0004-6361/201628550
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DX9NO
UT WOS:000384722600132
ER
PT J
AU Schoeberl, M
Dessler, A
Ye, H
Wang, T
Avery, M
Jensen, E
AF Schoeberl, Mark
Dessler, Andrew
Ye, Hao
Wang, Tao
Avery, Melody
Jensen, Eric
TI The impact of gravity waves and cloud nucleation threshold on
stratospheric water and tropical tropospheric cloud fraction
SO EARTH AND SPACE SCIENCE
LA English
DT Article
ID TROPOPAUSE LAYER; ICE NUCLEATION; DEHYDRATION; TEMPERATURE; CIRCULATION;
PARAMETERIZATION; MECHANISMS; MODELS; VAPOR
AB Using the Modern Era Retrospective-Analysis for Research and Applications (MERRA) and MERRA-2 reanalysis winds, temperatures, and anvil cloud ice, we explore the impact of varying the cloud nucleation threshold relative humidity (RH) and high-frequency gravity waves on stratospheric water vapor (H2O) and upper tropical tropopause cloud fraction (TCF). Our model results are compared to 2008/2009 winter TCF derived from Cloud-Aerosol Lidar with Orthogonal Polarization and H2O observations from the Microwave Limb Sounder (MLS). The RH threshold affects both model H2O and TCF, while high-frequency gravity waves mostly impact TCF. Adjusting the nucleation RH and the amplitude of high-frequency gravity waves allows us to tune the model to observations. Reasonable observational agreement is obtained with a nucleation threshold between 130% and 150% RH consistent with airborne observations. For the MERRA reanalysis, we lower the tropopause temperature by 0.5 K roughly consistent with GPS radio occultation measurements and include similar to 0.1 K high-frequency gravity wave temperature oscillations in order to match TCF and H2O observations. For MERRA-2 we do not need to adjust the tropopause temperature nor add gravity waves, because there are sufficient high-frequency temperature oscillations already present in the MERRA-2 reanalysis to reproduce the observed TCF.
C1 [Schoeberl, Mark] Sci & Technol Corp, Columbia, MD 21046 USA.
[Dessler, Andrew; Ye, Hao] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Wang, Tao] NASA, Jet Prop Lab, CALTECH, Pasadena, CA USA.
[Avery, Melody] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Jensen, Eric] NASA, Ames Res Ctr, Mountain View, CA USA.
RP Schoeberl, M (reprint author), Sci & Technol Corp, Columbia, MD 21046 USA.
EM mark.schoeberl@mac.com
RI Dessler, Andrew/G-8852-2012; Wang, Tao/C-2381-2011
OI Dessler, Andrew/0000-0003-3939-4820; Wang, Tao/0000-0003-3430-8508
NR 35
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 EARTH SPACE SCI
JI Earth Space Sci.
PD AUG
PY 2016
VL 3
IS 8
BP 295
EP 305
DI 10.1002/2016EA000180
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DZ3GZ
UT WOS:000385734600002
ER
PT J
AU Shirley, JH
Jamieson, CS
Dalton, JB
AF Shirley, James H.
Jamieson, Corey S.
Dalton, J. Bradley, III
TI Europa's surface composition from near-infrared observations: A
comparison of results from linear mixture modeling and radiative
transfer modeling
SO EARTH AND SPACE SCIENCE
LA English
DT Article
ID HAPKE PHOTOMETRIC MODEL; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY;
SULFURIC-ACID HYDRATE; WATER-ICE; GALILEAN SATELLITES; GRAIN-SIZE;
PARTICULATE MIXTURES; SUBSURFACE OCEAN; MARTIAN SURFACE; SPECTRA
AB Quantitative estimates of the abundance of surface materials and of water ice particle grain sizes at five widely separated locations on the surface of Europa have been obtained by two independent methods in order to search for possible discrepancies that may be attributed to differences in the methods employed. Results of radiative transfer (RT) compositional modeling (also known as intimate mixture modeling) from two prior studies are here employed without modification. Areal (or "checkerboard") mixture modeling, also known as linear mixture (LM) modeling, was performed to allow direct comparisons. The failure to model scattering processes (whose effects may be strongly nonlinear) in the LM approach is recognized as a potential source of errors. RT modeling accounts for nonlinear spectral responses due to scattering but is subject to other uncertainties. By comparing abundance estimates for H2SO4 center dot nH(2)O and water ice, obtained through both methods as applied to identical spectra, we may gain some insight into the importance of "volume scattering" effects for investigations of Europa's surface composition. We find that both methods return similar abundances for each location analyzed; linear correlation coefficients of >= 0.98 are found between the derived H2SO4 center dot nH(2)O and water ice abundances returned by both methods. We thus find no evidence of a significant influence of volume scattering on the compositional solutions obtained by LM modeling for these locations. Some differences in the results obtained for water ice grain sizes are attributed to the limited selection of candidate materials allowed in the RT investigations.
C1 [Shirley, James H.; Jamieson, Corey S.; Dalton, J. Bradley, III] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Jamieson, Corey S.] SETI Inst, Mountain View, CA USA.
RP Shirley, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM James.H.Shirley@jpl.nasa.gov
NR 74
TC 1
Z9 1
U1 6
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 EARTH SPACE SCI
JI Earth Space Sci.
PD AUG
PY 2016
VL 3
IS 8
BP 326
EP 344
DI 10.1002/2015EA000149
PG 19
WC Geosciences, Multidisciplinary
SC Geology
GA DZ3GZ
UT WOS:000385734600005
ER
PT J
AU Parker, SR
West, RF
Boyd, ES
Feyhl-Buska, J
Gammons, CH
Johnston, TB
Williams, GP
Poulson, SR
AF Parker, Stephen R.
West, Robert F.
Boyd, Eric S.
Feyhl-Buska, Jayme
Gammons, Christopher H.
Johnston, Tyler B.
Williams, George P.
Poulson, Simon R.
TI Biogeochemical and microbial seasonal dynamics between water column and
sediment processes in a productive mountain lake: Georgetown Lake, MT,
USA
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID SULFATE-REDUCING BACTERIUM; SP-NOV.; METHANE EMISSIONS; ORGANIC-MATTER;
STABLE CARBON; GEN. NOV.; ISOTOPE; SULFUR; REDUCTION; ACETATE
AB This manuscript details investigations of a productive, mountain freshwater lake and examines the dynamic relationship between the chemical and stable isotopes and microbial composition of lake bed sediments with the geochemistry of the lake water column. A multidisciplinary approach was used in order to better understand the lake water- sediment interactions including quantification and sequencing of microbial 16S rRNA genes in a sediment core as well as stable isotope analysis of C, S, and N. One visit included the use of a pore water sampler to gain insight into the composition of dissolved solutes within the sediment matrix. Sediment cores showed a general decrease in total C with depth which included a decrease in the fraction of organic C combined with an increase in the fraction of inorganic C. One sediment core showed a maximum concentration of dissolved organic C, dissolved inorganic C, and dissolved methane in pore water at 4 cm depth which corresponded with a sharp increase in the abundance of 16S rRNA templates as a proxy for the microbial population size as well as the peak abundance of a sequence affiliated with a putative methanotroph. The isotopic separation between dissolved inorganic and dissolved organic carbon is consistent with largely aerobic microbial processes dominating the upper water column, while anaerobic microbial activity dominates the sediment bed. Using sediment core carbon concentrations, predictions were made regarding the breakdown and return of stored carbon per year from this temperate climate lake with as much as 1.3 Gg C yr(-1) being released in the form of CO2 and CH4.
C1 [Parker, Stephen R.; West, Robert F.; Johnston, Tyler B.; Williams, George P.] Montana Tech Univ Montana, Dept Chem & Geochem, Butte, MT 59701 USA.
[Boyd, Eric S.; Feyhl-Buska, Jayme] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
[Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA USA.
[Gammons, Christopher H.] Montana Tech Univ Montana, Dept Geol Engn, Butte, MT USA.
[Poulson, Simon R.] Univ Nevada, Dept Geol Sci & Engn, Reno, NV 89557 USA.
RP Parker, SR (reprint author), Montana Tech Univ Montana, Dept Chem & Geochem, Butte, MT 59701 USA.
EM sparker@mtech.edu
FU Montana Institute on Ecosystems; National Science Foundation [0739054,
1338040]; MSU Undergraduate Scholars Program; [NNA15BB02A]
FX We thank J. Timmer for analytical assistance and L. Johnston for field
assistance. Thanks to R. West Sr. for the gracious use of his boat. This
work was funded in part by grants from the Montana Institute on
Ecosystems and the National Science Foundation (0739054, 1338040). The
NASA Astrobiology Institute is supported by grant NNA15BB02A. Funding
for J. Feyhl-Buska was provided in part by the MSU Undergraduate
Scholars Program. All data generated as part of this project are
included in figures, tables, and text within this manuscript or in the
supporting information. This manuscript has been greatly improved by the
comments of two anonymous reviewers.
NR 70
TC 0
Z9 0
U1 6
U2 6
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 AUG
PY 2016
VL 121
IS 8
BP 2064
EP 2081
DI 10.1002/2015JG003309
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DZ2ZP
UT WOS:000385712400001
ER
PT J
AU Broiles, TW
Livadiotis, G
Burch, JL
Chae, K
Clark, G
Cravens, TE
Davidson, R
Eriksson, A
Frahm, RA
Fuselier, SA
Goldstein, J
Goldstein, R
Henri, P
Madanian, H
Mandt, K
Mokashi, P
Pollock, C
Rahmati, A
Samara, M
Schwartz, SJ
AF Broiles, T. W.
Livadiotis, G.
Burch, J. L.
Chae, K.
Clark, G.
Cravens, T. E.
Davidson, R.
Eriksson, A.
Frahm, R. A.
Fuselier, S. A.
Goldstein, J.
Goldstein, R.
Henri, P.
Madanian, H.
Mandt, K.
Mokashi, P.
Pollock, C.
Rahmati, A.
Samara, M.
Schwartz, S. J.
TI Characterizing cometary electrons with kappa distributions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GIACOBINI-ZINNER; SOLAR-WIND; SPACE PLASMAS; BOW SHOCK; ROSETTA;
67P/CHURYUMOV-GERASIMENKO; COMA; ION; HALLEY; SENSOR
AB The Rosetta spacecraft has escorted comet 67P/Churyumov-Gerasimenko since 6 August 2014 and has offered an unprecedented opportunity to study plasma physics in the coma. We have used this opportunity to make the first characterization of cometary electrons with kappa distributions. Two three-dimensional kappa functions were fit to the observations, which we interpret as two populations of dense and warm (density = 10 cm(-3), temperature = 2 x 10(5) K, invariant kappa index = 10 -> 1000), and rarefied and hot (density = 0.005 cm(-3), temperature = 5 x 10(5) K, invariant kappa index = 1-10) electrons. We fit the observations on 30 October 2014 when Rosetta was 20 km from 67P, and 3 AU from the Sun. We repeated the analysis on 15 August 2015 when Rosetta was 300 km from the comet and 1.3 AU from the Sun. Comparing the measurements on both days gives the first comparison of the cometary electron environment between a nearly inactive comet far from the Sun and an active comet near perihelion. We find that the warm population density increased by a factor of 3, while the temperature cooled by a factor of 2, and the invariant kappa index was unaffected. We find that the hot population density increased by a factor of 10, while the temperature and invariant kappa index were unchanged. We conclude that the hot population is likely the solar wind halo electrons in the coma. The warm population is likely of cometary origin, but its mechanism for production is not known.
C1 [Broiles, T. W.; Livadiotis, G.; Burch, J. L.; Chae, K.; Frahm, R. A.; Fuselier, S. A.; Goldstein, J.; Goldstein, R.; Mandt, K.; Mokashi, P.] Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
[Clark, G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Cravens, T. E.; Madanian, H.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Davidson, R.] Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA.
[Eriksson, A.] Swedish Inst Space Phys, Kiruna, Sweden.
[Fuselier, S. A.; Goldstein, J.; Mandt, K.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Henri, P.] CNRS, LPC2E, Orleans, France.
[Pollock, C.] Denali Sci, Healy, AK USA.
[Rahmati, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Samara, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Schwartz, S. J.] Imperial Coll London, Blackett Lab, London, England.
[Schwartz, S. J.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA.
RP Broiles, TW (reprint author), Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
EM tbroiles@swri.edu
OI Mandt, Kathleen/0000-0001-8397-3315
FU NASA [1345493]; Jet Propulsion Laboratory, California Institute of
Technology
FX Rosetta is a European Space Agency (ESA) mission with support by member
nations and U.S. National Aeronautics and Space Administration (NASA).
The work on IES was supported, in part, by NASA 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. All of the data shown from the
Rosetta mission can be found on the European Space Agency's Planetary
Science Archive
(http://www.rssd.esa.int/index.php?project=PSA&page=ftpaccess) with the
exception of the kappa function fit parameters to the electron
distributions, which can be requested from the author at
tbroiles@swri.edu.
NR 45
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7407
EP 7422
DI 10.1002/2016JA022972
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500006
ER
PT J
AU Nose, M
Keika, K
Kletzing, CA
Spence, HE
Smith, CW
MacDowall, RJ
Reeves, GD
Larsen, BA
Mitchell, DG
AF Nose, M.
Keika, K.
Kletzing, C. A.
Spence, H. E.
Smith, C. W.
MacDowall, R. J.
Reeves, G. D.
Larsen, B. A.
Mitchell, D. G.
TI Van Allen Probes observations of magnetic field dipolarization and its
associated O+ flux variations in the inner magnetosphere at L < 6.6
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID NEAR-EARTH MAGNETOTAIL; ENERGETIC PARTICLE; PLASMA SHEET;
ELECTRIC-FIELDS; GEOSYNCHRONOUS OBSERVATIONS; GEOMAGNETIC CONDITIONS;
SUBSTORM ONSETS; ION INJECTIONS; ACCELERATION; PHASE
AB We investigate the magnetic field dipolarization in the inner magnetosphere and its associated ion flux variations, using the magnetic field and energetic ion flux data acquired by the Van Allen Probes. From a study of 74 events that appeared at L = 4.5-6.6 between 1 October 2012 and 31 October 2013, we reveal the following characteristics of the dipolarization in the inner magnetosphere: (1) its time scale is approximately 5 min; (2) it is accompanied by strong magnetic fluctuations that have a dominant frequency close to the O+ gyrofrequency; (3) ion fluxes at 20-50 keV are simultaneously enhanced with larger magnitudes for O+ than for H+; (4) after a few minutes of the dipolarization, the flux enhancement at 0.1-5 keV appears with a clear energy-dispersion signature only for O+; and (5) the energy-dispersed O+ flux enhancement appears in directions parallel or antiparallel to the magnetic field. From these characteristics, we discuss possible mechanisms that can provide selective acceleration to O+ ions at > 20 keV. We conclude that O+ ions at L = 5.4-6.6 undergo nonadiabatic local acceleration caused by oscillating electric field associated with the magnetic fluctuations and/or adiabatic convective transport from the plasma sheet to the inner magnetosphere by the impulsive electric field. At L = 4.5-5.4, however, only the former acceleration is plausible. We also conclude that the field-aligned energy-dispersed O+ ions at 0.1-5 keV originate from the ionosphere and are extracted nearly simultaneously to the onset of the dipolarization.
C1 [Nose, M.] Kyoto Univ, Grad Sch Sci, Kyoto, Japan.
[Keika, K.] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi, Japan.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Spence, H. E.; Smith, C. W.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[MacDowall, R. J.] Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
[Reeves, G. D.; Larsen, B. A.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
[Reeves, G. D.; Larsen, B. A.] New Mexico Consortium, Div Space Sci, Los Alamos, NM USA.
[Mitchell, D. G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Nose, M (reprint author), Kyoto Univ, Grad Sch Sci, Kyoto, Japan.
EM nose@kugi.kyoto-u.ac.jp
OI Nose, Masahito/0000-0002-2789-3588; Reeves, Geoffrey/0000-0002-7985-8098
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT)
[25287127, 16H04057, 26800257]; GEMSIS project at Institute for
Space-Earth Environmental Research (ISEE), Nagoya University; EMFISIS by
JHU/APL under NASA [921648, NAS5-01072]; RBSP-ECT by JHU/APL under NASA
[NAS5-01072, 967399]; U.S. Department of Energy [LA-UR-15-20090];
JHU/APL under NASA [NAS5-01072, 937836]
FX The AL and ASY indices are provided by the World Data Center for
Geomagnetism, Kyoto, and are available at http://wdc.kugi.kyoto-u.ac.jp.
The Wp index can be downloaded from http://s-cubed.info and referred as
doi:10.17593/13437-46800. The EMFISIS and ECT-HOPE data are available at
http://emfisis.physics.uiowa.edu and http://www.rbsp-ect.lanl.gov,
respectively. Geomagnetic field by the IGRF model is calculated with
GEOPACK routines developed by N.A. Tsyganenko and coded by H. Korth. We
are thankful to K. Takahashi for his helpful comments. We thank L.J.
Lanzerotti for discussing ion flux variations observed by the RBSPICE
instrument. We also thank M. Gkioulidou, D. Turner, K. Min, and H. Korth
for their supports in software to read the RBSPICE data. This study is
supported by the Ministry of Education, Culture, Sports, Science and
Technology (MEXT), grant-in-aid for Scientific Research (B) (grants
25287127 and 16H04057) and grant-in-aid for Young Scientists (B) (grant
26800257). One of coauthors (K. K.) is supported by the GEMSIS project
at Institute for Space-Earth Environmental Research (ISEE), Nagoya
University, and his work has been done at the ERG-Science Center
operated by ISAS/JAXA and ISEE/Nagoya University. This work was
supported by EMFISIS investigation funding provided by JHU/APL contract
921648 under NASA Prime contract NAS5-01072. This work was supported by
RBSP-ECT funding provided by JHU/APL contract 967399 under NASA Prime
contract NAS5-01072. Work at Los Alamos National Laboratory was
performed under the auspices of the U.S. Department of Energy,
LA-UR-15-20090. The RBSPICE instrument was supported by JHU/APL contract
937836 to the New Jersey Institute of Technology under NASA Prime
contract NAS5-01072.
NR 57
TC 0
Z9 0
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 AUG
PY 2016
VL 121
IS 8
BP 7572
EP 7589
DI 10.1002/2016JA022549
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500019
ER
PT J
AU Aryan, H
Sibeck, D
Balikhin, M
Agapitov, O
Kletzing, C
AF Aryan, Homayon
Sibeck, David
Balikhin, Michael
Agapitov, Oleksiy
Kletzing, Craig
TI Observation of chorus waves by the Van Allen Probes: Dependence on solar
wind parameters and scale size
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID RADIATION-BELT ELECTRONS; WHISTLER-MODE CHORUS; INNER MAGNETOSPHERE;
RELATIVISTIC ELECTRONS; SOURCE REGION; EQUATORWARD BOUNDARY; OUTER
MAGNETOSPHERE; PLASMASPHERIC HISS; AURORAL SUBSTORMS; GEOMAGNETIC STORM
AB Highly energetic electrons in the Earth's Van Allen radiation belts can cause serious damage to spacecraft electronic systems and affect the atmospheric composition if they precipitate into the upper atmosphere. Whistler mode chorus waves have attracted significant attention in recent decades for their crucial role in the acceleration and loss of energetic electrons that ultimately change the dynamics of the radiation belts. The distribution of these waves in the inner magnetosphere is commonly presented as a function of geomagnetic activity. However, geomagnetic indices are nonspecific parameters that are compiled from imperfectly covered ground based measurements. The present study uses wave data from the two Van Allen Probes to present the distribution of lower band chorus waves not only as functions of single geomagnetic index and solar wind parameters but also as functions of combined parameters. Also the current study takes advantage of the unique equatorial orbit of the Van Allen Probes to estimate the average scale size of chorus wave packets, during close separations between the two spacecraft, as a function of radial distance, magnetic latitude, and geomagnetic activity, respectively. Results show that the average scale size of chorus wave packets is approximately 1300-2300 km. The results also show that the inclusion of combined parameters can provide better representation of the chorus wave distributions in the inner magnetosphere and therefore can further improve our knowledge of the acceleration and loss of radiation belt electrons.
C1 [Aryan, Homayon; Sibeck, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Balikhin, Michael] Univ Sheffield, Dept Automat Control & Syst Engn, Sheffield, S Yorkshire, England.
[Agapitov, Oleksiy] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Agapitov, Oleksiy] Taras Shevchenko Natl Univ Kiev, Astron & Space Phys Dept, Kiev, Ukraine.
[Kletzing, Craig] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Aryan, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM aryan.homayon@gmail.com
FU NASA; Van Allen Probes program; NASA [NNX16AF85G]
FX This study was supported by the NASA postdoctoral program. Portion of
this work was supported by the Van Allen Probes program. We would also
like to acknowledge NASA Grant NNX16AF85G. The authors would like to
thank Alexa Halford, Kyle Murphy, Alexander Lipatov, and Quintin
Schiller for their very useful science discussions. The EMFISIS waves
data used in this study are available online
(http://emfisis.physics.uiowa.edu/Flight/). The solar wind data were
obtained by NASA's GSFC SPDF OMNIWEB and are also available online
(http://omniweb.gsfc.nasa.gov).
NR 97
TC 0
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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 AUG
PY 2016
VL 121
IS 8
BP 7608
EP 7621
DI 10.1002/2016JA022775
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500021
ER
PT J
AU Kanekal, SG
Baker, DN
Fennell, JF
Jones, A
Schiller, Q
Richardson, IG
Li, X
Turner, DL
Califf, S
Claudepierre, SG
Wilson, LB
Jaynes, A
Blake, JB
Reeves, GD
Spence, HE
Kletzing, CA
Wygant, JR
AF Kanekal, S. G.
Baker, D. N.
Fennell, J. F.
Jones, A.
Schiller, Q.
Richardson, I. G.
Li, X.
Turner, D. L.
Califf, S.
Claudepierre, S. G.
Wilson, L. B., III
Jaynes, A.
Blake, J. B.
Reeves, G. D.
Spence, H. E.
Kletzing, C. A.
Wygant, J. R.
TI Prompt acceleration of magnetospheric electrons to ultrarelativistic
energies by the 17 March 2015 interplanetary shock
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD SIGNATURES; ALLEN PROBES
OBSERVATIONS; RADIATION BELT ELECTRONS; SOLAR-WIND; RELATIVISTIC
ELECTRONS; INNER MAGNETOSPHERE; ENERGETIC PARTICLE; STORM; EVENTS
AB Trapped electrons in Earth's outer Van Allen radiation belt are influenced profoundly by solar phenomena such as high-speed solar wind streams, coronal mass ejections (CME), and interplanetary (IP) shocks. In particular, strong IP shocks compress the magnetosphere suddenly and result in rapid energization of electrons within minutes. It is believed that the electric fields induced by the rapid change in the geomagnetic field are responsible for the energization. During the latter part of March 2015, a CME impact led to the most powerful geomagnetic storm (minimum Dst = -223 nT at 17 March, 23 UT) observed not only during the Van Allen Probe era but also the entire preceding decade. Magnetospheric response in the outer radiation belt eventually resulted in elevated levels of energized electrons. The CME itself was preceded by a strong IP shock whose immediate effects vis-a-vis electron energization were observed by sensors on board the Van Allen Probes. The comprehensive and high-quality data from the Van Allen Probes enable the determination of the location of the electron injection, timescales, and spectral aspects of the energized electrons. The observations clearly show that ultrarelativistic electrons with energies E > 6 MeV were injected deep into the magnetosphere at L approximate to 3 within about 2 min of the shock impact. However, electrons in the energy range of approximate to 250 keV to approximate to 900 keV showed no immediate response to the IP shock. Electric and magnetic fields resulting from the shock-driven compression complete the comprehensive set of observations that provide a full description of the near-instantaneous electron energization.
C1 [Kanekal, S. G.; Jones, A.; Schiller, Q.; Richardson, I. G.; Li, X.; Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baker, D. N.; Califf, S.; Jaynes, A.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Jones, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Fennell, J. F.; Turner, D. L.; Claudepierre, S. G.; Blake, J. B.] Aerosp Corp, POB 92957, Los Angeles, CA 90009 USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Wygant, J. R.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA.
RP Kanekal, SG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM shrikanth.g.kanekal@nasa.gov
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Richardson,
Ian/0000-0002-3855-3634
FU JHU/APL under NASA [967399, NAS5-01072]
FX The work at LASP, University of Colorado, is supported by JHU/APL
contract 967399 under NASAs prime contract NAS5-01072. All the MagEIS,
REPT, and Van Allen Probes data used are publicly available at
(www.rbsp-ect.lanl.gov). The ACE data are from the ACE Science Center
www.srl.caltech.edu/ACE/ASC/.
NR 61
TC 4
Z9 4
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7622
EP 7635
DI 10.1002/2016JA022596
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500022
ER
PT J
AU Lyatsky, W
Pollock, C
Goldstein, ML
Lyatskaya, S
Avanov, L
AF Lyatsky, Wladislaw
Pollock, Craig
Goldstein, Melvyn L.
Lyatskaya, Sonya
Avanov, Levon
TI Penetration of magnetosheath plasma into dayside magnetosphere: 1.
Density, velocity, and rotation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID 2-DIMENSIONAL HYBRID SIMULATIONS; SOLAR-WIND; IMPULSIVE PENETRATION;
TANGENTIAL DISCONTINUITY; MAGNETOPAUSE; TRANSPORT; IRREGULARITIES;
FILAMENT; VORTICES; ELEMENTS
AB In this study, we examine a large number of plasma structures (filaments), observed with the Cluster spacecraft during 2 years (2007-2008) in the dayside magnetosphere but consisting of magnetosheath plasma. To reduce the effects observed in the cusp regions and on magnetosphere flanks, we consider these events predominantly inside the narrow cone <= 30 degrees about the subsolar point. Two important features of these filaments are (i) their stable antisunward (earthward) motion inside the magnetosphere, whereas the ambient magnetospheric plasma moves usually in the opposite direction (sunward), and (ii) between these filaments and the magnetopause, there is a region of magnetospheric plasma, which separates these filaments from the magnetosheath. The stable earthward motion of these filaments and the presence of a region of magnetospheric plasma between these filaments and the magnetopause show the possible disconnection of these filaments from the magnetosheath, as suggested earlier by many researchers. The results also show that these events cannot be a result of back-and-forth motions of magnetopause position or surface waves propagating on the magnetopause. Another important feature of these filaments is their rotation about the filament axis, which might be a result of their passage through the velocity shear on magnetopause boundary. After crossing the velocity shear, the filaments get a rotational velocity, which has opposite directions in the noon-dusk and noon-dawn sectors. This rotation velocity may be an important factor, supporting the stability of these filaments and providing their motion into the magnetosphere.
C1 [Lyatsky, Wladislaw] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Lyatsky, Wladislaw; Pollock, Craig; Goldstein, Melvyn L.; Lyatskaya, Sonya; Avanov, Levon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lyatsky, W (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.; Lyatsky, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lyatsky@gmail.com
FU NASA Heliophysics Guest Investigator Program; NASA Cluster Project
FX This work was funded in part by a NASA Heliophysics Guest Investigator
Program grant to the Goddard Space Flight Center and by the NASA Cluster
Project. We particularly thank Chris Gurgiolo for the help with some of
the analysis and David Sibeck for the interesting comments and advices.
We also wish to thank the operations and science teams of the CIS,
PEACE, and FGM instruments for their work on the Cluster data and for
providing these data through the Cluster Science Archive.
NR 30
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7699
EP 7712
DI 10.1002/2015JA022119
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500027
ER
PT J
AU Lyatsky, W
Pollock, C
Goldstein, ML
Lyatskaya, S
Avanov, L
AF Lyatsky, Wladislaw
Pollock, Craig
Goldstein, Melvyn L.
Lyatskaya, Sonya
Avanov, Levon
TI Penetration of magnetosheath plasma into dayside magnetosphere: 2.
Magnetic field in plasma filaments
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND; IMPULSIVE PENETRATION; TANGENTIAL DISCONTINUITY;
MAGNETOPAUSE; SIMULATIONS; TRANSPORT; WAVES; IRREGULARITIES; ELEMENTS;
TUBES
AB In this paper, we examined plasma structures (filaments), observed in the dayside magnetosphere but containing magnetosheath plasma. These filaments show the stable antisunward motion (while the ambient magnetospheric plasma moved in the opposite direction) and the existence of a strip of magnetospheric plasma, separating these filaments from the magnetosheath. These results, however, contradict both theoretical studies and simulations by Schindler (1979), Ma et al. (1991), Dai and Woodward (1994, 1998), and other researchers, who reported that the motion of such filaments through the magnetosphere is possible only when their magnetic field is directed very close to the ambient magnetic field, which is not the situation that is observed. In this study, we show that this seeming contradiction may be related to different events as the theoretical studies and simulations are related to the case when the filament magnetic field is about aligned with filament orientation, whereas the observations show that the magnetic field in these filaments may be rotating. In this case, the rotating magnetic field, changing incessantly its direction, drastically affects the penetration of plasma filaments into the magnetosphere. In this case, the filaments with rotating magnetic field, even if in each moment it is significantly inclined to the ambient magnetic field, may propagate through the magnetosphere, if their average (for the rotation period) magnetic field is aligned with the ambient magnetic field. This shows that neglecting the rotation of magnetic field in these filaments may lead to wrong results.
C1 [Lyatsky, Wladislaw] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Lyatsky, Wladislaw; Pollock, Craig; Goldstein, Melvyn L.; Lyatskaya, Sonya; Avanov, Levon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lyatsky, W (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.; Lyatsky, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lyatsky@gmail.com
FU NASA Heliophysics Guest Investigator Program; NASA Cluster Project
FX This work was funded in part by a NASA Heliophysics Guest Investigator
Program grant to the Goddard Space Flight Center and by the NASA Cluster
Project. We also thank Cluster instrument teams and the Cluster Active
Archive for providing the data, which are available at
http://www.cosmos.esa.int/web/csa/access. We particularly thank Chris
Gurgiolo for the help with some of the analysis and David Sibeck for the
interesting comments and advices.
NR 26
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7713
EP 7727
DI 10.1002/2015JA022120
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500028
ER
PT J
AU Hajra, R
Tsurutani, BT
Echer, E
Gonzalez, WD
Gjerloev, JW
AF Hajra, Rajkumar
Tsurutani, Bruce T.
Echer, Ezequiel
Gonzalez, Walter D.
Gjerloev, Jesper W.
TI Supersubstorms (SML <-2500nT): Magnetic storm and solar cycle
dependences
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ACTIVITY HILDCAA EVENTS; DST LESS-THAN-OR-EQUAL-TO-50 NT; INTENSE
GEOMAGNETIC STORMS; AURORAL ELECTROJET INDEXES; UNIVERSAL TIME
VARIATIONS; LONG-DURATION; SUBSTORM ONSET; LESS-THAN; AE; ACCELERATION
AB We study extremely intense substorms with SuperMAG AL (SML) peak intensities < -2500 nT ("supersubstorms"/SSSs) for the period from 1981 to 2012. The SSS events were often found to be isolated SML peaks and not statistical fluctuations of the indices. The SSSs occur during all phases of the solar cycle with the highest occurrence (3.8 year(-1)) in the descending phase. The SSSs exhibited an annual variation with equinoctial maximum altering between spring in solar cycle 22 and fall in solar cycle 23. The occurrence rate and strength of the SSSs did not show any strong relationship with the intensity of the associated geomagnetic storms. All SSS events were associated with strong southward interplanetary magnetic field B-s component. The B-s fields were part of interplanetary magnetic clouds in 46% and of interplanetary sheath fields in 54% of the cases. About 77% of the SSSs were associated with small regions of very high density solar wind plasma parcels or pressure pulses impinging upon the magnetosphere. Comments on how SSS events may cause power outages at Earth are discussed at the end of the paper.
C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil.
[Hajra, Rajkumar] CNRS, Lab Phys & Chim Environm & Espace, Orleans, France.
[Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gjerloev, Jesper W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Gjerloev, Jesper W.] Univ Bergen, Birkeland Ctr, Bergen, Norway.
RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil.; Hajra, R (reprint author), CNRS, Lab Phys & Chim Environm & Espace, Orleans, France.
EM rajkumarhajra@yahoo.co.in
OI Hajra, Rajkumar/0000-0003-0447-1531
FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) at INPE;
ANR at LPC2E/CNRS [ANR-15-CE31-0009-01]; Brazilian CNPq agency
[302583/2015-7]; NASA
FX The work of R.H. is financially supported by Fundacao de Amparo a
Pesquisa do Estado de Sao Paulo (FAPESP) through a postdoctoral research
fellowship at INPE and by ANR under the financial agreement
ANR-15-CE31-0009-01 at LPC2E/CNRS. E.E. would like to thank Brazilian
CNPq (302583/2015-7) agency for financial support. Portions of this
research were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. The SuperMAG data
were collected from the website: http://supermag.jhuapl.edu/. The solar
wind/interplanetary data were collected from OMNI website:
http://omniweb.gsfc.nasa.gov/. The geomagnetic indices we collected are
from the World Data Center for Geomagnetism, Kyoto, Japan
http://wdc.kugi.kyoto-u.ac.jp/, and the F10.7 solar flux from
http://www.drao.nrc.ca/icarus.
NR 73
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7805
EP 7816
DI 10.1002/2015JA021835
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500034
ER
PT J
AU Fung, SF
Tepper, JA
Cai, X
AF Fung, Shing F.
Tepper, Julia A.
Cai, Xia
TI Magnetospheric state of sawtooth events
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND; SUBSTORMS
AB Magnetospheric sawtooth events, first identified in the early 1990s, are named for their characteristic appearance of multiple quasiperiodic intervals of slow decrease followed by sharp increase of proton differential energy fluxes in the geosynchronous region. The successive proton flux oscillations have been interpreted as recurrences of stretching and dipolarization of the nightside geomagnetic field. Due to their often extended intervals with 2-10 cycles, sawteeth occurrences are sometimes referred to as a magnetospheric mode. While studies of sawtooth events over the past two decades have yielded a wealth of information about such events, the magnetospheric state conditions for the occurrence of sawtooth events and how sawtooth oscillations may depend on the magnetospheric state conditions remain unclear. In this study, we investigate the characteristic magnetospheric state conditions (specified by Psw interplanetary magnetic field (IMF) Btot, IMF Bz Vsw, AE, Kp and Dst, all time shifted with respect to one another) associated with the intervals before, during, and after sawteeth occurrences. Applying a previously developed statistical technique, wehave determined the most probable magnetospheric states propitious for the development and occurrence of sawtooth events, respectively. The statistically determined sawtooth magnetospheric state has also been validated by using out-of-sample events, confirming the notion that sawtooth intervals might represent a particular global state of the magnetosphere. We propose that the "sawtooth state" of the magnetosphere may be a state of marginal stability in which a slight enhancement in the loading rate of an otherwise continuous loading process can send the magnetosphere into the marginally unstable regime, causing it to shed limited amount of energy quickly and return to the marginally stable regime with the loading process continuing. Sawtooth oscillations result as the magnetosphere switches between the marginally stable (loading) and unstable (unloading) phases.
C1 [Fung, Shing F.; Tepper, Julia A.] NASA, Geophys Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tepper, Julia A.] Univ Maryland, College Pk, MD 20742 USA.
[Cai, Xia] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Fung, SF (reprint author), NASA, Geophys Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM shing.f.fung@nasa.gov
FU National Space Club Scholar Program
FX The authors would like to thank the NASA Space Physics Data Facility
(SPDF) for making the OMNI data set available. One of us (J. Tepper)
would like to thank the National Space Club Scholar Program for a 2015
summer internship opportunity to work at the NASA Goddard Space Flight
Center, Greenbelt, MD.
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7860
EP 7869
DI 10.1002/2016JA022693
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500038
ER
PT J
AU Collinson, GA
McFadden, JP
Chornay, DJ
Gershman, D
Moore, TE
AF Collinson, Glyn A.
McFadden, James P.
Chornay, Dennis J.
Gershman, Daniel
Moore, Thomas E.
TI Constraining electric fields from electrostatic deflector plates: A
brief report and case study from the Fast Plasma Investigation for the
Magnetospheric Multiscale Mission
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EXPRESS MISSION; SPACE PLASMAS; ANALYZER; INSTRUMENT
AB A common feature of top hat space plasma analyzers are electrostatic "deflector plates" mounted externally to the aperture which steer the incoming particles and permit the sensor to rapidly scan the sky without moving. However, the electric fields generated by these plates can penetrate the mesh or grid on the outside of the sensor, potentially violating spacecraft electromagnetic cleanliness requirements. In this brief report we discuss how this issue was addressed for the Dual Electron Spectrometer for the Magnetospheric Multiscale Mission using a double-grid system and the simple modeling technique employed to assure the safe containment of the stray fields from its deflector plates.
C1 [Collinson, Glyn A.; Chornay, Dennis J.; Gershman, Daniel; Moore, Thomas E.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[McFadden, James P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chornay, Dennis J.; Gershman, Daniel] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Collinson, GA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
EM glyn.collinson@gmail.com
NR 23
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7887
EP 7894
DI 10.1002/2016JA022590
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500041
ER
PT J
AU Murphy, KR
Mann, IR
Rae, IJ
Sibeck, DG
Watt, CEJ
AF Murphy, Kyle R.
Mann, Ian R.
Rae, I. Jonathan
Sibeck, David G.
Watt, Clare E. J.
TI Accurately characterizing the importance of wave-particle interactions
in radiation belt dynamics: The pitfalls of statistical wave
representations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Editorial Material
ID SOLAR-WIND; DIFFUSION; ELECTRONS; CHORUS; ACCELERATION; MAGNETOPAUSE;
MODEL
AB Wave-particle interactions play a crucial role in energetic particle dynamics in the Earth's radiation belts. However, the relative importance of different wave modes in these dynamics is poorly understood. Typically, this is assessed during geomagnetic storms using statistically averaged empirical wave models as a function of geomagnetic activity in advanced radiation belt simulations. However, statistical averages poorly characterize extreme events such as geomagnetic storms in that storm-time ultralow frequency wave power is typically larger than that derived over a solar cycle and Kp is a poor proxy for storm-time wave power.
C1 [Murphy, Kyle R.; Sibeck, David G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Mann, Ian R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada.
[Rae, I. Jonathan] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking, Surrey, England.
[Watt, Clare E. J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Murphy, KR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM kyle.r.murphy@nasa.gov
RI Watt, Clare/C-5218-2008;
OI Watt, Clare/0000-0003-3193-8993; Mann, Ian/0000-0003-1004-7841
NR 32
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7895
EP 7899
DI 10.1002/2016JA022618
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500042
PM 27867798
ER
PT J
AU Clark, G
Cohen, I
Westlake, JH
Andrews, GB
Brandt, P
Gold, RE
Gkioulidou, MA
Hacala, R
Haggerty, D
Hill, ME
Ho, GC
Jaskulek, SE
Kollmann, P
Mauk, BH
McNutt, RL
Mitchell, DG
Nelson, KS
Paranicas, C
Paschalidis, N
Schlemm, CE
AF Clark, G.
Cohen, I.
Westlake, J. H.
Andrews, G. B.
Brandt, P.
Gold, R. E.
Gkioulidou, M. A.
Hacala, R.
Haggerty, D.
Hill, M. E.
Ho, G. C.
Jaskulek, S. E.
Kollmann, P.
Mauk, B. H.
McNutt, R. L., Jr.
Mitchell, D. G.
Nelson, K. S.
Paranicas, C.
Paschalidis, N.
Schlemm, C. E.
TI The "Puck" energetic charged particle detector: Design, heritage, and
advancements
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Review
ID SOLAR-WIND; SATURNS MAGNETOSPHERE; DAYSIDE MAGNETOPAUSE; OUTER
HELIOSPHERE; CARBON FOILS; FIELD LINES; SPACECRAFT; IONS; INSTRUMENT;
ELECTRON
AB Energetic charged particle detectors characterize a portion of the plasma distribution function that plays critical roles in some physical processes, from carrying the currents in planetary ring currents to weathering the surfaces of planetary objects. For several low-resource missions in the past, the need was recognized for a low-resource but highly capable, mass-species-discriminating energetic particle sensor that could also obtain angular distributions without motors or mechanical articulation. This need led to the development of a compact Energetic Particle Detector (EPD), known as the "Puck" EPD (short for hockey puck), that is capable of determining the flux, angular distribution, and composition of incident ions between an energy range of similar to 10 keV to several MeV. This sensor makes simultaneous angular measurements of electron fluxes from the tens of keV to about 1 MeV. The same measurements can be extended down to approximately 1 keV/nucleon, with some composition ambiguity. These sensors have a proven flight heritage record that includes missions such as MErcury Surface, Space ENvironment, GEochemistry, and Ranging and New Horizons, with multiple sensors on each of Juno, Van Allen Probes, and Magnetospheric Multiscale. In this review paper we discuss the Puck EPD design, its heritage, unexpected results from these past missions and future advancements. We also discuss high-voltage anomalies that are thought to be associated with the use of curved foils, which is a new foil manufacturing processes utilized on recent Puck EPD designs. Finally, we discuss the important role Puck EPDs can potentially play in upcoming missions.
C1 [Clark, G.; Cohen, I.; Westlake, J. H.; Andrews, G. B.; Brandt, P.; Gold, R. E.; Gkioulidou, M. A.; Hacala, R.; Haggerty, D.; Hill, M. E.; Ho, G. C.; Jaskulek, S. E.; Kollmann, P.; Mauk, B. H.; McNutt, R. L., Jr.; Mitchell, D. G.; Nelson, K. S.; Paranicas, C.; Schlemm, C. E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Paschalidis, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Clark, G (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM george.clark@jhuapl.edu
RI Cohen, Ian/K-3038-2015; Paranicas, Christopher/B-1470-2016; Mauk,
Barry/E-8420-2017
OI Cohen, Ian/0000-0002-9163-6009; Paranicas,
Christopher/0000-0002-4391-8255; Mauk, Barry/0000-0001-9789-3797
FU APL; NASA
FX We would like to recognize and thank the many engineers and scientists
(too many to mention by name) that have contributed to the development
and delivery of the Puck instruments. It is their hard work, innovative
ASIC, mechanical and electrical designs, and their very long hours spent
testing, calibrating, and qualifying the hardware, that have directly
made the Pucks the innovative and successful instruments that they are.
We would also like to acknowledge the support of APL and NASA. Data
supporting this work will be made available upon request
(george.clark@jhuapl.edu).
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG
PY 2016
VL 121
IS 8
BP 7900
EP 7913
DI 10.1002/2016JA022579
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4EQ
UT WOS:000385811500043
PM 27867799
ER
PT J
AU Ohta, Y
Fukagawa, M
Sitko, ML
Muto, T
Kraus, S
Grady, CA
Wisniewski, JP
Swearingen, JR
Shibai, H
Sumi, T
Hashimoto, J
Kudo, T
Kusakabe, N
Momose, M
Okamoto, Y
Kotani, T
Takami, M
Currie, T
Thalmann, C
Janson, M
Akiyama, E
Follette, KB
Mayama, S
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Egner, SE
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, H
Takato, N
Terada, H
Tomono, D
Turner, EL
Usuda, T
Watanabe, M
Yamada, T
Tamura, M
AF Ohta, Yurina
Fukagawa, Misato
Sitko, Michael L.
Muto, Takayuki
Kraus, Stefan
Grady, Carol A.
Wisniewski, John P.
Swearingen, Jeremy R.
Shibai, Hiroshi
Sumi, Takahiro
Hashimoto, Jun
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Momose, Munetake
Okamoto, Yoshiko
Kotani, Takayuki
Takami, Michihiro
Currie, Thayne
Thalmann, Christian
Janson, Markus
Akiyama, Eiji
Follette, Katherine B.
Mayama, Satoshi
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
McElwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Hideki
Takato, Naruhisa
Terada, Hiroshi
Tomono, Daigo
Turner, Edwin L.
Usuda, Tomonori
Watanabe, Makoto
Yamada, Toru
Tamura, Motohide
TI Extreme asymmetry in the polarized disk of V1247 Orionis
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE planetary systems; protoplatenary disks; stars: individual (V1247
Orionis); techniques: polarimetric; techniques: high angular resolution
ID PRE-MAIN-SEQUENCE; HERBIG AE STARS; PROTOPLANETARY DISK; TRANSITIONAL
DISK; HD 142527; SCATTERED-LIGHT; CIRCUMSTELLAR DISK; PLANET FORMATION;
SAO 206462; MWC 758
AB We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of similar to 0.'' 14-0.'' 86 (54-330 au) from the central star. The polarized intensity image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0.'' 28 +/- 0.'' 09 in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at less than or similar to 46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc.
C1 [Ohta, Yurina; Fukagawa, Misato; Shibai, Hiroshi; Sumi, Takahiro; Matsuo, Taro] Osaka Univ, Grad Sch Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
[Fukagawa, Misato; Hashimoto, Jun; Kotani, Takayuki; Akiyama, Eiji; Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Terada, Hiroshi; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Fukagawa, Misato] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
[Sitko, Michael L.; Swearingen, Jeremy R.] Univ Cincinnati, Dept Phys, 400 Geol Phys Bldg,POB 210011, Cincinnati, OH 45221 USA.
[Sitko, Michael L.] Space Sci Inst, 475 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinijuku Ku, 1-24-2 Nishi Shinjuku, Tokyo 1638677, Japan.
[Kraus, Stefan] Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Grady, Carol A.] Eureka Sci Inc, 2452 Delmer St Suite 100, Oakland, CA 94602 USA.
[Grady, Carol A.; McElwain, Michael W.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Takato, Naruhisa; Tomono, Daigo] Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA.
[Momose, Munetake; Okamoto, Yoshiko] Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Follette, Katherine B.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange UMR 7293, 28 Ave Valrose, F-06108 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Muunchen, Scheinerstr 1, D-81679 Munich, Germany.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Kwon, Jungmi; Takahashi, Yasuhiro H.; Tamura, Motohide] Univ Tokyo, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan.
[Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, 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 Fukagawa, M (reprint author), Osaka Univ, Grad Sch Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.; Fukagawa, M (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Fukagawa, M (reprint author), Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
EM fukagawa@u.phys.nagoya-u.ac.jp
RI MIYAMA, Shoken/A-3598-2015;
OI Feldt, Markus/0000-0002-4188-5242
FU MEXT KAKENHI [23103005]; STFC Ernest Rutherford Fellowship
[ST/J004030/1]; Marie Curie CIG grant [SH-06192]
FX This work is supported by MEXT KAKENHI No. 23103005. S.K. acknowledges
support from an STFC Ernest Rutherford Fellowship (ST/J004030/1) and
Marie Curie CIG grant (SH-06192).
NR 61
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD AUG
PY 2016
VL 68
IS 4
AR 53
DI 10.1093/pasj/psw051
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ1XB
UT WOS:000385634000007
ER
PT J
AU Tanaka, YT
Gonzalez, JB
Itoh, R
Finke, JD
Inoue, Y
Ojha, R
Carpenter, B
Lindfors, E
Krauss, F
Desiante, R
Shiki, K
Fukazawa, Y
Longo, F
McEnery, JE
Buson, S
Nilsson, K
Ramazani, VF
Reinthal, R
Takalo, L
Pursimo, T
Boschin, W
AF Tanaka, Yasuyuki T.
Gonzalez, Josefa Becerra
Itoh, Ryosuke
Finke, Justin D.
Inoue, Yoshiyuki
Ojha, Roopesh
Carpenter, Bryce
Lindfors, Elina
Krauss, Felicia
Desiante, Rachele
Shiki, Kensei
Fukazawa, Yasushi
Longo, Francesco
McEnery, Julie E.
Buson, Sara
Nilsson, Kari
Ramazani, Vandad Fallah
Reinthal, Riho
Takalo, Leo
Pursimo, Tapio
Boschin, Walter
TI A significant hardening and rising shape detected in the MeV/GeV nu F-nu
spectrum from the recently discovered very-high-energy blazar S4 0954+65
during the bright optical flare in 2015 February
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE BL Lacertae objects: individual (S4 0954+65); galaxies: active;
galaxies: jets; gamma rays: galaxies; X-rays: galaxies
ID LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; BL-LAC OBJECTS;
GAMMA-RAY; COMPTON ANALYSIS; COMPLETE SAMPLE; SOURCE CATALOG; RADIO
QUASARS; PKS 1441+25; FERMI-LAT
AB We report on Fermi Large Area Telescope (LAT) and multi-wavelength results on the recently discovered very-high-energy (VHE, E > 100 GeV) blazar S4 0954+65 (z = 0.368) during an exceptionally bright optical flare in 2015 February. During the time period (2015 February 13/14, or MJD57067) when the MAGIC telescope detected VHE gamma-ray emission from the source, the Fermi-LAT data indicated a significant spectral hardening at GeV energies, with a power-law photon index of 1.8 +/- 0.1-compared with the 3FGL (The Fermi LAT 4-Year Point Source Catalog) value (averaged over four years of observation) of 2.34 +/- 0.04. In contrast, Swift X-Ray Telescope data showed a softening of the X-ray spectrum, with a photon index of 1.72 +/- 0.08 (compared with 1.38 +/- 0.03 averaged during the flare from MJD 57066 to 57077), possibly indicating a modest contribution of synchrotron photons by the highest-energy electrons superposed on the inverse Compton component. Fitting of the quasi-simultaneous (<1 d) broad-band spectrum with a one-zone synchrotron plus inverse-Compton model revealed that GeV/TeV emission could be produced by inverse-Compton scattering of external photons from the dust torus. We emphasize that a flaring blazar showing high flux of greater than or similar to 1.0 x 10(-6) photons cm(-2) s(-1) (E > 100 MeV) and a hard spectral index of Gamma(GeV) < 2.0 detected by Fermi-LAT on daily timescales is a promising target for TeV follow-up by ground-based Cherenkov telescopes to discover high-redshift blazars, investigate their temporal variability and spectral features in the VHE band, and also constrain the intensity of the extragalactic background light.
C1 [Tanaka, Yasuyuki T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan.
[Gonzalez, Josefa Becerra; Ojha, Roopesh; Carpenter, Bryce; McEnery, Julie E.; Buson, Sara] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Gonzalez, Josefa Becerra; McEnery, Julie E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, Josefa Becerra; McEnery, Julie E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Itoh, Ryosuke; Shiki, Kensei; Fukazawa, Yasushi] Hiroshima Univ, Dept Phys Sci, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan.
[Finke, Justin D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Inoue, Yoshiyuki] JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Ojha, Roopesh; Buson, Sara] Univ Maryland, Ctr Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Ojha, Roopesh; Carpenter, Bryce] Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
[Lindfors, Elina; Ramazani, Vandad Fallah; Reinthal, Riho; Takalo, Leo] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Krauss, Felicia] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
[Krauss, Felicia] Univ Wurzburg, Inst Theoret Phys & Astrophys, Emil Fischer Str 31, D-97074 Wurzburg, Germany.
[Desiante, Rachele] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Desiante, Rachele] Univ Udine, Dipartimento Sci Matemat Informat & Fis, Via Palladio 8, I-33100 Udine, Italy.
[Longo, Francesco] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Udine, Italy.
[Longo, Francesco] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Nilsson, Kari] Univ Turku, Finnish Ctr Astron ESO, Vaisalantie, FI-21500 Piikkio, Finland.
[Pursimo, Tapio] Nord Opt Telescope, Apartado 474, E-38700 Santa Cruz De La Palma, Santa Cruz De T, Spain.
[Boschin, Walter] Fdn G Galilei INAF Telescopio Nazl Galileo, Rambla JA Fernandez Perez 7, E-38712 Brena Baja, La Palma, Spain.
[Boschin, Walter] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Boschin, Walter] Univ La Laguna, Dept Astrofis, Av Astrofis F Sanchez S-N, E-38205 San Cristobal la Laguna, Tenerife, Spain.
RP Tanaka, YT (reprint author), Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan.
EM ytanaka@hep01.hepl.hiroshima-u.ac.jp
FU NASA [NNH12ZDA001N, NNH13ZDA001N-FERMI]; Kakenhi [15K17652]
FX We appreciate the referee's careful reading and valuable comments. The
Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. This
research was funded in part by NASA through Fermi Guest Investigator
grants NNH12ZDA001N and NNH13ZDA001N-FERMI. This research has made use
of NASA's Astrophysics Data System. YTT is supported by Kakenhi
15K17652.
NR 55
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD AUG
PY 2016
VL 68
IS 4
AR 51
DI 10.1093/pasj/psw049
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ1XB
UT WOS:000385634000005
ER
PT J
AU Thomas, BF
Landerer, FW
Wiese, DN
Famiglietti, JS
AF Thomas, Brian F.
Landerer, Felix W.
Wiese, David N.
Famiglietti, James S.
TI A comparison of watershed storage trends over the eastern and upper
Midwestern regions of the United States, 2003-2015
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE base flow recession; watershed Storage; GRACE
ID RENEWABLE GROUNDWATER STRESS; BASEFLOW RECESSION ANALYSIS; HYDROLOGICAL
MODELS; CLIMATE MODELS; TIME-SERIES; MIDDLE-EAST; RIVER-BASIN; LOW-FLOW;
GRACE; DROUGHT
AB Basin-scale groundwater storage trends calculated from long-term streamflow records provide insight into the evolution of watershed behaviors. Our study presents the first spatially relevant validation of recession-based trend approaches by comparing three independent storage trend estimates using GRACE-derived groundwater storage, in situ groundwater elevation observations, and recession-based approaches for the time period of 2003-2015. Results documented consistent agreement between spatially interpolated groundwater observation trends and recession-based storage trends, while GRACE-derived groundwater trends were found to exhibit variable, poor comparisons. A decreasing trend in watershed storage was identified in the southeastern U.S. while increasing trends were identified in the northeast and upper Midwest estimated from recession-based approaches. Our recession-based approach conducted using nested watershed streamflow records identified variable watershed storage trends at scales directly applicable for comparative hydrology studies and for assisting in watershed-based water resources management decisions.
C1 [Thomas, Brian F.; Landerer, Felix W.; Wiese, David N.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Thomas, Brian F.] Univ Pittsburgh, Dept Geol & Environm Sci, Pittsburgh, PA 15260 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 Thomas, BF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Thomas, BF (reprint author), Univ Pittsburgh, Dept Geol & Environm Sci, Pittsburgh, PA 15260 USA.
EM bfthomas@pitt.edu
FU National Aeronautics and Space Administration; NASA MEaSUREs Program;
NASA GRACE Science Team
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. GRACE land data are available at
http://grace.jpl.nasa.gov, supported by the NASA MEaSUREs Program.
Support from the NASA GRACE Science Team is gratefully acknowledged. The
authors also express their appreciation to the associate editor and
three anonymous reviewers whose comments contributed to substantial
improvements to the original manuscript.
NR 122
TC 0
Z9 0
U1 11
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD AUG
PY 2016
VL 52
IS 8
BP 6335
EP 6347
DI 10.1002/2016WR018617
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA DW5KT
UT WOS:000383684400035
ER
PT J
AU Burgin, MS
van Zyl, JJ
AF Burgin, Mariko S.
van Zyl, Jakob J.
TI Analysis of Polarimetric Radar Data and Soil Moisture From Aquarius:
Towards a Regression-Based Soil Moisture Estimation Algorithm
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Moisture; polarimetric radar; soil; synthetic aperture radar (SAR); time
series
ID GEIGER CLIMATE CLASSIFICATION; BARE SOIL; BACKSCATTERING
AB Many soil moisture radar retrieval algorithms depend on substantial amounts of ancillary data, such as land cover type and soil composition. To address this issue, we examine and expand an empirical approach by Kim and van Zyl as an alternative; it describes radar backscatter of a vegetated scene as a linear function of volumetric soil moisture, thus reducing the dependence on ancillary data. We use 2.5 years of L-band Aquarius radar and radiometer derived soil moisture data to determine the two polarization dependent parameters on a global scale and on a weekly basis. We propose a look-up table based soil moisture estimation approach; it is promising due to its simplicity and independence of ancillary data. However, the estimation performance is found to be impacted by the used land cover classification scheme. Our results show that the sensitivity of the radar signal to soil moisture changes seasonally, and that the variation differs depending on vegetation class. While this seasonal variation can be relatively small, it must be properly accounted for as it impacts the soil moisture retrieval accuracy.
C1 [Burgin, Mariko S.; van Zyl, Jakob J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Burgin, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mariko.s.burgin@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 18
TC 0
Z9 0
U1 10
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD AUG
PY 2016
VL 9
IS 8
SI SI
BP 3497
EP 3504
DI 10.1109/JSTARS.2016.2526899
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DY2EZ
UT WOS:000384907200014
ER
PT J
AU Domagal-Goldman, SD
Wright, KE
Adamala, K
de la Rubia, LA
Bond, J
Dartnell, LR
Goldman, AD
Lynch, K
Naud, ME
Paulino-Lima, IG
Singer, K
Walter-Antonio, M
Abrevaya, XC
Anderson, R
Arney, G
Atri, D
Azua-Bustos, A
Bowman, JS
Brazelton, WJ
Brennecka, GA
Carns, R
Chopra, A
Colangelo-Lillis, J
Crockett, CJ
DeMarines, J
Frank, EA
Frantz, C
de la Fuente, E
Galante, D
Glass, J
Gleeson, D
Glein, CR
Goldblatt, C
Horak, R
Horodyskyj, L
Kacar, B
Kereszturi, A
Knowles, E
Mayeur, P
McGlynn, S
Miguel, Y
Montgomery, M
Neish, C
Noack, L
Rugheimer, S
Stuken, EE
Tamez-Hidalgo, P
Walker, SI
Wong, T
AF Domagal-Goldman, Shawn D.
Wright, Katherine E.
Adamala, Katarzyna
de la Rubia, Leigh Arina
Bond, Jade
Dartnell, Lewis R.
Goldman, Aaron D.
Lynch, Kennda
Naud, Marie-Eve
Paulino-Lima, Ivan G.
Singer, Kelsi
Walter-Antonio, Marina
Abrevaya, Ximena C.
Anderson, Rika
Arney, Giada
Atri, Dimitra
Azua-Bustos, Armando
Bowman, Jeff S.
Brazelton, William J.
Brennecka, Gregory A.
Carns, Regina
Chopra, Aditya
Colangelo-Lillis, Jesse
Crockett, Christopher J.
DeMarines, Julia
Frank, Elizabeth A.
Frantz, Carie
de la Fuente, Eduardo
Galante, Douglas
Glass, Jennifer
Gleeson, Damhnait
Glein, Christopher R.
Goldblatt, Colin
Horak, Rachel
Horodyskyj, Lev
Kacar, Betul
Kereszturi, Akos
Knowles, Emily
Mayeur, Paul
McGlynn, Shawn
Miguel, Yamila
Montgomery, Michelle
Neish, Catherine
Noack, Lena
Rugheimer, Sarah
Stueken, Eva E.
Tamez-Hidalgo, Paulina
Walker, Sara Imari
Wong, Teresa
TI The Astrobiology Primer v2.0
SO ASTROBIOLOGY
LA English
DT Article
ID MARTIAN METEORITE ALH84001; EARTH-LIKE PLANETS; LATE HEAVY BOMBARDMENT;
TEMPLATE-DIRECTED SYNTHESIS; SITE-SPECIFIC INCORPORATION; UNIVERSAL
COMMON ANCESTOR; TRANSITION-METAL SULFIDES; HORIZONTAL GENE-TRANSFER;
PERMIAN MASS EXTINCTION; BANDED IRON FORMATIONS
C1 [Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Domagal-Goldman, Shawn D.] Virtual Planetary Lab, Seattle, WA USA.
[Wright, Katherine E.] Univ Colorado, Boulder, CO 80309 USA.
[Wright, Katherine E.] UK Space Agcy, Swindon, Wilts, England.
[Adamala, Katarzyna] Univ Minnesota, Dept Genet Cell Biol & Dev, Minneapolis, MN USA.
[de la Rubia, Leigh Arina] Tennessee State Univ, Nashville, TN 37203 USA.
[Bond, Jade] Univ New South Wales, Dept Phys, Sydney, NSW, Australia.
[Dartnell, Lewis R.] Univ Westminster, London, England.
[Goldman, Aaron D.] Oberlin Coll, Oberlin, OH 44074 USA.
[Lynch, Kennda] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA.
[Naud, Marie-Eve] Univ Montreal, Inst Res Exoplanets IREx, Montreal, PQ, Canada.
[Paulino-Lima, Ivan G.] Univ Space Res Assoc, Mountain View, CA USA.
[Paulino-Lima, Ivan G.; Atri, Dimitra; Azua-Bustos, Armando; DeMarines, Julia; Walker, Sara Imari] Blue Marble Space Inst Sci, Seattle, WA USA.
[Singer, Kelsi] Southwest Res Inst, Boulder, CO USA.
[Walter-Antonio, Marina] Mayo Clin, Rochester, MN USA.
[Abrevaya, Ximena C.] UBA, CONICET, IAFE, Buenos Aires, DF, Argentina.
[Anderson, Rika] Carleton Coll, Dept Biol, Northfield, MN 55057 USA.
[Arney, Giada] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Arney, Giada] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Azua-Bustos, Armando] Univ Autonoma Chile, Ctr Invest Biomed, Santiago, Chile.
[Bowman, Jeff S.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Brazelton, William J.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Brennecka, Gregory A.] Univ Munster, Inst Planetol, Munster, Germany.
[Carns, Regina] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[Chopra, Aditya] Australian Natl Univ, Planetary Sci Inst, Res Sch Earth Sci, Res Sch Astron & Astrophys, Canberra, ACT, Australia.
[Colangelo-Lillis, Jesse] McGill Univ, Earth & Planetary Sci, Montreal, PQ, Canada.
[Colangelo-Lillis, Jesse] McGill Space Inst, Montreal, PQ, Canada.
[Crockett, Christopher J.] Soc Sci & Publ, Washington, DC USA.
[Frank, Elizabeth A.] Carnegie Inst Sci, Washington, DC 20005 USA.
[Frantz, Carie] Weber State Univ, Dept Geosci, Ogden, UT 84408 USA.
[de la Fuente, Eduardo] Univ Guadalajara, Dept Fis, CUCEI, IAM, Guadalajara, Jalisco, Mexico.
[Galante, Douglas] Brazilian Synchrotron Light Lab, Campinas, SP, Brazil.
[Glass, Jennifer] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Gleeson, Damhnait] Sci Fdn Ireland, Dublin, Ireland.
[Glein, Christopher R.] Southwest Res Inst, San Antonio, TX USA.
[Goldblatt, Colin] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC, Canada.
[Horak, Rachel] Amer Soc Microbiol, Washington, DC USA.
[Horodyskyj, Lev] Arizona State Univ, Tempe, AZ USA.
[Kacar, Betul] Harvard Univ, Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Kereszturi, Akos] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Budapest, Hungary.
[Knowles, Emily] Johnson & Wales Univ, Denver, CO USA.
[Mayeur, Paul] Rensselaer Polytech Inst, Troy, NY USA.
[McGlynn, Shawn] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo, Japan.
[Miguel, Yamila] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, UMR 7293,CNRS, Nice, France.
[Montgomery, Michelle] Univ Cent Florida, Orlando, FL 32816 USA.
[Neish, Catherine] Univ Western Ontario, Dept Earth Sci, London, ON, Canada.
[Noack, Lena] Royal Observ Belgium, Brussels, Belgium.
[Rugheimer, Sarah] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Rugheimer, Sarah] Univ St Andrews, St Andrews, Fife, Scotland.
[Stueken, Eva E.] Univ Washington, Seattle, WA 98195 USA.
[Stueken, Eva E.] Univ Calif Riverside, Riverside, CA 92521 USA.
[Tamez-Hidalgo, Paulina] Novozymes AS, Bagsvaerd, Denmark.
[Walker, Sara Imari] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Walker, Sara Imari] Arizona State Univ, Ctr Fundamental Concepts Sci, Tempe, AZ USA.
[Wong, Teresa] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
RP Domagal-Goldman, SD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.; Domagal-Goldman, SD (reprint author), Virtual Planetary Lab, Seattle, WA USA.; Domagal-Goldman, SD (reprint author), NASA, Planetary Environments Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Stop 699-0, Washington, MD 20771 USA.
EM shawn.goldman@nasa.gov
RI azua-bustos, armando/P-8787-2016; Galante, Douglas/G-8752-2011; Lynch,
Kennda/C-4011-2011;
OI Galante, Douglas/0000-0002-3265-2527; Lynch, Kennda/0000-0001-5229-5515;
Frantz, Carie/0000-0003-2544-9245; Rugheimer, Sarah/0000-0003-1620-7658
FU NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team;
National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH05ZDA001C, NNH12ZDA002C, NNA08CN87A,
NNA13AA93A]; Baldrich Chile and Kingston Technology, Chile; Australian
National University; University of Washington Astrobiology Program; NASA
Astrobiology Postdoctoral Fellowship Program; Virtual Planetary
Laboratory; (NKFIH) projects [COST TD1308, COOP-NN-116927]; NAI
Astrobiology Biogeocatalysis Research Center; NSF-IGERT Program in
Geobiological Systems at Montana State University; Helmholtz Alliance
"Planetary Evolution and Life"; Interuniversity Attraction Poles
Programme - Belgian Science Policy Office through the Planet Topers
alliance; Carnegie Institution for Science; NASA Astrobiology Institute
through a NASA Postdoctoral Program Fellowship; NAI Early Career
Research Collaboration Fellowship; NASA Exobiology and Evolutionary
Biology [NNX13AI08G]; NASA Astrobiology Institute through the NASA
Postdoctoral Program; NASA Harriet Jenkins Pre-doctoral Fellowship; CSM
Bechtel K-5 Excellence in Education Initiative; NSF; ARC; CONICET;
Lamont-Doherty Earth Observatory; Argentinian National Council of
Scientific and Technological Research (CONICET)
FX Individual author acknowledgements follow. S.D.D.G. would like to
acknowledge support from the NASA Astrobiology Institute's Virtual
Planetary Laboratory Lead Team, supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
solicitations NNH05ZDA001C and NNH12ZDA002C and Cooperative Agreement
NNA08CN87A and NNA13AA93A. K.E.W. acknowledges the David and Lucille
Packard Foundation. A.A.B. would like to acknowledge support from
Baldrich Chile and Kingston Technology, Chile. A.C. acknowledges support
from the Australian National University. E.E.S. acknowledges support
from the University of Washington Astrobiology Program. W.J.B.
acknowledges support from the University of Washington Astrobiology
Program and the NASA Astrobiology Postdoctoral Fellowship Program.
R.E.A. acknowledges support from the University of Washington
Astrobiology Program and the NASA Astrobiology Postdoctoral Fellowship
Program. G.N.A. acknowledges support from the University of Washington
Astrobiology Program and the Virtual Planetary Laboratory. P.M.
acknowledges the New York Center for Astrobiology NASA Astrobiology
Institute. D.G. would like to acknowledge the Brazilian Research Unity
in Astrobiology (NAP/Astrobio) from the University of Sao Paulo, and the
Sao Paulo Research Foundation (Fapesp). I.G.P.L. would like to
acknowledge the Brazilian National Council for Scientific and
Technological Development (CNPq), Coordination for the Improvement of
Higher Education Personnel in Brazil (CAPES), NASA Postdoctoral Program
administered by Oak Ridge Associated Universities (NPP/ORAU), and Blue
Marble Space Institute of Science (BMSIS). A.K. acknowledges support
from COST TD1308 and COOP-NN-116927 (NKFIH) projects. S.E.M.
acknowledges support from the NAI Astrobiology Biogeocatalysis Research
Center and the NSF-IGERT Program in Geobiological Systems at Montana
State University. L.N. acknowledges funding by the Helmholtz Alliance
"Planetary Evolution and Life" and the Interuniversity Attraction Poles
Programme initiated by the Belgian Science Policy Office through the
Planet Topers alliance. This work results within the collaboration of
the COST Action TD 1308. C.R.G. acknowledges support from the Carnegie
Institution for Science. B.K. acknowledges support from the NASA
Astrobiology Institute through a NASA Postdoctoral Program Fellowship,
the NAI Early Career Research Collaboration Fellowship and the NASA
Exobiology and Evolutionary Biology grant under solicitation NNX13AI08G.
S.I.W. acknowledges support from the NASA Astrobiology Institute through
the NASA Postdoctoral Program. J.C.L. acknowledges support from the
University of Washington Astrobiology Program. K.L.L. would like to
acknowledge support from the NASA Harriet Jenkins Pre-doctoral
Fellowship and the CSM Bechtel K-5 Excellence in Education Initiative.
C.F. acknowledges the support of an NSF graduate research fellowship.
J.B. acknowledges the support of the ARC. Y.M. acknowledges the support
of the CONICET graduate research fellowship. A.D.G. acknowledges support
from the NASA Astrobiology Institute through the NASA Postdoctoral
Program. J.S.B. acknowledges an institutional postdoctoral fellowship
from the Lamont-Doherty Earth Observatory. J.B. acknowledges the support
of the ARC. Y.M. acknowledges the support of the Argentinian National
Council of Scientific and Technological Research (CONICET) graduate
research fellowship. A.D.G. acknowledges support from the NASA
Astrobiology Institute through the NASA Postdoctoral Program. X.C.A.;
acknowledges the support from the Argentinian National Council of
Scientific and Technological Research (CONICET).
NR 865
TC 0
Z9 0
U1 33
U2 33
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 AUG
PY 2016
VL 16
IS 8
BP 561
EP 653
DI 10.1089/ast.2015.1460
PG 93
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DU4TW
UT WOS:000382206500001
PM 27532777
ER
PT J
AU Voytek, MA
AF Voytek, Mary A.
TI NASA Astrobiology Strategy 2015
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 [Voytek, Mary A.] NASA Headquarters, Astrobiol, Sci Mission Directorate, Room 3B52, Washington, DC 20546 USA.
RP Voytek, MA (reprint author), NASA Headquarters, Astrobiol, Sci Mission Directorate, Room 3B52, Washington, DC 20546 USA.
EM mary.voytek-1@nasa.gov
NR 0
TC 0
Z9 0
U1 7
U2 7
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 AUG
PY 2016
VL 16
IS 8
BP 654
EP 656
DI 10.1089/ast.2016.78201.es
PG 3
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DU4TW
UT WOS:000382206500002
ER
PT J
AU Cady, SL
Boston, P
AF Cady, Sherry L.
Boston, Penelope
TI Interview with Penelope Boston, Director of the NASA Astrobiology
Institute
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 [Cady, Sherry L.] Pacific Northwest Natl Lab EMSL, Richland, WA 99354 USA.
[Boston, Penelope] NASA, Ames Res Ctr, NASA Astrobiol Inst, Moffett Field, CA 94035 USA.
RP Cady, SL (reprint author), Pacific Northwest Natl Lab EMSL, Richland, WA 99354 USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
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 AUG
PY 2016
VL 16
IS 8
BP 657
EP 660
DI 10.1089/ast.2016.79002.pb
PG 4
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DU4TW
UT WOS:000382206500003
PM 27532779
ER
PT J
AU Chan, AA
Bashir, M
Duval, K
Vaishampayan, PA
Love, S
Lee, DJ
AF Chan, A. A.
Bashir, M.
Duval, K.
Vaishampayan, P. A.
Love, S.
Lee, D. J.
TI Differences in the breast ductal fluid microbiome from healthy women vs.
women with a history of breast cancer
SO EUROPEAN JOURNAL OF IMMUNOLOGY
LA English
DT Meeting Abstract
CT International Congress of Immunology (ICI)
CY AUG 21-26, 2016
CL Melbourne, AUSTRALIA
C1 [Chan, A. A.; Lee, D. J.] John Wayne Canc Inst, Translat Immunol, Santa Monica, CA USA.
[Bashir, M.; Vaishampayan, P. A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA.
[Bashir, M.] Med Univ Graz, Div Endocrinol & Metab, Graz, Austria.
[Duval, K.] Univ Calif Los Angeles, Breast Ctr, Westwood, CA USA.
[Duval, K.; Love, S.] Doctor Susan Love Res Fdn, Encino, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0014-2980
EI 1521-4141
J9 EUR J IMMUNOL
JI Eur. J. Immunol.
PD AUG
PY 2016
VL 46
SU 1
SI SI
MA 455
BP 456
EP 456
PG 1
WC Immunology
SC Immunology
GA DW4KA
UT WOS:000383610401109
ER
PT J
AU Gilbert, A
Flowers, GE
Miller, GH
Rabus, BT
Van Wychen, W
Gardner, AS
Copland, L
AF Gilbert, A.
Flowers, G. E.
Miller, G. H.
Rabus, B. T.
Van Wychen, W.
Gardner, A. S.
Copland, L.
TI Sensitivity of Barnes Ice Cap, Baffin Island, Canada, to climate state
and internal dynamics
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE ice cap stability; climate; Canadian Arctic
ID SEA-LEVEL RISE; ARCTIC ARCHIPELAGO; BYLOT ISLAND; THERMAL REGIME; SHEET
MODEL; MASS-LOSS; GLACIERS; TEMPERATURE; FLOW; PRECIPITATION
AB Barnes Ice Cap is a remnant of the Laurentide Ice Sheet, which covered much of northern North America during the Last Glacial Maximum. Barnes reached a quasi-equilibrium state similar to 2000years ago and has remained similar in size since then, with a small increase during the Little Ice Age. In this study, we combine historical observations (1960-1980) with more recent satellite and airborne data (1995-2010) to drive a mass balance model coupled to a transient thermomechanical model with an adaptive mesh geometry. The model is used to characterize the current state of the ice cap and to investigate its stability as a function of climate and its own internal dynamics. On millennial time scales we show that ice flow is influenced by adjustment of an unsteady shape, by gently sloping bedrock, and by contrasting viscosities between the Pleistocene and Holocene ice. On shorter time scales, Barnes is affected by surge activity. Sensitivity tests reveal that Barnes experienced climate conditions which enabled its stability 2000 to 3000years ago but will disappear under current climate conditions in the next millennium.
C1 [Gilbert, A.; Flowers, G. E.; Rabus, B. T.] Simon Fraser Univ, Dept Earth Sci, Burnaby, BC, Canada.
[Miller, G. H.] Univ Colorado, INSTAAR, Boulder, CO 80309 USA.
[Miller, G. H.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Van Wychen, W.; Copland, L.] Univ Ottawa, Dept Geog Environm & Geomat, Ottawa, ON, Canada.
[Gardner, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Gilbert, A (reprint author), Simon Fraser Univ, Dept Earth Sci, Burnaby, BC, Canada.
EM adrieng@sfu.ca
OI Gardner, Alex/0000-0002-8394-8889
FU Natural Sciences and Engineering Research Council of Canada; Simon
Fraser University
FX We are grateful for financial support provided by the Natural Sciences
and Engineering Research Council of Canada and Simon Fraser University.
This research was enabled in part by WestGrid (www.westgrid.ca) and
Compute Canada/Calcul Canada (www.computecanada.ca). We thank Gerry
Holdsworth for providing an abundance of original literature on Barnes,
Roger Hooke and John Andrews for literature and conversations, Valentina
Radic and Alex Cannon for supplying gridded climate data, and Dan Shugar
for pointing us to the InSAR velocity data. We would like to thank
3vGeomatics Inc for the ERS SAR raw data sets and for providing access
to their computer environment to calculate the InSAR displacement map.
Bedrock topography data used in this paper were acquired by NASA's
Operation IceBridge Project. Meteorological data are available on
http://climate.weather.gc.ca/ and all other data used are available in
the cited references or included in the figures of the manuscript. We
are grateful to Roger Hooke and Andy Aschwanden for their careful
reviews of the manuscript and to Bryn Hubbard for editorial oversight.
NR 58
TC 1
Z9 1
U1 8
U2 8
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 AUG
PY 2016
VL 121
IS 8
BP 1516
EP 1539
DI 10.1002/2016JF003839
PG 24
WC Geosciences, Multidisciplinary
SC Geology
GA DX5SN
UT WOS:000384442100006
ER
PT J
AU Konduru, V
Bellur, K
Medici, EF
Allen, JS
Choi, CK
Hussey, DS
Jacobson, D
Leao, JB
McQuillen, J
Hermanson, JC
AF Konduru, Vinaykumar
Bellur, Kishan
Medici, Ezequiel F.
Allen, Jeffrey S.
Choi, Chang Kyoung
Hussey, Daniel S.
Jacobson, David
Leao, Juscelino B.
McQuillen, John
Hermanson, James C.
TI Examining Liquid Hydrogen Wettability Using Neutron Imaging
SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME
LA English
DT News Item
C1 [Konduru, Vinaykumar; Bellur, Kishan; Medici, Ezequiel F.; Allen, Jeffrey S.; Choi, Chang Kyoung] Michigan Technol Univ, Houghton, MI 49931 USA.
[Hussey, Daniel S.; Jacobson, David; Leao, Juscelino B.] NIST, Gaithersburg, MD 20899 USA.
[McQuillen, John] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
[Hermanson, James C.] Univ Washington, Seattle, WA 98195 USA.
RP Choi, CK (reprint author), Michigan Technol Univ, Houghton, MI 49931 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0022-1481
EI 1528-8943
J9 J HEAT TRANS-T ASME
JI J. Heat Transf.-Trans. ASME
PD AUG
PY 2016
VL 138
IS 8
AR 080901
PG 2
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DW9HC
UT WOS:000383966300003
ER
PT J
AU Wada, Y
Lo, MH
Yeh, PJF
Reager, JT
Famiglietti, JS
Wu, RJ
Tseng, YH
AF Wada, Yoshihide
Lo, Min-Hui
Yeh, Pat J. -F.
Reager, John T.
Famiglietti, James S.
Wu, Ren-Jie
Tseng, Yu-Heng
TI Fate of water pumped from underground and contributions to sea-level
rise
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID GROUNDWATER DEPLETION; IRRIGATION; STORAGE; CLIMATE; STRESS; TRENDS;
GRACE; CYCLE; MODEL
AB The contributions from terrestrial water sources to sea-level rise, other than ice caps and glaciers, are highly uncertain and heavily debated(1-5). Recent assessments indicate that ground-water depletion (GWD) may become the most important positive terrestrial contribution(6-10) over the next 50 years, probably equal in magnitude to the current contributions from glaciers and ice caps(6). However, the existing estimates assume that nearly 100% of groundwater extracted eventually ends up in the oceans. Owing to limited knowledge of the pathways and mechanisms governing the ultimate fate of pumped groundwater, the relative fraction of global GWD that contributes to sea-level rise remains unknown. Here, using a coupled climate-hydrological model(11,12) simulation, we show that only 80% of GWD ends up in the ocean. An increase in runoff to the ocean accounts for roughly two-thirds, whereas the remainder results from the enhanced net flux of precipitation minus evaporation over the ocean, due to increased atmospheric vapour transport from the land to the ocean. The contribution of GWD to global sea-level rise amounted to 0.02 (+/- 0.004) mm yr(-1) in 1900 and increased to 0.27 (+/- 0.04) mm yr(-1) in 2000. This indicates that existing studies have substantially overestimated the contribution of GWD to global sea-level rise by a cumulative amount of at least 10 mm during the twentieth century and early twenty-first century. With other terrestrial water contributions included, we estimate the net terrestrial water contribution during the period 1993-2010 to be +0.12 (+/- 0.04) mm yr(-1), suggesting that the net terrestrialwater contribution reported in the IPCC Fifth Assessment Report report is probably overestimated by a factor of three.
C1 [Wada, Yoshihide] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, NL-3584 CS Utrecht, Netherlands.
[Wada, Yoshihide] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Lo, Min-Hui; Wu, Ren-Jie] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10617, Taiwan.
[Yeh, Pat J. -F.] Natl Univ Singapore, Dept Civil & Environm Engn, Singapore 117576, Singapore.
[Reager, John T.; Famiglietti, James S.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Tseng, Yu-Heng] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
RP Wada, Y (reprint author), NASA Goddard Inst Space Studies, New York, NY 10025 USA.; Wada, Y (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.; Wada, Y (reprint author), Univ Utrecht, Dept Phys Geog, NL-3584 CS Utrecht, Netherlands.; Wada, Y (reprint author), Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
EM y.wada@uu.nl; minhuilo@ntu.edu.tw
RI YEH, Pat/B-2758-2011;
OI YEH, Pat/0000-0001-7629-3362; LO, MIN-HUI/0000-0002-8653-143X; Tseng,
Yu-heng/0000-0002-4816-4974
FU Japan Society for the Promotion of Science (JSPS) Oversea Research
Fellowship [JSPS-2014-878]; NASA from GRACE; Sea Level Program; Water
Initiative at the Jet Propulsion Laboratory, California Institute of
Technology; University of California Office of the President,
Multicampus Research Programs and Initiatives;
[MOST-104-2923-M-002-002-MY4]; [MOST-100-2119-M-001-029-MY5]
FX Y.W. is supported by Japan Society for the Promotion of Science (JSPS)
Oversea Research Fellowship (grant no. JSPS-2014-878). M.-H.L. is
supported by grants MOST-104-2923-M-002-002-MY4 and
MOST-100-2119-M-001-029-MY5 to National Taiwan University. J.T.R. and
J.S.F. are supported by NASA grants from the GRACE Science Team, the Sea
Level Program and by Water Initiative at the Jet Propulsion Laboratory,
California Institute of Technology. M.-H.L., J.T.R. and J.S.F. are also
supported by a grant from the University of California Office of the
President, Multicampus Research Programs and Initiatives.
NR 42
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Z9 5
U1 14
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 AUG
PY 2016
VL 6
IS 8
BP 777
EP +
DI 10.1038/NCLIMATE3001
PG 6
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU3TJ
UT WOS:000382134800016
ER
PT J
AU Deryng, D
Elliott, J
Folberth, C
Muller, C
Pugh, TAM
Boote, KJ
Conway, D
Ruane, AC
Gerten, D
Jones, JW
Khabarov, N
Olin, S
Schapho, S
Schmid, E
Yang, H
Rosenzweig, C
AF Deryng, Delphine
Elliott, Joshua
Folberth, Christian
Mueller, Christoph
Pugh, Thomas A. M.
Boote, Kenneth J.
Conway, Declan
Ruane, Alex C.
Gerten, Dieter
Jones, James W.
Khabarov, Nikolay
Olin, Stefan
Schapho, Sibyll
Schmid, Erwin
Yang, Hong
Rosenzweig, Cynthia
TI Regional disparities in the beneficial effects of rising CO2
concentrations on crop water productivity
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID CARBON-DIOXIDE ENRICHMENT; CLIMATE-CHANGE; ELEVATED CO2; WHEAT
EVAPOTRANSPIRATION; STOMATAL CONDUCTANCE; USE EFFICIENCY; MODEL; YIELD;
SOIL; NITROGEN
AB Rising atmospheric CO2 concentrations ([CO2]) are expected to enhance photosynthesis and reduce crop water use(1). However, there is high uncertainty about the global implications of these effects for future crop production and agricultural water requirements under climate change. Here we combine results from networks of field experiments(1,2) and global crop models(3) to present a spatially explicit global perspective on crop water productivity (CWP, the ratio of crop yield to evapotranspiration) for wheat, maize, rice and soybean under elevated [CO2] and associated climate change projected for a high-end greenhouse gas emissions scenario. We find CO2 effects increase global CWP by 10[0;47]%-27[7;37]% ( median[interquartile range] across the model ensemble) by the 2080s depending on crop types, with particularly large increases in arid regions (by up to 48[25; 56]% for rainfed wheat). If realized in the fields, the effects of elevated [CO2] could considerably mitigate global yield losses whilst reducing agricultural consumptive water use (4-17%). We identify regional disparities driven by differences in growing conditions across agro-ecosystems that could have implications for increasing food production without compromising water security. Finally, our results demonstrate the need to expand field experiments and encourage greater consistency in modelling the effects of rising [CO2] across crop and hydrological modelling communities.
C1 [Deryng, Delphine; Elliott, Joshua] Univ Chicago, Computat Inst, Chicago, IL 60637 USA.
[Deryng, Delphine; Elliott, Joshua; Ruane, Alex C.; Rosenzweig, Cynthia] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Deryng, Delphine] Univ East Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England.
[Folberth, Christian; Yang, Hong] Swiss Fed Inst Aquat Sci & Technol EAWAG, CH-8600 Dubendorf, Switzerland.
[Folberth, Christian; Khabarov, Nikolay] IIASA, Ecosyst Serv & Management Program, Schlosspl 1, A-2361 Laxenburg, Austria.
[Mueller, Christoph; Gerten, Dieter; Schapho, Sibyll] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Pugh, Thomas A. M.] Karlsruhe Inst Technol, IMK IFU, D-82467 Garmisch Partenkirchen, Germany.
[Pugh, Thomas A. M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
[Boote, Kenneth J.; Jones, James W.] Univ Florida, Gainesville, FL 32611 USA.
[Conway, Declan] London Sch Econ & Polit Sci, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England.
[Ruane, Alex C.; Rosenzweig, Cynthia] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Gerten, Dieter] Humboldt Univ, Dept Geog, D-10099 Berlin, Germany.
[Olin, Stefan] Lund Univ, Dept Phys Geog & Ecosyst Sci, SE-22362 Lund, Sweden.
[Schmid, Erwin] Univ Nat Resources & Life Sci, A-1180 Vienna, Austria.
RP Deryng, D (reprint author), Univ Chicago, Computat Inst, Chicago, IL 60637 USA.; Deryng, D (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.; Deryng, D (reprint author), Univ East Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England.
EM deryng@uchicago.edu
RI Deryng, Delphine/F-7417-2010; Pugh, Thomas/A-3790-2010
OI Deryng, Delphine/0000-0001-6214-7241; Pugh, Thomas/0000-0002-6242-7371
FU German Federal Ministry of Education and Research (BMBF) [01LS1201A];
Tyndall Centre for Climate Change Research; Belmont Forum grant from UK
Natural Environment Research Council [NE/L008785/1]; National Science
Foundation [SBE-0951576, GEO-1215910]; BMBF [01LN1317A]; Formas Strong
Research Environment 'land use today and tomorrow'; EU FP7 project
EMBRACE [282672]
FX This work has been conducted under the framework of ISI-MIP and in
partnership with the AgMIP community. The ISI-MIP Fast Track project was
funded by the German Federal Ministry of Education and Research (BMBF)
with project funding reference number 01LS1201A. We acknowledge the
World Climate Research Programme's Working Group on Coupled Modelling,
which is responsible for CMIP, and we thank the climate modelling groups
for producing and making available their model output. For CMIP the US
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. This work was also supported by a research
stipend from the Tyndall Centre for Climate Change Research and a
Belmont Forum grant from the UK Natural Environment Research Council
(grant no. NE/L008785/1) to D.D., by the National Science Foundation
under grants SBE-0951576 and GEO-1215910 to J.E., by the BMBF grant
01LN1317A to C.M., and by the Formas Strong Research Environment 'land
use today and tomorrow' to S.O., T.A.M.P. was supported by EU FP7
project EMBRACE (grant no. 282672). We are grateful to B. A. Kimball and
A. Leakey for pointing out appropriate literature on the FACE
experiments.
NR 64
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U1 27
U2 27
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 AUG
PY 2016
VL 6
IS 8
BP 786
EP +
DI 10.1038/NCLIMATE2995
PG 8
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU3TJ
UT WOS:000382134800018
ER
PT J
AU Tian, ZH
Yu, LY
Leckey, C
AF Tian, Zhenhua
Yu, Lingyu
Leckey, Cara
TI Rapid guided wave delamination detection and quantification in
composites using global-local sensing
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE delamination detection; phased array; spatial wavenumber imaging; laser
vibrometer; guided waves
ID PLATE-LIKE STRUCTURES; LAMB WAVE; NUMBER ANALYSIS; PHASED-ARRAY;
TRANSDUCER ARRAYS; DAMAGE DETECTION; INSPECTION; INTEGRITY; SENSORS
AB This paper presents a rapid guided ultrasonic wave inspection approach through global inspection by phased array beamforming and local damage evaluation via wavenumber analysis. The global-local approach uses a hybrid system consisting of a PZT wafer and a non-contact laser vibrometer. The overall inspection is performed in two steps. First, a phased array configured by a small number of measurements performs beamforming and beamsteering over the entire plate in order to detect and locate the presence of the damage. A local area is identified as target damage area for the second step. Then a high density wavefield measurement is taken over the target damage area and a spatial wavenumber imaging is performed to quantitatively evaluate the damage. The two-step inspection has been applied to locate and quantify impact-induced delamination damage in a carbon fiber reinforced polymer composite plate. The detected delamination location, size and shape agree well with those of an ultrasonic C-scan. For the test case studied in this work the global-local approach reduced the total composite inspection (damage detection and characterization) time by similar to 97% compared to using a full scan approach.
C1 [Tian, Zhenhua; Yu, Lingyu] Univ South Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
[Leckey, Cara] NASA, Nondestruct Evaluat Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Tian, ZH (reprint author), Univ South Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
EM tianz@email.sc.edu
FU South Carolina Research Foundation (SCRF) [SAA1-18124]; National
Aeronautics and Space Administration (NASA) Langley Research Center
[SAA1-18124]; SC NASA EPSCoR Research Grant Program [521192-USCYu]
FX The authors would like to thank (1) the non-reimbursement space act
umbrella agreement SAA1-18124 between South Carolina Research Foundation
(SCRF) and the National Aeronautics and Space Administration (NASA)
Langley Research Center, and (2) SC NASA EPSCoR Research Grant Program
521192-USCYu.
NR 55
TC 0
Z9 0
U1 6
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD AUG
PY 2016
VL 25
IS 8
AR 085042
DI 10.1088/0964-1726/25/8/085042
PG 11
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA DV9QD
UT WOS:000383275000062
ER
PT J
AU Acharya, N
Wolak, MA
Tan, T
Lee, N
Lang, AC
Taheri, M
Cunnane, D
Karasik, BS
Xi, XX
AF Acharya, Narendra
Wolak, Matthaus A.
Tan, Teng
Lee, Namhoon
Lang, Andrew C.
Taheri, Mitra
Cunnane, Dan
Karasik, Boris. S.
Xi, X. X.
TI MgB2 ultrathin films fabricated by hybrid physical chemical vapor
deposition and ion milling
SO APL MATERIALS
LA English
DT Article
ID MOLECULAR-BEAM EPITAXY; THIN-FILMS
AB In this letter, we report on the structural and transport measurements of ultrathin MgB2 films grown by hybrid physical-chemical vapor deposition followed by low incident angle Ar ion milling. The ultrathin films as thin as 1.8 nm, or 6 unit cells, exhibit excellent superconducting properties such as high critical temperature (T-c) and high critical current density (J(c)). The results show the great potential of these ultrathin films for superconducting devices and present a possibility to explore superconductivity in MgB2 at the 2D limit. (C) 2016 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution (CC BY) license.
C1 [Acharya, Narendra; Wolak, Matthaus A.; Tan, Teng; Lee, Namhoon; Xi, X. X.] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA.
[Lang, Andrew C.; Taheri, Mitra] Drexel Univ, Dept Mat Sci & Engn, Philadelphia, PA 19104 USA.
[Cunnane, Dan; Karasik, Boris. S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Tan, Teng] Chinese Acad Sci, Inst Modern Phys, Lanzhou 730000, Peoples R China.
RP Acharya, N (reprint author), Temple Univ, Dept Phys, Philadelphia, PA 19122 USA.
EM tud53450@temple.edu
FU DoD DURIP Award from office of Naval Research [N0014-12-1-077]; College
of Engineering, Temple University; NASA's Astrophysics Research and
Analysis Program - from JPL; National Aeronautics and Space
Administration
FX This work made use of CoE-NIC facility at Temple University. The CoE-NIC
is based on DoD DURIP Award No. N0014-12-1-077 from the office of Naval
Research and sponsored by the College of Engineering, Temple University.
The work at Temple University was supported by the NASA's Astrophysics
Research and Analysis Program through a contract from JPL. The work at
the Jet Propulsion Laboratory, California Institute of Technology, was
carried out under a contract with the National Aeronautics and Space
Administration.
NR 31
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Z9 4
U1 11
U2 11
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 2166-532X
J9 APL MATER
JI APL Mater.
PD AUG
PY 2016
VL 4
IS 8
AR 086114
DI 10.1063/1.4961635
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA DW8ML
UT WOS:000383910000015
ER
PT J
AU Battaglia, A
Mroz, K
Tanelli, S
Tridon, F
Kirstetter, PE
AF Battaglia, Alessandro
Mroz, Kamil
Tanelli, Simone
Tridon, Frederic
Kirstetter, Pierre-Emmanuel
TI Multiple-Scattering-Induced "Ghost Echoes" in GPM DPR Observations of a
Tornadic Supercell
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PART II; PROFILING ALGORITHM; PRECIPITATION RADAR; FAST LIDAR
AB Evidence of multiple-scattering-induced pulse stretching for the signal of both frequencies of the Dual Frequency Precipitation Radar (DPR) on the Global Precipitation Measurement (GPM) mission Core Observatory satellite is presented on the basis of collocated ground-based WSR-88D S-band observations of an extreme case: a tornadic supercell. The ground-based observations clearly show a tilted convective core with a so-called bounded weak-echo region that is, locations where precipitation is absent or extremely light at the ground while large amounts of liquid or frozen precipitation are present aloft. The satellite observations in this region show reflectivity profiles that extend all the way to the surface despite the absence of near-surface precipitation: these are here referred to as "ghost echoes." Furthermore, the Ku- and Ka-band profiles exhibit similar slopes, which is a typical sign that the observed power is almost entirely due to multiple scattering. A novel microphysical retrieval that is based on triple-frequency (S-Ku-Ka) observations shows that a dense ice core located between 4 and 14 km with particle sizes exceeding 2.5 cm and integrated ice contents exceeding 7.0 kg m(-2) is the source of the ghost echoes of the signal in the lower layers. The level of confidence of this assessment is strengthened by the availability of the S-band data, which provide the necessary additional constraints to the radar retrieval that is based on DPR data. This study shows not only that multiple-scattering contributions may become predominant at Ka already very high up in the atmosphere but also that they play a key role at Ku band within the layers close to the surface. As a result, extreme caution must be paid even in the interpretation of Ku-based retrievals (e.g., the TRMM PR dataset or any DPR retrievals that are based on the assumption that Ku band is not affected by multiple scattering) when examining extreme surface rain rates that occur in the presence of deep dense ice layers.
C1 [Battaglia, Alessandro; Mroz, Kamil] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.
[Battaglia, Alessandro; Tridon, Frederic] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England.
[Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kirstetter, Pierre-Emmanuel] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK USA.
[Kirstetter, Pierre-Emmanuel] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
RP Battaglia, A (reprint author), Univ Leicester, Univ Rd, Leicester LE1 7RH, Leics, England.
EM ab474@le.ac.uk
RI Kirstetter, Pierre/E-2305-2013; Tridon, Frederic/M-4127-2013;
OI Kirstetter, Pierre/0000-0002-7381-0229; Tridon,
Frederic/0000-0002-0436-283X; Battaglia, Alessandro/0000-0001-9243-3484
FU project "Calibration and validation studies over the North Atlantic and
United Kingdom for the Global Precipitation Mission" - United Kingdom
NERC [NE/L007169/1]
FX The work done by A. Battaglia and F. Tridon was funded by the project
"Calibration and validation studies over the North Atlantic and United
Kingdom for the Global Precipitation Mission" funded by the United
Kingdom 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; support by Dr. Ramesh Kakar is gratefully
acknowledged. Level-1 V03B-GPM data were downloaded from the
Precipitation Processing System. KCRP data were downloaded from the
National Oceanic and Atmospheric Administration National Climatic Data
Center. This research used the SPECTRE High Performance Computing
Facility at the University of Leicester.
NR 31
TC 1
Z9 1
U1 4
U2 4
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 AUG
PY 2016
VL 55
IS 8
BP 1653
EP 1666
DI 10.1175/JAMC-D-15-0136.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0DF
UT WOS:000383310400001
ER
PT J
AU Campbell, JR
Lolli, S
Lewis, JR
Gu, Y
Welton, EJ
AF Campbell, James R.
Lolli, Simone
Lewis, Jasper R.
Gu, Yu
Welton, Ellsworth J.
TI Daytime Cirrus Cloud Top-of-the-Atmosphere Radiative Forcing Properties
at a Midlatitude Site and Their Global Consequences
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID TROPICAL CIRRUS; A-TRAIN; LIDAR; PARAMETERIZATION; SCATTERING;
RETRIEVALS; CLIMATE; SENSITIVITY; AEROSOLS; FEEDBACK
AB One year of continuous ground-based lidar observations (2012) is analyzed for single-layer cirrus clouds at the NASA Micro Pulse Lidar Network site at the Goddard Space Flight Center to investigate top-of-the-atmosphere (TOA) annual net daytime radiative forcing properties. A slight positive net daytime forcing is estimated (i.e., warming): 0.07-0.67 Wm(-2) in sample-relative terms, which reduces to 0.03-0.27 W m(-2) in absolute terms after normalising to unity based on a 40% midlatitude occurrence frequency rate estimated from satellite data. Results are based on bookend solutions for lidar extinction-to-backscatter (20 and 30 sr) and corresponding retrievals of the 532-nm cloud extinction coefficient. Uncertainties due to cloud undersampling, attenuation effects, sample selection, and lidar multiple scattering are described. A net daytime cooling effect is found from the very thinnest clouds (cloud optical depth <= 0.01), which is attributed to relatively high solar zenith angles. A relationship involving positive/negative daytime cloud forcing is demonstrated as a function of solar zenith angle and cloud-top temperature. These properties, combined with the influence of varying surface albedos, are used to conceptualise how daytime cloud forcing likely varies with latitude and season, with cirrus clouds exerting less positive forcing and potentially net TOA cooling approaching the summer poles (not ice and snow covered) versus greater warming at the equator. The existence of such a gradient would lead cirrus to induce varying daytime TOA forcing annually and seasonally, making it a far greater challenge than presently believed to constrain the daytime and diurnal cirrus contributions to global radiation budgets.
C1 [Campbell, James R.] Naval Res Lab, Monterey, CA USA.
[Lolli, Simone; Lewis, Jasper R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Gu, Yu] Univ Calif Los Angeles, Los Angeles, CA USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Campbell, JR (reprint author), 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA.
EM james.campbell@nrlmry.navy.mil
RI Campbell, James/C-4884-2012
OI Campbell, James/0000-0003-0251-4550
FU NASA Radiation Sciences Program; NASA Interagency Agreement on behalf of
MPLNET [NNG15JA17P]
FX The NASA Micro Pulse Lidar Network (MPLNET) is supported by the NASA
Radiation Sciences Program (H. Maring). JRC acknowledges the support of
NASA Interagency Agreement NNG15JA17P on behalf of MPLNET.
NR 42
TC 3
Z9 3
U1 4
U2 4
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 AUG
PY 2016
VL 55
IS 8
BP 1667
EP 1679
DI 10.1175/JAMC-D-15-0217.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0DF
UT WOS:000383310400002
ER
PT J
AU Leinonen, J
Lebsock, MD
Stephens, GL
Suzuki, K
AF Leinonen, Jussi
Lebsock, Matthew D.
Stephens, Graeme L.
Suzuki, Kentaroh
TI Improved Retrieval of Cloud Liquid Water from CloudSat and MODIS
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID RADAR; ALGORITHM; CUMULUS; MODEL; LIDAR; RAIN
AB A revised version of the CloudSat MODIS cloud liquid water retrieval algorithm is presented. The new algorithm, which combines measurements of radar reflectivity and cloud optical depth, addresses issues discovered in the current CloudSat MODIS cloud water content (CWC) product. This current product is shown to be underconstrained by observations and to be too dependent on prior information incorporated into the Bayesian optimal-estimation algorithm. The most significant change made to the algorithm in this study was decreasing the number of independent variables to allow the observations to constrain the retrieved values better. The retrieval was also reformulated for improved compliance with the mathematical assumptions of the optimal-estimation algorithm. To validate the accuracy of the revised algorithm, the path integrated attenuation (PIA) of the CloudSat radar signal was computed from the algorithm results. These modeled values were compared with independent measurements of the PIA that were obtained using a surface reference technique. This comparison shows that the cloud liquid water retrieved by the algorithm is close to being unbiased. The revised algorithm was also found to be an improvement over the current CloudSat CWC product and, to a lesser degree, the MODIS-derived cloud liquid water path.
C1 [Leinonen, Jussi; Lebsock, Matthew D.; Stephens, Graeme L.] CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Suzuki, Kentaroh] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan.
RP Leinonen, J (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jussi.s.leinonen@jpl.nasa.gov
RI Suzuki, Kentaroh/C-3624-2011
FU CloudSat project
FX We are grateful to Simone Tanelli and Joseph Hardin for valuable
discussions. The research of JL, ML, and GS was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA and was supported by the CloudSat project.
NR 42
TC 1
Z9 1
U1 15
U2 15
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 AUG
PY 2016
VL 55
IS 8
BP 1831
EP 1844
DI 10.1175/JAMC-D-16-0077.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0DF
UT WOS:000383310400012
ER
PT J
AU Corsaro, RD
Giovane, F
Liou, JC
Burchell, MJ
Cole, MJ
Williams, EG
Lagakos, N
Sadilek, A
Anderson, CR
AF Corsaro, Robert D.
Giovane, Frank
Liou, Jer-Chyi
Burchell, Mark J.
Cole, Michael J.
Williams, Earl G.
Lagakos, Nicholas
Sadilek, Albert
Anderson, Christopher R.
TI Characterization of space dust using acoustic impact detection
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID INSTRUMENT
AB This paper describes studies leading to the development of an acoustic instrument for measuring properties of micrometeoroids and other dust particles in space. The instrument uses a pair of easily penetrated membranes separated by a known distance. Sensors located on these films detect the transient acoustic signals produced by particle impacts. The arrival times of these signals at the sensor locations are used in a simple multilateration calculation to measure the impact coordinates on each film. Particle direction and speed are found using these impact coordinates and the known membrane separations. This ability to determine particle speed, direction, and time of impact provides the information needed to assign the particle's orbit and identify its likely origin. In many cases additional particle properties can be estimated from the signal amplitudes, including approximate diameter and (for small particles) some indication of composition/morphology. Two versions of this instrument were evaluated in this study. Fiber optic displacement sensors are found advantageous when very thin membranes can be maintained in tension (solar sails, lunar surface). Piezoelectric strain sensors are preferred for thicker films without tension (long duration free flyers). The latter was selected for an upcoming installation on the International Space Station.
C1 [Corsaro, Robert D.; Lagakos, Nicholas] Sotera Def Solut, 7230 Lee DeForest Dr, Columbia, MD 21046 USA.
[Giovane, Frank] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24060 USA.
[Liou, Jer-Chyi] NASA JSC, NASA Orbital Debris Program Off, Houston, TX 77058 USA.
[Burchell, Mark J.; Cole, Michael J.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NH, Kent, England.
[Williams, Earl G.; Lagakos, Nicholas] Naval Res Lab, Code 7130, Washington, DC 20375 USA.
[Sadilek, Albert; Anderson, Christopher R.] US Naval Acad, Annapolis, MD 21402 USA.
RP Corsaro, RD (reprint author), Sotera Def Solut, 7230 Lee DeForest Dr, Columbia, MD 21046 USA.
EM Bob@AstroAcoustics.com
FU NASA Orbital Debris Office; NASA LASER program
FX We wish to thank the NASA Orbital Debris Office, and the NASA LASER
program for providing support. Also we are indebted to the Science and
Technology Facilities Council (UK) for supporting the hypervelocity
facility at the University of Kent.
NR 20
TC 1
Z9 1
U1 2
U2 2
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
EI 1520-8524
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD AUG
PY 2016
VL 140
IS 2
BP 1429
EP 1438
DI 10.1121/1.4960782
PG 10
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA DW8OT
UT WOS:000383916100072
PM 27586768
ER
PT J
AU Schneider, SM
Lee, SMC
Feiveson, AH
Watenpaugh, DE
Macias, BR
Hargens, AR
AF Schneider, Suzanne M.
Lee, Stuart M. C.
Feiveson, Alan H.
Watenpaugh, Donald E.
Macias, Brandon R.
Hargens, Alan R.
TI Treadmill exercise within lower body negative pressure protects leg lean
tissue mass and extensor strength and endurance during bed rest
SO PHYSIOLOGICAL REPORTS
LA English
DT Article
DE Body composition; head down tilt; isokinetic; microgravity; muscle
atrophy; spaceflight
ID INTERNATIONAL-SPACE-STATION; HUMAN SKELETAL-MUSCLE; INDUCED BONE LOSS;
SIMULATED MICROGRAVITY; UPRIGHT EXERCISE; GRAVITY REPLACEMENT; GENDER
DIFFERENCES; IDENTICAL-TWINS; DISUSE ATROPHY; OLDER WOMEN
AB Leg muscle mass and strength are decreased during reduced activity and non-weight-bearing conditions such as bed rest (BR) and spaceflight. Supine treadmill exercise within lower body negative pressure (LBNPEX) provides full-body weight loading during BR and may prevent muscle deconditioning. We hypothesized that a 40-min interval exercise protocol performed against LBNPEX 6 days week(-1) would attenuate losses in leg lean mass (LLM), strength, and endurance during 6 degrees head-down tilt BR, with similar benefits for men and women. Fifteen pairs of healthy monozygous twins (8 male and 7 female pairs) completed 30 days of BR with one sibling of each twin pair assigned randomly as the non-exercise control (CON) and the other twin as the exercise subject (EX). Before and after BR, LLM and isokinetic leg strength and endurance were measured. Mean knee and ankle extensor and flexor strength and endurance and LLM decreased from pre- to post-BR in the male CON subjects (P < 0.01), but knee extensor strength and endurance, ankle extensor strength, and LLM were maintained in the male EX subjects. In contrast, no pre-to post-BR changes were significant in the female subjects, either CON or EX, likely due to their lower pre-BR values. Importantly, the LBNPEX countermeasure prevents or attenuates declines in LLM as well as extensor leg strength and endurance. Individuals who are stronger, have higher levels of muscular endurance, and/or have greater LLM are likely to experience greater losses during BR than those who are less fit.
C1 [Schneider, Suzanne M.] Univ New Mexico, Albuquerque, NM 87111 USA.
[Lee, Stuart M. C.; Macias, Brandon R.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Feiveson, Alan H.; Macias, Brandon R.] NASA, Johnson Space Ctr, Houston, TX USA.
[Watenpaugh, Donald E.] Univ North Texas, Hlth Sci Ctr, Ft Worth, TX USA.
[Hargens, Alan R.] Univ Calif San Diego, San Diego, CA 92103 USA.
RP Schneider, SM (reprint author), Univ New Mexico, Albuquerque, NM 87111 USA.
EM sschneid@unm.edu
NR 67
TC 1
Z9 1
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2051-817X
J9 PHYSIOL REP
JI PHYSIOL. REP.
PD AUG
PY 2016
VL 4
IS 15
AR e12892
DI 10.14814/phy2.12892
PG 14
WC Physiology
SC Physiology
GA DW1ZE
UT WOS:000383441900014
ER
PT J
AU Sunday, C
Murdoch, N
Cherrier, O
Serrano, SM
Nardi, CV
Janin, T
Martinez, IA
Gourinat, Y
Mimoun, D
AF Sunday, C.
Murdoch, N.
Cherrier, O.
Serrano, S. Morales
Nardi, C. Valeria
Janin, T.
Martinez, I. Avila
Gourinat, Y.
Mimoun, D.
TI A novel facility for reduced-gravity testing: A setup for studying
low-velocity collisions into granular surfaces
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID GEOLOGY; IMPACT; DUST; SPACECRAFT; REGOLITH; SHAPE; SIZE; EROS
AB This work presents an experimental design for studying low-velocity collisions into granular surfaces in low-gravity. In the experiment apparatus, reduced-gravity is simulated by releasing a free-falling projectile into a surface container with a downward acceleration less than that of Earth's gravity. The acceleration of the surface is controlled through the use of an Atwood machine, or a system of pulleys and counterweights. The starting height of the surface container and the initial separation distance between the projectile and surface are variable and chosen to accommodate collision velocities up to 20 cm/s and effective accelerations of similar to 0.1 to 1.0 m/s(2). Accelerometers, placed on the surface container and inside the projectile, provide acceleration data, while high-speed cameras capture the collision and act as secondary data sources. The experiment is built into an existing 5.5 m drop tower frame and requires the custom design of all components, including the projectile, surface sample container, release mechanism, and deceleration system. Data from calibration tests verify the efficiency of the experiment's deceleration system and provide a quantitative understanding of the performance of the Atwood system. Published by AIP Publishing.
C1 [Sunday, C.; Murdoch, N.; Serrano, S. Morales; Nardi, C. Valeria; Janin, T.; Martinez, I. Avila; Mimoun, D.] Univ Toulouse, DEOS, Syst Spatiaux SSPA, ISAE,SUPAERO, F-31055 Toulouse, France.
[Cherrier, O.; Gourinat, Y.] Univ Toulouse, ISAE, DMSM, SUPAERO, F-31055 Toulouse, France.
[Cherrier, O.; Gourinat, Y.] Inst Clement Ader, CNRS, UMR 5312, F-31400 Toulouse, France.
[Sunday, C.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91107 USA.
RP Sunday, C (reprint author), Univ Toulouse, DEOS, Syst Spatiaux SSPA, ISAE,SUPAERO, F-31055 Toulouse, France.; Sunday, C (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91107 USA.
FU Centre National d'Etudes Spatiales (CNES)
FX This project benefited from some financial support from the Centre
National d'Etudes Spatiales (CNES) and was a collaborative effort
between several departments at ISAE-SUPAERO. Alexandre Cadu and Anthony
Sournac, both from the Departement Electronique, Optronique et Signal
(DEOS) and Systemes Spatiaux (SSPA), provided extremely valuable help
and advice concerning the installation of the electromagnetic release
system. Emmanuel Zenou, from the Departement d'Ingenierie des Systemes
Complexes (DISC), helped prepare the experiment in such a way to
facilitate the image analyses during the data processing. Daniel Gagneux
and Thierry Faure, from the Departement Mecanique des Structures et
Materiaux (DMSM), completed the experiment's detailed design and
fabrication. Lastly, we thank Jens Biele for his helpful comments on
this manuscript.
NR 45
TC 0
Z9 0
U1 4
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD AUG
PY 2016
VL 87
IS 8
AR 084504
DI 10.1063/1.4961575
PG 10
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA DW8CE
UT WOS:000383880100047
PM 27587140
ER
PT J
AU Inoue, M
Morino, I
Uchino, O
Nakatsuru, T
Yoshida, Y
Yokota, T
Wunch, D
Wennberg, PO
Roehl, CM
Griffith, DWT
Velazco, VA
Deutscher, NM
Warneke, T
Notholt, J
Robinson, J
Sherlock, V
Hase, F
Blumenstock, T
Rettinger, M
Sussmann, R
Kyro, E
Kivi, R
Shiomi, K
Kawakami, S
De Maziere, M
Arnold, SG
Feist, DG
Barrow, EA
Barney, J
Dubey, M
Schneider, M
Iraci, LT
Podolske, JR
Hillyard, PW
Machida, T
Sawa, Y
Tsuboi, K
Matsueda, H
Sweeney, C
Tans, PP
Andrews, AE
Biraud, SC
Fukuyama, Y
Pittman, JV
Kort, EA
Tanaka, T
AF Inoue, Makoto
Morino, Isamu
Uchino, Osamu
Nakatsuru, Takahiro
Yoshida, Yukio
Yokota, Tatsuya
Wunch, Debra
Wennberg, Paul O.
Roehl, Coleen M.
Griffith, David W. T.
Velazco, Voltaire A.
Deutscher, Nicholas M.
Warneke, Thorsten
Notholt, Justus
Robinson, John
Sherlock, Vanessa
Hase, Frank
Blumenstock, Thomas
Rettinger, Markus
Sussmann, Ralf
Kyro, Esko
Kivi, Rigel
Shiomi, Kei
Kawakami, Shuji
De Maziere, Martine
Arnold, Sabrina G.
Feist, Dietrich G.
Barrow, Erica A.
Barney, James
Dubey, Manvendra
Schneider, Matthias
Iraci, Laura T.
Podolske, James R.
Hillyard, Patrick W.
Machida, Toshinobu
Sawa, Yousuke
Tsuboi, Kazuhiro
Matsueda, Hidekazu
Sweeney, Colm
Tans, Pieter P.
Andrews, Arlyn E.
Biraud, Sebastien C.
Fukuyama, Yukio
Pittman, Jasna V.
Kort, Eric A.
Tanaka, Tomoaki
TI Bias corrections of GOSAT SWIR XCO2 and XCH4 with TCCON data and their
evaluation using aircraft measurement data
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID COLUMN OBSERVING NETWORK; CO2 RETRIEVAL ALGORITHM; GAS REFERENCE
NETWORK; CARBON-DIOXIDE; GREENHOUSE GASES; ATMOSPHERIC CO2; TANSO-FTS;
INFRARED-SPECTRA; CH4 MEASUREMENTS; MOLE FRACTIONS
AB We describe a method for removing systematic biases of column-averaged dry air mole fractions of CO2 (XCO2 /and CH4 (XCH4 derived from short-wavelength infrared (SWIR) spectra of the Greenhouse gases Observing SATellite (GOSAT). We conduct correlation analyses between the GOSAT biases and simultaneously retrieved auxiliary parameters. We use these correlations to bias correct the GOSAT data, removing these spurious correlations. Data from the Total Carbon Column Observing Network (TC-CON) were used as reference values for this regression analysis. To evaluate the effectiveness of this correction method, the uncorrected/corrected GOSAT data were compared to independent XCO2 and XCH4 data derived from aircraft measurements taken for the Comprehensive Observation Network for TRace gases by AIrLiner (CONTRAIL) project, the National Oceanic and Atmospheric Administration (NOAA), the US Department of Energy (DOE), the National Institute for Environmental Studies (NIES), the Japan Meteorological Agency (JMA), the HIAPER Pole-to-Pole observations (HIPPO) program, and the GOSAT validation aircraft observation campaign over Japan. These comparisons demonstrate that the empirically derived bias correction improves the agreement between GOSAT XCO2/XCH4 and the aircraft data. Finally, we present spatial distributions and temporal variations of the derived GOSAT biases.
C1 [Inoue, Makoto; Morino, Isamu; Uchino, Osamu; Nakatsuru, Takahiro; Yoshida, Yukio; Yokota, Tatsuya; Machida, Toshinobu; Tanaka, Tomoaki] NIES, Tsukuba, Ibaraki, Japan.
[Wunch, Debra; Wennberg, Paul O.; Roehl, Coleen M.; Kort, Eric A.] CALTECH, Pasadena, CA 91125 USA.
[Griffith, David W. T.; Velazco, Voltaire A.; Deutscher, Nicholas M.] Univ Wollongong, Ctr Atmospher Chem, Wollongong, NSW 2522, Australia.
[Deutscher, Nicholas M.; Warneke, Thorsten; Notholt, Justus] Univ Bremen, Inst Environm Phys, Bremen, Germany.
[Robinson, John; Sherlock, Vanessa] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Hase, Frank; Blumenstock, Thomas; Schneider, Matthias] Karlsruhe Inst Technol, IMK ASF, Karlsruhe, Germany.
[Rettinger, Markus; Sussmann, Ralf] Karlsruhe Inst Technol, IMK IFU, Garmisch Partenkirchen, Germany.
[Kyro, Esko; Kivi, Rigel] FMI, Arctic Res Ctr, Sodankyla, Finland.
[Shiomi, Kei; Kawakami, Shuji; Tanaka, Tomoaki] Japan Aerosp Explorat Agcy JAXA, Tsukuba, Ibaraki, Japan.
[De Maziere, Martine] Belgian Inst Space Aeron IASB BIRA, Brussels, Belgium.
[Arnold, Sabrina G.; Feist, Dietrich G.] Max Planck Inst Biogeochem MPI BGC, Jena, Germany.
[Barrow, Erica A.; Barney, James] Ivy Tech Community Coll Indiana, Indianapolis, IN USA.
[Dubey, Manvendra] Los Alamos Natl Lab, Los Alamos, NM USA.
[Iraci, Laura T.; Podolske, James R.; Hillyard, Patrick W.; Tanaka, Tomoaki] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hillyard, Patrick W.] Bay Area Environm Res Inst, Petaluma, CA USA.
[Sawa, Yousuke; Tsuboi, Kazuhiro; Matsueda, Hidekazu] Mission Res Inc, Tsukuba, Ibaraki, Japan.
[Sweeney, Colm; Tans, Pieter P.; Andrews, Arlyn E.] NOAA, Boulder, CO USA.
[Biraud, Sebastien C.] LBNL, Berkeley, CA USA.
[Fukuyama, Yukio] Japan Meteorol Agcy, Tokyo, Japan.
[Pittman, Jasna V.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
[Kort, Eric A.] Jet Prop Lab, Pasadena, CA USA.
[Inoue, Makoto] Akita Prefectural Univ, Dept Environm Biol, Akita, Japan.
[Wunch, Debra] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Sherlock, Vanessa] Lab Meteorol Dynam, Palaiseau, France.
[Kort, Eric A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Inoue, M (reprint author), NIES, Tsukuba, Ibaraki, Japan.; Inoue, M (reprint author), Akita Prefectural Univ, Dept Environm Biol, Akita, Japan.
EM makoto@akita-pu.ac.jp
RI Biraud, Sebastien/M-5267-2013; Kort, Eric/F-9942-2012; Feist,
Dietrich/B-6489-2013; Dubey, Manvendra/E-3949-2010; Morino,
Isamu/K-1033-2014; Schneider, Matthias/B-1441-2013; Sussmann,
Ralf/K-3999-2012; Notholt, Justus/P-4520-2016
OI Biraud, Sebastien/0000-0001-7697-933X; Kort, Eric/0000-0003-4940-7541;
Feist, Dietrich/0000-0002-5890-6687; Dubey,
Manvendra/0000-0002-3492-790X; Morino, Isamu/0000-0003-2720-1569;
Notholt, Justus/0000-0002-3324-885X
FU Office of Biological and Environmental Research of the US Department of
Energy [DE-AC02-05CH11231]; National Science Foundation (NSF); Canadian
Space Agency (CSA); Environment Research and Technology Development Fund
of the Ministry of the Environment, Japan [2A-1102]; NASA [NNX14AI60G];
NASA Orbiting Carbon Observatory Program; Australian Research Council
[DP140101552]; ARC-DECRA Fellowship [DE140100178]; EU project InGOS; EU
project ICOS-INWIRE; Max Planck Society; Academy of Finland [140408]
FX The authors thank the many staff members of Japan Airlines, the JAL
Foundation, and JAMCO Tokyo for supporting the CONTRAIL project. We are
grateful to the NOAA ESRL/GMD tall tower network (K. Davis, A. Desai, R.
Teclaw, D. Baumann, and C. Stanier) for providing CO2 tower
data for Park Falls and West Branch. DOE flights were supported by the
Office of Biological and Environmental Research of the US Department of
Energy under contract no. DE-AC02-05CH11231 as part of the Atmospheric
Radiation Measurement Program (ARM), ARM Aerial Facility, and
Terrestrial Ecosystem Science Program. We gratefully thank many staff
members of the Japan Ministry of Defense for supporting the JMA's
ground-based and aircraft measurements. We also acknowledge the HIPPO
team members for CO2 and CH4 profile data from
HIPPO missions. The HIPPO program is supported by the National Science
Foundation (NSF), and its operation is managed by the Earth Observing
Laboratory (EOL) of the National Center for Atmospheric Research (NCAR).
We also thank the Canadian Space Agency (CSA), which provides most of
the funding support for ACE. We are grateful to the HALOE team for
publishing their data for scientific use. This research was supported in
part by the Environment Research and Technology Development Fund
(2A-1102) of the Ministry of the Environment, Japan. TCCON measurements
from Pasadena, Lamont, Park Falls and Darwin are funded by NASA grant
NNX14AI60G and NASA Orbiting Carbon Observatory Program. We are grateful
to the DOE ARM program for technical support of TCCON in Lamont and
Darwin and to Jeff Ayers for technical support of the TCCON measurements
in Park Falls. Darwin and Wollongong TCCON measurements are also
supported by Australian Research Council grant DP140101552 and Nicholas
Deutscher is supported by an ARC-DECRA Fellowship, DE140100178. The
University of Bremen acknowledges the support of the EU projects InGOS,
and ICOS-INWIRE, and the Senate of Bremen for support of TCCON
measurements in Bialystok, Bremen, Ny-Alesund, and Orleans. Operation of
the Ascension Island site was funded by the Max Planck Society. Research
at the FMI was supported by the Academy of Finland under grant no.
140408.
NR 60
TC 3
Z9 3
U1 19
U2 19
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD AUG 1
PY 2016
VL 9
IS 8
BP 3491
EP 3512
DI 10.5194/amt-9-3491-2016
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3MN
UT WOS:000382826600003
ER
PT J
AU Evans, JP
Bormann, K
Katzfey, J
Dean, S
Arritt, R
AF Evans, J. P.
Bormann, K.
Katzfey, J.
Dean, S.
Arritt, R.
TI Regional climate model projections of the South Pacific Convergence Zone
SO CLIMATE DYNAMICS
LA English
DT Article
DE Regional climate model; South Pacific Convergence Zone; Precipitation;
Tropical pacific
ID GLOBAL PRECIPITATION; RESOLUTION; SIMULATION; REGCNET; GRIDS; SPCZ
AB This study presents results from regional climate model (RCM) projections for the south-west Pacific Ocean. The regional models used bias corrected sea surface temperatures. Six global climate models (GCMs) were used to drive a global variable resolution model on a quasi-uniform 60 km grid. One of these simulations was used to drive three limited area regional models. Thus a four member ensemble was produced by different RCMs downscaling the same GCM (GFDL2.1), and a six member ensemble was produced by the same RCM (Conformal Cubic Atmospheric Model-CCAM) downscaling six different GCMs. Comparison of the model results with precipitation observations shows the differences to be dominated by the choice of RCM, with all the CCAM simulations performing similarly and generally having lower error than the other RCMs. However, evaluating aspects of the model representation of the South Pacific Convergence Zone (SPCZ) does not show CCAM to perform better in this regard. In terms of the future projections of the SPCZ for the December-January-February season, the ensemble showed no consensus change in most characteristics though a majority of the ensemble members project a decrease in the SPCZ strength. Thus, similar to GCM based studies, there is large uncertainty concerning future changes in the SPCZ and there is no evidence to suggest that future changes will be outside the natural variability. These RCM simulations do not support an increase in the frequency of zonal SPCZ events.
C1 [Evans, J. P.] Univ New South Wales, ARC Ctr Excellence Climate Syst Sci, Climate Change Res Ctr, Sydney, NSW, Australia.
[Bormann, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Katzfey, J.] Ctr Australian Weather & Climate Res, PB1, Aspendale, Vic 3195, Australia.
[Dean, S.] Natl Inst Water & Atmospher Res, Wellington, New Zealand.
[Arritt, R.] Iowa State Univ, Dept Agron, Ames, IA USA.
RP Evans, JP (reprint author), Univ New South Wales, ARC Ctr Excellence Climate Syst Sci, Climate Change Res Ctr, Sydney, NSW, Australia.
EM Jason.evans@unsw.edu.au
RI Evans, Jason/F-3716-2011
OI Evans, Jason/0000-0003-1776-3429
FU Pacific Climate Change Science Program; AusAID; Department of Climate
Change and Energy Efficiency; U.S. Department of Agriculture National
Institute of Food and Agriculture (NIFA)
FX The research discussed in this paper was conducted with the support of
the Pacific Climate Change Science Program, a program supported by
AusAID, in collaboration with the Department of Climate Change and
Energy Efficiency, and delivered by the Bureau of Meteorology and the
Commonwealth Scientific and Industrial Research Organisation (CSIRO).
The research also was supported in part by the U.S. Department of
Agriculture National Institute of Food and Agriculture (NIFA). We
acknowledge the modelling groups, the Program for Climate Model
Diagnosis and Intercomparison (PCMDI) and the WCRP's Working Group on
Coupled Modelling (WGCM), for their roles in making available the WCRP
CMIP3 multi-model dataset. Support of this dataset is provided by the
Office of Science, U.S. Department of Energy. More details on model
documentation are available at the PCMDI Web site
(http://www.pcmdi.llnl.gov).
NR 53
TC 1
Z9 1
U1 5
U2 5
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 AUG
PY 2016
VL 47
IS 3-4
BP 817
EP 829
DI 10.1007/s00382-015-2873-x
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU3LE
UT WOS:000382111300010
ER
PT J
AU Tanaka, T
Yates, E
Iraci, LT
Johnson, MS
Gore, W
Tadic, J
Loewenstein, M
Kuze, A
Frankenberg, C
Butz, A
Yoshida, Y
AF Tanaka, Tomoaki
Yates, Emma
Iraci, Laura T.
Johnson, Matthew S.
Gore, Warren
Tadic, JovanM.
Loewenstein, Max
Kuze, Akihiko
Frankenberg, Christian
Butz, Andre
Yoshida, Yukio
TI Two-Year Comparison of Airborne Measurements of CO2 and CH4 With GOSAT
at Railroad Valley, Nevada
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Atmospheric measurements; remote sensing; satellites
ID GASES OBSERVING SATELLITE; AIRCRAFT MEASUREMENT DATA; RETRIEVAL
ALGORITHM; ATMOSPHERIC CO2; CARBON-DIOXIDE; SWIR SPECTRA; TANSO-FTS;
CALIBRATION; VALIDATION; TCCON
AB The Alpha Jet Atmospheric eXperiment (AJAX) is a project to measure the atmospheric profiles of greenhouse gases (GHGs) and ozone (O-3) regularly over California and Nevada. Airborne instruments measuring GHGs and O-3 are installed in a wing pod of an Alpha Jet aircraft and operated from the National Aeronautics and Space Administration Ames Research Center at Moffett Field, CA. The instruments yield precise and accurate in situ vertical profiles of atmospheric carbon dioxide (CO2), methane (CH4), and O-3. Measurements of vertical profiles of GHGs and O-3 over Railroad Valley, NV have been conducted directly under the Greenhouse gases Observing SATellite (GOSAT) over passes on a monthly basis as part of the AJAX project since June 2011. The purpose of this work is to calculate aircraft-based dry-air mole fractions of the GHGs for the validation of GOSAT data products. This study expands and improves our previous comparisons by evaluating three algorithms against 24 months of in situ data collected over a Gain-M target. We used three different algorithms: Atmospheric CO2 Observations from Space (ACOS v3.4r3), Remote Sensing of Greenhouse Gases for Carbon Cycle Modeling (RemoteC v2.3.5FP), and National Institute for Environmental Studies (NIES v2.11). We find that the CO2 average differences of ACOS and RemoteC from AJAX are 0.26% and 0.24%, respectively. The difference between NIES and AJAX is 0.96%, which is higher than that of ACOS and RemoteC. The CH4 average differences for RemoteC and NIES are 2.1% and 1.7%, respectively.
C1 [Tanaka, Tomoaki] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tanaka, Tomoaki; Yates, Emma] Bay Area Environm Res Inst, Pittsburg, CA 94952 USA.
[Iraci, Laura T.; Johnson, Matthew S.; Gore, Warren; Loewenstein, Max] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tadic, JovanM.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Kuze, Akihiko] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan.
[Frankenberg, Christian] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Butz, Andre] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Eggenstein Leopoldshafen, Germany.
[Yoshida, Yukio] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
RP Tanaka, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM akimo.tanaka@gmail.com; emma.l.yates@nasa.gov; Laura.T.Iraci@nasa.gov;
matthew.s.johnson@nasa.gov; warren.gore@nasa.gov; jtadic@stanford.edu;
max.loewenstein7@gmail.com; kuze.akihiko@jaxa.jp;
Christian.Frankenberg@jpl.nasa.gov; andre.butz@kit.edu;
yoshida.yukio@nies.go.jp
RI Tadic, Jovan/P-3677-2016; Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
FU NASA's OCO; Ames Research Center; NASA Advanced Supercomputing Division;
NASA Ames Research Center through High-End Computing Program; NASA
Postdoctoral Program
FX This work was supported in part by NASA's OCO Science Team (K. Jucks,
Program Manager); by the Ames Research Center Director's Funds for
instrumentation and aircraft integration; and by the NASA Advanced
Supercomputing Division, NASA Ames Research Center through the High-End
Computing Program. The work of T. Tanaka, E. Yates, and J. Tadic was
supported by the NASA Postdoctoral Program.
NR 35
TC 1
Z9 1
U1 4
U2 4
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 AUG
PY 2016
VL 54
IS 8
BP 4367
EP 4375
DI 10.1109/TGRS.2016.2539973
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DT4FD
UT WOS:000381434600001
ER
PT J
AU Simard, M
Riel, BV
Denbina, M
Hensley, S
AF Simard, Marc
Riel, Bryan V.
Denbina, Michael
Hensley, Scott
TI Radiometric Correction of Airborne Radar Images Over Forested Terrain
With Topography
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Biomass; forest; radar; radiometric correction; topography
ID SAR DATA; SLOPE CORRECTION; BACKSCATTER
AB Radiometric correction of radar images is essential to produce accurate estimates of biophysical parameters related to forest structure and biomass. We present a new algorithm to correct radiometry for 1) terrain topography and 2) variations of canopy reflectivity with viewing and tree-terrain geometry. This algorithm is applicable to radar images spanning a wide range of incidence angles over terrain with significant topography and can also take into account aircraft attitude, antenna steering angle, and target geometry. The approach includes elements of both homomorphic and heteromorphic terrain corrections to correct for topographic effects and is followed by an additional radiometric correction to compensate for variations of canopy reflectivity with viewing and tree-terrain geometry. The latter correction is based on lookup tables and enables derivation of biophysical parameters irrespective of viewing geometry and terrain topography. We evaluate the performance of the new algorithm with airborne radar data and show that it performs better than classical homomorphic methods followed by cosine-based corrections.
C1 [Simard, Marc; Denbina, Michael; Hensley, Scott] Jet Prop Lab, Pasadena, CA 91109 USA.
[Riel, Bryan V.] CALTECH, Pasadena, CA 91125 USA.
RP Simard, M (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA.
EM marc.simard@jpl.nasa.gov
OI Simard, Marc/0000-0002-9442-4562
FU National Aeronautics and Space Administration (NASA); NASA's Terrestrial
Ecology Program [WBS 281945.02.61.03.26]
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). This work was supported by NASA's
Terrestrial Ecology Program (WBS 281945.02.61.03.26).
NR 17
TC 0
Z9 0
U1 1
U2 1
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 AUG
PY 2016
VL 54
IS 8
BP 4488
EP 4500
DI 10.1109/TGRS.2016.2543142
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 DT4FD
UT WOS:000381434600010
ER
PT J
AU Lebsock, MD
Suzuki, K
AF Lebsock, Matthew D.
Suzuki, Kentaroh
TI Uncertainty Characteristics of Total Water Path Retrievals in Shallow
Cumulus Derived from Spaceborne Radar/Radiometer Integral Constraints
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID LARGE-EDDY SIMULATION; PART II; MICROWAVE-FREQUENCIES; RADAR; OCEAN;
APPROXIMATION; CALIBRATION; ALGORITHM; MODELS; CLOUDS
AB A precipitating marine cumulus cloud simulation is coupled to radiation propagation models to simulate active and passive microwave observations at 94 GHz. The simulations are used to examine the error characteristics of the total water path retrieved from the integral constraints of the passive microwave brightness temperature or the path-integrated attenuation (PIA) using a spatial interpolation technique. Three sources of bias are considered: 1) the misdetection of cloudy pixels as clear, 2) the systematic differences in the column water vapor between cloudy and clear skies, and 3) the nonuniform beamfilling effects on the observables. The first two sources result in biases on the order of 5-10 g m(-2) of opposite signs that tend to cancel. The third source results in a bias that increases monotonically with the water path that approaches 50%. Nonuniform beamfilling is sensitive to footprint size. Random error results from both instrument measurement precision and the natural variability in the relationship between the water path and the observables. Random errors for the retrievals using the CloudSat PIA are estimated to be the larger of either 20 g m(-2) or 30%. A radar/radiometer system with a measurement precision of 0.3 K or 0.05 dB could reduce this error to the larger of either 10 g m(-2) or 30%. All error mechanisms reported here result from variability in either the spatial structure of the atmosphere or the hydrometeor drop size distribution. The results presented here are specific to the cloud simulation and in general the magnitude will vary globally.
C1 [Lebsock, Matthew D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Suzuki, Kentaroh] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo, Japan.
RP Lebsock, MD (reprint author), Jet Prop Lab, M-S 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM matthew.d.lebsock@jpl.nasa.gov
RI Suzuki, Kentaroh/C-3624-2011
FU National Aeronautics and Space Administration; CloudSat project;
Aerosol-Cloud Ecosystems (ACE) project
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration and was
partially funded by the CloudSat project and the Aerosol-Cloud
Ecosystems (ACE) project.
NR 38
TC 1
Z9 1
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2016
VL 33
IS 8
BP 1597
EP 1609
DI 10.1175/JTECH-D-16-0023.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA DV4LI
UT WOS:000382896700003
ER
PT J
AU Seo, EK
Yang, SD
Grecu, M
Ryu, GH
Liu, G
Hristova-Veleva, S
Noh, YJ
Haddad, Z
Shin, J
AF Seo, Eun-Kyoung
Yang, Sung-Dae
Grecu, Mircea
Ryu, Geun-Hyeok
Liu, Guosheng
Hristova-Veleva, Svetla
Noh, Yoo-Jeong
Haddad, Ziad
Shin, Jinho
TI Optimization of Cloud-Radiation Databases for Passive Microwave
Precipitation Retrievals over Ocean
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID PROFILING ALGORITHM; MODEL MICROPHYSICS; KOREAN PENINSULA; RAIN
RETRIEVALS; SATELLITE MEASUREMENTS; PARAMETRIC RETRIEVAL; HEAVY
RAINFALL; COMBINED RADAR; PART I; TRMM
AB Using Tropical Rainfall Measuring Mission (TRMM) observations from storms collected over the oceans surrounding East Asia, during summer, a method of creating physically consistent cloud-radiation databases to support satellite radiometer retrievals is introduced. In this method, vertical profiles of numerical model simulated cloud and precipitation fields are optimized against TRMM radar and radiometer observations using a hybrid empirical orthogonal function (EOF)-one-dimensional variational (1DVAR) approach.The optimization is based on comparing simulated to observed radar reflectivity profiles and the corresponding passive microwave observations at the frequencies of the TRMM Microwave Imager (TMI) instrument. To minimize the discrepancies between the actual and the synthetic observations, the simulated cloud and precipitation profiles are optimized by adjusting the contents of the hydrometeors. To reduce the dimension of the hydrometeor content profiles in the optimization, multivariate relations among hydrometeor species are used.
After applying the optimization method to modify the simulated clouds, the optimized cloud-radiation database has a joint distribution of reflectivity and associated brightness temperatures that is considerably closer to that observed by TRMM PR and TMI, especially at 85 GHz. This implies that the EOF-1DVAR approach can generate profiles with realistic distributions of frozen hydrometeors, such as snow and graupel. This approach may be similarly adapted to operate with the variety and capabilities of the passive microwave radiometers that compose the Global Precipitation Measurement (GPM) constellation. Furthermore, it can be extended to other oceanic regions and seasons.
C1 [Seo, Eun-Kyoung] Kongju Natl Univ, Dept Earth Sci Educ, 56 GongjuDaehak Ro, Kong Ju 32588, Chungnam, South Korea.
[Yang, Sung-Dae] Natl Inst Meteorol Sci, Appl Meteorol Res Div, Jeju, South Korea.
[Grecu, Mircea] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Baltimore, MD 21239 USA.
[Grecu, Mircea] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Ryu, Geun-Hyeok; Shin, Jinho] Korea Meteorol Adm, Natl Meteorol Satellite Ctr, Jincheon Gun, South Korea.
[Liu, Guosheng] Florida State Univ, Tallahassee, FL 32306 USA.
[Haddad, Ziad] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Noh, Yoo-Jeong] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Seo, EK (reprint author), Kongju Natl Univ, Dept Earth Sci Educ, 56 GongjuDaehak Ro, Kong Ju 32588, Chungnam, South Korea.
EM ekseo@kongju.ac.kr
RI Liu, Guosheng/D-3479-2011
OI Liu, Guosheng/0000-0001-7899-6125
FU "Development of Meteorological Data Utilization and Operation Supportive
Technology" of the National Meteorological Satellite Center (NMSC) of
the Korea Meteorological Administration (KMA)
FX We acknowledge the anonymous reviewers for their constructive comments.
TRMM data were provided by NASA's Precipitation Processing System. The
WRF simulation data were provided by Prof. Song-You Hong at Yonsei
University. This research was supported by "the Development of
Meteorological Data Utilization and Operation Supportive Technology" of
the National Meteorological Satellite Center (NMSC) of the Korea
Meteorological Administration (KMA).
NR 72
TC 0
Z9 0
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2016
VL 33
IS 8
BP 1649
EP 1671
DI 10.1175/JTECH-D-15-0198.1
PG 23
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA DV4LI
UT WOS:000382896700006
ER
PT J
AU Ubelmann, C
Cornuelle, B
Fu, LL
AF Ubelmann, Clement
Cornuelle, Bruce
Fu, Lee-Lueng
TI Dynamic Mapping of Along-Track Ocean Altimetry: Method and Performance
from Observing System Simulation Experiments
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MODEL
AB Simulated along-track ocean altimetry data were used to implement the use of a nonlinear dynamic propagator to perform three-dimensional (time and 2D space) interpolation of mesoscale sea surface height (SSH). The method is an inverse approach to processing altimetry data unevenly sampled in time and space into high-level gridded altimetry maps. The inverse approach, similar to the standard objective mapping, contains some correction terms to the innovation vectors to account for nonlinear dynamics. Another key improvement is to solve for the covariance functions through a Green's function approach. From the Observing System Simulation Experiments carried out to simulate a three-satellite constellation over the Gulf Stream region, the new method can significantly reduce mapping errors and improve the resolving capabilities compared to the standard linear objective analysis such as that used by the AVISO gridding.
C1 [Ubelmann, Clement; Fu, Lee-Lueng] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Cornuelle, Bruce] Scripps Inst Oceanog, La Jolla, CA USA.
RP Ubelmann, C (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM clement.ubelmann@jpl.nasa.gov
OI Cornuelle, Bruce/0000-0003-2110-3319
FU National Aeronautics and Space Administration; SWOT project
FX Part of the research presented in the paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. Support
from the SWOT project is acknowledged.
NR 11
TC 0
Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2016
VL 33
IS 8
BP 1691
EP 1699
DI 10.1175/JTECH-D-15-0163.1
PG 9
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA DV4LI
UT WOS:000382896700008
ER
PT J
AU Young, SA
Vaughan, MA
Kuehn, RE
Winker, DM
AF Young, Stuart A.
Vaughan, Mark A.
Kuehn, Ralph E.
Winker, David M.
TI The retrieval of profiles of particulate extinction from Cloud Aerosol
Lidar Infrared Pathfinder Satellite Observations (CALIPSO) data:
Uncertainty and error sensitivity analyses (vol 30, pg 395, 2013)
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Correction
AB An error in a recent analysis of the sensitivity of retrievals of Cloud Aerosol Lidar with Orthogonal Polarization (CALIOP) particulate optical properties to errors in various input parameters is described. This error was in the specification of an intermediate variable that was used to write a general equation for the sensitivities to errors in either the renormalization (calibration) factor or in the lidar ratio used in the retrieval, or both. The result of this incorrect substitution (an additional multiplicative factor to the exponent of the particulate transmittance) was then copied to some intermediate equations; the corrected versions of which are presented here. Fortunately, however, all of the final equations for the specific cases of renormalization and lidar ratio errors are correct, as are all of the figures and approximations, because these were derived directly from equations for the specific errors and not from the equation for the general case. All of the other sections, including the uncertainty analyses and the analyses of sensitivities to low signal-to-noise ratios and errors in constrained retrievals, and the presentations of errors and uncertainties in simulated and actual data are unaffected.
C1 [Young, Stuart A.] CSIRO Oceans & Atmosphere, Private Bag 1, Aspendale, Vic 3195, Australia.
[Vaughan, Mark A.; Winker, David M.] Natl Aeronaut & Space Adm, Hampton, VA 23681 USA.
[Kuehn, Ralph E.] Univ Wisconsin, Ctr Space Sci & Engn, 1225 W Dayton St, Madison, WI 53706 USA.
RP Young, SA (reprint author), CSIRO Oceans & Atmosphere, Private Bag 1, Aspendale, Vic 3195, Australia.
EM stuart.young01@gmail.com
NR 5
TC 0
Z9 0
U1 9
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2016
VL 33
IS 8
BP 1795
EP 1798
DI 10.1175/JTECH-D-16-0081.1
PG 4
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA DV4LI
UT WOS:000382896700016
ER
PT J
AU Zhou, YP
Wu, D
Lau, WKM
Tao, WK
AF Zhou, Yaping
Wu, Di
Lau, William K. -M.
Tao, Wei-Kuo
TI Scale Dependence of Land-Atmosphere Interactions in Wet and Dry Regions
as Simulated with NU-WRF over the Southwestern and South-Central United
States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SOIL-MOISTURE; NORTH-AMERICA; INTERANNUAL VARIABILITY; SUMMER
PRECIPITATION; CLIMATE FEEDBACKS; SURFACE PROCESSES; SEMIARID REGIONS;
GREAT-PLAINS; MODEL; RAINFALL
AB Large-scale forcing and land atmosphere interactions on precipitation are investigated with NASA-Unified WRF (NU-WRF) simulations during fast transitions of ENSO phases from spring to early summer of 2010 and 2011. The model is found to capture major precipitation episodes in the 3-month simulations without resorting to nudging. However, the mean intensity of the simulated precipitation is underestimated by 46% and 57% compared with the observations in dry and wet regions in the southwestern and south-central United States, respectively. Sensitivity studies show that large-scale atmospheric forcing plays a major role in producing regional precipitation. A methodology to account for moisture contributions to individual precipitation events, as well as total precipitation, is presented under the same moisture budget framework. The analysis shows that the relative contributions of local evaporation and large-scale moisture convergence depend on the dry/wet regions and are a function of temporal and spatial scales. While the ratio of local and large-scale moisture contributions vary with domain size and weather system, evaporation provides a major moisture source in the dry region and during light rain events, which leads to greater sensitivity to soil moisture in the dry region and during light rain events. The feedback of land surface processes to large-scale forcing is well simulated, as indicated by changes in atmospheric circulation and moisture convergence. Overall, the results reveal an asymmetrical response of precipitation events to soil moisture, with higher sensitivity under dry than wet conditions. Drier soil moisture tends to suppress further existing below-normal precipitation conditions via a positive soil moisture land surface flux feedback that could worsen drought conditions in the southwestern United States.
C1 [Zhou, Yaping] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
[Zhou, Yaping; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Atmospheres Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Wu, Di] Sci Syst & Applicat Inc, Lanham, MD USA.
[Lau, William K. -M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Joint Global Change Res Inst, College Pk, MD 20742 USA.
RP Zhou, YP (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM yaping.zhou-1@nasa.gov
FU NASA Precipitation Measuring Mission [NNX13AF73G]
FX This work was supported by NASA Precipitation Measuring Mission under
Project NNX13AF73G. Computational and storage support was provided by
NASA's Center for Climate Simulation (NCCS). We also thank two anonymous
reviewers for their helpful comments.
NR 81
TC 0
Z9 0
U1 6
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD AUG
PY 2016
VL 17
IS 8
BP 2121
EP 2136
DI 10.1175/JHM-D-16-0024.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW0DG
UT WOS:000383310500001
ER
PT J
AU Richardson, IG
von Rosenvinge, TT
Cane, HV
AF Richardson, I. G.
von Rosenvinge, T. T.
Cane, H. V.
TI North/South Hemispheric Periodicities in the > 25 Solar Proton Event
Rate During the Rising and Peak Phases of Solar Cycle 24
SO SOLAR PHYSICS
LA English
DT Article
DE Solar energetic particles; Solar cycle; Sunspot area
ID ENERGETIC PARTICLE EVENT; CORONAL MASS EJECTIONS; COSMIC-RAY MODULATION;
PHOTOSPHERIC MAGNETIC-FLUX; ACTIVE-REGION 12192; 2013 APRIL 11; SUNSPOT
AREAS; STEREO MISSION; SPACED DATA; FLARES
AB We present evidence that solar proton events show a clustering in time at intervals of about six months that persisted during the rising and peak phases of Solar Cycle 24. This phenomenon is most clearly demonstrated by considering events originating in the northern or southern solar hemispheres separately. We examine how these variations in the solar energetic particle (SEP) event rate are related to other phenomena, such as hemispheric sunspot numbers and areas, rates of coronal mass ejections, and the mean solar magnetic field. Most obviously, the SEP event rate closely follows the sunspot number and area in the same hemisphere. The variations of about six months are associated with features in many of the other parameters we examine, indicating that they are just one signature of the episodic development of Cycle 24. They may be related to periodicities of about 150 days reported in various solar and interplanetary phenomena during previous solar cycles. The clear presence of periodicities of about six months in Cycle 24 that evolve independently in each hemisphere contradicts a scenario suggested by McIntosh et al. (Nature Com. 6, 6491, 2015) for the variational timescales of solar magnetism.
C1 [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, I. G.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Cane, H. V.] Univ Tasmania, Dept Math & Phys, Hobart, Tas, Australia.
RP Richardson, IG (reprint author), Univ Maryland, CRESST, College Pk, MD 20742 USA.; Richardson, IG (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov; tycho.t.vonrosenvinge@nasa.gov;
hilary.cane@utas.edu.au
OI Richardson, Ian/0000-0002-3855-3634
FU NASA
FX We thank the many researchers who have compiled the various data sets
used in this article. The STEREO High Energy Telescope data are
available at http://www.srl.caltech.edu/STEREO/Public/HET_public.html.
The ERNE data are from the Space Research Laboratory at the University
of Turku (http://www.srl.utu.fi/erne_data/). This work was supported by
the NASA Living With a Star science program as part of the activities of
the Focused Science Team "Physics-based methods to predict connectivity
of SEP sources to points in the inner heliosphere, tested by location,
timing, and longitudinal separation of SEPs".
NR 65
TC 1
Z9 1
U1 3
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 AUG
PY 2016
VL 291
IS 7
BP 2117
EP 2134
DI 10.1007/s11207-016-0948-4
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU3EQ
UT WOS:000382094000011
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Ansseau, I
Anton, G
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
Beiser, E
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Clark, K
Classen, L
Coenders, S
Collin, GH
Conrad, JM
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Rosendo, ED
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
di Lorenzo, V
Dujmovic, H
Dumm, JP
Dunkman, M
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fahey, S
Fazely, AR
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Flis, S
Fosig, CC
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Gier, D
Gladstone, L
Glagla, M
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Griffith, Z
Ha, C
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansen, E
Hansmann, B
Hansmann, T
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hulth, PO
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jeong, M
Jero, K
Jones, BJP
Jurkovic, M
Kappes, A
Karg, T
Karle, A
Katz, U
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kim, M
Kintscher, T
Kiryluk, J
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Konietz, R
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, G
Kroll, M
Kruckl, G
Kunnen, J
Kunwar, S
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lennarz, D
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lu, L
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Mandelartz, M
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meier, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Neer, G
Niederhausen, H
Nowicki, SC
Nygren, DR
Pollmann, AO
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Pankova, DV
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Quinnan, M
Raab, C
Radel, L
Rameez, M
Rawlins, K
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Richter, S
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ryckbosch, D
Sabbatini, L
Sander, HG
Sandrock, A
Sandroos, J
Sarkar, S
Schatto, K
Schimp, M
Schlunder, P
Schmidt, T
Schoenen, S
Schoneberg, S
Schonwald, A
Schumacher, L
Seckel, D
Seunarine, S
Soldin, D
Song, M
Spiczak, GM
Spiering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stasik, A
Steuer, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Tatar, J
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Santen, J
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wills, L
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Ansseau, I.
Anton, G.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
Beiser, E.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Clark, K.
Classen, L.
Coenders, S.
Collin, G. H.
Conrad, J. M.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Rosendo, E. del Pino
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
di Lorenzo, V.
Dujmovic, H.
Dumm, J. P.
Dunkman, M.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fahey, S.
Fazely, A. R.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Flis, S.
Foesig, C. -C.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Gier, D.
Gladstone, L.
Glagla, M.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Griffith, Z.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansen, E.
Hansmann, B.
Hansmann, T.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jeong, M.
Jero, K.
Jones, B. J. P.
Jurkovic, M.
Kappes, A.
Karg, T.
Karle, A.
Katz, U.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kim, M.
Kintscher, T.
Kiryluk, J.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Konietz, R.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, G.
Kroll, M.
Krueckl, G.
Kunnen, J.
Kunwar, S.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lennarz, D.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Lu, L.
Luenemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Mandelartz, M.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meier, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Neer, G.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Pollmann, A. Obertacke
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Pankova, D. V.
Paul, L.
Pepper, J. A.
Heros, C. Perez de los
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Quinnan, M.
Raab, C.
Raedel, L.
Rameez, M.
Rawlins, K.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Richter, S.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Sabbatini, L.
Sander, H. -G.
Sandrock, A.
Sandroos, J.
Sarkar, S.
Schatto, K.
Schimp, M.
Schlunder, P.
Schmidt, T.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schumacher, L.
Seckel, D.
Seunarine, S.
Soldin, D.
Song, M.
Spiczak, G. M.
Spiering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stasik, A.
Steuer, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Stroem, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Tatar, J.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Santen, J.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wills, L.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zoll, M.
CA IceCube Collaboration
TI ANISOTROPY IN COSMIC-RAY ARRIVAL DIRECTIONS IN THE SOUTHERN HEMISPHERE
BASED ON SIX YEARS OF DATA FROM THE ICECUBE DETECTOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; cosmic rays
ID AIR-SHOWER ARRAY; LARGE-SCALE ANISOTROPY; UNUSUAL SOLAR MINIMUM;
MAGNETIC RECONNECTION; SIDEREAL ANISOTROPY; ANGULAR SCALES; TEV;
HELIOSPHERE; DIFFUSION; TRANSPORT
AB The IceCube Neutrino Observatory accumulated a total of 318 billion cosmic-ray-induced muon events between 2009 May and 2015 May. This data set was used for a detailed analysis of the sidereal anisotropy in the arrival directions of cosmic rays in the TeV to PeV energy range. The observed global sidereal anisotropy features large regions of relative excess and deficit, with amplitudes of the order of 10(-3) up to about 100 TeV. A decomposition of the arrival direction distribution into spherical harmonics shows that most of the power is contained in the low-multipole (l <= 4) moments. However, higher multipole components are found to be statistically significant down to an angular scale of less than 10 degrees, approaching the angular resolution of the detector. Above 100 TeV, a change in the morphology of the arrival direction distribution is observed, and the anisotropy is characterized by a wide relative deficit whose amplitude increases with primary energy up to at least 5 PeV, the highest energies currently accessible to IceCube. No time dependence of the large-and small-scale structures is observed in the period of six years covered by this analysis. The high-statistics data set reveals more details of the properties of the anisotropy and is potentially able to shed light on the various physical processes that are responsible for the complex angular structure and energy evolution.
C1 [Aartsen, M. G.; Adams, J.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Abraham, K.; Bernhard, A.; Coenders, S.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, D-85748 Garching, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kintscher, T.; Kowalski, M.; Kunwar, S.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Ahlers, M.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Ahlers, M.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, 1150 Univ Ave, Madison, WI 53706 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Altmann, D.; Anton, G.; Classen, L.; Kappes, A.; Katz, U.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C. -C.; Koepke, L.; Kroll, G.; Krueckl, G.; Sander, H. -G.; Sandroos, J.; Schatto, K.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Arguelles, C.; Collin, G. H.; Conrad, J. M.; Jones, B. J. P.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Glagla, M.; Ha, C.; Haack, C.; Hansmann, B.; Hansmann, T.; Kemp, J.; Konietz, R.; Leuermann, M.; Leuner, J.; Miarecki, S.; Paul, L.; Raedel, L.; Reimann, R.; Rongen, M.; Schimp, M.; Schoenen, S.; Schumacher, L.; Stahlberg, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Klein, S. R.; Price, P. B.; Tatar, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Kroll, M.; Mandelartz, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Becker, K. -H.; Bindig, D.; Helbing, K.; Hickford, S.; Hoffmann, R.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[BenZvi, S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Tatar, J.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Fuchs, T.; Hallgren, A.; Heros, C. Perez de los; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Boerner, M.; Meier, M.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Schlunder, P.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bose, D.; Dujmovic, H.; In, S.; Jeong, M.; Kim, M.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Luenemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Weaver, Ch.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Casey, J.; Daughhetee, J.; Taboada, I.; Toale, P. A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.; Toale, P. A.] 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, Canada.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Lennarz, D.; Mahn, K. B. M.; Neer, G.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Lu, L.; 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.; Voge, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[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.
[Kurahashi, N.; Richman, M.; Wills, L.] Drexel Univ, Dept Phys, 3141 Chestnut St, 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.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Palczewski, T.; Pepper, J. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Providence Dr, Anchorage, AK 99508 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McNally, F.] Carleton Coll, Dept Phys & Astron, Northfield, MN 55057 USA.
RP McNally, F (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.; McNally, F (reprint author), Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, 1150 Univ Ave, Madison, WI 53706 USA.; McNally, F (reprint author), Carleton Coll, Dept Phys & Astron, Northfield, MN 55057 USA.
EM fmcnally@wisc.edu
RI Beatty, James/D-9310-2011; Sarkar, Subir/G-5978-2011; Koskinen,
David/G-3236-2014; Tjus, Julia/G-8145-2012; Katz, Uli/E-1925-2013;
Maruyama, Reina/A-1064-2013; Anton, Gisela/C-4840-2013; Wiebusch,
Christopher/G-6490-2012
OI Beatty, James/0000-0003-0481-4952; Sarkar, Subir/0000-0002-3542-858X;
Koskinen, David/0000-0002-0514-5917; Perez de los Heros,
Carlos/0000-0002-2084-5866; Katz, Uli/0000-0002-7063-4418; Maruyama,
Reina/0000-0003-2794-512X; Anton, Gisela/0000-0003-2039-4724; Wiebusch,
Christopher/0000-0002-6418-3008
FU US National Science Foundation-Office of Polar Programs; US 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; US 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); Villum Fonden; Danish National Research Foundation (DNRF),
Denmark
FX We acknowledge the support from the following agencies: US National
Science Foundation-Office of Polar Programs, US 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; US 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); Villum Fonden,
Danish National Research Foundation (DNRF), Denmark.
NR 80
TC 4
Z9 4
U1 5
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 220
DI 10.3847/0004-637X/826/2/220
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900120
ER
PT J
AU Burke-Spolaor, S
Trott, CM
Brisken, WF
Deller, AT
Majid, WA
Palaniswamy, D
Thompson, DR
Tingay, SJ
Wagstaff, KL
Wayth, RB
AF Burke-Spolaor, S.
Trott, Cathryn M.
Brisken, Walter F.
Deller, Adam T.
Majid, Walid A.
Palaniswamy, Divya
Thompson, David R.
Tingay, Steven J.
Wagstaff, Kiri L.
Wayth, Randall B.
TI LIMITS ON FAST RADIO BURSTS FROM FOUR YEARS OF THE V-FASTR EXPERIMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; radio continuum: general
ID COSMOLOGICAL DISTANCES; TRANSIENTS; SEARCH; ARRAY; GALAXY; MHZ
AB The V-FASTR experiment on the Very Long Baseline Array was designed to detect dispersed pulses of milliseconds in duration, such as fast radio bursts (FRBs). We use all V-FASTR data through 2015 February to report V-FASTR's upper limits on the rates of FRBs, and compare these with rederived rates from Parkes FRB detection experiments. V-FASTR's operation at lambda = 20 cm allows direct comparison with the 20 cm Parkes rate, and we derive a power-law limit of gamma < -0.4 (95% confidence limit) on the index of FRB source counts, N(>S) proportional to S-gamma. Using the previously measured FRB rate and the unprecedented amount of survey time spent searching for FRBs at a large range of wavelengths (0.3 cm > lambda > 90 cm), we also place frequency-dependent limits on the spectral distribution of FRBs. The most constraining frequencies place two-point spectral index limits of alpha(4cm)(20cm) < 5.8 and alpha(20cm)(90cm) > -7.6, where fluence F proportional to f(alpha) if we assume that the burst rate reported by Champion et al. of R(F similar to 0.6 Jy ms) = 7 x 10(3) sky(-1) day(-1) is accurate (for bursts of similar to 3 ms duration). This upper limit on alpha suggests that if FRBs are extragalactic but noncosmological, on average they are not experiencing excessive free-free absorption due to a medium with high optical depth (assuming temperature similar to 8000 K), which excessively inverts their low-frequency spectrum. This in turn implies that the dispersion of FRBs arises in either or both of the intergalactic medium or the host galaxy, rather than from the source itself.
C1 [Burke-Spolaor, S.; Brisken, Walter F.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
[Burke-Spolaor, S.] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Burke-Spolaor, S.; Majid, Walid A.; Thompson, David R.; Wagstaff, Kiri L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Trott, Cathryn M.; Palaniswamy, Divya; Tingay, Steven J.; Wayth, Randall B.] Curtin Univ, ICRAR, Bentley, WA 6845, Australia.
[Brisken, Walter F.] Univ Minnesota, Minneapolis, MN 55155 USA.
[Deller, Adam T.] ASTRON, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands.
[Trott, Cathryn M.; Tingay, Steven J.; Wayth, Randall B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia.
RP Burke-Spolaor, S (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.; Burke-Spolaor, S (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.; Burke-Spolaor, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sspolaor@nrao.edu
RI Wayth, Randall/B-2444-2013;
OI Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766;
Deller, Adam/0000-0001-9434-3837; Tingay, Steven/0000-0002-8195-7562;
Wagstaff, Kiri/0000-0003-4401-5506
FU Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Australian Research Council DECRA
Fellowship [DE140100316]
FX The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. We acknowledge the exellent commentary by two
referees and the ApJ statistician on the paper's manuscripts. This work
was carried out in part at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. Parts of this research were conducted by the
Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO), through project number CE110001020. C.M.T. is
supported by an Australian Research Council DECRA Fellowship through
project number DE140100316.
NR 33
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 223
DI 10.3847/0004-637X/826/2/223
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900123
ER
PT J
AU Cheung, CC
Jean, P
Shore, SN
Stawarz, L
Corbet, RHD
Knodlseder, J
Starrfield, S
Wood, DL
Desiante, R
Longo, F
Pivato, G
Wood, KS
AF Cheung, C. C.
Jean, P.
Shore, S. N.
Stawarz, L.
Corbet, R. H. D.
Knodlseder, J.
Starrfield, S.
Wood, D. L.
Desiante, R.
Longo, F.
Pivato, G.
Wood, K. S.
TI FERMI-LAT GAMMA-RAY DETECTIONS OF CLASSICAL NOVAE V1369 CENTAURI 2013
AND V5668 SAGITTARII 2015
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-rays: stars novae; cataclysmic variables radiation mechanisms:
general
ID LARGE-AREA TELESCOPE; V407 CYGNI; PARTICLE-ACCELERATION; BLAST WAVE;
EMISSION; OUTBURST; MISSION; DWARF; LINES
AB We report the Fermi Large Area Telescope (LAT) detections of high-energy (>100 MeV) gamma-ray emission from two recent optically bright classical novae, V1369 Centauri 2013 and V5668 Sagittarii 2015. At early times, Fermi target-of-opportunity observations prompted by their optical discoveries provided enhanced LAT exposure that enabled the detections of gamma-ray onsets beginning 2 days after their first optical peaks. Significant gamma-ray emission was found extending to 39-55 days after their initial LAT detections, with systematically fainter and longer duration emission compared to previous gamma-ray-detected classical novae. These novae were distinguished by multiple bright optical peaks that encompassed the time spans of the observed gamma-ray. The gamma-ray light curves and spectra of the two novae are presented along with representative hadronic and leptonic models, and comparisons with other novae detected by the LAT are discussed.
C1 [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Jean, P.; Knodlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Jean, P.; Knodlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France.
[Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Corbet, R. H. D.] CRESST, Greenbelt, MD 20771 USA.
[Corbet, R. H. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA.
[Wood, D. L.; Wood, K. S.] Praxis Inc, Alexandria, VA 22303 USA.
[Wood, D. L.; Wood, K. S.] Naval Res Lab, Washington, DC 20375 USA.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Desiante, R.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Pivato, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
RP Cheung, CC (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM Teddy.Cheung@nrl.navy.mil; Pierre.Jean@irap.omp.eu;
steven.neil.shore@unipi.it
FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes
Spatiales in France; NRL by a Karles' Fellowship; NASA through Guest
Investigator programs [12-FERMI12-0026, 13-FERMI13-0008]; Polish NSC
grant [DEC-2012/04/A/ST9/00083]; NSF; NASA
FX 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.; C.C.C. was
supported at NRL by a Karles' Fellowship and by NASA through Guest
Investigator programs 12-FERMI12-0026 and 13-FERMI13-0008. L.S. was
supported by Polish NSC grant DEC-2012/04/A/ST9/00083. S.S. acknowledges
partial support from NSF and NASA grants to ASU.
NR 59
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 142
DI 10.3847/0004-637X/826/2/142
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900042
ER
PT J
AU Clautice, D
Perlman, ES
Georganopoulos, M
Lister, ML
Tombesi, F
Cara, M
Marshall, HL
Hogan, B
Kazanas, D
AF Clautice, Devon
Perlman, Eric S.
Georganopoulos, Markos
Lister, Matthew L.
Tombesi, Francesco
Cara, Mihai
Marshall, Herman L.
Hogan, Brandon
Kazanas, Demos
TI THE SPECTACULAR RADIO-NEAR-IR-X-RAY JET OF 3C 111: THE X-RAY EMISSION
MECHANISM AND JET KINEMATICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; radio continuum: galaxies; X-rays:
galaxies
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; INVERSE-COMPTON;
HOT-SPOTS; PKS 0637-752; QUASAR JETS; SYNCHROTRON-RADIATION; CHANDRA
OBSERVATIONS; GAMMA-RAY; SPECTRA
AB Relativistic jets are the most energetic manifestation of the active galactic nucleus (AGN) phenomenon. AGN jets are observed from the radio through gamma-rays and carry copious amounts of matter and energy from the sub-parsec central regions out to the kiloparsec and often megaparsec scale galaxy and cluster environs. While most spatially resolved jets are seen in the radio, an increasing number have been discovered to emit in the optical/near-IR and/or X-ray bands. Here we discuss a spectacular example of this class, the 3C 111 jet, housed in one of the nearest, double-lobed FR II radio galaxies known. We discuss new, deep Chandra and Hubble Space Telescope (HST) observations that reveal both near-IR and X-ray emission from several components of the 3C 111 jet, as well as both the northern and southern hotspots. Important differences are seen between the morphologies in the radio, X-ray, and near-IR bands. The long (over 100 kpc on each side), straight nature of this jet makes it an excellent prototype for future, deep observations, as it is one of the longest such features seen in the radio, near-IR/optical, and X-ray bands. Several independent lines of evidence, including the X-ray and broadband spectral shape as well as the implied velocity of the approaching hotspot, lead us to strongly disfavor the EC/CMB model and instead favor a two-component synchrotron model to explain the observed X-ray emission for several jet components. Future observations with NuSTAR, HST, and Chandra will allow us to further constrain the emission mechanisms.
C1 [Clautice, Devon; Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
[Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Lister, Matthew L.; Hogan, Brandon] Purdue Univ, Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
[Tombesi, Francesco] Univ Maryland, Dept Astron, Laurel, MD 20723 USA.
[Tombesi, Francesco; Kazanas, Demos] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 663, Greenbelt, MD 20771 USA.
[Cara, Mihai] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Clautice, D (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
OI Clautice, Devon/0000-0002-7096-8573
FU National Aeronautics and Space Administration (NASA) [G03-14113A,
G04-15103A, NAS8-03060]; HST [GO-13114.01]; Space Telescope Science
Institute; NASA [NAS 5-26555]
FX These results are based on observations made by the Chandra X-ray
Observatory (data sets 702798 and 703007) and Hubble Space Telescope
(program 13114), as well as the Very Large Array (VLA, program AB534).
E.P., D.C., and F.T. acknowledge support for this work by the National
Aeronautics and Space Administration (NASA) through Chandra awards
G03-14113A (E.P. and D.C.) and G04-15103A (F.T.) issued by the Chandra
X-ray Observatory Center, which is operated by the Smithsonian
Astronomical Observatory for and on behalf of the National Aeronautics
and Space Administration under contract NAS8-03060. E.P. and D.C. also
acknowledge support from HST grant GO-13114.01, which 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. 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 Astropy, a community-developed core Python
package for Astronomy (Astropy Collaboration et al. 2013), hosted at
http://www.astropy.org. This research also made use of APLpy, an
open-source plotting package for Python hosted at
http://aplpy.github.com.
NR 54
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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 AUG 1
PY 2016
VL 826
IS 2
AR 109
DI 10.3847/0004-637X/826/2/109
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900009
ER
PT J
AU Draper, ZH
Duchene, G
Millar-Blanchaer, MA
Matthews, BC
Wang, JJ
Kalas, P
Graham, JR
Padgett, D
Ammons, SM
Bulger, J
Chen, C
Chilcote, JK
Doyon, R
Fitzgerald, MP
Follette, KB
Gerard, B
Greenbaum, AZ
Hibon, P
Hinkley, S
Macintosh, B
Ingraham, P
Lafreniere, D
Marchis, F
Marois, C
Nielsen, EL
Oppenheimer, R
Patel, R
Patience, J
Perrin, M
Pueyo, L
Rajan, A
Rameau, J
Sivaramakrishnan, A
Vega, D
Ward-Duong, K
Wolf, SG
AF Draper, Zachary H.
Duchene, Gaspard
Millar-Blanchaer, Maxwell A.
Matthews, Brenda C.
Wang, Jason J.
Kalas, Paul
Graham, James R.
Padgett, Deborah
Ammons, S. Mark
Bulger, Joanna
Chen, Christine
Chilcote, Jeffrey K.
Doyon, Rene
Fitzgerald, Michael P.
Follette, Kate B.
Gerard, Benjamin
Greenbaum, Alexandra Z.
Hibon, Pascale
Hinkley, Sasha
Macintosh, Bruce
Ingraham, Patrick
Lafreniere, David
Marchis, Franck
Marois, Christian
Nielsen, Eric L.
Oppenheimer, Rebecca
Patel, Rahul
Patience, Jenny
Perrin, Marshall
Pueyo, Laurent
Rajan, Abhijith
Rameau, Julien
Sivaramakrishnan, Anand
Vega, David
Ward-Duong, Kimberly
Wolf, Schuyler G.
TI THE PECULIAR DEBRIS DISK OF HD 111520 AS RESOLVED BY THE GEMINI PLANET
IMAGER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: individual (HD 111520)
ID SCORPIUS-CENTAURUS; CIRCUMSTELLAR DISK; POLARIZED-LIGHT; INNER DISK; 1ST
LIGHT; STARS; POLARIMETRY; ASYMMETRIES; CENSUS; SYSTEM
AB Using the Gemini Planet Imager, we have resolved the circumstellar debris disk around HD 111520 at a projected range of similar to 30-100 AU in both total and polarized H-band intensity. The disk is seen edge-on at a position angle of 165 along the spine of emission. A slight inclination and asymmetric warp are covariant and alter the interpretation of the observed disk emission. We employ three point-spread function subtraction methods to reduce the stellar glare and instrumental artifacts to confirm that there is a roughly 2:1 brightness asymmetry between the NW and SE extension. This specific feature makes HD 111520 the most extreme example of asymmetric debris disks observed in scattered light among similar highly inclined systems, such as HD 15115 and HD 106906. We further identify a tentative localized brightness enhancement and scale height enhancement associated with the disk at similar to 40 AU away from the star on the SE extension. We also find that the fractional polarization rises from 10% to 40% from 0.'' 15 to 0.'' 8 from the star. The combination of large brightness asymmetry and symmetric polarization fraction leads us to believe that an azimuthal dust density variation is causing the observed asymmetry.
C1 [Draper, Zachary H.; Matthews, Brenda C.; Gerard, Benjamin; Marois, Christian] Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
[Draper, Zachary H.; Matthews, Brenda C.; Gerard, Benjamin; Marois, Christian] Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada.
[Duchene, Gaspard; Wang, Jason J.; Kalas, Paul; Graham, James R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, Gaspard] Univ Grenoble Alpes, CNRS, Inst Planetol & Astrophys Grenoble, F-38000 Grenoble, France.
[Millar-Blanchaer, Maxwell A.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Millar-Blanchaer, Maxwell A.; Chilcote, Jeffrey K.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Padgett, Deborah] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Ammons, S. Mark] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94551 USA.
[Bulger, Joanna] NAOJ, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA.
[Chen, Christine; Greenbaum, Alexandra Z.; Perrin, Marshall; Pueyo, Laurent; Sivaramakrishnan, Anand; Wolf, Schuyler G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Doyon, Rene; Lafreniere, David; Rameau, Julien] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, Montreal, PQ H3C 3J7, Canada.
[Fitzgerald, Michael P.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Follette, Kate B.; Macintosh, Bruce; Nielsen, Eric L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Greenbaum, Alexandra Z.; Wolf, Schuyler G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hibon, Pascale] European So Observ, Casilla 19001, Santiago 19, Chile.
[Hinkley, Sasha] Univ Exeter, Astrophys Grp, Phys Bldg,Stocker Rd, Exeter EX4 4QL, Devon, England.
[Ingraham, Patrick] Large Synopt Survey Telescope, 950 N Cherry Ave, Tucson, AZ 85719 USA.
[Marchis, Franck; Nielsen, Eric L.; Vega, David] Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Oppenheimer, Rebecca] Amer Museum Nat Hist, New York, NY 10024 USA.
[Patel, Rahul] CALTECH, Infrared Proc & Anal Ctr, 770 South Wilson Ave, Pasadena, CA 91125 USA.
[Patience, Jenny; Rajan, Abhijith; Ward-Duong, Kimberly] Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA.
RP Draper, ZH (reprint author), Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.; Draper, ZH (reprint author), Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada.
OI Draper, Zachary/0000-0002-1834-3496; Nielsen, Eric/0000-0001-6975-9056;
Duchene, Gaspard/0000-0002-5092-6464; Fitzgerald,
Michael/0000-0002-0176-8973; Wang, Jason/0000-0003-0774-6502; Greenbaum,
Alexandra/0000-0002-7162-8036
FU Natural Science and Engineering Research Council of Canada; NSF
[AST-0909188, AST-1313718, AST-141378, AST 1411868]; NASA
[NNX15AD95G/NEXSS, NNX14AJ80G, NNX11AD21G]
FX Z.H.D. and B.C.M. acknowledge a Discovery Grant and Accelerator
Supplement from the Natural Science and Engineering Research Council of
Canada.; Supported by NSF grants AST-0909188, AST-1313718 (J.R.G.,
J.J.W., P.G.K.), AST-141378 (G.D., M.F.), and AST 1411868 (K.F., J.L.P.,
A.R., K.W.D.).; Supported by NASA grants NNX15AD95G/NEXSS, NNX14AJ80G,
and NNX11AD21G (J.R.G., J.J.W., P.G.K.).; Portions of this work were
performed under the auspices of the U.S. Department of Energy by
Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344
(S.M.A.).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
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DI 10.3847/0004-637x/826/2/147
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900047
ER
PT J
AU Gordon, KD
Fouesneau, M
Arab, H
Tchernyshyov, K
Weisz, DR
Dalcanton, JJ
Williams, BF
Bell, EF
Bianchi, L
Boyer, M
Choi, Y
Dolphin, A
Girardi, L
Hogg, DW
Kalirai, JS
Kapala, M
Lewis, AR
Rix, HW
Sandstrom, K
Skillman, ED
AF Gordon, Karl D.
Fouesneau, Morgan
Arab, Heddy
Tchernyshyov, Kirill
Weisz, Daniel R.
Dalcanton, Julianne J.
Williams, Benjamin F.
Bell, Eric F.
Bianchi, Luciana
Boyer, Martha
Choi, Yumi
Dolphin, Andrew
Girardi, Leo
Hogg, David W.
Kalirai, Jason S.
Kapala, Maria
Lewis, Alexia R.
Rix, Hans-Walter
Sandstrom, Karin
Skillman, Evan D.
TI THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. XV. THE BEAST: BAYESIAN
EXTINCTION AND STELLAR TOOL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; galaxies: individual (M31); methods: data analysis;
methods: statistical; stars: fundamental parameters
ID SMALL-MAGELLANIC-CLOUD; INITIAL MASS FUNCTION; BLANKETED MODEL
ATMOSPHERES; STAR-FORMING REGIONS; DIGITAL SKY SURVEY; ULTRAVIOLET
EXTINCTION; INTERSTELLAR DUST; MILKY-WAY; PHOTOMETRIC SURVEY; ADVANCED
CAMERA
AB We present the Bayesian Extinction And Stellar Tool (BEAST), a probabilistic approach to modeling the dust extinguished photometric spectral energy distribution of an individual star while accounting for observational uncertainties common to large resolved star surveys. Given a set of photometric measurements and an observational uncertainty model, the BEAST infers the physical properties of the stellar source using stellar evolution and atmosphere models and constrains the line of sight extinction using a newly developed mixture model that encompasses the full range of dust extinction curves seen in the Local Group. The BEAST is specifically formulated for use with large multi-band surveys of resolved stellar populations. Our approach accounts for measurement uncertainties and any covariance between them due to stellar crowding (both systematic biases and uncertainties in the bias) and absolute flux calibration, thereby incorporating the full information content of the measurement. We illustrate the accuracy and precision possible with the BEAST using data from the Panchromatic Hubble Andromeda Treasury. While the BEAST has been developed for this survey, it can be easily applied to similar existing and planned resolved star surveys.
C1 [Gordon, Karl D.; Arab, Heddy; Kalirai, Jason S.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Gordon, Karl D.] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281 S9, B-9000 Ghent, Belgium.
[Fouesneau, Morgan; Hogg, David W.; Kapala, Maria; Rix, Hans-Walter] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
[Tchernyshyov, Kirill; Bianchi, Luciana] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Weisz, Daniel R.; Dalcanton, Julianne J.; Williams, Benjamin F.; Choi, Yumi; Lewis, Alexia R.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
[Boyer, Martha] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, Martha] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dolphin, Andrew] Raytheon Co, Tucson, AZ 85734 USA.
[Girardi, Leo] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Hogg, David W.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[Sandstrom, Karin] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Skillman, Evan D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
RP Gordon, KD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM kgordon@stsci.edu
OI Weisz, Daniel/0000-0002-6442-6030; Bell, Eric/0000-0002-5564-9873
FU NASA through Space Telescope Science Institute [12055]; NASA [NAS
5-26555]; NASA through Hubble Fellowship - Space Telescope Science
Institute [HST-HF-51331.01]; National Science Foundation [ACI-1053575]
FX We thank the referee for insightful comments that motivated us to
significantly improve the content and presentation of this paper.
Support for program # 12055 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. Support for DRW is provided by NASA through Hubble
Fellowship grants HST-HF-51331.01 awarded by the Space Telescope Science
Institute. This work used the Extreme Science and Engineering Discovery
Environment (XSEDE), which is supported by National Science Foundation
grant number ACI-1053575. The authors acknowledge the Texas Advanced
Computing Center (TACC) at The University of Texas at Austin for
providing High Performance Computing (HPC) resources that have
contributed to the research results reported within this paper. URL:
http://www.tacc.utexas.edu.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
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PY 2016
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DI 10.3847/0004-637X/826/2/104
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900004
ER
PT J
AU Hailey, CJ
Mori, K
Perez, K
Canipe, AM
Hong, J
Tomsick, JA
Boggs, SE
Christensen, FE
Craig, WW
Fornasini, F
Grindlay, JE
Harrison, FA
Nynka, M
Rahoui, F
Stern, D
Zhang, S
Zhang, WW
AF Hailey, Charles J.
Mori, Kaya
Perez, Kerstin
Canipe, Alicia M.
Hong, Jaesub
Tomsick, John A.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Fornasini, Francesca
Grindlay, Jonathan E.
Harrison, Fiona A.
Nynka, Melania
Rahoui, Farid
Stern, Daniel
Zhang, Shuo
Zhang, William W.
TI EVIDENCE FOR INTERMEDIATE POLARS AS THE ORIGIN OF THE GALACTIC CENTER
HARD X-RAY EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; novae, cataclysmic variables; X-rays: diffuse background
ID MAGNETIC CATACLYSMIC VARIABLES; WHITE-DWARF MASSES; XMM-NEWTON
OBSERVATIONS; TV-COLUMBAE; LUMINOSITY FUNCTION; INTERSTELLAR-MEDIUM;
LINE DIAGNOSTICS; RIDGE EMISSION; SPACE DENSITY; CENTER REGION
AB Recently, unresolved hard (20-40 keV) X-ray emission has been discovered within the central 10 pc of the Galaxy, possibly indicating a large population of intermediate polars (IPs). Chandra and XMM-Newton measurements in the surrounding similar to 50 pc imply a much lighter population of IPs with < M-WD > approximate to 0.5M(circle dot). Here we use broadband NuSTAR observations of two IPs: TV Columbae, which has a fairly typical but widely varying reported mass of M-WD approximate to 0.5-1.0M(circle dot), and IGR J17303-0601, with a heavy reported mass of M-WD approximate to 1.0-1.2M(circle dot). We investigate how varying spectral models and observed energy ranges influences estimated white dwarf mass. Observations of the inner 10 pc can be accounted for by IPs with < M-WD > approximate to 0.9M(circle dot), consistent with that of the CV population in general and the X-ray observed field IPs in particular. The lower mass derived by Chandra and XMM-Newton appears to be an artifact of narrow energy-band fitting. To explain the (unresolved) central hard X-ray emission (CHXE) by IPs requires an X-ray (2-8 keV) luminosity function (XLF) extending down to at least 5 x 10(31) erg s(-1). The CHXE XLF, if extended to the surrounding similar to 50 pc observed by Chandra and XMM-Newton, requires that at least similar to 20%-40% of the similar to 9000 point sources are IPs. If the XLF extends just a factor of a few lower in luminosity, then the vast majority of these sources are IPs. This is in contrast to recent observations of the Galactic ridge, where the bulk of the 2-8 keV emission is ascribed to non-magnetic CVs.
C1 [Hailey, Charles J.; Mori, Kaya; Canipe, Alicia M.; Nynka, Melania; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Perez, Kerstin] Haverford Coll, 370 Lancaster Ave,KINSC L109, Haverford, PA 19041 USA.
[Hong, Jaesub; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Tomsick, John A.; Boggs, Steven E.; Craig, William W.; Fornasini, Francesca] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Nynka, Melania] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA.
[Rahoui, Farid] European Southern Observ, K Schwarzschild Str 2, D-85798 Garching, Germany.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hailey, CJ (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM chuckh@astro.columbia.edu
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX This work was supported under NASA Contract No. NNG08FD60C, and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA). The authors thank K Mukai and QD Wang for
valuable discussions.
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
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PY 2016
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SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900060
ER
PT J
AU Johns-Krull, CM
McLane, JN
Prato, L
Crockett, CJ
Jaffe, DT
Hartigan, PM
Beichman, CA
Mahmud, NI
Chen, W
Skiff, BA
Cauley, PW
Jones, JA
Mace, GN
AF Johns-Krull, Christopher M.
McLane, Jacob N.
Prato, L.
Crockett, Christopher J.
Jaffe, Daniel T.
Hartigan, Patrick M.
Beichman, Charles A.
Mahmud, Naved I.
Chen, Wei
Skiff, B. A.
Cauley, P. Wilson
Jones, Joshua A.
Mace, G. N.
TI A CANDIDATE YOUNG MASSIVE PLANET IN ORBIT AROUND THE CLASSICAL T TAURI
STAR CI TAU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; stars: individual (CI Tau); stars:
low-mass; stars: pre-main sequence; star spots; techniques: radial
velocities
ID SUB-STELLAR COMPANION; RADIAL-VELOCITY VARIABILITY; MAIN-SEQUENCE STARS;
NEARBY M DWARFS; MAGNETOSPHERIC ACCRETION; LIGHT CURVES; NGC 2264; BROWN
DWARF; PHOTOMETRIC VARIABILITY; CIRCUMSTELLAR DISKS
AB The similar to 2 Myr old classical T Tauri star CI Tau shows periodic variability in its radial velocity (RV) variations measured at infrared (IR) and optical wavelengths. We find that these observations are consistent with a massive planet in a similar to 9 day period orbit. These results are based on 71 IR RV measurements of this system obtained over five years, and on 26 optical RV measurements obtained over nine years. CI Tau was also observed photometrically in the optical on 34 nights over similar to one month in 2012. The optical RV data alone are inadequate to identify an orbital period, likely the result of star spot and activity-induced noise for this relatively small data set. The infrared RV measurements reveal significant periodicity at similar to 9 days. In addition, the full set of optical and IR RV measurements taken together phase coherently and with equal amplitudes to the similar to 9 day period. Periodic RV signals can in principle be produced by cool spots, hotspots, and reflection of the stellar spectrum off the inner disk, in addition to resulting from a planetary companion. We have considered each of these and find the planet hypothesis most consistent with the data. The RV amplitude yields an M sin i of similar to 8.1 M-Jup; in conjunction with a 1.3 mm continuum emission measurement of the circumstellar disk inclination from the literature, we find a planet mass of similar to 11.3 M-Jup, assuming alignment of the planetary orbit with the disk.
C1 [Johns-Krull, Christopher M.; Hartigan, Patrick M.; Mahmud, Naved I.; Chen, Wei; Cauley, P. Wilson; Jones, Joshua A.] Rice Univ, Dept Phys & Astron, MS-108,6100 Main St, Houston, TX 77005 USA.
[McLane, Jacob N.; Prato, L.; Skiff, B. A.] Lowell Observ, 1400 West Mars Hill Rd, Flagstaff, AZ 86001 USA.
[McLane, Jacob N.] No Arizona Univ, Dept Phys & Astron, S San Francisco St, Flagstaff, AZ 86011 USA.
[Crockett, Christopher J.] Sci News, 1719 N St NW, Washington, DC 20036 USA.
[Jaffe, Daniel T.; Mace, G. N.] Univ Texas Austin, Dept Astron, RL Moore Hall, Austin, TX 78712 USA.
[Beichman, Charles A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Beichman, Charles A.] CALTECH, NASA Exoplanet Sci Inst NExScI, 770 S Wilson Ave, Pasadena, CA 91125 USA.
[Cauley, P. Wilson] Wesleyan Univ, Dept Astron, 45 Wyllys Ave, Middletown, CT 06459 USA.
RP McLane, JN (reprint author), Lowell Observ, 1400 West Mars Hill Rd, Flagstaff, AZ 86001 USA.; McLane, JN (reprint author), No Arizona Univ, Dept Phys & Astron, S San Francisco St, Flagstaff, AZ 86011 USA.
EM jmclane@lowell.edu; lprato@lowell.edu
FU SIM Young Planets Key Project; NASA Origins grants [05-SSO05-86,
07-SSO07-86]; NSF [AST-1212122]; National Aeronautics and Space
Administration; National Science Foundation; U.S. National Science
Foundation [AST-1229522]; University of Texas at Austin; Korean GMT
Project of KASI; W. M. Keck Foundation; Arizona Space Grant consortium
FX We thank the IRTF TOs Dave Griep, Bill Golisch, and Eric Volquardsen and
SAs John Rayner, Mike Connelly, and Bobby Bus, the Keck Observatory OAs
Cynthia Wilburn and Heather Hershley and SAs Scott Dahm and Greg Wirth,
KPNO staff Dave Summers, Di Harmer, and Dick Joyce, and Dave Doss of
McDonald Observatory for their exceptional observing support over the
many years of this program. L.P. is grateful to Peter Bodenheimer, Joe
Llama, Evgenya Shkolnik, and Ben Zuckerman for insightful discussions.
Partial support for this research was provided by the SIM Young Planets
Key Project and by NASA Origins grants 05-SSO05-86 and 07-SSO07-86 to
L.P. Additional support for this work was provided by the NSF through
grant AST-1212122 made to Rice University. We are grateful to the
Arizona Space Grant consortium for support of J.N.M.'s participation in
this work. We wish to thank an anonymous referee for many helpful
comments that improved the manuscript. This work made use of the SIMBAD
reference database, the NASA Astrophysics Data System, and the 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 work made use of the Immersion Grating Infrared
Spectrograph (IGRINS) that was developed under a collaboration between
the University of Texas at Austin and the Korea Astronomy and Space
Science Institute (KASI) with the financial support of the U.S. National
Science Foundation under grant AST-1229522, of the University of Texas
at Austin, and of the Korean GMT Project of KASI. Some data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California, and the National Aeronautics and Space
Administration. The observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors recognize
and acknowledge the significant cultural role that the summit of Mauna
Kea plays within the indigenous Hawaiian community. We are grateful for
the opportunity to conduct observations from this special mountain.
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SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900106
ER
PT J
AU Kay, C
Opher, M
Kornbleuth, M
AF Kay, C.
Opher, M.
Kornbleuth, M.
TI PROBABILITY OF CME IMPACT ON EXOPLANETS ORBITING M DWARFS AND SOLAR-LIKE
STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: low-mass; stars: solar-type
ID CORONAL MASS EJECTIONS; IN HABITABLE ZONES; ACTIVITY-ROTATION
RELATIONSHIP; EARTH-LIKE EXOPLANETS; MAIN-SEQUENCE STARS; DIGITAL SKY
SURVEY; MAGNETIC-FIELDS; COOL STARS; TERRESTRIAL EXOPLANETS; EXTRASOLAR
PLANET
AB Solar coronal mass ejections (CMEs) produce adverse space weather effects at Earth. Planets in the close habitable zone of magnetically active M dwarfs may experience more extreme space weather than at Earth, including frequent CME impacts leading to atmospheric erosion and leaving the surface exposed to extreme flare activity. Similar erosion may occur for hot Jupiters with close orbits around solar-like stars. We have developed a model, Forecasting a CME's Altered Trajectory (ForeCAT), which predicts a CME's deflection. We adapt ForeCAT to simulate CME deflections for the mid-type M dwarf V374 Peg and hot Jupiters with solar-type hosts. V374 Peg's strong magnetic fields can trap CMEs at the M dwarfs's Astrospheric Current Sheet, that is, the location of the minimum in the background magnetic field. Solar-type CMEs behave similarly, but have much smaller deflections and do not become trapped at the Astrospheric Current Sheet. The probability of planetary impact decreases with increasing inclination of the planetary orbit with respect to the Astrospheric Current Sheet: 0.5-5 CME impacts per day for M dwarf exoplanets, 0.05-0.5 CME impacts per day for solar-type hot Jupiters. We determine the minimum planetary magnetic field necessary to shield a planet's atmosphere from CME impacts. M dwarf exoplanets require values between tens and hundreds of Gauss. Hot Jupiters around a solar-type star, however, require a more reasonable <30 G. These values exceed the magnitude required to shield a planet from the stellar wind, suggesting that CMEs may be the key driver of atmospheric losses.
C1 [Kay, C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Kay, C.; Opher, M.; Kornbleuth, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
RP Kay, C (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.; Kay, C (reprint author), Boston Univ, Dept Astron, Boston, MA 02215 USA.
EM ckay@bu.edu
OI Kay, Christina/0000-0002-2827-6012
FU NSF Career Grant [ATM-0747654]
FX M.O. acknowledges the support of NSF Career Grant ATM-0747654.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900095
ER
PT J
AU Ko, YK
Young, PR
Muglach, K
Warren, HP
Ugarte-Urra, I
AF Ko, Yuan-Kuen
Young, Peter R.
Muglach, Karin
Warren, Harry P.
Ugarte-Urra, Ignacio
TI CORRELATION OF CORONAL PLASMA PROPERTIES AND SOLAR MAGNETIC FIELD IN A
DECAYING ACTIVE REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: abundances; Sun: corona; Sun: magnetic fields
ID EUV IMAGING SPECTROMETER; LONG-TERM EVOLUTION; NON-WKB MODELS; ABUNDANCE
MEASUREMENTS; ELEMENTAL ABUNDANCES; CHEMICAL-COMPOSITION; ATOMIC
DATABASE; EMISSION; WIND; HINODE
AB We present the analysis of a decaying active region observed by the EUV Imaging Spectrometer on Hinode during 2009 December 7-11. We investigated the temporal evolution of its structure exhibited by plasma at temperatures from 300,000 to 2.8 million degrees, and derived the electron density, differential emission measure, effective electron temperature, and elemental abundance ratios of Si/S and Fe/S (as a measure of the First Ionization Potential (FIP) Effect). We compared these coronal properties to the temporal evolution of the photospheric magnetic field strength obtained from the Solar and Heliospheric Observatory Michelson Doppler Imager magnetograms. We find that, while these coronal properties all decreased with time during this decay phase, the largest change was at plasma above 1.5 million degrees. The photospheric magnetic field strength also decreased with time but mainly for field strengths lower than about 70 Gauss. The effective electron temperature and the FIP bias seem to reach a "basal" state (at 1.5 x 10(6) K and 1.5, respectively) into the quiet Sun when the mean photospheric magnetic field (excluding all areas < 10 G) weakened to below 35 G, while the electron density continued to decrease with the weakening field. These physical properties are all positively correlated with each other and the correlation is the strongest in the high-temperature plasma. Such correlation properties should be considered in the quest for our understanding of how the corona is heated. The variations in the elemental abundance should especially be considered together with the electron temperature and density.
C1 [Ko, Yuan-Kuen; Warren, Harry P.; Ugarte-Urra, Ignacio] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Young, Peter R.] George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA.
[Young, Peter R.] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
[Muglach, Karin] Artep Inc, Ellicott City, MD 21042 USA.
[Muglach, Karin] NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
RP Ko, YK (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM yuan-kuen.ko@nrl.navy.mil
OI Ugarte-Urra, Ignacio/0000-0001-5503-0491
FU JAXA; NAOJ (Japan); STFC (UK); NASA [HGI NNH10AN82I]; ESA; NSC (Norway);
NASA's Hinode program
FX We thank E. Landi for executing these EIS observations, U. Feldman for
helpful discussions, and the referee for valuable comments. Hinode is a
Japanese mission developed and launched by ISAS/JAXA, collaborating with
NAOJ as a domestic partner, NASA and STFC (UK) as international
partners. Scientific operation of the Hinode mission is conducted by the
Hinode science team organized at ISAS/JAXA. This team mainly consists of
scientists from institutes in the partner countries. Support for the
post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK),
NASA, ESA, and NSC (Norway). SOHO is a project of international
cooperation between ESA and NASA. CHIANTI is a collaborative project
involving George Mason University, the University of Michigan (USA) and
the University of Cambridge (UK). This work was supported by the Chief
of Naval Research, NASA's Hinode program, and NASA grant HGI NNH10AN82I.
NR 53
TC 0
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 126
DI 10.3847/0004-637X/826/2/126
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900026
ER
PT J
AU Kogut, A
Fixsen, DJ
AF Kogut, A.
Fixsen, D. J.
TI FOREGROUND BIAS FROM PARAMETRIC MODELS OF FAR-IR DUST EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dust, extinction; methods: data analysis
ID INTERSTELLAR DUST; AMORPHOUS SOLIDS; SPECTRAL OBSERVATIONS; GALACTIC
EMISSION; LOW-TEMPERATURE; POLARIZATION; SUBMILLIMETER; GALAXY; COBE;
RADIATION
AB We use simple toy models of far-IR dust emission to estimate the accuracy to which the polarization of the cosmic microwave background can be recovered using multi-frequency fits, if the parametric form chosen for the fitted dust model differs from the actual dust emission. Commonly used approximations to the far-IR dust spectrum yield CMB residuals comparable to or larger than the sensitivities expected for the next generation of CMB missions, despite fitting the combined CMB + foreground emission to precision 0.1% or better. The Rayleigh-Jeans approximation to the dust spectrum biases the fitted dust spectral index by Delta beta(d) = 0.2 and the inflationary B-mode amplitude by Delta r = 0.03. Fitting the dust to a modified blackbody at a single temperature biases the best-fit CMB by Delta r > 0.003 if the true dust spectrum contains multiple temperature components. A 13-parameter model fitting two temperature components reduces this bias by an order of magnitude if the true dust spectrum is in fact a simple superposition of emission at different temperatures, but fails at the level Delta r = 0.006 for dust whose spectral index varies with frequency. Restricting the observing frequencies to a narrow region near the foreground minimum reduces these biases for some dust spectra but can increase the bias for others. Data at THz frequencies surrounding the peak of the dust emission can mitigate these biases while providing a direct determination of the dust temperature profile.
C1 [Kogut, A.; Fixsen, D. J.] Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
[Fixsen, D. J.] Univ Maryland, College Pk, MD 20742 USA.
RP Kogut, A (reprint author), Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Alan.J.Kogut@nasa.gov
NR 48
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 101
DI 10.3847/0004-637X/826/2/101
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900001
ER
PT J
AU Millan-Gabet, R
Che, X
Monnier, JD
Sitko, ML
Russell, RW
Grady, CA
Day, AN
Perry, RB
Harries, TJ
Aarnio, AN
Colavita, MM
Wizinowich, PL
Ragland, S
Woillez, J
AF Millan-Gabet, Rafael
Che, Xiao
Monnier, John D.
Sitko, Michael L.
Russell, Ray W.
Grady, Carol A.
Day, Amanda N.
Perry, R. B.
Harries, Tim J.
Aarnio, Alicia N.
Colavita, Mark M.
Wizinowich, Peter L.
Ragland, Sam
Woillez, Julien
TI CONFRONTING STANDARD MODELS OF PROTO-PLANETARY DISKS WITH NEW
MID-INFRARED SIZES FROM THE KECK INTERFEROMETER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; protoplanetary disks; stars: pre-main sequence;
techniques: high angular resolution
ID MAIN-SEQUENCE STARS; HERBIG-AE/BE STARS; YOUNG STELLAR OBJECTS;
INTERMEDIATE-MASS STARS; FU ORIONIS STARS; T TAURI STARS; CIRCUMSTELLAR
DISKS; AB-AURIGAE; DG-TAU; PLANET FORMATION
AB We present near- and mid-infrared (MIR) interferometric observations made with the Keck Interferometer Nuller and near- contemporaneous spectro-photometry from the infrared telescope facilities (IRTFs) of 11 well-known young stellar objects, several of which were observed for the first time in these spectral and spatial resolution regimes. With au-level spatial resolution, we first establish characteristic sizes of the infrared emission using a simple geometrical model consisting of a hot inner rim and MIR disk emission. We find a high degree of correlation between the stellar luminosity and the MIR disk sizes after using near- infrared data to remove the contribution from the inner rim. We then use a semi-analytical physical model to also find that the very widely used "star + inner dust rim + flared disk" class of models strongly fails to reproduce the spectral energy distribution (SED) and spatially resolved MIR data simultaneously; specifically a more compact source of MIR emission is required than results from the standard flared disk model. We explore the viability of a modification to the model whereby a second dust rim containing smaller dust grains is added, and find that the 2-rim model leads to significantly improved fits in most cases. This complexity is largely missed when carrying out SED modeling alone, although detailed silicate feature fitting by McClure et al. recently came to a similar conclusion. As has been suggested recently by Menu et al., the difficulty in predicting MIR sizes from the SED alone might hint at "transition disk"-like gaps in the inner au; however, the relatively high correlation found in our MIR disk size versus stellar luminosity relation favors layered disk morphologies and points to missing disk model ingredients instead.
C1 [Millan-Gabet, Rafael] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Che, Xiao; Monnier, John D.; Aarnio, Alicia N.] Univ Michigan, Dept Astron, 1085 S Univ Ave,303B West Hall, Ann Arbor, MI 48109 USA.
[Sitko, Michael L.; Day, Amanda N.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Sitko, Michael L.] Space Sci Inst, Ctr Extrasolar Planetary Syst, Boulder, CO 80301 USA.
[Russell, Ray W.] Aerosp Corp, POB 92957, Los Angeles, CA 90009 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Fukushima 9600231, Japan.
[Perry, R. B.] NASA, Langley Res Ctr, MS 160, Hampton, VA 23681 USA.
[Harries, Tim J.] Univ Exeter, Dept Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Colavita, Mark M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wizinowich, Peter L.; Ragland, Sam; Woillez, Julien] Keck Observ, 65-1120 Mamalahoa Hwy, Kamuela, HI 96743 USA.
RP Millan-Gabet, R (reprint author), CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
EM R.Millan-Gabet@caltech.edu
FU National Aeronautics and Space Administration, Exoplanet Exploration
Program; W.M. Keck Foundation; National Aeronautics and Space
Administration [NNH14CK55B]; NASA ADAP [NNX09AC73G]; IR&D program of The
Aerospace Corporation.
FX The authors acknowledge fruitful discussions with Nuria Calvet and
Melissa McClure. Part of this work was performed while XC was a Visiting
Graduate Student Research Fellow at the Infrared Processing and Analysis
Center (IPAC), California Institute of Technology. The Keck
Interferometer was funded by the National Aeronautics and Space
Administration as part of its Exoplanet Exploration Program. Data
presented herein were obtained at the W.M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California and the National Aeronautics
and Space Administration. The Observatory was made possible by the
generous financial support of the W.M. Keck Foundation. The authors
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. Data presented
in this paper were obtained at the Infrared Telescope Facility, which is
operated by the University of Hawaii under contract NNH14CK55B with the
National Aeronautics and Space Administration. We gratefully acknowledge
support and participation in the IRTF/BASS observing runs by Daryl Kim,
The Aerospace Corporation. This work has made use of services produced
by the NASA Exoplanet Science Institute at the California Institute of
Technology. M.S. was supported by NASA ADAP grant NNX09AC73G. R.W.R. was
supported by the IR&D program of The Aerospace Corporation.
NR 81
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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 AUG 1
PY 2016
VL 826
IS 2
AR 120
DI 10.3847/0004-637X/826/2/120
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900020
ER
PT J
AU Stone, M
Veilleux, S
Melendez, M
Sturm, E
Gracia-Carpio, J
Gonzalez-Alfonso, E
AF Stone, M.
Veilleux, S.
Melendez, M.
Sturm, E.
Gracia-Carpio, J.
Gonzalez-Alfonso, E.
TI THE SEARCH FOR MOLECULAR OUTFLOWS IN LOCAL VOLUME AGNs WITH
HERSCHEL-PACS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING
GALAXIES; NARROW-LINE REGION; SPECTRAL ENERGY-DISTRIBUTIONS;
SUPERMASSIVE BLACK-HOLES; SPITZER-SPACE-TELESCOPE; PALOMAR-GREEN
QUASARS; SEYFERT 1 GALAXIES; HOST GALAXIES
AB We present the results from a systematic search for galactic-scale, molecular (OH 119 mu m) outflows in a sample of 52 Local Volume (d < 50 Mpc) Burst Alert Telescope detected active galactic nuclei (BAT AGNs) with Herschel-PACS. We combine the results from our analysis of the BAT AGNs with the published Herschel/PACS data of 43 nearby (z < 0.3) galaxy mergers, mostly ultra-luminous infrared galaxies (ULIRGs) and QSOs. The objects in our sample of BAT AGNs have, on average, similar to 10-100 times lower AGN luminosities, star formation rates, and stellar masses than those of the ULIRG and QSO samples. OH 119 mu m is detected in 42 of our BAT AGN targets. Evidence for molecular outflows (i.e., OH absorption profiles with median velocities more blueshifted than -50 km s(-1) and/or blueshifted wings with 84% velocities less than -300 km s(-1)) is seen in only four BAT AGNs (NGC 7479 is the most convincing case). Evidence for molecular inflows (i.e., OH absorption profiles with median velocities more redshifted than 50 km s(-1)) is seen in seven objects, although an inverted P-Cygni profile is detected unambiguously in only one object (Circinus). Our data show that both the starburst and AGN contribute to driving OH outflows, but the fastest OH winds require AGNs with quasar-like luminosities. We also confirm that the total absorption strength of OH 119 mu m is a good proxy for dust optical depth as it correlates strongly with the 9.7 mu m silicate absorption feature, a measure of obscuration originating in both the nuclear torus and host galaxy disk.
C1 [Stone, M.; Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Melendez, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Melendez, M.] Wyle Sci, Technol & Engn Grp, 1290 Hercules Ave, Houston, TX 77058 USA.
[Sturm, E.; Gracia-Carpio, J.] Max Planck Inst Extraterr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany.
[Gonzalez-Alfonso, E.] Univ Alcala De Henares, Dept Fis & Matemat, Campus Univ, E-28871 Madrid, Spain.
RP Stone, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM mjstone@astro.umd.edu; veilleux@astro.umd.edu; marcio@astro.umd.edu
OI Veilleux, Sylvain/0000-0002-3158-6820
FU NASA [1427277, 1454738]
FX Support for this work was provided by NASA through Herschel contracts
1427277 and 1454738 (M.S., S.V., and M.M.). We thank Lisa Winter,
Michael Koss, Richard Mushotsky, Ranjan Vasudevan, Steve
Hailey-Dunsheath, Ric Davies, Linda Tacconi, David Rupke, Jack Tueller,
and Wayne Baumgartner who were Co-Investigators of the original OT-2
Herschel proposal. We also thank Alessandra Contursi for her technical
assistance and the referee whose thoughtful suggestions helped to
improve this paper. This research made use of PySpecKit, an open-source
spectroscopic toolkit hosted at http://pyspeckit.bitbucket.org. This
work has made use of NASA's Astrophysics Data System Abstract Service
and 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 86
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2016
VL 826
IS 2
AR 111
DI 10.3847/0004-637X/826/2/111
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900011
ER
PT J
AU Venumadhav, T
Chang, TC
Dore, O
Hirata, CM
AF Venumadhav, Tejaswi
Chang, Tzu-Ching
Dore, Olivier
Hirata, Christopher M.
TI A PRACTICAL THEOREM ON USING INTERFEROMETRY TO MEASURE THE GLOBAL 21 cm
SIGNAL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; dark ages, reionization, first stars;
instrumentation: interferometers
ID SIMILAR-TO 20; INTERGALACTIC MEDIUM; HIGH-REDSHIFT; CENTIMETER
FLUCTUATIONS; COSMIC REIONIZATION; POWER SPECTRUM; DARK-MATTER;
LY-ALPHA; EPOCH; CONSTRAINTS
AB The sky-averaged, or global, background of redshifted 21 cm radiation is expected to be a rich source of information on cosmological reheating and reionization. However, measuring the signal is technically challenging: one must extract a small, frequency-dependent signal from under much brighter spectrally smooth foregrounds. Traditional approaches to study the global signal have used single antennas, which require one to calibrate out the frequency-dependent structure in the overall system gain (due to internal reflections, for example) as well as remove the noise bias from auto-correlating a single amplifier output. This has motivated proposals to measure the signal using cross-correlations in interferometric setups, where additional calibration techniques are available. In this paper we focus on the general principles driving the sensitivity of the interferometric setups to the global signal. We prove that this sensitivity is directly related to two characteristics of the setup: the cross-talk between readout channels (i.e., the signal picked up at one antenna when the other one is driven) and the correlated noise due to thermal fluctuations of lossy elements (e.g., absorbers or the ground) radiating into both channels. Thus in an interferometric setup, one cannot suppress cross-talk and correlated thermal noise without reducing sensitivity to the global signal by the same factor-instead, the challenge is to characterize these effects and their frequency dependence. We illustrate our general theorem by explicit calculations within toy setups consisting of two short-dipole antennas in free space and above a perfectly reflecting ground surface, as well as two well-separated identical lossless antennas arranged to achieve zero cross-talk.
C1 [Venumadhav, Tejaswi] Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA.
[Chang, Tzu-Ching] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Dore, Olivier] CALTECH, Mail Code 350-17, Pasadena, CA 91125 USA.
[Dore, Olivier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hirata, Christopher M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Lane, Columbus, OH 43210 USA.
RP Venumadhav, T (reprint author), Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA.
FU Schmidt Fellowship; Fund for Memberships in Natural Sciences at the
Institute for Advanced Study; US Department of Energy; David & Lucile
Packard Foundation; Simons Foundation; MoST [103-2112-M-001-002-MY3]
FX TV gratefully acknowledges support from the Schmidt Fellowship and the
Fund for Memberships in Natural Sciences at the Institute for Advanced
Study. CH is supported by the US Department of Energy, the David &
Lucile Packard Foundation, and the Simons Foundation. T.-C. C.
acknowledges support from MoST grant 103-2112-M-001-002-MY3. Part of the
research described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 62
TC 0
Z9 0
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 AUG 1
PY 2016
VL 826
IS 2
AR 116
DI 10.3847/0004-637X/826/2/116
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU1ON
UT WOS:000381977900016
ER
PT J
AU Johnson, MS
Kuang, S
Wang, LH
Newchurch, MJ
AF Johnson, Matthew S.
Kuang, Shi
Wang, Lihua
Newchurch, M. J.
TI Evaluating Summer-Time Ozone Enhancement Events in the Southeast United
States
SO ATMOSPHERE
LA English
DT Article
DE ozone; air quality; source attribution; TOLNet Lidar
ID SURFACE OZONE; POTENTIAL VORTICITY; TROPOSPHERIC OZONE; EASTERN US;
CHEMISTRY; TRANSPORT; MODEL; FLUX; NOX; CLIMATOLOGY
AB This study evaluates source attribution of ozone (O-3) in the southeast United States (US) within O-3 lamina observed by the University of Alabama in Huntsville (UAH) Tropospheric Ozone Lidar Network (TOLNet) system during June 2013. This research applies surface-level and airborne in situ data and chemical transport model simulations (GEOS-Chem) in order to quantify the impact of North American anthropogenic emissions, wildfires, lightning NOx, and long-range/stratospheric transport on the observed O-3 lamina. During the summer of 2013, two anomalous O-3 layers were observed: (1) a nocturnal near-surface enhancement and (2) a late evening elevated (3-6 km above ground level) O-3 lamina. A "brute force" zeroing method was applied to quantify the impact of individual emission sources and transport pathways on the vertical distribution of O-3 during the two observed lamina. Results show that the nocturnal O-3 enhancement on 12 June 2013 below 3 km was primarily due to wildfire emissions and the fact that daily maximum anthropogenic emission contributions occurred during these night-time hours. During the second case study it was predicted that above average contributions from long-range/stratospheric transport was largely contributing to the O-3 lamina observed between 3 and 6 km on 29 June 2013. Other models, remote-sensing observations, and ground-based/airborne in situ data agree with the source attribution predicted by GEOS-Chem simulations. Overall, this study demonstrates the dynamic atmospheric chemistry occurring in the southeast US and displays the various emission sources and transport processes impacting O-3 enhancements at different vertical levels of the troposphere.
C1 [Johnson, Matthew S.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Kuang, Shi; Wang, Lihua] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
[Newchurch, M. J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
RP Johnson, MS (reprint author), NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
EM matthew.s.johnson@nasa.gov; kuang@nsstc.uah.edu;
lihuawang@nsstc.uah.edu; mike@nsstc.uah.edu
RI Chem, GEOS/C-5595-2014
FU TOLNet program
FX This work is supported by the TOLNet program developed by NASA's Science
Mission Directorate. Matthew Johnson would also like to thank Daniel
Jacob, Katie Travis, and the Harvard University Atmospheric Chemistry
Modeling Group for providing the base model GEOS-Chem used during our
research. We would also like to thank the SENEX science, instrument, and
aircraft teams, with particular thanks to Ilana Pollack and Thomas
Ryerson (O3, NOx), Joshua Schwarz (BC), John S.
Holloway (CO), and Martin Graus (Isoprene) for specific trace gas and
aerosol data. Resources supporting this work were provided by the NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at NASA Ames Research Center. All the
authors express gratitude to the support from NASA's Earth Science
Division at Ames Research Center. Finally, the views, opinions, and
findings contained in this report are those of the authors and should
not be construed as an official NASA or United States Government
position, policy, or decision.
NR 46
TC 1
Z9 1
U1 9
U2 11
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2073-4433
J9 ATMOSPHERE-BASEL
JI Atmosphere
PD AUG
PY 2016
VL 7
IS 8
AR 108
DI 10.3390/atmos7080108
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU8PT
UT WOS:000382476600013
ER
PT J
AU Boutin, J
Chao, Y
Asher, WE
Delcroix, T
Drucker, R
Drushka, K
Kolodziejczyk, N
Lee, T
Reul, N
Reverdin, G
Schanze, J
Soloviev, A
Yu, L
Anderson, J
Brucker, L
Dinnat, E
Santos-Garcia, A
Jones, WL
Maes, C
Meissner, T
Tang, W
Vinogradova, N
Ward, B
AF Boutin, J.
Chao, Y.
Asher, W. E.
Delcroix, T.
Drucker, R.
Drushka, K.
Kolodziejczyk, N.
Lee, T.
Reul, N.
Reverdin, G.
Schanze, J.
Soloviev, A.
Yu, L.
Anderson, J.
Brucker, L.
Dinnat, E.
Santos-Garcia, A.
Jones, W. L.
Maes, C.
Meissner, T.
Tang, W.
Vinogradova, N.
Ward, B.
TI SATELLITE AND IN SITU SALINITY Understanding Near-Surface Stratification
and Subfootprint Variability
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID PACIFIC WARM POOL; BAND RADIOMETER/SCATTEROMETER OBSERVATIONS; WESTERN
EQUATORIAL PACIFIC; AIR-SEA INTERACTION; NORTH-ATLANTIC; OCEAN SALINITY;
BOUNDARY-LAYER; BARRIER LAYER; RIVER PLUME; TROPICAL OCEANS
AB Remote sensing of salinity using satellite-mounted microwave radiometers provides new perspectives for studying ocean dynamics and the global hydrological cycle. Calibration and validation of these measurements is challenging because satellite and in situ methods measure salinity differently. Microwave radiometers measure the salinity in the top few centimeters of the ocean, whereas most in situ observations are reported below a depth of a few meters. Additionally, satellites measure salinity as a spatial average over an area of about 100 x 100 km(2). In contrast, in situ sensors provide pointwise measurements at the location of the sensor. Thus, the presence of vertical gradients in, and horizontal variability of, sea surface salinity complicates comparison of satellite and in situ measurements. This paper synthesizes present knowledge of the magnitude and the processes that contribute to the formation and evolution of vertical and horizontal variability in near surface salinity. Rainfall, freshwater plumes, and evaporation can generate vertical gradients of salinity, and in some cases these gradients can be large enough to affect validation of satellite measurements. Similarly, mesoscale to submesoscale processes can lead to horizontal variability that can also affect comparisons of satellite data to in situ data. Comparisons between satellite and in situ salinity measurements must take into account both vertical stratification and horizontal variability.
C1 [Boutin, J.; Kolodziejczyk, N.; Reverdin, G.] Univ Paris 06, Sorbonne Univ, LOCEAN Lab, CNRS,IRD,MNHN, Paris, France.
[Chao, Y.] Remote Sensing Solut, Pasadena, CA USA.
[Asher, W. E.; Drushka, K.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Delcroix, T.] Lab Etud Geophys & Oceanog Spatiale, Toulouse, France.
[Drucker, R.; Anderson, J.] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Lee, T.; Tang, W.] Jet Prop Lab, Pasadena, CA USA.
[Reul, N.] IFREMER, Lab Oceanog Space, Toulon, France.
[Schanze, J.] Earth & Space Res, Seattle, WA USA.
[Soloviev, A.] Nova Southeastern Univ, Dania, FL USA.
[Yu, L.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Brucker, L.] Univ Space Res Assoc, Greenbelt, MD USA.
[Brucker, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Dinnat, E.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD USA.
[Dinnat, E.] Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA USA.
[Santos-Garcia, A.; Jones, W. L.] Univ Cent Florida, Elect & Comp Engn Dept, Orlando, FL 32816 USA.
[Maes, C.] UBO, Ifremer, IRD, Lab Phys Oceans,CNRS, Plouzane, France.
[Meissner, T.] Remote Sensing Syst, Santa Rosa, CA USA.
[Vinogradova, N.] Atmospher & Environm Res, Lexington, MA USA.
[Ward, B.] Natl Univ Ireland, Sch Phys, AirSea Lab, Galway, Ireland.
[Ward, B.] Natl Univ Ireland, Ryan Inst, Galway, Ireland.
RP Boutin, J (reprint author), LOCEAN Lab, 4 Pl Jussieu, F-75005 Paris, France.
EM jb@locean-ipsl.upmc.fr
RI Delcroix, Thierry/I-6103-2016; Kolodziejczyk, Nicolas/P-3553-2015;
Brucker, Ludovic/A-8029-2010;
OI Delcroix, Thierry/0000-0002-8850-4865; Kolodziejczyk,
Nicolas/0000-0002-0751-1351; Brucker, Ludovic/0000-0001-7102-8084; Reul,
Nicolas/0000-0003-4881-2967
FU SISS
FX This paper was developed from discussions of the Satellite and In Situ
Salinity (SISS) mailing list (http://siss.locean-ipsl.upmc.fr) and
several SISS-sponsored working group meetings at the American
Geophysical Union (AGU) Fall Meeting and European Geosciences Union
(EGU) General Assembly. We thank the following people who read the
manuscript and provided comments: Eric Bayler, Rafael J. Catany, Meike
Sena Martins, and Yuhe Tony Song.
NR 98
TC 7
Z9 7
U1 6
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2016
VL 97
IS 8
BP 1391
EP +
DI 10.1175/BAMS-D-15-00032.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU7YO
UT WOS:000382430700011
ER
PT J
AU Bauschlicher, CW
AF Bauschlicher, Charles W., Jr.
TI The low-lying electronic states of SiO
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
DE Electronic transition
ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS;
CONFIGURATION-INTERACTION; RADIATIVE LIFETIMES; OSCILLATOR-STRENGTHS;
TRANSITION
AB The singlet states of SiO that correlate with ground state atoms have been studied. The computed spectroscopic constants are in good agreement with experiment. The lifetime of the E state has been calculated to be 10.9 ns; this is larger than the results of previous computations and is in excellent agreement with the experimental value of 10.5 +/- 1.1 ns. The lifetime of the A state is about three times larger than found in experiment. We suggest that absorption from the X state to the (2)(1)Pi state is responsible for the unidentified lines in the experiment of Hormes et al. Published by Elsevier B.V.
C1 [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bauschlicher, CW (reprint author), Entry Syst & Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov
NR 20
TC 0
Z9 0
U1 3
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD AUG 1
PY 2016
VL 658
BP 76
EP 79
DI 10.1016/j.cplett.2016.06.023
PG 4
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DU7QN
UT WOS:000382409800012
ER
PT J
AU Strong, AL
Lowry, KE
Brown, ZW
Mills, MM
van Dijken, GL
Pickart, RS
Cooper, LW
Frey, KE
Benner, R
Fichot, CG
Mathis, JT
Bates, NR
Arrigo, KR
AF Strong, Aaron L.
Lowry, Kate E.
Brown, Zachary W.
Mills, Matthew M.
van Dijken, Gert L.
Pickart, Robert S.
Cooper, Lee W.
Frey, Karen E.
Benner, Ron
Fichot, Cedric G.
Mathis, Jeremy T.
Bates, Nicholas R.
Arrigo, Kevin R.
TI Mass balance estimates of carbon export in different water masses of the
Chukchi Sea shelf
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Carbon export; Pelagic-benthic coupling; Phytoplankton; Chukchi; Sea ice
ID NET COMMUNITY PRODUCTION; WESTERN ARCTIC-OCEAN; DISSOLVED
ORGANIC-CARBON; BEAUFORT SEAS; CONTINENTAL-SHELF; PACIFIC WATER; BARROW
CANYON; ICE COVER; DENITRIFICATION RATES; PHYTOPLANKTON BLOOMS
AB We construct mass-balance based estimates of carbon (C) export fractions from the water column across the Chukchi Sea shelf. Export is calculated as the difference between phytoplankton drawdown of dissolved inorganic C (DIC) and the accumulation of autochthonous particulate and dissolved organic C in the water column. Organic carbon (C-org) exports of > 50% of DIC drawdown are ubiquitous across the shelf, even during, or shortly after, phytoplankton blooms, suggesting widespread and strong pelagic-benthic coupling. Export fractions on the shelf were generally greater in the less-productive Alaska Coastal Water than in the more productive Bering Shelf-Anadyr Water. Additionally, export fractions were greater in 2011 than in 2010, highlighting the significant spatial and inter-annual variability of the fate of Corg in this ecologically and biogeochemically important, and rapidly changing, ecosystem. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Strong, Aaron L.] Stanford Univ, Emmett Interdisciplinary Program Environm & Resou, Stanford, CA 94305 USA.
[Lowry, Kate E.; Brown, Zachary W.; Mills, Matthew M.; van Dijken, Gert L.; Arrigo, Kevin R.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Pickart, Robert S.] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
[Cooper, Lee W.] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA.
[Frey, Karen E.] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA.
[Benner, Ron; Fichot, Cedric G.] Univ South Carolina, Marine Sci Program, Columbia, SC 29208 USA.
[Mathis, Jeremy T.] NOAA, Pacific Marine Environm Lab, 7600 Sand Point Way Ne, Seattle, WA 98115 USA.
[Bates, Nicholas R.] Bermuda Inst Ocean Sci, St Georges GE 01, Bermuda.
[Fichot, Cedric G.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
RP Strong, AL (reprint author), 473 Via Ortega Suite 226, Stanford, CA 94305 USA.
EM alstrong@stanford.edu
NR 69
TC 1
Z9 1
U1 9
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD AUG
PY 2016
VL 130
BP 88
EP 99
DI 10.1016/j.dsr2.2016.05.003
PG 12
WC Oceanography
SC Oceanography
GA DT6KK
UT WOS:000381592900008
ER
PT J
AU Kegerise, MA
Rufer, SJ
AF Kegerise, Michael A.
Rufer, Shann J.
TI Unsteady heat-flux measurements of second-mode instability waves in a
hypersonic flat-plate boundary layer
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
ID HOT-WIRE ANEMOMETERS; TRANSITION; ROUGHNESS; TUNNEL
AB In this paper, we report on the application of the atomic layer thermopile (ALTP) heat-flux sensor to the measurement of laminar-to-turbulent transition in a hypersonic flat-plate boundary layer. The centerline of the flatplate model was instrumented with a streamwise array of ALTP sensors, and the flat-plate model was exposed to a Mach 6 freestream over a range of unit Reynolds numbers. Here, we observed an unstable band of frequencies that are associated with second-mode instability waves in the laminar boundary layer that forms on the flat-plate surface. The measured frequencies, group velocities, phase speeds, and wavelengths of these instability waves are consistent with data previously reported in the literature. Heat flux time series, and the Morlet wavelet transforms of them, revealed the wave-packet nature of the second-mode instability waves. In addition, a laser-based radiative heating system was used to measure the frequency response functions (FRF) of the ALTP sensors used in the wind tunnel test. These measurements were used to assess the stability of the sensor FRFs over time and to correct spectral estimates for any attenuation caused by the finite sensor bandwidth.
C1 [Kegerise, Michael A.] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA.
[Rufer, Shann J.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Kegerise, MA (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA.
EM michael.a.kegerise@nasa.gov
NR 34
TC 0
Z9 0
U1 6
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
EI 1432-1114
J9 EXP FLUIDS
JI Exp. Fluids
PD AUG
PY 2016
VL 57
IS 8
DI 10.1007/s00348-016-2214-9
PG 15
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA DT1TJ
UT WOS:000381264700007
ER
PT J
AU Tan, SR
Xiong, C
Xu, XL
Tsang, L
AF Tan, Shurun
Xiong, Chuan
Xu, Xiaolan
Tsang, Leung
TI Uniaxial Effective Permittivity of Anisotropic Bicontinuous Random Media
Using NMM3D
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Anisotropy; bicontinuous medium; correlation function; effective
permittivity; Maxwell-Garnett; numerical solutions of Maxwell equations
in 3-dimensions (NMM3D); strong permittivity fluctuations (SPFs)
ID SNOW; SCATTERING; BAND
AB In this letter, we generate anisotropic bicontinuous media with different vertical and horizontal correlation functions. With the computer-generated bicontinuous medium, we then use numerical solutions of Maxwell equations in 3-dimensions (NMM3D) to calculate the anisotropic effective permittivities and the effective propagation constants of V and H polarizations. The copolarization phase difference (CPD) of VV and HH is then derived. The CPDs have recently been applied to the retrieval of snow water equivalent, snow depth, and anisotropy. The NMM3D simulation results are also compared with the results of the strong permittivity fluctuations in the low frequency limit and compared against the Maxwell-Garnett mixing formula.
C1 [Tan, Shurun; Xiong, Chuan; Tsang, Leung] Univ Michigan, Dept Elect Engn & Comp Sci, Radiat Lab, Ann Arbor, MI 48109 USA.
[Xiong, Chuan] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Beijing 100101, Peoples R China.
[Xu, Xiaolan] Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tan, SR (reprint author), Univ Michigan, Dept Elect Engn & Comp Sci, Radiat Lab, Ann Arbor, MI 48109 USA.
EM srtan@umich.edu; xiongchuan@radi.ac.cn; xiaolan.xu@jpl.nasa.gov;
leutsang@umich.edu
FU National Aeronautics and Space Administration (NASA) [NNX15AU15G]; NASA;
NASA [NNX15AI13G]; National Science Foundation (NSF) Polar Science
Division [1503917]; NSF XSEDE [TG-EAR100002]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) Terrestrial Hydrology Program under Grant
NNX15AU15G, by the NASA Instrument Incubator Program "Enhancement,
Demonstration, and Validation of the Wideband Instrument for Snow
Measurements (WISM)," by the NASA Remote Sensing Theory Program under
Grant NNX15AI13G, by National Science Foundation (NSF) Polar Science
Division Grant 1503917, and by NSF XSEDE Grant TG-EAR100002.
NR 18
TC 0
Z9 0
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD AUG
PY 2016
VL 13
IS 8
BP 1168
EP 1172
DI 10.1109/LGRS.2016.2574759
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1LR
UT WOS:000382683100027
ER
PT J
AU Ricko, M
Adler, RF
Huffman, GJ
AF Ricko, Martina
Adler, Robert F.
Huffman, George J.
TI Climatology and Interannual Variability of Quasi-Global Intense
Precipitation Using Satellite Observations
SO JOURNAL OF CLIMATE
LA English
DT Article
ID EXTREME RAINFALL EVENTS; SOUTH-AMERICA; TROPICAL RAINFALL; INTERDECADAL
VARIABILITY; MONSOON SEASON; ANALYSIS TMPA; TRMM; RESOLUTION; GPCP;
VALIDATION
AB Climatology and variations of recent mean and intense precipitation over a near-global (50 degrees S-50 degrees N) domain on a monthly and annual time scale are analyzed. Data used to derive daily precipitation to examine the effects of spatial and temporal coverage of intense precipitation are from the current Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) 3B42 version 7 precipitation product, with high spatial and temporal resolution during 1998-2013. Intense precipitation is defined by several different parameters, such as a 95th percentile threshold of daily precipitation, a mean precipitation that exceeds that percentile, or a fixed threshold of daily precipitation value (e.g., 25 and 50 mm day(-1)). All parameters are used to identify the main characteristics of spatial and temporal variation of intense precipitation. High correlations between examined parameters are observed, especially between climatological monthly mean precipitation and intense precipitation, over both tropical land and ocean. Among the various parameters examined, the one best characterizing intense rainfall is a fraction of daily precipitation >= 25 mm day(-1), defined as a ratio between the intense precipitation above the used threshold and mean precipitation. Regions that experience an increase in mean precipitation likely experience a similar increase in intense precipitation, especially during the El Nino-Southern Oscillation (ENSO) events. Improved knowledge of this intense precipitation regime and its strong connection to mean precipitation given by the fraction parameter can be used for monitoring of intense rainfall and its intensity on a global to regional scale.
C1 [Ricko, Martina] SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA.
[Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Ricko, M (reprint author), SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA.
EM mricko@sgt-inc.com
FU NASA NEWS Program; NASA PMM Program
FX This research was supported by the NASA NEWS Program and the NASA PMM
Program. TRMM 3B42V7 product data were provided by the NASA
Precipitation Processing System (PPS) at
ftp://trmmopen.pps.eosdis.nasa.gov/trmmdata/.
NR 43
TC 1
Z9 1
U1 6
U2 6
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 AUG
PY 2016
VL 29
IS 15
BP 5447
EP 5468
DI 10.1175/JCLI-D-15-0662.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DS4PR
UT WOS:000380763500005
ER
PT J
AU Stephens, GL
Kahn, BH
Richardson, M
AF Stephens, Graeme L.
Kahn, Brian H.
Richardson, Mark
TI The Super Greenhouse Effect in a Changing Climate
SO JOURNAL OF CLIMATE
LA English
DT Article
ID STRATOSPHERIC WATER-VAPOR; SURFACE-TEMPERATURE; RADIATIVE-TRANSFER;
FEEDBACKS; MODELS; CO2; OCEAN
AB In all outputs of the 1% yr (1) increase in CO2 climate model experiments archived under the World Climate Research Programme's (WCRP) phase 5 of the Coupled Model Intercomparison Project (CMIP5), regions exist in the low latitudes where both the clear-sky and all-sky OLR decrease with surface warming. These are identified as regions of positive longwave feedback and are regions of a super greenhouse effect (SGE). These SGE regions are identified from feedback analysis of the 4 x CO2 abrupt experiments of CMIP5, and despite their existence, there is little agreement across models as to the magnitude of the effect. The general effects of clouds on the SGE are to amplify the clear-sky SGE, but there is also poor agreement on the magnitude of the amplification that varies by an order of magnitude across models. Sensitivity analyses indicate that localized SGE regions are spatially aligned with a large moistening of the upper troposphere. The reduction in clear-sky OLR arises from a reduction in emission in the far IR with nonnegligible contributions from mid-IR emission from the midtroposphere. When viewed in the broader context of meridional heat transport, it is found that of the 1.03-PW rate of heat gained globally, 0.8 PW is absorbed in the tropics and is contributed almost equally by reductions in clear-sky longwave emission (i.e., the clear-sky SGE) and increased absorbed clear-sky solar radiation associated with increased water vapor. The processes that define the clear-sky SGE are shown to be fundamental to the way models accumulate heat and then transport it poleward.
C1 [Stephens, Graeme L.; Kahn, Brian H.; Richardson, Mark] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Stephens, Graeme L.] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Stephens, GL (reprint author), Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 233-304, Pasadena, CA 91109 USA.
EM graeme.stephens@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The HadGEM2-ES data used for the offline calculations was furnished by
Alejandro Bodas-Salcedo of the UKMO. The authors and content of the
paper also benefited from discussions with Tim Andrews of the UKMO and
in particular Kyle Armour of the University of Washington. The research
described in this paper was carried out at the Jet Propulsion Laboratory
(JPL), California Institute of Technology, under a contract with the
National Aeronautics and Space Administration. The AIRS version 6
datasets were processed by and obtained from the Goddard Earth Services
Data and Information Services Center (http://daac.gsfc.nasa.gov/;
Teixeira et al. 2013). The JPL author's copyright for this publication
is held by the California Institute of Technology. Government
sponsorship acknowledged.
NR 41
TC 1
Z9 1
U1 17
U2 17
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 AUG
PY 2016
VL 29
IS 15
BP 5469
EP 5482
DI 10.1175/JCLI-D-15-0234.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DS4PR
UT WOS:000380763500006
ER
PT J
AU Scott, RC
Bartels, RE
Funk, CJ
Allen, TJ
Sexton, BW
Dykman, JR
Coulson, DA
AF Scott, Robert C.
Bartels, Robert E.
Funk, Christie J.
Allen, Timothy J.
Sexton, Bradley W.
Dykman, John R.
Coulson, David A.
TI Aeroservoelastic Test of the Subsonic Ultra-Green Aircraft Research
Truss-Braced Wing Model
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID DESIGN OPTIMIZATION; SCHEMES
AB The Subsonic Ultra Green Aircraft Research Truss-Braced Wing aeroservoelastic wind-tunnel test was conducted in the NASA Langley Transonic Dynamics Tunnel. The primary goals of the test were to identify the open-loop flutter boundary and then demonstrate flutter suppression. A secondary goal was to demonstrate gust load alleviation. Open-loop flutter and limit cycle oscillation onset boundaries were identified for a range of Mach numbers and various angles of attack. Two sets of control laws were designed for the model, and both sets of control laws were successful in suppressing flutter. Control laws optimized for gust load alleviation were not designed; however, the flutter suppression control laws were assessed using the Transonic Dynamics Tunnnel airstream oscillation system. This paper describes the experimental apparatus, procedures, and results of the truss-braced wing wind-tunnel model test. Acquired system identification data used to generate aeroservoelastic models are also discussed.
C1 [Scott, Robert C.; Bartels, Robert E.; Funk, Christie J.] NASA Langley Res Ctr, MS 340, Hampton, VA 23681 USA.
[Allen, Timothy J.] Boeing Res & Technol, Loads & Aeroelast, 14900 Bolsa Chica Rd,MS H017-D601, Huntington Beach, CA 92647 USA.
[Sexton, Bradley W.] Boeing Res & Technol, Navigat & Control, 325 James S McDonnell Blvd,MS S306-4030, Huntington Beach, CA 92647 USA.
[Dykman, John R.] Boeing Res & Technol, 14900 Bolsa Chica Rd,MS H017-D601, St Louis, MO 63042 USA.
[Coulson, David A.] Analyt Serv Mat Inc, NASA Langley Res Ctr, MS 340, Hampton, VA 23681 USA.
RP Scott, RC (reprint author), NASA Langley Res Ctr, MS 340, Hampton, VA 23681 USA.
NR 31
TC 0
Z9 0
U1 8
U2 8
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 AUG
PY 2016
VL 39
IS 8
BP 1820
EP 1833
DI 10.2514/1.G000265
PG 14
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DU8YM
UT WOS:000382502500010
ER
PT J
AU Aunai, N
Hesse, M
Lavraud, B
Dargent, J
Smets, R
AF Aunai, N.
Hesse, M.
Lavraud, B.
Dargent, J.
Smets, R.
TI Orientation of the X-line in asymmetric magnetic reconnection
SO JOURNAL OF PLASMA PHYSICS
LA English
DT Article
ID MAGNETOPAUSE RECONNECTION; SOLAR-WIND; FIELDS; RECONSTRUCTION;
MAGNETOSPHERE; PLASMAS; LAYERS
AB Magnetic reconnection can occur in current sheets separating magnetic fields sheared by any angle and of arbitrarily different amplitudes. In such asymmetric and noncoplanar systems, it is not yet understood what the orientation of the X-line will be. Studying how this orientation is determined locally by the reconnection process is important to understand systems such as the Earth magnetopause, where reconnection occurs in regions with large differences in upstream plasma and field properties. This study aims at determining what the local X-line orientation is for different upstream magnetic shear angles in an asymmetric set-up relevant to the Earth's magnetopause. We use two-dimensional hybrid simulations and vary the simulation plane orientation with regard to the fixed magnetic field profile and search for the plane maximizing the reconnection rate. We find that the plane defined by the bisector of upstream fields maximizes the reconnection rate and this appears not to depend on the magnetic shear angle, domain size or upstream plasma and asymmetries.
C1 [Aunai, N.; Dargent, J.; Smets, R.] Univ Paris 11, Univ Paris 06, Ecole Polytech, Lab Phys Plasmas,CNRS,Observ Paris, Orsay, France.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD USA.
[Lavraud, B.] Univ Toulouse 3, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
RP Aunai, N (reprint author), Univ Paris 11, Univ Paris 06, Ecole Polytech, Lab Phys Plasmas,CNRS,Observ Paris, Orsay, France.
EM nicolas.aunai@lpp.polytechnique.fr
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU ANR project MONANR [ANR-13-PDOC-0027]; [x2016047231]
FX The authors would like to thank the two anonymous reviewers for their
comments. The numerical simulations presented in this study have been
performed at IDRIS on supercomputer ADA in the project x2016047231. This
work is part of the ANR project MONANR: ANR-13-PDOC-0027.
NR 46
TC 0
Z9 0
U1 8
U2 8
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 AUG
PY 2016
VL 82
AR 535820401
DI 10.1017/S0022377816000647
PN 4
PG 15
WC Physics, Fluids & Plasmas
SC Physics
GA DT5IQ
UT WOS:000381516900001
ER
PT J
AU Kadler, M
Krauss, F
Mannheim, K
Ojha, R
Muller, C
Schulz, R
Anton, G
Baumgartner, W
Beuchert, T
Buson, S
Carpenter, B
Eberl, T
Edwards, PG
Glawion, DE
Elsasser, D
Gehrels, N
Grafe, C
Gulyaev, S
Hase, H
Horiuchi, S
James, CW
Kappes, A
Kappes, A
Katz, U
Kreikenbohm, A
Kreter, M
Kreykenbohm, I
Langejahn, M
Leiter, K
Litzinger, E
Longo, F
Lovell, JEJ
McEnery, J
Natusch, T
Phillips, C
Plotz, C
Quick, J
Ros, E
Stecker, FW
Steinbring, T
Stevens, J
Thompson, DJ
Trustedt, J
Tzioumis, AK
Weston, S
Wilms, J
Zensus, JA
AF Kadler, M.
Krauss, F.
Mannheim, K.
Ojha, R.
Mueller, C.
Schulz, R.
Anton, G.
Baumgartner, W.
Beuchert, T.
Buson, S.
Carpenter, B.
Eberl, T.
Edwards, P. G.
Glawion, D. Eisenacher
Elsaesser, D.
Gehrels, N.
Graefe, C.
Gulyaev, S.
Hase, H.
Horiuchi, S.
James, C. W.
Kappes, A.
Kappes, A.
Katz, U.
Kreikenbohm, A.
Kreter, M.
Kreykenbohm, I.
Langejahn, M.
Leiter, K.
Litzinger, E.
Longo, F.
Lovell, J. E. J.
McEnery, J.
Natusch, T.
Phillips, C.
Ploetz, C.
Quick, J.
Ros, E.
Stecker, F. W.
Steinbring, T.
Stevens, J.
Thompson, D. J.
Truestedt, J.
Tzioumis, A. K.
Weston, S.
Wilms, J.
Zensus, J. A.
TI Coincidence of a high-fluence blazar outburst with a PeV-energy neutrino
event
SO NATURE PHYSICS
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EMISSION; COUNTERPARTS;
1ES-1959+650; ORIGIN; JETS
AB The astrophysical sources of the extraterrestrial, very high-energy neutrinos detected by the IceCube collaboration remain to be identified. Gamma-ray (gamma-ray) blazars have been predicted to yield a cumulative neutrino signal exceeding the atmospheric background above energies of 100 TeV, assuming that both the neutrinos and the gamma-ray photons are produced by accelerated protons in relativistic jets. As the background spectrum falls steeply with increasing energy, the individual events with the clearest signature of being of extraterrestrial origin are those at petaelectronvolt energies. Inside the large positional-uncertainty fields of the first two petaelectronvolt neutrinos detected by IceCube, the integrated emission of the blazar population has a sufficiently high electromagnetic flux to explain the detected IceCube events, but fluences of individual objects are too low to make an unambiguous source association. Here, we report that a major outburst of the blazar PKS B1424-418 occurred in temporal and positional coincidence with a third petaelectronvolt-energy neutrino event (HESE-35) detected by IceCube. On the basis of an analysis of the full sample of gamma-ray blazars in the HESE-35 field, we show that the long-term average gamma-ray emission of blazars as a class is in agreement with both the measured all-sky flux of petaelectronvolt neutrinos and the spectral slope of the IceCube signal. The outburst of PKS B1424-418 provides an energy output high enough to explain the observed petaelectronvolt event, suggestive of a direct physical association.
C1 [Kadler, M.; Krauss, F.; Mannheim, K.; Mueller, C.; Schulz, R.; Beuchert, T.; Glawion, D. Eisenacher; Elsaesser, D.; Graefe, C.; Kappes, A.; Kreikenbohm, A.; Kreter, M.; Langejahn, M.; Leiter, K.; Litzinger, E.; Steinbring, T.; Truestedt, J.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Emil Fischer Str 31, D-97074 Wurzburg, Germany.
[Krauss, F.; Schulz, R.; Beuchert, T.; Kreikenbohm, A.; Kreykenbohm, I.; Langejahn, M.; Leiter, K.; Litzinger, E.; Steinbring, T.; Truestedt, J.; Wilms, J.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany.
[Ojha, R.; Baumgartner, W.; Gehrels, N.; McEnery, J.; Stecker, F. W.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ojha, R.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ojha, R.; Carpenter, B.] Catholic Univ Amer, Washington, DC 20064 USA.
[Mueller, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Anton, G.; Eberl, T.; James, C. W.; Kappes, A.; Katz, U.; Kreter, M.] Univ Erlangen Nurnberg, ECAP, Erwin Rommel Str 1, D-91058 Erlangen, Germany.
[Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Buson, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Edwards, P. G.; Phillips, C.; Stevens, J.; Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, POB 76, Epping, NSW 1710, Australia.
[Gulyaev, S.; Natusch, T.; Weston, S.] Auckland Univ Technol, Inst Radio Astron & Space Res, Auckland 1010, New Zealand.
[Hase, H.; Ploetz, C.] Bundesamt Kartog & Geodasie, D-93444 Bad Kotzting, Germany.
[Horiuchi, S.] CSIRO Astron & Space Sci, Canberra Deep Space Commun Complex, POB 1035, Tuggeranong, ACT 2901, Australia.
[Longo, F.] Univ Trieste, Dipartimento Fis, I-34128 Trieste, Italy.
[Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Private Bag 37, Hobart, Tas 7001, Australia.
[Quick, J.] Hartebeesthoek Radio Astron Observ, POB 443, ZA-1740 Krugersdorp, South Africa.
[Ros, E.; Zensus, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Ros, E.] Univ Valencia, Astron Observ, C Catedratico Jose Beltran 2, Valencia 46980, Spain.
[Ros, E.] Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, E-46100 Valencia, Spain.
[Stecker, F. W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Kadler, M (reprint author), Univ Wurzburg, Inst Theoret Phys & Astrophys, Emil Fischer Str 31, D-97074 Wurzburg, Germany.
EM matthias.kadler@astro.uni-wuerzburg.de
RI Wilms, Joern/C-8116-2013; Katz, Uli/E-1925-2013; Anton,
Gisela/C-4840-2013; James, Clancy/G-9178-2015;
OI Wilms, Joern/0000-0003-2065-5410; Katz, Uli/0000-0002-7063-4418; Anton,
Gisela/0000-0003-2039-4724; James, Clancy/0000-0002-6437-6176; Krauss,
Felicia/0000-0001-6191-1244; Kadler, Matthias/0000-0001-5606-6154
FU Deutsche Forschungsgemeinschaft [WI 1860-10/1, GRK 1147]; Deutsches
Zentrum fur Luft- und Raumfahrt grant [50 OR 1311/50 OR 1303/50 OR
1401]; German Ministry for Education and Research (BMBF) [05A11WEA,
05A14WE3]; Helmholtz Alliance for Astroparticle Physics (HAP); Spanish
MINECO [AYA2012-38491-C02-01]; Generalitat Valenciana
[PROMETEOII/2014/057]; COST MP0905 action 'Black Holes in a Violent
Universe'; NASA [NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N,
NNH13ZDA001N]; Commonwealth of Australia; National Collaborative
Research Infrastructure Strategy (NCRIS), an Australian Commonwealth
Government Programme
FX The authors thank B. Lott, L. Baldini, P. Bruel, S. Digel, J. Finke, D.
Gasparini, N. Omodei, J. S. Perkins and A. Reimer for discussions that
have significantly improved this publication. We acknowledge support and
partial funding by the Deutsche Forschungsgemeinschaft grant WI
1860-10/1 (TANAMI) and GRK 1147, Deutsches Zentrum fur Luft- und
Raumfahrt grant 50 OR 1311/50 OR 1303/50 OR 1401, the German Ministry
for Education and Research (BMBF) grants 05A11WEA and 05A14WE3, the
Helmholtz Alliance for Astroparticle Physics (HAP), the Spanish MINECO
project AYA2012-38491-C02-01, the Generalitat Valenciana project
PROMETEOII/2014/057, the COST MP0905 action 'Black Holes in a Violent
Universe' and NASA through Fermi Guest Investigator grants NNH09ZDA001N,
NNH10ZDA001N, NNH12ZDA001N and NNH13ZDA001N. This study made use of data
collected by the Australian Long Baseline Array (LBA) and the AuScope
initiative. The LBA 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. AuScope Ltd is funded under the
National Collaborative Research Infrastructure Strategy (NCRIS), an
Australian Commonwealth Government Programme. This paper made use of
data from the ALMA calibrator database:
https://almascience.eso.org/alma-data/calibrator-catalogue. ALMA is a
partnership of ESO (representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This paper
also made use of up-to-date SMARTS optical/near-infrared light curves
that are available at www.astro.yale.edu/smarts/glast/home.php. The
Fermi-LAT Collaboration acknowledges support for LAT development,
operation and data analysis from NASA and DOE (United States), CEA/Irfu
and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA
(Japan), and the K. A. Wallenberg Foundation, the Swedish Research
Council and the National Space Board (Sweden). Science analysis support
in the operations phase from INAF (Italy) and CNES (France) is also
gratefully acknowledged. We thank J. E. Davis and T. Johnson for the
development of the slxfig module and the SED scripts that have been used
to prepare the figures in this work.
NR 43
TC 8
Z9 8
U1 3
U2 4
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1745-2473
EI 1745-2481
J9 NAT PHYS
JI Nat. Phys.
PD AUG
PY 2016
VL 12
IS 8
BP 807
EP 814
DI 10.1038/NPHYS3715
PG 8
WC Physics, Multidisciplinary
SC Physics
GA DT1KA
UT WOS:000381239800024
ER
PT J
AU Carroll, M
Wooten, M
DiMiceli, C
Sohlberg, R
Kelly, M
AF Carroll, Mark
Wooten, Margaret
DiMiceli, Charlene
Sohlberg, Robert
Kelly, Maureen
TI Quantifying Surface Water Dynamics at 30 Meter Spatial Resolution in the
North American High Northern Latitudes 1991-2011
SO REMOTE SENSING
LA English
DT Article
DE remote sensing; inland water; land cover; Landsat; ABoVE
ID LAKES; DATABASE
AB The availability of a dense time series of satellite observations at moderate (30 m) spatial resolution is enabling unprecedented opportunities for understanding ecosystems around the world. A time series of data from Landsat was used to generate a series of three maps at decadal time step to show how surface water has changed from 1991 to 2011 in the high northern latitudes of North America. Previous attempts to characterize the change in surface water in this region have been limited in either spatial or temporal resolution, or both. This series of maps was generated for the NASA Arctic and Boreal Vulnerability Experiment (ABoVE), which began in fall 2015. These maps show a "nominal" extent of surface water by using multiple observations to make a single map for each time step. This increases the confidence that any detected changes are related to climate or ecosystem changes not simply caused by short duration weather events such as flood or drought. The methods and comparison to other contemporary maps of the region are presented here. Initial verification results indicate 96% producer accuracy and 54% user accuracy when compared to 2-m resolution WorldView-2 data. All water bodies that were omitted were one Landsat pixel or smaller, hence below detection limits of the instrument.
C1 [Carroll, Mark; Wooten, Margaret] NASA, GSFC Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Carroll, Mark; Wooten, Margaret] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[DiMiceli, Charlene; Sohlberg, Robert; Kelly, Maureen] Univ Maryland, College Pk, MD 20740 USA.
RP Carroll, M (reprint author), NASA, GSFC Biospher Sci Lab, Greenbelt, MD 20771 USA.; Carroll, M (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM mark.carroll@nasa.gov; margaret.wooten@nasa.gov; cdimicel@umd.edu;
sohlberg@umd.edu; mkelly17@umd.edu
OI Kelly, Maureen/0000-0001-5231-8465
FU NASA [NNX15AH06G]
FX The authors would like to thank the Carbon Cycle and Ecosystems office
(responsible for overseeing the ABoVE project coordination) for their
continuous support. We would like to thank Elizabeth Hoy who did the
figure layout for Figures 1 and 3. This work was funded as a pre-ABoVE
data product through the NASA Terrestrial Ecology program grant #
NNX15AH06G. Resources supporting this work were provided by the NASA
High-End Computing (HEC) Program through the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. Lastly the authors
would like to acknowledge the anonymous reviewers whose thoughtful
comments helped to improve this manuscript.
NR 22
TC 2
Z9 2
U1 12
U2 12
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 AUG
PY 2016
VL 8
IS 8
AR 622
DI 10.3390/rs8080622
PG 14
WC Remote Sensing
SC Remote Sensing
GA DU8JI
UT WOS:000382458700009
ER
EF