FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Law, NM
Fors, O
Ratzloff, J
Wulfken, P
Kavanaugh, D
Sitar, DJ
Pruett, Z
Birchard, MN
Barlow, BN
Cannon, K
Cenko, SB
Dunlap, B
Kraus, A
Maccarone, TJ
AF Law, Nicholas M.
Fors, Octavi
Ratzloff, Jeffrey
Wulfken, Philip
Kavanaugh, Dustin
Sitar, David J.
Pruett, Zachary
Birchard, Mariah N.
Barlow, Brad N.
Cannon, Kipp
Cenko, S. Bradley
Dunlap, Bart
Kraus, Adam
Maccarone, Thomas J.
TI Evryscope Science: Exploring the Potential of All-Sky Gigapixel-Scale
Telescopes
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID WHITE-DWARF STARS; LOW-MASS STARS; BLUE OBJECT SURVEY; SUPERNOVA SN
2011FE; FAST RADIO-BURSTS; GAMMA-RAY-BURSTS; 1ST DATA RELEASE;
EXTRASOLAR-PLANET; X-RAY; ECLIPSING BINARIES
AB Low-cost mass-produced sensors and optics have recently made it feasible to build telescope arrays which observe the entire accessible sky simultaneously. In this article, we discuss the scientific motivation for these telescopes, including exoplanets, stellar variability, and extragalactic transients. To provide a concrete example we detail the goals and expectations for the Evryscope, an under-construction 780MPix telescope which covers 8660 sq. deg. in each 2-minute exposure; each night, 18,400 sq. deg. will be continuously observed for an average of approximate to 6hr. Despite its small 61mm aperture, the system's large field of view provides an etendue which is approximate to 10% of LSST. The Evryscope, which places 27 separate individual telescopes into a common mount which tracks the entire accessible sky with only one moving part, will return 1%-precision, many-year-length, high-cadence light curves for every accessible star brighter than approximate to 16th magnitude. The camera readout times are short enough to provide near-continuous observing, with a 97% survey time efficiency. The array telescope will be capable of detecting transiting exoplanets around every solar-type star brighter than m(V)=12, providing at least few-millimagnitude photometric precision in long-term light curves. It will be capable of searching for transiting giant planets around the brightest and most nearby stars, where the planets are much easier to characterize; it will also search for small planets nearby M-dwarfs, for planetary occultations of white dwarfs, and will perform comprehensive nearby microlensing and eclipse-timing searches for exoplanets inaccessible to other planet-finding methods. The Evryscope will also provide comprehensive monitoring of outbursting young stars, white dwarf activity, and stellar activity of all types, along with finding a large sample of very-long-period M-dwarf eclipsing binaries. When relatively rare transients events occur, such as gamma-ray bursts (GRBs), nearby supernovae, or even gravitational wave detections from the Advanced LIGO/Virgo network, the array will return minute-by-minute light curves without needing pointing toward the event as it occurs. By coadding images, the system will reach V approximate to 19 in 1-hr integrations, enabling the monitoring of faint objects. Finally, by recording all data, the Evryscope will be able to provide pre-event imaging at 2-minute cadence for bright transients and variable objects, enabling the first high-cadence searches for optical variability before, during and after all-sky events.
C1 [Law, Nicholas M.; Fors, Octavi; Ratzloff, Jeffrey; Wulfken, Philip; Kavanaugh, Dustin; Dunlap, Bart] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Sitar, David J.; Pruett, Zachary; Birchard, Mariah N.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
[Barlow, Brad N.] High Point Univ, Dept Phys, High Point, NC 27268 USA.
[Cannon, Kipp] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kraus, Adam] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
RP Law, NM (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
OI Fors Aldrich, Octavi/0000-0002-4227-9308
FU NSF [AST-1407589]
FX We thank the referee, Benjamin Shappee, for comments which significantly
improved the paper. We also thank Raymond Carlberg, Rick Murowinski and
Suresh Sivanandam for interesting discussions during the conceptual
design of the Arctic Evryscope. This research was supported by the NSF
grant AST-1407589.
NR 141
TC 12
Z9 12
U1 1
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD MAR
PY 2015
VL 127
IS 949
BP 234
EP 249
DI 10.1086/680521
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE4BC
UT WOS:000351774600003
ER
PT J
AU Cowan, NB
Greene, T
Angerhausen, D
Batalha, NE
Clampin, M
Colon, K
Crossfield, IJM
Fortney, JJ
Gaudi, BS
Harrington, J
Iro, N
Lillie, CF
Linsky, JL
Lopez-Morales, M
Mandell, AM
Stevenson, KB
AF Cowan, N. B.
Greene, T.
Angerhausen, D.
Batalha, N. E.
Clampin, M.
Colon, K.
Crossfield, I. J. M.
Fortney, J. J.
Gaudi, B. S.
Harrington, J.
Iro, N.
Lillie, C. F.
Linsky, J. L.
Lopez-Morales, M.
Mandell, A. M.
Stevenson, K. B.
CA ExoPAG SAG-10
TI Characterizing Transiting Planet Atmospheres through 2025
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID SUPER-EARTH EXOPLANET; INFRARED TRANSMISSION SPECTROSCOPY; SYSTEMATIC
RETRIEVAL ANALYSIS; HUBBLE-SPACE-TELESCOPE; HD 189733B; EXTRASOLAR
PLANET; SECONDARY-ECLIPSE; GJ 1214B; MU-M; HOT JUPITERS
AB The discovery of planets around other stars is revolutionizing our notions of planet formation and is poised to do the same for planetary climate. Studying transiting planets is complementary to eventual studies of directly imaged planets: (1)we can readily measure the mass and radius of transiting planets, linking atmospheric properties to bulk composition and formation, (2)many transiting planets are strongly irradiated and exhibit novel atmospheric physics, and (3)the most common temperate terrestrial planets orbit close to red dwarf stars and are difficult to image directly. We have only been able to comprehensively characterize the atmospheres of a handful of transiting planets, because most orbit faint stars. The Transiting Exoplanet Survey Satellite (TESS) will discover transiting planets orbiting the brightest stars, enabling, in principle, an atmospheric survey of 10(2)-10(3) bright hot Jupiters and warm sub-Neptunes. Uniform observations of such a statistically significant sample would provide leverage to understandand learn fromthe diversity of short-period planets, and would identify the minority of truly special planets worthy of more intensive follow-up. We argue that the best way to maximize the scientific returns of TESS is to adopt a triage approach. A space mission consisting of a approximate to 1m telescope with an optical-NIR spectrograph could measure molecular absorption for nonterrestrial planets discovered by TESS, as well as eclipses and phase variations for the hottest jovians. Such a mission could observe up to 10(3) transits per year, thus enabling it to survey a large fraction of the bright (J<11) hot-Jupiters and warm sub-Neptunes TESS is expected to find. The James Webb Space Telescope (JWST) could be used to perform detailed atmospheric characterization of the most interesting transiting targets (transit, eclipse, andwhen possiblephase-resolved spectroscopy). TESS is also expected to discover a few temperate terrestrial planets transiting nearby M-Dwarfs. Characterizing these worlds will be time-intensive: JWST will need months to provide tantalizing constraints on the presence of an atmosphere, planetary rotational state, clouds, and greenhouse gases. Future flagship missions should be designed to provide better constraints on the habitability of M-Dwarf temperate terrestrial planets.
C1 [Cowan, N. B.] Amherst Coll, Amherst, MA 01002 USA.
[Greene, T.; Mandell, A. M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Angerhausen, D.; Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Batalha, N. E.] Penn State Univ, State Coll, PA 16801 USA.
[Colon, K.] Lehigh Univ, Bethlehem, PA 18015 USA.
[Crossfield, I. J. M.] Univ Arizona, Tucson, AZ 85721 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Gaudi, B. S.] Ohio State Univ, Columbus, OH 43210 USA.
[Harrington, J.] Univ Cent Florida, Orlando, FL 32816 USA.
[Iro, N.] Univ Hamburg, Hamburg, Germany.
[Lillie, C. F.] Lillie Consulting, Houston, TX 77008 USA.
[Linsky, J. L.] Univ Colorado, Boulder, CO 80309 USA.
[Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stevenson, K. B.] Univ Chicago, Chicago, IL 60637 USA.
RP Cowan, NB (reprint author), Amherst Coll, Amherst, MA 01002 USA.
EM ncowan@amherst.edu
RI Harrington, Joseph/E-6250-2011;
OI Harrington, Joseph/0000-0002-8955-8531
NR 136
TC 17
Z9 17
U1 1
U2 16
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD MAR
PY 2015
VL 127
IS 949
BP 311
EP 327
DI 10.1086/680855
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CE4BC
UT WOS:000351774600008
ER
PT J
AU Kourdis, PD
Bellan, J
AF Kourdis, Panayotis D.
Bellan, Josette
TI High-pressure reduced-kinetics mechanism for n-hexadecane autoignition
and oxidation at constant pressure
SO COMBUSTION AND FLAME
LA English
DT Article
DE Reduced kinetics for n-hexadecane; High-pressure reduced kinetics;
Self-similarity
ID SELF-SIMILAR BEHAVIOR; CHEMISTRY TABULATION; PREMIXED FLAMES;
IMPLEMENTATION; HYDROCARBONS; SIMULATIONS; SIMILARITY; COMBUSTION;
REDUCTION; STATE
AB In previous work, a local full self similarity (LFS2) was identified between (properly) normalized thermo-kinetic quantities when plotted against a normalized temperature. The local partial self similarity (LPS2), which is the computationally efficient companion of LFS2, was coupled with a simple tabulation scheme and yielded highly-accurate twenty-light-species reduced mechanisms for constant-mass and constant-volume autoignition and oxidation of n-heptane, n-decane, n-dodecane and iso-octane. The LFS2 and LPS2 reduction framework coupled with tabulation were combined into a method here called Local Self Similarity Tabulation (LS2T). The LS2T method is here extended and validated for constructing reduced kinetics mechanisms for the constant-mass autoignition and oxidation of an even heavier hydrocarbon, n-hexadecane, but now at constant pressure conditions for a wide range of initial conditions. The method employs the same twenty light species as species progress variables as in the lighter alkanes previously studied, and tabulates through the LPS2 all information involving any heavy species. The template mechanism used for reduction is the detailed 2115-species kinetics from the Lawrence Livermore National Laboratory. Results are presented for the n-hexadecane autoignition and oxidation at the high pressures encountered during engine operation and for several initial temperatures and equivalence ratios. We show that the utilization of a real-gas equation of state (the Peng-Robinson equation of state with a volume correction) is essential in obtaining accurate results. Reduced-kinetics plots of the temperature and the major species, including the OH temporal evolution, computed with the LS2T method accurately duplicated those obtained with the LLNL detailed mechanism. (C) 2014 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Kourdis, Panayotis D.; Bellan, Josette] CALTECH, Pasadena, CA 91125 USA.
[Bellan, Josette] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Josette.Bellan@jpl.nasa.gov
FU United States Army Research Office
FX This study was conducted at the California Institute of Technology and
the Jet Propulsion Laboratory (JPL) Division of the California Institute
of Technology, and was sponsored by the United States Army Research
Office, with Dr. Ralph Anthenien as Program Manager. Interesting
discussions with, as well as suggestions and information from Dr.
Kenneth G. Harstad are gratefully acknowledged. Computations were
performed using the Army Research Office and the JPL/NASA Supercomputing
facilities.
NR 21
TC 2
Z9 2
U1 4
U2 18
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 MAR
PY 2015
VL 162
IS 3
BP 571
EP 579
DI 10.1016/j.combustflame.2014.09.008
PG 9
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CD7DG
UT WOS:000351250400005
ER
PT J
AU Ma, XG
Fox, P
Narock, T
Wilson, B
AF Ma, Xiaogang
Fox, Peter
Narock, Thomas
Wilson, Brian
TI Semantic e-Science
SO EARTH SCIENCE INFORMATICS
LA English
DT Editorial Material
C1 [Ma, Xiaogang; Fox, Peter] Rensselaer Polytech Inst, Tetherless World Constellat, Troy, NY 12180 USA.
[Narock, Thomas] Marymount Univ, Dept Informat Technol & Management Sci, Arlington, VA 22201 USA.
[Wilson, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ma, XG (reprint author), Rensselaer Polytech Inst, Tetherless World Constellat, 110 8th St, Troy, NY 12180 USA.
EM max7@rpi.edu; pfox@cs.rpi.edu; tnarock@marymount.edu;
bdwilson@jpl.nasa.gov
OI Ma, Xiaogang/0000-0002-9110-7369
NR 4
TC 1
Z9 1
U1 0
U2 10
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
EI 1865-0481
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD MAR
PY 2015
VL 8
IS 1
SI SI
BP 1
EP 3
DI 10.1007/s12145-015-0212-8
PG 3
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA CD9UN
UT WOS:000351444100001
ER
PT J
AU Jones, F
Holzer, TH
Eveleigh, T
Sarkani, S
AF Jones, Felicia
Holzer, Thomas H.
Eveleigh, Timothy
Sarkani, Shahryar
TI Managing Technical Performance Margins to Control Earth and Space
Science Instrument Costs
SO EMJ-ENGINEERING MANAGEMENT JOURNAL
LA English
DT Article
DE Design Margin; Aerospace Instruments; Regression Analysis; Cost
Estimation
AB Design margins are additional resources carried in technical performance parameters to account for uncertainties in designs. Margins are traditionally derived and allocated based upon historical experience as opposed to quantitative methods, jeopardizing the development of low-cost, space-based instruments. This article examines 62 instruments, assessing the interrelationships between pre-launch and actual launch margins, and utilizes multiple linear regression to examine margins and actual launch costs. Findings confirm use of margins above suggested industry standards in implementing space-based instruments, impacting affordability Results provide a methodology to detect deficiencies or excesses in performance parameters, which can be used in making trade-offs to reduce cost growth.
C1 [Jones, Felicia; Holzer, Thomas H.; Eveleigh, Timothy; Sarkani, Shahryar] George Washington Univ, Dept Engn Management & Syst Engn, Washington, DC USA.
RP Jones, F (reprint author), NASA, Goddard Space Flight Ctr, Appl Engn & Technol Directorate, Mail Code 500,Bldg 11,Room 200L, Greenbelt, MD 20771 USA.
EM felicia.selden@nasa.gov
NR 38
TC 0
Z9 0
U1 2
U2 5
PU AMER SOC ENGINEERING MANAGEMENT
PI ROLLA
PA PO BOX 820, ROLLA, MO 65402 USA
SN 1042-9247
J9 EMJ-ENG MANAG J
JI EMJ-Eng. Manag. J.
PD MAR
PY 2015
VL 27
IS 1
BP 23
EP 31
PG 9
WC Engineering, Industrial; Management
SC Engineering; Business & Economics
GA CD8GH
UT WOS:000351332700003
ER
PT J
AU Schneider, A
Mertes, CM
Tatem, AJ
Tan, B
Sulla-Menashe, D
Graves, SJ
Patel, NN
Horton, JA
Gaughan, AE
Rollo, JT
Schelly, IH
Stevens, FR
Dastur, A
AF Schneider, A.
Mertes, C. M.
Tatem, A. J.
Tan, B.
Sulla-Menashe, D.
Graves, S. J.
Patel, N. N.
Horton, J. A.
Gaughan, A. E.
Rollo, J. T.
Schelly, I. H.
Stevens, F. R.
Dastur, A.
TI A new urban landscape in East-Southeast Asia, 2000-2010
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE urbanization; urban sprawl; land cover change; remote sensing; change
detection; urban density; population density
ID LAND-USE CHANGE; CLIMATE-CHANGE; MEGA CITIES; MODIS DATA; URBANIZATION;
GROWTH; METRICS; PATTERNS; CHINA; EXPANSION
AB East-Southeast Asia is currently one of the fastest urbanizing regions in the world, with countries such as China climbing from 20 to 50% urbanized in just a few decades. By 2050, these countries are projected to add 1 billion people, with 90% of that growth occurring in cities. This population shift parallels an equally astounding amount of built-up land expansion. However, spatially-and temporally-detailed information on regional-scale changes in urban land or population distribution do not exist; previous efforts have been either sample-based, focused on one country, or drawn conclusions from datasets with substantial temporal/spatial mismatch and variability in urban definitions. Using consistent methodology, satellite imagery and census data for >1000 agglomerations in the East-Southeast Asian region, we show that urban land increased >22% between 2000 and 2010 (from 155 000 to 189 000 km(2)), an amount equivalent to the area of Taiwan, while urban populations climbed >31% (from 738 to 969 million). Although urban land expanded at unprecedented rates, urban populations grew more rapidly, resulting in increasing densities for the majority of urban agglomerations, including those in both more developed (Japan, South Korea) and industrializing nations (China, Vietnam, Indonesia). This result contrasts previous sample-based studies, which conclude that cities are universally declining in density. The patterns and rates of change uncovered by these datasets provide a unique record of the massive urban transition currently underway in East-Southeast Asia that is impacting local-regional climate, pollution levels, water quality/availability, arable land, as well as the livelihoods and vulnerability of populations in the region.
C1 [Schneider, A.; Mertes, C. M.; Horton, J. A.; Rollo, J. T.; Schelly, I. H.] Univ Wisconsin, Nelson Inst Environm Studies, Ctr Sustainabil & Global Environm, Madison, WI 53706 USA.
[Schneider, A.; Mertes, C. M.; Horton, J. A.; Rollo, J. T.; Schelly, I. H.] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA.
[Tatem, A. J.] Univ Southampton, Dept Geog & Environm, Southampton SO9 5NH, Hants, England.
[Tatem, A. J.] Fogarty Int Ctr, NIH, Bethesda, MD USA.
[Tan, B.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Lanham, MD USA.
[Sulla-Menashe, D.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Graves, S. J.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA.
[Patel, N. N.] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA 22030 USA.
[Gaughan, A. E.; Stevens, F. R.] Univ Louisville, Dept Geog & Geosci, Louisville, KY 40292 USA.
[Dastur, A.] World Bank, Washington, DC 20433 USA.
RP Schneider, A (reprint author), Univ Wisconsin, Nelson Inst Environm Studies, Ctr Sustainabil & Global Environm, Madison, WI 53706 USA.
EM aschneider4@wisc.edu
FU World Bank; RAPIDD program of the Science and Technology Directorate,
Department of Homeland Security; Fogarty International Center, National
Institutes of Health; Bill and Melinda Gates Foundation [49446, 1032350]
FX AS acknowledges funding support from the World Bank for preparation of
datasets. AJT acknowledges funding support from the RAPIDD program of
the Science and Technology Directorate, Department of Homeland Security,
and the Fogarty International Center, National Institutes of Health, and
is also supported by grants from the Bill and Melinda Gates Foundation
(#49446, #1032350). The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript. The authors also wish to thank Caitlin Kontgis, Mutlu
Ozdogan, and four anonymous reviewers for their helpful comments on an
earlier draft of this manuscript.
NR 44
TC 12
Z9 12
U1 15
U2 61
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 MAR
PY 2015
VL 10
IS 3
AR 034002
DI 10.1088/1748-9326/10/3/034002
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CD9KB
UT WOS:000351416100004
ER
PT J
AU Stolarski, RS
Douglass, AR
Oman, LD
Waugh, DW
AF Stolarski, Richard S.
Douglass, Anne R.
Oman, Luke D.
Waugh, Darryn W.
TI Impact of future nitrous oxide and carbon dioxide emissions on the
stratospheric ozone layer
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE ozone layer; nitrous oxide; carbon dioxide
ID CLIMATE-CHANGE; DEPLETION; PERTURBATIONS; GASES; MODEL
AB The atmospheric levels of human-produced chlorocarbons and bromocarbons are projected to make only small contributions to ozone depletion by 2100. Increases in carbon dioxide (CO2) and nitrous oxide (N2O) will become increasingly important in determining the future of the ozone layer. N2O increases lead to increased production of nitrogen oxides (NOx), contributing to ozone depletion. CO2 increases cool the stratosphere and affect ozone levels in several ways. Cooling decreases the rate of many photochemical reactions, thus slowing ozone loss rates. Cooling also increases the chemical destruction of nitrogen oxides, thereby moderating the effect of increased N2O on ozone depletion. The stratospheric ozone level projected for the end of this century therefore depends on future emissions of both CO2 and N2O. We use a two-dimensional chemical transport model to explore a wide range of values for the boundary conditions for CO2 and N2O, and find that all of the current scenarios for growth of greenhouse gases project the global average ozone to be larger in 2100 than in 1960.
C1 [Stolarski, Richard S.; Waugh, Darryn W.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Douglass, Anne R.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Stolarski, RS (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA.
EM rstolar1@jhu.edu
RI Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013; Oman,
Luke/C-2778-2009; Waugh, Darryn/K-3688-2016
OI Stolarski, Richard/0000-0001-8722-4012; Oman, Luke/0000-0002-5487-2598;
Waugh, Darryn/0000-0001-7692-2798
NR 33
TC 2
Z9 2
U1 6
U2 58
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 MAR
PY 2015
VL 10
IS 3
AR 034011
DI 10.1088/1748-9326/10/3/034011
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CD9KB
UT WOS:000351416100013
ER
PT J
AU Sites, JV
Lee, C
Lin, R
Chattopadhyay, G
Reck, T
Jung-Kubiak, C
Mehdi, I
Cooper, KB
AF Sites, Jose V.
Lee, Choonsup
Lin, Robert
Chattopadhyay, Goutam
Reck, Theodore
Jung-Kubiak, Cecile
Mehdi, Imran
Cooper, Ken B.
TI A High-Power 105-120 GHz Broadband On-Chip Power-Combined Frequency
Tripler
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Frequency multipliers; local oscillator; millimeter-wave sources;
power-combining; Schottky diode; varactor
AB We report on the design, fabrication and characterization of a high-power and broadband 105-120 GHz Schottky diode frequency tripler based on a novel on-chip power combining concept that allows superior power handling than traditional approaches. The chip features twelve anodes on a 50 mu m thick GaAs substrate. At room temperature, the tripler exhibits a 17% 3 dB bandwidth and a similar to 30% peak conversion efficiency for a nominal input power of around 350-400 mW, and similar to 20% efficiency for its maximum operational input power of 800-900 mW. This tripler can deliver maximum power levels very close to 200 mW. The on-chip power-combined frequency tripler is compared with a traditional tripler designed for the same band using the same design parameters.
C1 [Sites, Jose V.; Lee, Choonsup; Lin, Robert; Chattopadhyay, Goutam; Reck, Theodore; Jung-Kubiak, Cecile; Mehdi, Imran; Cooper, Ken B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sites, JV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jose.v.siles@jpl.nasa.gov
FU Department of Homeland Security; Jet Propulsion Laboratory, California
Institute of Technology, under National Aeronautics and Space
Administration
FX This work was supported by the Department of Homeland Security and by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
NR 12
TC 5
Z9 5
U1 0
U2 8
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 MAR
PY 2015
VL 25
IS 3
BP 157
EP 159
DI 10.1109/LMWC.2015.2390539
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA CE0AG
UT WOS:000351463200005
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Code Inflation
SO IEEE SOFTWARE
LA English
DT Editorial Material
C1 [Holzmann, Gerard J.] NASA JPL, La Canada Flintridge, CA USA.
RP Holzmann, GJ (reprint author), Jet Prop Lab, La Canada Flintridge, CA 91011 USA.
EM gholzmann@acm.org
NR 0
TC 0
Z9 0
U1 2
U2 2
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 MAR-APR
PY 2015
VL 32
IS 2
BP 10
EP 13
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA CD9WJ
UT WOS:000351450600003
ER
PT J
AU Decrossas, E
Glover, MD
Porter, K
Cannon, T
Stegeman, T
Allen-McCormack, N
Hamilton, MC
Mantooth, HA
AF Decrossas, Emmanuel
Glover, Michael D.
Porter, Kaoru
Cannon, Tom
Stegeman, Thomas
Allen-McCormack, Nicholas
Hamilton, Michael C.
Mantooth, H. Alan
TI High-Performance and High-Data-Rate Quasi-Coaxial LTCC Vertical
Interconnect Transitions for Multichip Modules and System-on-Package
Applications
SO IEEE TRANSACTIONS ON COMPONENTS PACKAGING AND MANUFACTURING TECHNOLOGY
LA English
DT Article
DE Full tape thickness feature; low-temperature cofired ceramic (LTCC)
interconnect; multichip module (MCM); quasi-coaxial vertical transition;
signal integrity; system on package
AB A new design of stripline transition structures and flip-chip interconnects for high-speed digital communication systems implemented in low-temperature cofired ceramic (LTCC) substrates is presented. Simplified fabrication, suitability for LTCC machining, suitability for integration with other components, and connection to integrated stripline or microstrip interconnects for LTCC multichip modules and system on package make this approach well suited for miniaturized, advanced broadband, and highly integrated multichip ceramic modules. The transition provides excellent signal integrity at high-speed digital data rates up to 28 Gbits/s. Full-wave simulations and experimental results demonstrate a cost-effective solution for a wide frequency range from dc to 30 GHz and beyond. Signal integrity and high-speed digital data rate performances are verified through eye diagram and time-domain reflectometry and time-domain transmissometry measurements over a 10-cm long stripline.
C1 [Decrossas, Emmanuel; Glover, Michael D.; Porter, Kaoru; Cannon, Tom] Univ Arkansas, High Dens Elect Ctr, Fayetteville, AR 72701 USA.
[Stegeman, Thomas; Allen-McCormack, Nicholas; Hamilton, Michael C.] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA.
[Mantooth, H. Alan] Univ Arkansas, Dept Elect Engn, Fayetteville, AR 72701 USA.
RP Decrossas, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM edecrossas@ieee.org; mglover@uark.edu; kmaner@uark.edu;
tcannon@uark.edu; thomas.p.stegeman@gmail.com;
nza0019@tigermail.auburn.edu; mchamilton@auburn.edu; mantooth@uark.edu
FU Auburn University, Auburn, AL, USA
FX This work was supported by Auburn University, Auburn, AL, USA.
Recommended for publication by Associate Editor T. J. Schoepf upon
evaluation of reviewers' comments.
NR 10
TC 3
Z9 3
U1 3
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-3950
EI 2156-3985
J9 IEEE T COMP PACK MAN
JI IEEE Trans. Compon. Pack. Manuf. Technol.
PD MAR
PY 2015
VL 5
IS 3
BP 307
EP 313
DI 10.1109/TCPMT.2015.2394234
PG 7
WC Engineering, Manufacturing; Engineering, Electrical & Electronic;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA CD9WU
UT WOS:000351451800003
ER
PT J
AU Reck, T
Jung-Kubiak, C
Siles, JV
Lee, C
Lin, R
Chattopadhyay, G
Mehdi, I
Cooper, K
AF Reck, Theodore
Jung-Kubiak, Cecile
Siles, Jose V.
Lee, Choonsup
Lin, Robert
Chattopadhyay, Goutam
Mehdi, Imran
Cooper, Ken
TI A Silicon Micromachined Eight-Pixel Transceiver Array for
Submillimeter-Wave Radar
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Silicon micromachining; terahertz (THz) imaging radar; transceiver array
ID IMAGING RADAR
AB An eight-pixel transceiver array for operation in a 340 GHz imaging radar is presented. Silicon micromachining is applied to fabricate the submillimeter-wave front-end components to increase the density and uniformity of the array while lowering the cost compared to metal machining. Performance comparable with discrete metal machined housings was achieved with the 340 GHz transmitter nominally producing 0.5 mW and the mixers having a DSB noise temperature of 2000 K with a conversion loss of 8 dB. Radar performance is primarily limited by the isolation of the hybrid coupler, which is typically 28 dB, but excellent imaging performance is still achieved and improvements in penetration compared to higher frequency imaging radars is demonstrated.
C1 [Reck, Theodore; Jung-Kubiak, Cecile; Siles, Jose V.; Lee, Choonsup; Lin, Robert; Chattopadhyay, Goutam; Mehdi, Imran; Cooper, Ken] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Reck, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Theodore.reck@jpl.nasa.gov
FU Department of Homeland Security Science and Technology Directorate;
National Aeronautics and Space Administration
FX Manuscript received September 12, 2014; revised January 14, 2015;
accepted January 19, 2015. Date of publication February 06, 2015; date
of current version March 05, 2015. This work was supported by the
Department of Homeland Security Science and Technology Directorate. This
work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, California, USA, under contract with
National Aeronautics and Space Administration.
NR 22
TC 6
Z9 6
U1 1
U2 8
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 MAR
PY 2015
VL 5
IS 2
BP 197
EP 206
DI 10.1109/TTHZ.2015.2397274
PG 10
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA CD4UO
UT WOS:000351080300006
ER
PT J
AU Didlake, AC
Heymsfield, GM
Tian, L
Guimond, SR
AF Didlake, Anthony C., Jr.
Heymsfield, Gerald M.
Tian, Lin
Guimond, Stephen R.
TI The Coplane Analysis Technique for Three-Dimensional Wind Retrieval
Using the HIWRAP Airborne Doppler Radar
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PRECIPITATION; CONVECTION; HURRICANES; MESOSCALE; GENESIS; FIELDS
AB The coplane analysis technique for mapping the three-dimensional wind field of precipitating systems is applied to the NASA High-Altitude Wind and Rain Airborne Profiler (HIWRAP). HIWRAP is a dual-frequency Doppler radar system with two downward-pointing and conically scanning beams. The coplane technique interpolates radar measurements onto a natural coordinate frame, directly solves for two wind components, and integrates the mass continuity equation to retrieve the unobserved third wind component. This technique is tested using a model simulation of a hurricane and compared with a global optimization retrieval. The coplane method produced lower errors for the cross-track and vertical wind components, while the global optimization method produced lower errors for the along-track wind component. Cross-track and vertical wind errors were dependent upon the accuracy of the estimated boundary condition winds near the surface and at nadir, which were derived by making certain assumptions about the vertical velocity field. The coplane technique was then applied successfully to HIWRAP observations of Hurricane Ingrid (2013). Unlike the global optimization method, the coplane analysis allows for a transparent connection between the radar observations and specific analysis results. With this ability, small-scale features can be analyzed more adequately and erroneous radar measurements can be identified more easily.
C1 [Didlake, Anthony C., Jr.; Heymsfield, Gerald M.; Tian, Lin; Guimond, Stephen R.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Didlake, Anthony C., Jr.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Tian, Lin] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA.
[Guimond, Stephen R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Didlake, AC (reprint author), NASA, GSFC, Mail Code 612, Greenbelt, MD 20771 USA.
EM anthony.didlake@nasa.gov
FU NASA
FX We thank Matthew McLinden, Lihua Li, Martin Perrine, Jaime Cervantes,
and Ed Zenker for their engineering support and data processing for the
HIWRAP radar. We thank Shuyi Chen for providing the model output used in
this study. We also thank the three anonymous reviewers of this
manuscript. The first author conducted this research at the NASA Goddard
Space Flight Center under the support of the NASA Postdoctoral Program
conducted by the Oak Ridge Associated Universities.
NR 35
TC 6
Z9 6
U1 1
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 MAR
PY 2015
VL 54
IS 3
BP 605
EP 623
DI 10.1175/JAMC-D-14-0203.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD6UV
UT WOS:000351226200006
ER
PT J
AU Wolff, DB
Marks, DA
Petersen, WA
AF Wolff, David B.
Marks, David A.
Petersen, Walter A.
TI General Application of the Relative Calibration Adjustment (RCA)
Technique for Monitoring and Correcting Radar Reflectivity Calibration
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID PROPAGATION
AB Accurate calibration of radar reflectivity is integral to quantitative radar measurements of precipitation and a myriad of other radar-based applications. A statistical method was developed that utilizes the probability distribution of clutter area reflectivity near a stationary, ground-based radar to provide near-real-time estimates of the relative calibration of reflectivity data. The relative calibration adjustment (RCA) method provides a valuable, automated near-real-time tool for maintaining consistently calibrated radar data with relative calibration uncertainty of +0.5 dB or better. The original application was to S-band data in a tropical oceanic location, where the stability of the method was thought to be related to the relatively mild ground clutter and limited anomalous propagation (AP). This study demonstrates, however, that the RCA technique is transferable to other S-band radars at locations with more intense ground clutter and AP. This is done using data from NASA's polarimetric (NPOL) surveillance radar data during the Iowa Flood Studies (IFloodS) Global Precipitation Measurement (GPM) field campaign during spring of 2013 and other deployments. Results indicate the RCA technique is well capable of monitoring the reflectivity calibration of NPOL, given proper generation of an areal clutter map. The main goal of this study is to generalize the RCA methodology for possible extension to other ground-based S-band surveillance radars and to show how it can be used both to monitor the reflectivity calibration and to correct previous data once an absolute calibration baseline is established.
C1 [Wolff, David B.; Marks, David A.; Petersen, Walter A.] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Marks, David A.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Wolff, DB (reprint author), NASA, Wallops Flight Facil, Code 610-W,Bldg N-159,Room E214, Wallops Isl, VA 23337 USA.
EM david.b.wolff@nasa.gov
RI Measurement, Global/C-4698-2015
NR 13
TC 1
Z9 1
U1 0
U2 4
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 MAR
PY 2015
VL 32
IS 3
BP 496
EP 506
DI 10.1175/JTECH-D-13-00185.1
PG 11
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CD6WI
UT WOS:000351230500007
ER
PT J
AU Piecuch, CG
Fukumori, I
Ponte, RM
Wang, O
AF Piecuch, Christopher G.
Fukumori, Ichiro
Ponte, Rui M.
Wang, Ou
TI Vertical Structure of Ocean Pressure Variations with Application to
Satellite-Gravimetric Observations
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID CURRENT TRANSPORT VARIABILITY; SEA-LEVEL VARIABILITY; BOTTOM PRESSURE;
GENERAL-CIRCULATION; NORTH PACIFIC; GLOBAL OCEAN; MODEL; ICE; GRAVITY;
GRACE
AB The nature of ocean bottom pressure (p(b)) variability is considered on large spatial scales and long temporal scales. Monthly gridded estimates from the Gravity Recovery and Climate Experiment (GRACE) Release-05 and the new version 4 bidecadal ocean state estimate of the Consortium for Estimating the Circulation and Climate of the Ocean (ECCO) are used. Estimates of p(b) from GRACE and ECCO are generally in good agreement, providing an independent measure of the quality of both products. Diagnostic fields from the state estimate are used to compute barotropic (depth independent) and baroclinic (depth dependent) p(b) components. The relative roles of baroclinic and barotropic processes are found to vary with latitude and time scale: variations in p(b) at higher latitudes and shorter periods are affected by barotropic processes, whereas p(b) fluctuations at lower latitudes and longer periods can be influenced by baroclinic effects, broadly consistent with theoretical scaling arguments. Wind-driven Rossby waves and coupling of baroclinic and barotropic modes due to flow-topography interactions appear to be important influences on the baroclinic p(b) variability. Decadal simulations of monthly p(b) variability based on purely barotropic frameworks are expected to be in error by about 30% on average (greater than or similar to 40% in the tropical ocean and less than or similar to 20% at higher latitudes). Results have implications for applying GRACE observations to problems such as estimating transports of the Antarctic Circumpolar Current.
C1 [Piecuch, Christopher G.; Ponte, Rui M.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Fukumori, Ichiro; Wang, Ou] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Piecuch, CG (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA.
EM cpiecuch@aer.com
FU NASA GRACE [NNX12AJ93G]; National Science Foundation [OCE-0961507]; NASA
MEaSUREs Program
FX 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 (NASA), and was further supported
by NASA GRACE Grant NNX12AJ93G and Grant OCE-0961507 from the National
Science Foundation. The GRACE ocean data were processed by Don P.
Chambers, supported by the NASA MEaSUREs Program, and are available
online (at http://grace.jpl.nasa.gov). A listing of available ECCO
products can be found on the group website (http://www.ecco-group.org).
The comments from two anonymous reviewers were appreciated.
NR 59
TC 4
Z9 4
U1 2
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 MAR
PY 2015
VL 32
IS 3
BP 603
EP 613
DI 10.1175/JTECH-D-14-00156.1
PG 11
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CD6WI
UT WOS:000351230500015
ER
PT J
AU Langseth, BJ
Cottrill, A
AF Langseth, Brian J.
Cottrill, Adam
TI Influence of fishing practices on lake trout bycatch in the Canadian
lake-whitefish commercial fishery in Lake Huron
SO JOURNAL OF GREAT LAKES RESEARCH
LA English
DT Article
DE Bycatch; Lake trout rehabilitation; Catch standardization; Great Lakes
ID MIXED-EFFECTS MODELS; GREAT-LAKES; SALVELINUS-NAMAYCUSH; CATCH;
ABUNDANCE; STANDARDIZATION; INDEXES; SELECTION; MICHIGAN; SUPERIOR
AB Rehabilitation of lake trout (Salvelinus namaycush) populations is a priority for fisheries management in the upper Laurentian Great Lakes. In Lake Huron, lake trout are frequently caught as bycatch in the commercial fishery for lake whitefish (Coregonus clupeaformis). Given the frequency of lake trout capture and the importance of limiting mortality for achieving rehabilitation goals, understanding factors that affect lake trout bycatch is valuable. We used catch and effort data from commercial logbooks and onboard observer reports to assess potential effects of factors in the operation of the lake whitefish fishery on lake trout bycatch and to develop standardized indices of lake trout abundance. Factors considered in our analysis were season, mesh size, region, and license holder, which were recorded in both datasets, and set type and depth, which were only recorded in the observer dataset In general, we found that environmental factors affected whether lake trout bycatch occurred, but that if bycatch occurred, factors related to the fishing gear affected its magnitude. Although we observed seasonal interactions with depth and mesh size, the probability of bycatch was lowest in shallow waters, and the magnitude of bycatch was lowest in shallow waters, alternative set types, and larger mesh sizes. Standardized indices of lake trout abundance from both datasets gave comparable estimates of relative trends; an increase in abundance up to 2004-2005 followed by a decline. Our findings show utility for the use of the observer dataset from the lake whitefish fishery as part of lake trout management in Lake Huron. Published by Elsevier B.V. on behalf of International Association for Great Lakes Research.
C1 [Langseth, Brian J.] Michigan State Univ, Quantitat Fisheries Ctr, E Lansing, MI 48824 USA.
[Langseth, Brian J.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Beaufort Lab, Beaufort, NC 28516 USA.
[Cottrill, Adam] Minist Nat Resources & Forestry, Upper Great Lakes Management Unit, Owen Sound, ON N4K 2Z1, Canada.
RP Langseth, BJ (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Inouye Reg Ctr, 1845 Wasp Blvd Bldg 176, Honolulu, HI 96818 USA.
EM brian.langseth@noaa.gov
NR 47
TC 0
Z9 0
U1 3
U2 16
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0380-1330
J9 J GREAT LAKES RES
JI J. Gt. Lakes Res.
PD MAR
PY 2015
VL 41
IS 1
BP 280
EP 291
DI 10.1016/j.jglr.2014.12.014
PG 12
WC Environmental Sciences; Limnology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA CE2NA
UT WOS:000351651100028
ER
PT J
AU Mattmann, CA
Garcia, J
Krka, I
Popescu, D
Medvidovic, N
AF Mattmann, Chris A.
Garcia, Joshua
Krka, Ivo
Popescu, Daniel
Medvidovic, Nenad
TI Revisiting the Anatomy and Physiology of the Grid
SO JOURNAL OF GRID COMPUTING
LA English
DT Article
DE DSSA; Physiology; Anatomy; OODT; Software architecture
ID MANAGEMENT
AB A domain-specific software architecture (DSSA) represents an effective, generalized, reusable solution to constructing software systems within a given application domain. In this paper, we revisit the widely cited DSSA for the domain of grid computing. We have studied systems in this domain over the last ten years. During this time, we have repeatedly observed that, while individual grid systems are widely used and deemed successful, the grid DSSA is actually underspecified to the point where providing a precise answer regarding what makes a software system a grid system is nearly impossible. Moreover, every one of the existing purported grid technologies actually violates the published grid DSSA. In response to this, based on an analysis of the source code, documentation, and usage of eighteen of the most pervasive grid technologies, we have significantly refined the original grid DSSA. We demonstrate that this DSSA much more closely matches the grid technologies studied. Our refinements allow us to more definitively identify a software system as a grid technology, and distinguish it from software libraries, middleware, and frameworks.
C1 [Mattmann, Chris A.; Medvidovic, Nenad] Univ So Calif, Dept Comp Sci, Los Angeles, CA 90089 USA.
[Mattmann, Chris A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Krka, Ivo; Popescu, Daniel] Google Inc, Santa Monica, CA USA.
[Garcia, Joshua] George Mason Univ, Fairfax, VA 22030 USA.
RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chris.a.mattmann@nasa.gov; joshuaga@usc.edu; krka@google.com;
popescudm@gmail.com; neno@usc.edu
NR 42
TC 1
Z9 1
U1 7
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1570-7873
EI 1572-9184
J9 J GRID COMPUT
JI J. Comput.
PD MAR
PY 2015
VL 13
IS 1
BP 19
EP 34
DI 10.1007/s10723-015-9324-0
PG 16
WC Computer Science, Information Systems; Computer Science, Theory &
Methods
SC Computer Science
GA CD7SU
UT WOS:000351293100002
ER
PT J
AU Pati, GS
Warren, Z
Yu, N
Shahriar, MS
AF Pati, G. S.
Warren, Z.
Yu, N.
Shahriar, M. S.
TI Computational studies of light shift in a Raman-Ramsey
interference-based atomic clock
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID RUBIDIUM VAPOR; TRANSITION; FRINGES; EXCITATION; RESONANCE; BEAM
AB Determining light shift in Raman-Ramsey (RR) interference is important for the development of atomic frequency standards based on a vapor cell. We have accurately calculated light shift in RR interference using the density-matrix equations for a three-level system without invoking the adiabatic approximation. Specifically, phase shifts associated with coherent density-matrix terms are studied as they are relevant to the detection of RR interference in transmission (or absorption) through the medium. For the single-velocity case, the numerically computed results are compared with the analytical results obtained using the adiabatic approximation. The result shows light shift suppression in conformity with the closed-form analytic solutions. The computational studies have also been extended to investigate RR interference for a Doppler-broadened vapor medium. Importantly, a velocity-induced frequency shift is found at the fringe center as an additional source of frequency error for a vapor cell Raman clock. (C) 2015 Optical Society of America
C1 [Pati, G. S.] Delaware State Univ, Dept Phys & Engn, Dover, DE 19901 USA.
[Yu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shahriar, M. S.] Northwestern Univ, Dept Elect Engn & Comp Sci, Evanston, IL 60308 USA.
[Shahriar, M. S.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60308 USA.
RP Pati, GS (reprint author), Delaware State Univ, Dept Phys & Engn, Dover, DE 19901 USA.
EM gspati@desu.edu
FU DoD grant [W911NF-13-10152]; NASA URC grant [NNX09AU90A]; DARPA
[D14PC00134]; AFOSR grant [FA9550-10-1-0228]
FX The authors acknowledge the support received from the DoD grant
#W911NF-13-10152, the NASA URC grant #NNX09AU90A, DARPA contract
#D14PC00134, and AFOSR grant # FA9550-10-1-0228 for conducting this
research.
NR 21
TC 4
Z9 4
U1 1
U2 21
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0740-3224
EI 1520-8540
J9 J OPT SOC AM B
JI J. Opt. Soc. Am. B-Opt. Phys.
PD MAR
PY 2015
VL 32
IS 3
BP 388
EP 394
DI 10.1364/JOSAB.32.000388
PG 7
WC Optics
SC Optics
GA CD5NG
UT WOS:000351134200004
ER
PT J
AU Burton, AS
McLain, H
Glavin, DP
Elsila, JE
Davidson, J
Miller, KE
Andronikov, AV
Lauretta, D
Dworkin, JP
AF Burton, Aaron S.
McLain, Hannah
Glavin, Daniel P.
Elsila, Jamie E.
Davidson, Jemma
Miller, Kelly E.
Andronikov, Alexander V.
Lauretta, Dante
Dworkin, Jason P.
TI Amino acid analyses of R and CK chondrites
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID LARGE ENANTIOMERIC EXCESSES; CARBONACEOUS CHONDRITES; PRIMITIVE
METEORITES; PARENT-BODY; ANTARCTIC METEORITES; MURCHISON METEORITE;
AQUEOUS ALTERATION; MASS SPECTROMETRY; LAPAZ ICEFIELD; EXTRATERRESTRIAL
AB Exogenous delivery of amino acids and other organic molecules to planetary surfaces may have played an important role in the origins of life on Earth and other solar system bodies. Previous studies have revealed the presence of indigenous amino acids in a wide range of carbon-rich meteorites, with the abundances and structural distributions differing significantly depending on parent body mineralogy and alteration conditions. Here we report on the amino acid abundances of seven type 3-6 CK chondrites and two Rumuruti (R) chondrites. Amino acid measurements were made on hot water extracts from these meteorites by ultrahigh-performance liquid chromatography with fluorescence detection and time-of-flight mass spectrometry. Of the nine meteorites analyzed, four were depleted in amino acids, and one had experienced significant amino acid contamination by terrestrial biology. The remaining four, comprised of two R and two CK chondrites, contained low levels of amino acids that were predominantly the straight chain, amino-terminal (n--amino) acids -alanine, and -amino-n-butyric acid. This amino acid distribution is similar to what we reported previously for thermally altered ureilites and CV and CO chondrites, and these n--amino acids appear to be indigenous to the meteorites and not the result of terrestrial contamination. The amino acids may have been formed by Fischer-Tropsch-type reactions, although this hypothesis needs further testing.
C1 [Burton, Aaron S.; Glavin, Daniel P.; Elsila, Jamie E.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[McLain, Hannah] Catholic Univ Amer, Washington, DC 20064 USA.
[Davidson, Jemma] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Miller, Kelly E.; Andronikov, Alexander V.; Lauretta, Dante] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Burton, AS (reprint author), NASA, Astromat Res & Explorat Sci Div, Johnson Space Ctr, Houston, TX 77586 USA.
EM aaron.s.burton@nasa.gov
RI Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Dworkin,
Jason/C-9417-2012
OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997
FU National Aeronautics and Space Administration (NASA); NASA Astrobiology
Institute and the Goddard Center for Astrobiology; NASA Cosmochemistry
Program; NASA Exobiology Program; Simons Foundation [302497]
FX A. S. B. was supported by a National Aeronautics and Space
Administration (NASA) Postdoctoral Program Fellowship administered by
Oak Ridge Associated Universities through a contract with NASA. D. P.
G., J. E. E., K. E. M., A. A., D. L., and J. P. D. acknowledge funding
support from one or more of the following programs: NASA Astrobiology
Institute and the Goddard Center for Astrobiology, the NASA
Cosmochemistry Program, and NASA Exobiology Program. This work was also
supported in part by a grant from the Simons Foundation (SCOL award
302497 to J. P. D.). We are grateful to ANSMET, K. Righter, and the
members of the Meteorite Working Group for allocating the Antarctic
meteorite samples analyzed in this study, M. Callahan for helpful
discussions and feedback on the manuscript, and T. McCollum and an
anonymous reviewer for insightful criticism and suggestions to improve
the manuscript.
NR 55
TC 6
Z9 6
U1 8
U2 28
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 MAR
PY 2015
VL 50
IS 3
BP 470
EP 482
DI 10.1111/maps.12433
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CE2UZ
UT WOS:000351676600009
ER
PT J
AU Bhalerao, V
Romano, P
Tomsick, J
Natalucci, L
Smith, DM
Bellm, E
Boggs, SE
Chakrabarty, D
Christensen, FE
Craig, WW
Fuerst, F
Hailey, CJ
Harrison, FA
Krivonos, RA
Lu, TN
Madsen, K
Stern, D
Younes, G
Zhang, W
AF Bhalerao, Varun
Romano, Patrizia
Tomsick, John
Natalucci, Lorenzo
Smith, David M.
Bellm, Eric
Boggs, Steven E.
Chakrabarty, Deepto
Christensen, Finn E.
Craig, William W.
Fuerst, Felix
Hailey, Charles J.
Harrison, Fiona A.
Krivonos, Roman A.
Lu, Ting-Ni
Madsen, Kristin
Stern, Daniel
Younes, George
Zhang, William
TI NuSTAR detection of a cyclotron line in the supergiant fast X-ray
transient IGR J17544-2619
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE X-rays: binaries; X-rays: individual: IGR J17544-2619
ID XTE J1739-302; INTEGRAL OBSERVATIONS; SWIFT OBSERVATIONS; NEUTRON-STAR;
OUTBURST; ABSORPTION; BINARIES; WINDS
AB We present NuSTAR spectral and timing studies of the supergiant fast X-ray transient (SFXT) IGR J17544-2619. The spectrum is well described by an similar to 1 keV blackbody and a hard continuum component, as expected from an accreting X-ray pulsar. We detect a cyclotron line at 17 keV, confirming that the compact object in IGR J17544-2619 is indeed a neutron star. This is the first measurement of the magnetic field in an SFXT. The inferred magnetic field strength, B = (1.45 +/- 0.03) x 10(12) G (1 + z) is typical of neutron stars in X-ray binaries, and rules out a magnetar nature for the compact object. We do not find any significant pulsations in the source on time-scales of 1-2000 s.
C1 [Bhalerao, Varun] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Romano, Patrizia] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Tomsick, John; Boggs, Steven E.; Craig, William W.; Krivonos, Roman A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy.
[Smith, David M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, David M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bellm, Eric; Fuerst, Felix; Harrison, Fiona A.; Lu, Ting-Ni; Madsen, Kristin] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lu, Ting-Ni] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Younes, George] NSSTC, USRA, Huntsville, AL 35801 USA.
[Zhang, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bhalerao, V (reprint author), Inter Univ Ctr Astron & Astrophys, PO Bag 4, Pune 411007, Maharashtra, India.
EM varunb@iucaa.ernet.in
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bhalerao, Varun/0000-0002-6112-7609;
Bellm, Eric/0000-0001-8018-5348
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Italian Space Agency (ASI) by ASI/INAF [I/037/12/0-011/13]; [ASI-INAF
I/004/11/0]
FX This work was supported in part 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 as well as the Swift team 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). PR acknowledges contract ASI-INAF I/004/11/0. LN wishes to
acknowledge the Italian Space Agency (ASI) for Financial support by
ASI/INAF grant I/037/12/0-011/13. VB thanks Dipankar Bhattacharya for
helpful discussions.
NR 44
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2015
VL 447
IS 3
BP 2274
EP 2281
DI 10.1093/mnras/stu2495
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TP
UT WOS:000350273200016
ER
PT J
AU Clementel, N
Madura, TI
Kruip, CJH
Paardekooper, JP
Gull, TR
AF Clementel, N.
Madura, T. I.
Kruip, C. J. H.
Paardekooper, J. -P.
Gull, T. R.
TI 3D radiative transfer simulations of Eta Carinae's inner colliding winds
- I. Ionization structure of helium at apastron
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; radiative transfer; binaries: close; stars: individual:
Eta Carinae; stars: mass-loss; stars: winds, outflows
ID SMOOTHED PARTICLE HYDRODYNAMICS; X-RAY MINIMUM; HOMUNCULUS NEBULA;
BINARY-SYSTEMS; IONIZING-RADIATION; SIMPLEX ALGORITHM; EMISSION-LINES;
COMPANION; STAR; SPH
AB The highly eccentric binary system Eta Carinae (eta Car) shows numerous time-variable emission and absorption features. These observational signatures are the result of interactions between the complex three-dimensional (3D) wind-wind collision regions and photoionization by the luminous stars. Specifically, helium presents several interesting spectral features that provide important clues on the geometry and physical proprieties of the system and the individual stars. We use the SIMPLEX algorithm to post-process 3D smoothed particle hydrodynamics simulation output of the interacting winds in eta Car in order to obtain the fractions of ionized helium assuming three different primary star (eta(A)) mass-loss rates. The resultant ionization maps constrain the regions where helium is singly-and doubly-ionized. We find that reducing eta(A)'s mass-loss rate ((M) over dot(eta A)) increases the volume of He+. Lowering (M) over dot(eta A) produces large variations in the volume of He+ in the pre-shock eta(A) wind on the periastron side of the system. Our results show that binary orientations in which apastron is on our side of the system are more consistent with available observations. We suggest that small variations in (M) over dot(eta A) might explain the observed increase in He+ absorption in recent decades, although numerous questions regarding this scenario remain open. We also propose that the absence of broad He I lines in the spectra of eta Car between its 1890's eruption and similar to 1944 might be explained by eta(B)'s He0+-ionizing photons not being able to penetrate the wind-wind interaction region, due to a higher (M) over dot(eta A) at that time (by a factor greater than or similar to 2, compared to the present value).
C1 [Clementel, N.; Kruip, C. J. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Madura, T. I.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Paardekooper, J. -P.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Paardekooper, J. -P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Clementel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM clementel@strw.leidenuniv.nl
FU NASA Postdoctoral Program at the Goddard Space Flight Center; NASA
through Space Telescope Science Institute [12013, 12508, 12750, 13054,
13395]; NASA [NAS 5-26555]
FX We thank Jose Groh, Noel Richardson, and Vincent Icke for useful
discussions and comments. TIM is supported by an appointment to the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA. Support
for TRG was through programs # 12013, 12508, 12750, 13054, and 13395,
provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555.
NR 71
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U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2015
VL 447
IS 3
BP 2445
EP 2458
DI 10.1093/mnras/stu2614
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TP
UT WOS:000350273200029
ER
PT J
AU Lange, R
Driver, SP
Robotham, ASG
Kelvin, LS
Graham, AW
Alpaslan, M
Andrews, SK
Baldry, IK
Bamford, S
Bland-Hawthorn, J
Brough, S
Cluver, ME
Conselice, CJ
Davies, LJM
Haeussler, B
Konstantopoulos, IS
Loveday, J
Moffett, AJ
Norberg, P
Phillipps, S
Taylor, EN
Lopez-Sanchez, AR
Wilkins, SM
AF Lange, Rebecca
Driver, Simon P.
Robotham, Aaron S. G.
Kelvin, Lee S.
Graham, Alister W.
Alpaslan, Mehmet
Andrews, Stephen K.
Baldry, Ivan K.
Bamford, Steven
Bland-Hawthorn, Joss
Brough, Sarah
Cluver, Michelle E.
Conselice, Christopher J.
Davies, Luke J. M.
Haeussler, Boris
Konstantopoulos, Iraklis S.
Loveday, Jon
Moffett, Amanda J.
Norberg, Peder
Phillipps, Steven
Taylor, Edward N.
Lopez-Sanchez, Angel R.
Wilkins, Stephen M.
TI Galaxy And Mass Assembly (GAMA): mass-size relations of z < 0.1 galaxies
subdivided by Sersic index, colour and morphology
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies:
fundamental parameters; galaxies: spiral; galaxies: statistics
ID DIGITAL SKY SURVEY; DWARF ELLIPTIC GALAXIES; ULTRA-DEEP-FIELD; DISK
GALAXIES; SURFACE-BRIGHTNESS; KORMENDY RELATION; LUMINOSITY-SIZE;
REDSHIFT SURVEY; SPIRAL GALAXIES; SPACE DENSITY
AB We use data from the Galaxy And Mass Assembly (GAMA) survey in the redshift range 0.01 < z < 0.1 (8399 galaxies in g to K-s bands) to derive the stellar mass-half-light radius relations for various divisions of 'early'- and 'late'-type samples. We find that the choice of division between early and late (i.e. colour, shape, morphology) is not particularly critical; however, the adopted mass limits and sample selections (i.e. the careful rejection of outliers and use of robust fitting methods) are important. In particular, we note that for samples extending to low stellar mass limits (< 1010 M-circle dot) the Sersic index bimodality, evident for high-mass systems, becomes less distinct and no-longer acts as a reliable separator of early- and late-type systems. The final set of stellar mass-half-light radius relations are reported for a variety of galaxy population subsets in 10 bands (ugrizZY JHK(s)) and are intended to provide a comprehensive low-z benchmark for the many ongoing high-z studies. Exploring the variation of the stellar mass-half-light radius relations with wavelength, we confirm earlier findings that galaxies appear more compact at longer wavelengths albeit at a smaller level than previously noted: at 10(10) M-circle dot both spiral systems and ellipticals show a decrease in size of 13 per cent from g to K-s (which is near linear in log wavelength). Finally, we note that the sizes used in this work are derived from 2D Sersic light profile fitting (using GALFIT3), i.e. elliptical semimajor half-light radii, improving on earlier low-z benchmarks based on circular apertures.
C1 [Lange, Rebecca; Driver, Simon P.; Robotham, Aaron S. G.; Andrews, Stephen K.; Davies, Luke J. M.; Moffett, Amanda J.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia.
[Driver, Simon P.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Kelvin, Lee S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Graham, Alister W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Alpaslan, Mehmet] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Baldry, Ivan K.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Bamford, Steven; Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bland-Hawthorn, Joss] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2088, Australia.
[Brough, Sarah; Lopez-Sanchez, Angel R.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Cluver, Michelle E.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa.
[Haeussler, Boris] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Haeussler, Boris] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
[Loveday, Jon; Wilkins, Stephen M.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Norberg, Peder] Univ Durham, ICC, Durham DH1 3, County Durham, England.
[Phillipps, Steven] Univ Bristol, Sch Phys, Bristol BS8 1TL, Avon, England.
[Taylor, Edward N.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia.
RP Lange, R (reprint author), Univ Western Australia, ICRAR, M468,35 Stirling Highway, Crawley, WA 6009, Australia.
EM rebecca.lange@icrar.org
RI Driver, Simon/H-9115-2014; Bamford, Steven/E-8702-2010;
OI Driver, Simon/0000-0001-9491-7327; Bamford, Steven/0000-0001-7821-7195;
Robotham, Aaron/0000-0003-0429-3579; Alpaslan,
Mehmet/0000-0003-0321-1033
FU International Centre for Radio Astronomy Research; University of Western
Australia; STFC (UK); ARC (Australia); AAO; ESO Telescopes at the La
Silla Paranal Observatory [179.A-2004]
FX RL would like to acknowledge funding from the International Centre for
Radio Astronomy Research and the University of Western Australia. GAMA
is a joint European-Australasian project based around a spectroscopic
campaign using the Anglo-Australian Telescope. The GAMA input catalogue
is based on data taken from the SDSS and the 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. The VISTA VIKING data used in this paper are based on
observations made with ESO Telescopes at the La Silla Paranal
Observatory under programme ID 179.A-2004. 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/.
NR 92
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2015
VL 447
IS 3
BP 2603
EP 2630
DI 10.1093/mnras/stu2467
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TP
UT WOS:000350273200042
ER
PT J
AU Zhang, SN
Ji, L
Kallman, TR
Yao, YS
Froning, CS
Gu, QS
Kriss, GA
AF Zhang, S. N.
Ji, L.
Kallman, T. R.
Yao, Y. S.
Froning, C. S.
Gu, Q. S.
Kriss, G. A.
TI Modelling warm absorption in HST/COS spectrum of Mrk 290 with XSTAR
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE quasars: absorption lines; quasars: individual: Mrk 290; ultraviolet:
galaxies
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; SEYFERT 1 GALAXIES;
X-RAY-ABSORPTION; INTRINSIC ABSORPTION; IONIZED-GAS; XMM-NEWTON;
MULTIWAVELENGTH CAMPAIGN; SIMULTANEOUS CHANDRA; PHYSICAL CONDITIONS
AB We present a new method to model an HST/COS (Hubble Space Telescope/Cosmic Origins Spectrograph) spectrum, aimed to analyse intrinsic UV absorption from the outflow of Mrk 290, a Seyfert I galaxy. We use newly updated XSTAR to generate photoionization models for the intrinsic absorption from the active galactic nuclei (AGN) outflow, the line emission from the AGN broad-and narrow-line regions, and the local absorption from high-velocity clouds and Galactic interstellar medium. The combination of these physical models accurately fits the COS spectrum. Three intrinsic absorbers outflowing with velocities similar to 500 km s(-1) are identified, two of which are found directly from two velocity components of the N V and C IV doublets, while the third is required by the extra absorption in the Ly alpha. Their outflow velocities, ionization states and column densities are consistent with the lowest and moderate ionization warm absorbers (WAs) in the X-ray domain found by Chandra observations, suggesting a one-to-one correspondence between the absorbing gas in the UV and X-ray bands. The small turbulent velocities of the WAs (v(turb) less than or similar to 100 km s(-1)) support our previous argument from the X-ray study that the absorbers originate from the inner side of the torus due to thermal evaporation. Given the covering fractions of similar to 65 per cent for the three WAs, we deduce that the lengths and the thicknesses of the WAs are comparable, which indicates that the geometry of WAs are more likely clouds rather than flat and thin layers. In addition, the modelling of the broad-line emission suggests a higher covering fraction of clouds when they are very closer to the black hole.
C1 [Zhang, S. N.; Ji, L.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Zhang, S. N.; Ji, L.] Chinese Acad Sci, PMO, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China.
[Zhang, S. N.; Ji, L.; Gu, Q. S.] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China.
[Zhang, S. N.; Gu, Q. S.] Nanjing Univ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yao, Y. S.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Froning, C. S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Gu, Q. S.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210008, Peoples R China.
[Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Zhang, SN (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
EM snzhang@pmo.ac.cn
FU National Natural Science Foundation of China [11203080]; Chinese Academy
of Sciences
FX The anonymous referee is thanked for careful reading of the manuscript
and for helpful comments. We thank John Houck for solving all ISIS
software problems, and Yanmei Chen for dealing with the SDSS spectrum of
Mrk 290. We are grateful to MIT Kavli institute for supplying computing
time of clusters. The work is partly supported by the National Natural
Science Foundation of China under the grant 11203080. Li Ji is also
supported by the 100 Talents program of Chinese Academy of Sciences.
NR 59
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U1 1
U2 1
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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 MAR 1
PY 2015
VL 447
IS 3
BP 2671
EP 2682
DI 10.1093/mnras/stu2594
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TP
UT WOS:000350273200046
ER
PT J
AU Rogers, BM
Soja, AJ
Goulden, ML
Randerson, JT
AF Rogers, Brendan M.
Soja, Amber J.
Goulden, Michael L.
Randerson, James T.
TI Influence of tree species on continental differences in boreal fires and
climate feedbacks
SO NATURE GEOSCIENCE
LA English
DT Article
ID INTERIOR ALASKA; BLACK SPRUCE; FOREST-FIRES; IMPACT; MANAGEMENT;
EMISSIONS; WILDFIRES; SAVANNA; BALANCE
AB Wildfires are common in boreal forests around the globe and strongly influence ecosystem processes. However, North American forests support more high-intensity crown fires than Eurasia, where lower-intensity surface fires are common. These two types of fire can result in different net effects on climate as a consequence of their contrasting impacts on terrestrial albedo and carbon stocks. Here we use remote-sensing imagery, climate reanalysis data and forest inventories to evaluate differences in boreal fire dynamics between North America and Eurasia and their key drivers. Eurasian fires were less intense, destroyed less live vegetation, killed fewer trees and generated a smaller negative shortwave forcing. As fire weather conditions were similar across continents, we suggest that different fire dynamics between the two continents resulted from their dominant tree species. In particular, species that have evolved to spread and be consumed by crown fires as part of their life cycle dominate North American boreal forests. In contrast, tree species that have evolved to resist and suppress crown fires dominate Eurasian boreal forests. We conclude that species-level traits must be considered in global evaluations of the effects of fire on emissions and climate.
C1 [Rogers, Brendan M.; Goulden, Michael L.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Soja, Amber J.] NASA, Langley Res Ctr, Climate Sci Branch, NIA, Hampton, VA 23681 USA.
[Soja, Amber J.] NASA, Langley Res Ctr, Chem & Dynam Branch, NIA, Hampton, VA 23681 USA.
RP Rogers, BM (reprint author), Woods Hole Res Ctr, Falmouth, MA 02540 USA.
EM brogers@whrc.org
RI Goulden, Michael/B-9934-2008
FU US National Science Foundation (NSF); National Aeronautics and Space
Administration (NASA); NSF [ID 2009067341]; Decadal and Regional Climate
Prediction using Earth System Models award [AGS-1048890]; NASA Carbon
Cycle program [NNX11AF96G]; NASA Atmosphere program [NNX10AT83G]; NASA
Interdisciplinary Research in Earth Science program [NNH09ZDA-IDS-0116];
Carbon in Arctic Reservoirs Vulnerability Experiment (CARVE)
FX This work was financially supported by the US National Science
Foundation (NSF) and the National Aeronautics and Space Administration
(NASA). NSF support included a Graduate Research Fellowship (ID
2009067341) to B.M.R. and a Decadal and Regional Climate Prediction
using Earth System Models award to J.T.R. (AGS-1048890). This work was
also supported by NASA Carbon Cycle (NNX11AF96G), Atmosphere
(NNX10AT83G), and Interdisciplinary Research in Earth Science
(NNH09ZDA-IDS-0116) programs, and the Carbon in Arctic Reservoirs
Vulnerability Experiment (CARVE). We thank S. Conard, W. Kurz, S. Goetz
and S. Davis for conversations on continental fire patterns, the
National Research Council Canada for providing mapped forest inventory
data, and the NASA LP DAAC for data distribution.
NR 50
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U1 8
U2 37
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2015
VL 8
IS 3
BP 228
EP 234
DI 10.1038/NGEO2352
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CD0NL
UT WOS:000350770900023
ER
PT J
AU Barnhart, WD
Murray, JR
Yun, SH
Svarc, JL
Samsonov, SV
Fielding, EJ
Brooks, BA
Milillo, P
AF Barnhart, W. D.
Murray, J. R.
Yun, S. -H.
Svarc, J. L.
Samsonov, S. V.
Fielding, E. J.
Brooks, B. A.
Milillo, P.
TI Geodetic Constraints on the 2014 M 6.0 South Napa Earthquake
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID FRANCISCO BAY AREA; FAULT SLIP RATES; STRESS TRANSFER; INSAR DATA;
DEFORMATION; MODELS; SPACE
C1 [Barnhart, W. D.] Univ Iowa, Dept Earth & Environm Sci, Iowa City, IA 52242 USA.
[Murray, J. R.; Svarc, J. L.; Brooks, B. A.] US Geol Survey, Earthquake Sci Ctr, Menlo Pk, CA 94025 USA.
[Yun, S. -H.; Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Samsonov, S. V.] Nat Resources Canada, Ottawa, ON K1A 0E4, Canada.
[Milillo, P.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
[Barnhart, W. D.] US Geol Survey, Geol Hazards Ctr, Golden, CO 80401 USA.
[Milillo, P.] Univ Basilicata, Sch Engn, I-85100 Potenza, Italy.
RP Barnhart, WD (reprint author), Univ Iowa, Dept Earth & Environm Sci, 121 Trowbridge Hall, Iowa City, IA 52242 USA.
EM william-barnhart-1@uiowa.edu
RI Barnhart, William/L-9446-2015;
OI Samsonov, Sergey/0000-0002-6798-4847; Milillo,
Pietro/0000-0002-1171-3976
FU National Science Foundation [EAR-0350028, EAR-0732947]; National
Aeronautics and Space Administration Earth Surface and Interior focus
area; Applied Sciences Program; U.S. Geological Survey (USGS) Mendenhall
Postdoctoral fellowship at the USGS Geological Hazards Center; USGS
Earthquake Science Center
FX The authors thank Gavin Hayes and three anonymous reviewers for helpful
reviews that improved the quality of this manuscript. This project, in
part, was carried out using CSK products ((c) Italian Space Agency
[ASI]), delivered under the ASI license provided under the
Caltech/JPL-ASI/CIDOT CaliMap project. Original RADARSAT-2 data is
copyrighted by MacDonald, Dettwiler and Associates Ltd. (MDA; (c) 2014).
Continuous Global Positioning System data used in this study were
recorded by instruments of the Plate Boundary Observatory (PBO,
http://pbo.unavco.org/; last accessed December 2014) and the Bay Area
Regional Deformation (BARD) network (http://seismo.berkeley.edu/bard/;
last accessed December 2014). The PBO is operated by UNAVCO for
EarthScope (www.earthscope.org; last accessed December 2014) and
supported by the National Science Foundation (Numbers EAR-0350028 and
EAR-0732947). Part of this research was supported by the National
Aeronautics and Space Administration Earth Surface and Interior focus
area and Applied Sciences Program and performed at the Jet Propulsion
Laboratory, California Institute of Technology. W. D. B. was supported
by a U.S. Geological Survey (USGS) Mendenhall Postdoctoral fellowship at
the USGS Geological Hazards Center. J. R. M., J. L. S., and B. A. B.
were supported by the USGS Earthquake Science Center. This is Natural
Resources Canada Earth Science Sector Contribution Number 20140320.
Several figures were generated using the Generic Mapping Tool (Wessel
and Smith, 1998). Any use of trade, product, or firm names is for
descriptive purposes only and does not imply endorsement by the U.S.
Government.
NR 38
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U1 0
U2 6
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD MAR-APR
PY 2015
VL 86
IS 2
BP 335
EP 343
DI 10.1785/0220140210
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CD8EK
UT WOS:000351327800008
ER
PT J
AU Wei, SJ
Barbot, S
Graves, R
Lienkaemper, JJ
Wang, T
Hudnut, K
Fu, YN
Helmberger, D
AF Wei, Shengji
Barbot, Sylvain
Graves, Robert
Lienkaemper, James J.
Wang, Teng
Hudnut, Kenneth
Fu, Yuning
Helmberger, Don
TI The 2014 M-W 6.1 South Napa Earthquake: A Unilateral Rupture with
Shallow Asperity and Rapid Afterslip
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID GROUND-MOTION; HAYWARD FAULT; HECTOR MINE; CHI-CHI; CALIFORNIA;
SIMULATION; SURFACE; TAIWAN; MODELS; CREEP
C1 [Wei, Shengji; Barbot, Sylvain] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore.
[Graves, Robert; Hudnut, Kenneth] US Geol Survey, Pasadena, CA 91106 USA.
[Lienkaemper, James J.] US Geol Survey, Menlo Pk, CA 94025 USA.
[Fu, Yuning] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wei, Shengji; Helmberger, Don] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
RP Wei, SJ (reprint author), Nanyang Technol Univ, Earth Observ Singapore, 50 Nanyang Ave Block N2-01a-15, Singapore 639798, Singapore.
EM shjwei@gmail.com
RI Hudnut, Kenneth/B-1945-2009; Wei, Shengji/M-2137-2015;
OI Hudnut, Kenneth/0000-0002-3168-4797; Wei, Shengji/0000-0002-0319-0714;
Wang, Teng/0000-0003-3729-0139
FU National Aeronautics and Space Administration
FX Strong-motion waveform data was downloaded from the Northern California
Data Center, California Geological Survey, and U.S. Geological Survey
(USGS) (strongmotioncenter.org; last accessed September 2014).
Interferometric Synthetic Aperture Radar data were obtained from the Jet
Propulsion Laboratory (JPL), static GPS data were made available by Tom
Herring from the Massachusetts Institute of Technology. Constructive
reviews by Annemarie Baltay, Art Frankel, and an anonymous reviewer led
to improvements in the manuscript. Figures were made using Generic
Mapping Tool (Wessel and Smith, 1991). Part of this research was carried
out at JPL (California Institute of Technology), sponsored by the
National Aeronautics and Space Administration.
NR 32
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U1 1
U2 7
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD MAR-APR
PY 2015
VL 86
IS 2
BP 344
EP 354
DI 10.1785/0220140249
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CD8EK
UT WOS:000351327800009
ER
PT J
AU Della Corte, C
Stanford, MK
Jett, TR
AF Della Corte, Christopher
Stanford, Malcolm K.
Jett, Timothy R.
TI Rolling Contact Fatigue of Superelastic Intermetallic Materials (SIM)
for Use as Resilient Corrosion Resistant Bearings
SO TRIBOLOGY LETTERS
LA English
DT Article
DE Bearings; Fatigue; Rolling contact; Super elastic; Materials
ID TINI
AB Superelastic intermetallic materials (SIM), such as 60NiTi, are emerging as candidates for corrosion and shock-resistant rolling element bearings. Compared with metals, the intermetallic materials are more brittle and may be prone to rolling contact fatigue degradation. In this paper, a series of three ball-on-rod rolling contact fatigue tests were conducted using polished steel balls and NiTi rods prepared by vacuum casting and powder metallurgy techniques. The test protocol matched that used in ASTM STP 771 except that the steel balls were not intentionally roughened. In general, the NiTi rods exhibit fatigue damage at much lower stress levels than commercial bearing steels. At the lowest stress level tested (1.7 GPa), 60NiTi rods that were largely free from processing defects gave acceptably long lives, and testing was terminated without failure after 800 h. At elevated stress (2.5 GPa), failure occurred for some specimens, while others reached the preset test length goal of 800 h. Improperly prepared 60NiTi rods that had unconsolidated particles or significant ceramic inclusions occasionally experienced surface fatigue prior to completion of the test period even at the lowest stress level. Alloyed NiTi rods containing small amounts of Hf as a microstructural processing aid generally endured higher stress levels than the baseline 60NiTi composition. Two predominant fatigue failure mechanisms were observed: intergranular (grain boundary) fracture and intragranular (through the grains) crack propagation. The results suggest that further fatigue capability improvements could be obtained through process improvements, microstructural refinements and alloying. SIM currently available are recommended for mechanically benign applications involving modest stress levels and rates of stress cycle accumulation. Applications that include high continuous loads (stress) and high speeds for long durations should be avoided.
C1 [Della Corte, Christopher; Stanford, Malcolm K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Jett, Timothy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Della Corte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Christopher.Dellacorte@grc.nasa.gov
FU NASA International Space Station Program; NASA Engineering and Safety
Center (NESC); Aerosciences Project within the NASA Fundamental
Aeronautics Program
FX The authors wish to thank Walt Wozniak, Olivia Leak and Joy Buehler of
NASA Glenn Research Center for their invaluable assistance in preparing
rod specimens and in the post-test examinations of the fatigue failures.
The support provided by the NASA International Space Station Program,
the NASA Engineering and Safety Center (NESC) and the Aerosciences
Project within the NASA Fundamental Aeronautics Program are greatly
appreciated.
NR 22
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U2 11
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1023-8883
EI 1573-2711
J9 TRIBOL LETT
JI Tribol. Lett.
PD MAR
PY 2015
VL 57
IS 3
AR 26
DI 10.1007/s11249-014-0456-3
PG 10
WC Engineering, Chemical; Engineering, Mechanical
SC Engineering
GA CD4KH
UT WOS:000351050800012
ER
PT J
AU Christofidou-Solomidou, M
Pietrofesa, RA
Arguiri, E
Schweitzer, KS
Berdyshev, EV
McCarthy, M
Corbitt, A
Alwood, JS
Yu, YJ
Globus, RK
Solomides, CC
Ullrich, RL
Petrache, I
AF Christofidou-Solomidou, Melpo
Pietrofesa, Ralph A.
Arguiri, Evguenia
Schweitzer, Kelly S.
Berdyshev, Evgeny V.
McCarthy, Maureen
Corbitt, Astrid
Alwood, Joshua S.
Yu, Yongjia
Globus, Ruth K.
Solomides, Charalambos C.
Ullrich, Robert L.
Petrache, Irina
TI Space radiation-associated lung injury in a murine model
SO AMERICAN JOURNAL OF PHYSIOLOGY-LUNG CELLULAR AND MOLECULAR PHYSIOLOGY
LA English
DT Article
DE Fe-56; Si-28; protons; gamma radiation; emphysema; oxidative stress;
senescence; lung injury; inflammation; hypoxemia
ID OBSTRUCTIVE PULMONARY-DISEASE; SMOKE-INDUCED EMPHYSEMA; SPHINGOSINE
1-PHOSPHATE; ANTIOXIDANT DEFENSES; PREMATURE SENESCENCE;
IONIZING-RADIATION; OXIDATIVE STRESS; MOUSE MODEL; FIBROSIS; APOPTOSIS
AB Despite considerable progress in identifying health risks to crewmembers related to exposure to galactic/cosmic rays and solar particle events (SPE) during space travel, its long-term effects on the pulmonary system are unknown. We used a murine risk projection model to investigate the impact of exposure to space-relevant radiation (SR) on the lung. C3H mice were exposed to Cs-137 gamma rays, protons (acute, low-dose exposure mimicking the 1972 SPE), 600 MeV/u Fe-56 ions, or 350 MeV/u Si-28 ions at the NASA Space Radiation Laboratory at Brookhaven National Laboratory. Animals were irradiated at the age of 2.5 mo and evaluated 23.5 mo postirradiation, at 26 mo of age. Compared with age-matched nonirradiated mice, SR exposures led to significant air space enlargement and dose-dependent decreased systemic oxygenation levels. These were associated with late mild lung inflammation and prominent cellular injury, with significant oxidative stress and apoptosis (caspase-3 activation) in the lung parenchyma. SR, especially high-energy Fe-56 or Si-28 ions markedly decreased sphingosine-1-phosphate levels and Akt- and p38 MAPK phosphorylation, depleted anti-senescence sirtuin-1 and increased biochemical markers of autophagy. Exposure to SR caused dose-dependent, pronounced late lung pathological sequelae consistent with alveolar simplification and cellular signaling of increased injury and decreased repair. The associated systemic hypoxemia suggested that this previously uncharacterized space radiation-associated lung injury was functionally significant, indicating that further studies are needed to define the risk and to develop appropriate lung-protective counter-measures for manned deep space missions.
C1 [Christofidou-Solomidou, Melpo; Pietrofesa, Ralph A.; Arguiri, Evguenia] Univ Penn, Perelman Sch Med, Dept Med, Pulm Allergy & Crit Care Div, Philadelphia, PA 19104 USA.
[Schweitzer, Kelly S.; Petrache, Irina] Indiana Univ, Sch Med, Dept Med, Div Pulm & Crit Care, Indianapolis, IN 46204 USA.
[Berdyshev, Evgeny V.] Univ Illinois, Dept Med, Chicago, IL USA.
[McCarthy, Maureen; Corbitt, Astrid; Yu, Yongjia; Ullrich, Robert L.] Univ Texas Med Branch, Galveston, TX 77555 USA.
[Alwood, Joshua S.] NASA, Postdoctoral Program, Oak Ridge Associated Univ, Moffett Field, CA USA.
[Globus, Ruth K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Solomides, Charalambos C.] Jefferson Univ Hosp, Dept Pathol, Philadelphia, PA USA.
[Petrache, Irina] Richard L Roudebush VA Med Ctr, Indianapolis, IN USA.
RP Christofidou-Solomidou, M (reprint author), Univ Penn, Dept Med, Pulm Allergy & Crit Care Div, 3615 Civ Ctr Blvd,Abramson Res Bldg,Suite 1016C, Philadelphia, PA 19104 USA.
EM melpo@mail.med.upenn.edu
FU NASA [NNX09AM08G]; DOE-NASA Interagency Award - Office of Science
(Biological and Environmental Research), US Department of Energy
[DE-SC0001507]; [NIH-R01 CA133470]; [NIH-RC1AI081251];
[NASA-NNJ11ZSA002NA]; [NIH-RO1HL077328]
FX This work was funded by NIH-R01 CA133470 (M. Christofidou-Solomidou),
NIH-RC1AI081251 (M. Christofidou-Solomidou), NASA-NNJ11ZSA002NA (M.
Christofidou-Solomidou), NIH-RO1HL077328 (I. Petrache), and NASA
NNX09AM08G (R. L. Ullrich) and DOE-NASA Interagency Award no.
DE-SC0001507, supported by the Office of Science (Biological and
Environmental Research), US Department of Energy (R. K. Globus).
NR 70
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U1 2
U2 12
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 1040-0605
EI 1522-1504
J9 AM J PHYSIOL-LUNG C
JI Am. J. Physiol.-Lung Cell. Mol. Physiol.
PD MAR 1
PY 2015
VL 308
IS 5
BP L416
EP L428
DI 10.1152/ajplung.00260.2014
PG 13
WC Physiology; Respiratory System
SC Physiology; Respiratory System
GA CD4OD
UT WOS:000351062000002
PM 25526737
ER
PT J
AU Almenara, JM
Damiani, C
Bouchy, F
Havel, M
Bruno, G
Hebrard, G
Diaz, RF
Deleuil, M
Barros, SCC
Boisse, I
Bonomo, AS
Montagnier, G
Santerne, A
AF Almenara, J. M.
Damiani, C.
Bouchy, F.
Havel, M.
Bruno, G.
Hebrard, G.
Diaz, R. F.
Deleuil, M.
Barros, S. C. C.
Boisse, I.
Bonomo, A. S.
Montagnier, G.
Santerne, A.
TI SOPHIE velocimetry of Kepler transit candidates XV. KOI-614b, KOI-206b,
and KOI-680b: a massive warm Jupiter orbiting a G0 metallic dwarf and
two highly inflated planets with a distant companion around evolved
F-type stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; techniques: photometric; techniques: radial
velocities; techniques: spectroscopic
ID COROT SPACE MISSION; RADIAL-VELOCITY MEASUREMENTS; SOLAR-TYPE STARS;
EXTRASOLAR PLANETS; HOT-JUPITER; GIANT PLANETS; FUNDAMENTAL PARAMETERS;
ABUNDANCE ANALYSIS; SUPER-EARTHS; EXOPLANETS
AB We report the validation and characterization of three new transiting exoplanets using SOPHIE radial velocities: KOI-614b, KOI-206b, and KOI-680b. KOI-614b has a mass of 2.86 +/- 0.35 M-Jup and a radius of 1.13(-0.18)(+0.26) R-Jup, and it orbits a G0, metallic ([Fe/H] = 0.35 +/- 0.15) dwarf in 12.9 days. Its mass and radius are familiar and compatible with standard planetary evolution models, so it is one of the few known transiting planets in this mass range to have an orbital period over ten days. With an equilibrium temperature of T-eq = 1000 +/- 45 K, this places KOI-614b at the transition between what is usually referred to as "hot" and "warm" Jupiters. KOI-206b has a mass of 2.82 +/- 0.52 M-Jup and a radius of 1.45 +/- 0.16 R-Jup, and it orbits a slightly evolved F7-type star in a 5.3-day orbit. It is a massive inflated hot Jupiter that is particularly challenging for planetary models because it requires unusually large amounts of additional dissipated energy in the planet. On the other hand, KOI-680b has a much lower mass of 0.84 +/- 0.15 M-Jup and requires less extra-dissipation to explain its uncommonly large radius of 1.99 +/- 0.18 R-Jup. It is one of the biggest transiting planets characterized so far, and it orbits a subgiant F9-star well on its way to the red giant stage, with an orbital period of 8.6 days. With host stars of masses of 1.46 +/- 0.17 M-circle dot and 1.54 +/- 0.09 M-circle dot, respectively, KOI-206b, and KOI-680b are interesting objects for theories of formation and survival of short-period planets around stars more massive than the Sun. For those two targets, we also find signs of a possible distant additional companion in the system.
C1 [Almenara, J. M.; Damiani, C.; Bouchy, F.; Bruno, G.; Deleuil, M.; Barros, S. C. C.; Boisse, I.; Santerne, A.] Aix Marseille Univ, CNRS, UMR 7326, Lab Astrophys Marseille, F-13388 Marseille, France.
[Almenara, J. M.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Almenara, J. M.] CNRS, IPAG, F-38000 Grenoble, France.
[Havel, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hebrard, G.; Montagnier, G.] Observ Haute Provence, F-04670 St Michel lObservatoire, France.
[Hebrard, G.; Montagnier, G.] Univ Paris 06, Inst Astrophys Paris, UMR CNRS 7095, F-75014 Paris, France.
[Diaz, R. F.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Bonomo, A. S.] INAF, Osserv Astrofis Torino, I-10025 Pino Torinese, Italy.
[Santerne, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Santerne, A.] Univ Porto, CAUP, Inst Astrofis Ciencias Espaco, P-4150762 Oporto, Portugal.
RP Almenara, JM (reprint author), Aix Marseille Univ, CNRS, UMR 7326, Lab Astrophys Marseille, F-13388 Marseille, France.
EM josemanuel.almenara@oamp.fr
OI Barros, Susana/0000-0003-2434-3625; Santerne,
Alexandre/0000-0002-3586-1316; Diaz, Rodrigo/0000-0001-9289-5160
FU NASA Science Mission directorate; Programme National de Planetologie
(PNP) of CNRS/INSU, France; French National Research Agency [ANR-08-
JCJC-0102-01]; NASA [NAS5-26555]; NASA Office of Space Science
[NNX09AF08G]; National Aeronautics and Space Administration; National
Science Foundation; CNES [98761, 426808, 251091]; European Research
Council/European Community [239953]; European Union [627202, 313014];
NASA; European Research Council under the ERC [337591-ExTrA]
FX This paper includes data collected with SOPHIE and ESPaDOnS and by the
Kepler mission. Funding for the Kepler mission is provided by the NASA
Science Mission directorate. We thank the technical team at the
Observatoire de Haute-Provence for their support with the SOPHIE
instrument and the 1.93-m telescope and, in particular, for the
essential work of the night assistants. Financial support for the SOPHIE
observations from the Programme National de Planetologie (PNP) of
CNRS/INSU, France is gratefully acknowledged. We also acknowledge
support from the French National Research Agency (ANR-08- JCJC-0102-01).
Some of the data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy. Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts. This publication makes use of data products from
the Two Micron All Sky Survey, which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation. This publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration. This research made use of the
Exoplanet Orbit Database and the Exoplanet Data Explorer at
exoplanets.org. The team at LAM acknowledges support by CNES grants
98761 (SCCB), 426808 (CD), and 251091 (JMA). A.S. acknowledge the
support from the European Research Council/European Community under the
FP7 through Starting Grant agreement number 239953. A.S. is supported by
the European Union under a Marie Curie Intra-European Fellowship for
Career Development with reference FP7-PEOPLE-2013-IEF, number 627202.
A.S.B. acknowledges funding from the European Union Seventh Framework
Program (FP7/2007-2013) under Grant agreement No. 313014 (ETAEARTH).
Part of this research was supported by an appointment to the NASA
Postdoctoral Program at the Ames Research Center, administered by Oak
Ridge Associated Universities through a contract with NASA. JMA
acknowledges funding from the European Research Council under the ERC
Grant Agreement No. 337591-ExTrA.
NR 70
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U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2015
VL 575
AR A71
DI 10.1051/0004-6361/201424291
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3LA
UT WOS:000350249100071
ER
PT J
AU Kostogryz, NM
Berdyugina, SV
AF Kostogryz, N. M.
Berdyugina, S. V.
TI Center-to-limb polarization in continuum spectra of F, G, K stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE polarization; radiative transfer; scattering; stars: atmospheres;
methods: numerical
ID SUNS CONTINUOUS-SPECTRUM; SOLAR SPECTRUM; ATMOSPHERES; RESOLUTION;
SYSTEM; DISK; BAND
AB Context. Scattering and absorption processes in stellar atmosphere affect the center-to-limb variations of the intensity (CLVI) and the linear polarization (CLVP) of stellar radiation.
Aims. There are several theoretical and observational studies of CLVI using different stellar models, however, most studies of CLVP have concentrated on the solar atmosphere and have not considered the CLVP in cooler non-gray stellar atmospheres at all. In this paper. N.ve present a theoretical study of the CLV of the intensity and the linear polarization in continuum spectra of different spectral type stars.
Methods. We solve the radiative transfer equations for polarized light iteratively assuming no magnetic field and considering a planeparallel model atmospheres and various opacities.
Results. We calculate the CLVI and the CLVP for Phoenix stellar model atmospheres for the range of effective temperatures (4500 K-6900 K), gravities (log g = 3.0-5.0), and wavelengths (4000-7001) angstrom), which are tabulated and available at the ('DS. In addition, we present several tests of our code and compare our results with measurements and calculations of CLNI and the CLVP for the Sun. The resulting CLVI are fitted with polynomials and their coefficients are presented in this paper.
Conclusions. For the stellar model atmospheres with lower gravity and effective temperature the CLVP is larger.
C1 [Kostogryz, N. M.; Berdyugina, S. V.] KIS, D-79104 Freiburg, Germany.
[Kostogryz, N. M.] NAS Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Berdyugina, S. V.] Univ Hawaii, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Kostogryz, NM (reprint author), KIS, Schoneckstr 6, D-79104 Freiburg, Germany.
EM kostogryz@kis.uni-freiburg.de; sveta@kis.uni-freiburg.de
FU European Research Council [ERC-2011-AdG291659]
FX This work was supported by the European Research Council Advanced Grant
HotMol(ERC-2011-AdG291659). We thank Martin Kurster for the comments and
suggestions and an anonymous referee for comments that improved this
paper.
NR 34
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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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2015
VL 575
AR A89
DI 10.1051/0004-6361/201424844
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3LA
UT WOS:000350249100089
ER
PT J
AU Mehdipour, M
Kaastra, JS
Kriss, GA
Cappi, M
Petrucci, PO
Steenbrugge, KC
Arav, N
Behar, E
Bianchi, S
Boissay, R
Branduardi-Raymont, G
Costantini, E
Ebrero, J
Di Gesu, L
Harrison, FA
Kaspi, S
De Marco, B
Matt, G
Paltani, S
Peterson, BM
Ponti, G
Nunez, FP
De Rosa, A
Ursini, F
de Vries, CP
Walton, DJ
Whewell, M
AF Mehdipour, M.
Kaastra, J. S.
Kriss, G. A.
Cappi, M.
Petrucci, P. -O.
Steenbrugge, K. C.
Arav, N.
Behar, E.
Bianchi, S.
Boissay, R.
Branduardi-Raymont, G.
Costantini, E.
Ebrero, J.
Di Gesu, L.
Harrison, F. A.
Kaspi, S.
De Marco, B.
Matt, G.
Paltani, S.
Peterson, B. M.
Ponti, G.
Nunez, F. Pozo
De Rosa, A.
Ursini, F.
de Vries, C. P.
Walton, D. J.
Whewell, M.
TI Anatomy of the AGN in NGC 5548
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: galaxies; galaxies: active; galaxies: Seyfert; galaxies:
individual: NGC 5548; techniques: spectroscopic
ID ACTIVE GALACTIC NUCLEI; X-RAY EXCESS; REFLECTION GRATING SPECTROMETER;
RADIUS-LUMINOSITY RELATIONSHIP; PHOTON IMAGING CAMERA; BROAD-LINE
REGION; K-ALPHA LINE; XMM-NEWTON; MULTIWAVELENGTH CAMPAIGN; WARM
ABSORBERS
AB An extensive multi-satellite campaign on NGC 5548 has revealed this archetypal Seyfert-1 galaxy to be in an exceptional state of persistent heavy absorption. Our observations taken in 2013-2014 with XMM-Newton, Swift, NuSTAR, INTEGRAL, Chandra, HST and two ground-based observatories have together enabled us to establish that this unexpected phenomenon is caused by an outflowing stream of weakly ionised gas (called the obscurer), extending from the vicinity of the accretion disk to the broad-line region. In this work we present the details of our campaign and the data obtained by all the observatories. We determine the spectral energy distribution of NGC 5548 from near-infrared to hard X-rays by establishing the contribution of various emission and absorption processes taking place along our line of sight towards the central engine. We thus uncover the intrinsic emission and produce a broadband continuum model for both obscured (average summer 2013 data) and unobscured (<2011) epochs of NGC 5548. Our results suggest that the intrinsic NIR/optical/UV continuum is a single Comptonised component with its higher energy tail creating the "soft X-ray excess". This component is compatible with emission from a warm, optically-thick corona as part of the inner accretion disk. We then investigate the effects of the continuum on the ionisation balance and thermal stability of photoionised gas for unobscured and obscured epochs.
C1 [Mehdipour, M.; Kaastra, J. S.; Costantini, E.; Ebrero, J.; Di Gesu, L.; de Vries, C. P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Mehdipour, M.; Branduardi-Raymont, G.; Whewell, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Kaastra, J. S.] Univ Utrecht, Dept Phys & Astron, NL-3508 TA Utrecht, Netherlands.
[Kaastra, J. S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Cappi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Petrucci, P. -O.; Ursini, F.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Petrucci, P. -O.; Ursini, F.] IPAG, CNRS, F-38000 Grenoble, France.
[Steenbrugge, K. C.] Univ Catolica Norte, Inst Astron, Antofagasta, Chile.
[Steenbrugge, K. C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, 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.
[Bianchi, S.; Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Boissay, R.; Paltani, S.] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland.
[Ebrero, J.] European Space Astron Ctr, Madrid 28691, Spain.
[Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[De Marco, B.; Ponti, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Peterson, B. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Peterson, B. M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Nunez, F. Pozo] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[De Rosa, A.] INAF IAPS, I-00133 Rome, Italy.
[Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mehdipour, M (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM M.Mehdipour@sron.nl
RI Bianchi, Stefano/B-4804-2010;
OI Bianchi, Stefano/0000-0002-4622-4240; De Rosa,
Alessandra/0000-0001-5668-6863
FU ESA Member States; USA (NASA); NASA; ESA member states (especially the
PI countries: Denmark, France, Germany, Italy, Switzerland, Spain),
Czech Republic, and Poland; International Space Science Institute (ISSI)
in Bern; NWO; Netherlands Organization for Scientific Research;
ordrhein-Westfalische Akademie der Wissenschaften und der Kunste in the
framework of the academy program by the Federal Republic of Germany;
state Nordrhein-Westfalen; UK STFC; NASA through grants for HST program
from the Space Telescope Science Institute [13184]; Association of
Universities for Research in Astronomy, Incorporated, under NASA
[NAS5-26555]; PRIN INAF; CNES; CNRS/PICS; Fondo Fortalecimiento de la
Productividad Cientifica VRIDT; ISF, MoST [1163/10]; iCORE program;
INAF/PICS; Italian Space Agency [ASI/INAF I/037/12/0-011/13]; US NSF
[AST-1008882]; EU Marie Curie Intra-European fellowship
[FP-PEOPLE-2012-IEF-331095]; Bundesministerium fur Wirtschaft und
Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR) [FKZ 50
OR 1408]; VINCI program of the French-Italian University; [ASI/INAF
n.I/037/12/0]
FX 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. It is also based on observations
with INTEGRAL, an ESA project with instrument and science data centre
funded by ESA member states (especially the PI countries: Denmark,
France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland
and with the participation of Russia and the USA. This work made use of
data supplied by the UK Swift Science Data Centre at the University of
Leicester. We thank the Chandra team for allocating the LETGS triggered
observations. 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. This
publication is supported as a project of the Nordrhein-Westfalische
Akademie der Wissenschaften und der Kunste in the framework of the
academy program by the Federal Republic of Germany and the state
Nordrhein-Westfalen. 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. is supported by grants from
the ISF, MoST (1163/10), and the iCORE program. 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. We thank the anonymous referee for their useful suggestions and
comments.
NR 87
TC 20
Z9 20
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2015
VL 575
AR A22
DI 10.1051/0004-6361/201425373
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3LA
UT WOS:000350249100022
ER
PT J
AU Pierbattista, M
Harding, AK
Grenier, IA
Johnson, TJ
Caraveo, PA
Kerr, M
Gonthier, PL
AF Pierbattista, M.
Harding, A. K.
Grenier, I. A.
Johnson, T. J.
Caraveo, P. A.
Kerr, M.
Gonthier, P. L.
TI Light-curve modelling constraints on the obliquities and aspect angles
of the young Fermi pulsars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; pulsars: general; gamma rays: stars; radiation
mechanisms: non-thermal; methods: statistical
ID GAMMA-RAY PULSARS; LARGE-AREA TELESCOPE; SLOT GAPS; MILLISECOND PULSARS;
SPACE-TELESCOPE; EMISSION; POPULATION; RADIO; GEOMETRY; ACCELERATION
AB In more than four years of observation the Large Area Telescope on board the Fermi satellite has identified pulsed gamma-ray emission from more than 80 young or middle-aged pulsars, in most cases providing light curves with high statistics. Fitting the observed profiles with geometrical models can provide estimates of the magnetic obliquity alpha and of the line of sight angle zeta, yielding estimates of the radiation beaming factor and radiated luminosity.
Using different gamma-ray emission geometries (Polar Cap, Slot Gap, Outer Gap, One Pole Caustic) and core plus cone geometries for the radio emission, we fit gamma-ray light curves for 76 young or middle-aged pulsars and we jointly fit their gamma-ray plus radio light curves when possible.
We find that a joint radio plus gamma-ray fit strategy is important to obtain (alpha,zeta) estimates that can explain simultaneously detectable radio and gamma-ray emission: when the radio emission is available, the inclusion of the radio light curve in the fit leads to important changes in the (alpha,zeta) solutions. The most pronounced changes are observed for Outer Gap and One Pole Caustic models for which the gamma-ray only fit leads to underestimated alpha or zeta when the solution is found to the left or to the right of the main alpha-zeta plane diagonal respectively. The intermediate-to-high altitude magnetosphere models, Slot Gap, Outer Gap, and One pole Caustic, are favoured in explaining the observations. We find no apparent evolution of a on a time scale of 10(6) years. For all emission geometries our derived gamma-ray beaming factors are generally less than one and do not significantly evolve with the spin-down power. A more pronounced beaming factor vs. spin-down power correlation is observed for Slot Gap model and radio-quiet pulsars and for the Outer Gap model and radio-loud pulsars. The beaming factor distributions exhibit a large dispersion that is less pronounced for the Slot Gap case and that decreases from radio-quiet to radio-loud solutions. For all models, the correlation between gamma-ray luminosity and spin-down power is consistent with a square root dependence. The gamma-ray luminosities obtained by using the beaming factors estimated in the framework of each model do not exceed the spin-down power. This suggests that assuming a beaming factor of one for all objects, as done in other studies, likely overestimates the real values. The data show a relation between the pulsar spectral characteristics and the width of the accelerator gap. The relation obtained in the case of the Slot Gap model is consistent with the theoretical prediction.
C1 [Pierbattista, M.] Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Pierbattista, M.; Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
[Pierbattista, M.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, Francois Arago Ctr,APC,CNRS IN2P3,CEA Irfu, F-75205 Paris 13, France.
[Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Grenier, I. A.] Univ Paris Diderot, CEA Saclay, CEA IRFU CNRS, Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Grenier, I. A.] Inst Univ France, Paris, France.
[Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Caraveo, P. A.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy.
[Kerr, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Gonthier, P. L.] Hope Coll, Dept Phys, Holland, MI 49423 USA.
RP Pierbattista, M (reprint author), Nicolaus Copernicus Astron Ctr, Rabianska 8, PL-87100 Torun, Poland.
EM mpierba@gmail.com
OI Caraveo, Patrizia/0000-0003-2478-8018
NR 42
TC 10
Z9 10
U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2015
VL 575
AR A3
DI 10.1051/0004-6361/201423815
PG 88
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3LA
UT WOS:000350249100003
ER
PT J
AU Podigachoski, P
Barthel, PD
Haas, M
Leipski, C
Wilkes, B
Kuraszkiewicz, J
Westhues, C
Willner, SP
Ashby, MLN
Chini, R
Clements, DL
Fazio, GG
Labiano, A
Lawrence, C
Meisenheimer, K
Peletier, RF
Siebenmorgen, R
Kleijn, GV
AF Podigachoski, P.
Barthel, P. D.
Haas, M.
Leipski, C.
Wilkes, B.
Kuraszkiewicz, J.
Westhues, C.
Willner, S. P.
Ashby, M. L. N.
Chini, R.
Clements, D. L.
Fazio, G. G.
Labiano, A.
Lawrence, C.
Meisenheimer, K.
Peletier, R. F.
Siebenmorgen, R.
Kleijn, G. Verdoes
TI Star formation in z > 1 3CR host galaxies as seen by Herschel
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; galaxies: star formation;
infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; REDSHIFT RADIO
GALAXIES; SPITZER-SPACE-TELESCOPE; FAR-INFRARED PROPERTIES; OLD STELLAR
POPULATIONS; CLUMPY TORUS MODELS; SUBMILLIMETER GALAXIES; DUST EMISSION;
BLACK-HOLE
AB We present Herschel (PACS and SPIRE) far-infrared (FIR) photometry of a complete sample of z > 1 3CR sources, from the Herschel guaranteed time project The Herschel Legacy of distant radio-loud AGN. Combining these with existing Spitzer photometric data, we perform an infrared (1.12) spectral energy distribution (SED) analysis of these landmark objects in extragalactic research to study the star formation in the hosts of some of the brightest active galactic nuclei (A(iN) known at any epoch. Accounting for the contribution from an AGN-powered warm dust component to the IR SED, about 40% of our objects undergo episodes of prodigious. ULIRG-strength star formation, with rates of hundreds of solar masses per year, coeval with the growth of the central supermassive black hole. Median SEDs imply that the quasar and radio galaxy hosts have similar FIR properties, in agreement with the orientation-based unification for radio-loud AGN. The star-forming properties of the AGN hosts are similar to those of the general population of equally massive non-AGN galaxies at comparable redshifts, thus there is no strong evidence of universal quenching of star formation (negative feedback) within this sample. Massive galaxies at high redshift may be forming stars prodigiously, regardless of whether their superm.assive black holes are accreting or not.
C1 [Podigachoski, P.; Barthel, P. D.; Peletier, R. F.; Kleijn, G. Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands.
[Haas, M.; Westhues, C.; Chini, R.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Leipski, C.; Meisenheimer, K.] MPIA, D-69117 Heidelberg, Germany.
[Wilkes, B.; Kuraszkiewicz, J.; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Labiano, A.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Lawrence, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Siebenmorgen, R.] European So Observ, D-85748 Garching, Germany.
RP Podigachoski, P (reprint author), Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands.
EM podigachoski@astro.rug.nl
FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); Akademie
der Wissenschaften und der Kunste Nordrhein-Westfalen; Deutsches Zentrum
fur Luft-und Raumfahrt (DLR); Thales Alenia Space (Cannes); BMVIT
(Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA
(France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB
(Sweden); STFC (UK); UKSA (UK); NASA (USA); NASA; National Aeronautics
and Space Administration
FX The authors acknowledge the expert referee for useful comments which
improved the paper, and thank Giulia Rodighiero for kindly providing the
PEP data from the deep GOODS South Odd. P.P. acknowledges the
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) for a
Ph.D. fellowship. M.H. and C.W. are supported by the Akademie der
Wissenschaften und der Kunste Nordrhein-Westfalen and by Deutsches
Zentrum fur Luft-und Raumfahrt (DLR). The Herschel spacecraft was
designed, built, tested, and launched under a contract to ESA managed by
the Herschel/Planck Project team by an industrial consortium under the
overall responsibility of the prime contractor Thales Alenia Space
(Cannes), and including Astrium (Friedrichshafen) responsible for the
payload module and for system testing at spacecraft level, Thales Alenia
Space (Turin) responsible for the service module, and Astrium (Toulouse)
responsible for the telescope, with in excess of a hundred
subcontractors. PACS has been developed by a consortium of institutes
led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC
(Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT,
LENS, SISSA (Italy); IAC (Spain). This development has been supported by
the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES
(France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE
has been developed by a consortium of institutes led by Cardiff
University (UK) and including Univ. Lethbridge (Canada); NAOC (China);
CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,
Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). HIPE is a joint
development by the Herschel Science Ground Segment Consortium,
consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS
and SPIRE consortia. This work is partly based on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. This research has made use of the NASA/IPAC Extragalactic Database
(NED) which is operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. This research made use of APLpy, an
open-source plotting package for Python hosted at
http://aplpy.github.com
NR 106
TC 15
Z9 15
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2015
VL 575
AR UNSP A80
DI 10.1051/0004-6361/201425137
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3LA
UT WOS:000350249100080
ER
PT J
AU Cook, BI
Shukla, SP
Puma, MJ
Nazarenko, LS
AF Cook, Benjamin I.
Shukla, Sonali P.
Puma, Michael J.
Nazarenko, Larissa S.
TI Irrigation as an historical climate forcing
SO CLIMATE DYNAMICS
LA English
DT Article
DE Climate modeling; Irrigation; Forcing; Historical simulations
ID LAND-COVER CHANGE; GROUNDWATER DEPLETION; CENTRAL VALLEY; GISS MODELE2;
HIGH-PLAINS; CMIP5; ATMOSPHERE; IMPACT; SIMULATIONS; TEMPERATURE
AB Irrigation is the single largest anthropogenic water use, a modification of the land surface that significantly affects surface energy budgets, the water cycle, and climate. Irrigation, however, is typically not included in standard historical general circulation model (GCM) simulations along with other anthropogenic and natural forcings. To investigate the importance of irrigation as an anthropogenic climate forcing, we conduct two 5-member ensemble GCM experiments. Both are setup identical to the historical forced (anthropogenic plus natural) scenario used in version 5 of the Coupled Model Intercomparison Project, but in one experiment we also add water to the land surface using a dataset of historically estimated irrigation rates. Irrigation has a negligible effect on the global average radiative balance at the top of the atmosphere, but causes significant cooling of global average surface air temperatures over land and dampens regional warming trends. This cooling is regionally focused and is especially strong in Western North America, the Mediterranean, the Middle East, and Asia. Irrigation enhances cloud cover and precipitation in these same regions, except for summer in parts of Monsoon Asia, where irrigation causes a reduction in monsoon season precipitation. Irrigation cools the surface, reducing upward fluxes of longwave radiation (increasing net longwave), and increases cloud cover, enhancing shortwave reflection (reducing net shortwave). The relative magnitude of these two processes causes regional increases (northern India) or decreases (Central Asia, China) in energy availability at the surface and top of the atmosphere. Despite these changes in net radiation, however, climate responses are due primarily to larger magnitude shifts in the Bowen ratio from sensible to latent heating. Irrigation impacts on temperature, precipitation, and other climate variables are regionally significant, even while other anthropogenic forcings (anthropogenic aerosols, greenhouse gases, etc.) dominate the long term climate evolution in the simulations. To better constrain the magnitude and uncertainties of irrigation-forced climate anomalies, irrigation should therefore be considered as another important anthropogenic climate forcing in the next generation of historical climate simulations and multimodel assessments.
C1 [Cook, Benjamin I.; Shukla, Sonali P.; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Puma, Michael J.] Columbia Univ, Earth Inst, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012;
OI Puma, Michael/0000-0002-4255-8454
FU NASA [NNX08AJ75A]
FX Simulations with the GISS ModelE2-R were made possible by the NASA
High-End Computing (HEC) Program through the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. Development of
ModelE2-R was supported by the NASA Modeling, Analysis and Prediction
(MAP) Program. Funding support for BIC provided by NASA. The authors
gratefully acknowledge funding for Interdisciplinary Global Change
Research under NASA cooperative agreement NNX08AJ75A supported by the
NASA Climate and Earth Observing Program. Two anonymous reviewers
provided valuable comments that improved the quality of this manuscript.
LDEO Publication number #. Lamont contribution #7808.
NR 49
TC 12
Z9 12
U1 4
U2 38
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 MAR
PY 2015
VL 44
IS 5-6
BP 1715
EP 1730
DI 10.1007/s00382-014-2204-7
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC4ZC
UT WOS:000350364500032
ER
PT J
AU Johnston, JC
Ruthruff, E
Lien, MC
AF Johnston, James C.
Ruthruff, Eric
Lien, Mei-Ching
TI Visual Information Processing From Multiple Displays
SO HUMAN FACTORS
LA English
DT Article
DE peripheral detection; aviation; attention; dual task; situation
awareness; monitoring; vigilance
ID ATTENTIONAL CONTROL SETTINGS; EVENT-RELATED POTENTIALS; CHRONOMETRIC
EVIDENCE; CAPTURE; SEARCH; INTERFERENCE; CONTINGENT; PERCEPTION; ONSETS;
TASKS
AB Objective: In this study, we examined how effectively people can monitor new stimuli on a peripheral display while carrying out judgments on an adjacent central display.
Background: Improved situation awareness is critical for improved operator performance in aviation and many other domains. Given the limited extent of foveal processing, acquiring additional information from peripheral vision offers high potential gains.
Method: Participants carried out a sequence of central perceptual judgments while simultaneously monitoring the periphery for new stimuli. Peripheral detection was measured as a function of central-judgment difficulty, the relative timing of the two tasks, and peripheral event rate.
Results: Participants accurately detected and located peripheral targets, even at the highest eccentricity explored here (30 degrees). Peripheral detection was not reduced by increased central-task difficulty but was reduced when peripheral targets arrived later in the processing of central stimuli and when peripheral events were relatively rare.
Conclusion: Under favorable conditionshigh-contrast stimuli and high event ratepeople can successfully monitor peripheral displays for new events while carrying out an unrelated continuous task on an adjacent display.
Application: In many fields, such as aviation, existing displays were designed with low-contrast stimuli that provide little opportunity for peripheral vision. With appropriate redesign, operators might successfully monitor multiple displays over a large visual field. Designers need to be aware of nonvisual factors, such as low event rate and relative event timing, that can lead to failures to detect peripheral stimuli.
C1 [Johnston, James C.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
[Ruthruff, Eric] Univ New Mexico, Dept Psychol, Albuquerque, NM 87131 USA.
[Lien, Mei-Ching] Oregon State Univ, Sch Psychol Sci, Corvallis, OR 97331 USA.
RP Johnston, JC (reprint author), NASA, Ames Res Ctr, MS 262-4, Moffett Field, CA 94035 USA.
EM James.C.Johnston@nasa.gov
FU NASA Aviation Safety program
FX This research was supported by the NASA Aviation Safety program; we
thank especially Michael Feary, Kara Latorella, Randy Bailey, and
Jessica Nowinsky for their assistance. We also thank Eric Adamic and
Eamon Dick for their help running the experiments.
NR 31
TC 2
Z9 2
U1 2
U2 15
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0018-7208
EI 1547-8181
J9 HUM FACTORS
JI Hum. Factors
PD MAR
PY 2015
VL 57
IS 2
BP 276
EP 297
DI 10.1177/0018720814545974
PG 22
WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology,
Applied; Psychology
SC Behavioral Sciences; Engineering; Psychology
GA CD0KO
UT WOS:000350761600008
PM 25850158
ER
PT J
AU Wissa, A
Grauer, J
Guerreiro, N
Hubbard, J
Altenbuchner, C
Tummala, Y
Frecker, M
Roberts, R
AF Wissa, Aimy
Grauer, Jared
Guerreiro, Nelson
Hubbard, James, Jr.
Altenbuchner, Cornelia
Tummala, Yashwanth
Frecker, Mary
Roberts, Richard
TI Free Flight Testing and Performance Evaluation of a Passively Morphing
Ornithopter
SO INTERNATIONAL JOURNAL OF MICRO AIR VEHICLES
LA English
DT Article
ID MICRO-AIR VEHICLES
AB Unmanned Aerial Vehicles (UAVs) are proliferating in both the civil and military markets. Flapping wing UAVs, or ornithopters, have the potential to combine the agility and maneuverability of rotary wing aircraft with excellent performance in the low Reynolds number flight regimes. The purpose of this paper is to present new free flight experimental results for an ornithopter equipped with single degree of freedom compliant spines. The compliant spines are designed and optimized in terms of mass, maximum von-Mises stress, and desired wing bending deflections. The spines are inserted in an experimental ornithopter wing leading edge spar, in order to achieve a set of desired kinematics during the up and down strokes of a flapping cycle. The ornithopter is flown at Wright Patterson Air Force Base in the Air Force Research Laboratory Small Unmanned Air Systems (SUAS) indoor flight facility. Vicon (R) motion tracking cameras are used to track the motion of the vehicle for four different wing configurations. The effect of the presence of the compliant spine on the wings and body kinematics, as well as the leading edge spar deflection during free flight is presented in this paper. Several metrics were used to evaluate the vehicle performance with various compliant spine designs inserted in the leading edge spar of the wings. Results show that passively morphing the wings, via adding compliance in the leading edge spar, does not require additional power expenditure and is beneficial to the overall vertical and horizontal propulsive force production.
C1 [Wissa, Aimy] Univ Illinois, Urbana, IL 61801 USA.
[Grauer, Jared] NASA, Langley Res Ctr, Dynam Syst & Controls Branch, Hampton, VA 23681 USA.
[Guerreiro, Nelson; Hubbard, James, Jr.; Altenbuchner, Cornelia] Univ Maryland, Hampton, VA 23666 USA.
[Tummala, Yashwanth; Frecker, Mary] Penn State Univ, University Pk, PA 18602 USA.
RP Wissa, A (reprint author), Univ Illinois, 1206 West Green St, Urbana, IL 61801 USA.
EM awissa@illinois.edu; jared.a.grauer@nasa.gov; nelsong@umd.edu;
jhubbard@nianet.org; cornelia.altenbuchner@nasa.gov; yash@psu.edu;
mxf36@psu.edu
RI Wissa, Aimy/C-5844-2016
OI Wissa, Aimy/0000-0002-8468-511X
FU AFOSR [FA9550-09-1-0632, FA9550-13-0126]; National Science Foundation
[OCI-0821527]
FX The authors gratefully acknowledge the support of AFOSR grants numbers
FA9550-09-1-0632 and FA9550-13-0126 and the support of the AFOSR program
manager, David Stargel. The computational work needed to design the
compliant spines was supported in part through instrumentation funded by
the National Science Foundation through grant OCI-0821527. Also the
authors are very thankful to the AFRL indoor flight lab team especially
Gregory Reich and Gregory Parker for their support during the flight
testing. The resources of the NASA Langley Research Center, Pennsylvania
State University, the University of Maryland and the Morpheus Lab are
also appreciated.
NR 24
TC 2
Z9 2
U1 2
U2 30
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 1756-8293
J9 INT J MICRO AIR VEH
JI Int. J. Micro Air Veh.
PD MAR
PY 2015
VL 7
IS 1
BP 21
EP 40
DI 10.1260/1756-8293.7.1.21
PG 20
WC Engineering, Aerospace
SC Engineering
GA CD5NC
UT WOS:000351133800002
ER
PT J
AU Stanfield, RE
Dong, XQ
Xi, BK
Del Genio, AD
Minnis, P
Doelling, D
Loeb, N
AF Stanfield, Ryan E.
Dong, Xiquan
Xi, Baike
Del Genio, Anthony D.
Minnis, Patrick
Doelling, David
Loeb, Norman
TI Assessment of NASA GISS CMIP5 and Post-CMIP5 Simulated Clouds and TOA
Radiation Budgets Using Satellite Observations. Part II: TOA Radiation
Budget and CREs
SO JOURNAL OF CLIMATE
LA English
DT Article
ID ENERGY SYSTEM INSTRUMENT; ANGULAR-DISTRIBUTION MODELS; OF-ATMOSPHERE
SHORTWAVE; TEMPORAL INTERPOLATION; FLUX ESTIMATION; CLIMATE; CERES;
EARTH; METHODOLOGY; IRRADIANCE
AB In Part I of this study, the NASA GISS Coupled Model Intercomparison Project (CMIP5) and post-CMIP5 (herein called C5 and P5, respectively) simulated cloud properties were assessed utilizing multiple satellite observations, with a particular focus on the southern midlatitudes (SMLs). This study applies the knowledge gained from Part I of this series to evaluate the modeled TOA radiation budgets and cloud radiative effects (CREs) globally using CERES EBAF (CE) satellite observations and the impact of regional cloud properties and water vapor on the TOA radiation budgets. Comparisons revealed that the P5- and C5-simulated global means of clear-sky and all-sky outgoing longwave radiation (OLR) match well with CE observations, while biases are observed regionally. Negative biases are found in both P5- and C5-simulated clear-sky OLR. P5-simulated all-sky albedo slightly increased over the SMLs due to the increase in low-level cloud fraction from the new planetary boundary layer (PBL) scheme. Shortwave, longwave, and net CRE are quantitatively analyzed as well. Regions of strong large-scale atmospheric upwelling/downwelling motion are also defined to compare regional differences across multiple cloud and radiative variables. In general, the P5 and C5 simulations agree with the observations better over the downwelling regime than over the upwelling regime. Comparing the results herein with the cloud property comparisons presented in Part I, the modeled TOA radiation budgets and CREs agree well with the CE observations. These results, combined with results in Part I, have quantitatively estimated how much improvement is found in the P5-simulated cloud and radiative properties, particularly over the SMLs and tropics, due to the implementation of the new PBL and convection schemes.
C1 [Stanfield, Ryan E.; Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Minnis, Patrick; Doelling, David; Loeb, Norman] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
OI Dong, Xiquan/0000-0002-3359-6117
FU NASA EPSCoR CAN [NNX11AM15A]; NASA CERES at the University of North
Dakota [NNX10AI05G]; NASA CloudSatICALIPSO and Modeling and Analysis
Program RTOPs at NASA/GISS
FX This work was supported by NASA EPSCoR CAN under Grant NNX11AM15A, NASA
CERES project under Grant NNX10AI05G at the University of North Dakota,
and by the NASA CloudSatICALIPSO and Modeling and Analysis Program RTOPs
at NASA/GISS. NASA GISS-E2 Post-CMIP5 GCM diagnostic run data are
provided by NASA GISS directly. NASA GISS-E2 CMIP5 GCM data are provided
by NASA GISS through the CMIP5 ESGF PCMDI database at
http://pcmdi9.llnl.gov/esgf-web-fe/. The simulations were performed at
the NASA Center for Climate Simulation at the Goddard Space Flight
Center. CERES EBAF products used in this study are produced by the NASA
CERES Team, available at http://ceres.larc.nasa.gov.
NR 47
TC 4
Z9 4
U1 2
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAR 1
PY 2015
VL 28
IS 5
BP 1842
EP 1864
DI 10.1175/JCLI-D-14-00249.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD1MP
UT WOS:000350839300007
ER
PT J
AU Guo, YJ
Waliser, DE
Jiang, XN
AF Guo, Yanjuan
Waliser, Duane E.
Jiang, Xianan
TI A Systematic Relationship between the Representations of Convectively
Coupled Equatorial Wave Activity and the Madden-Julian Oscillation in
Climate Model Simulations
SO JOURNAL OF CLIMATE
LA English
DT Article
ID TROPICAL CONVECTION; KELVIN WAVES; PART I; INTRASEASONAL OSCILLATIONS;
MOMENTUM TRANSPORT; MULTISCALE MODELS; WESTERN PACIFIC; FORECAST SYSTEM;
INDIAN-OCEAN; MJO
AB The relationship between a model's performance in simulating the Madden-Julian oscillation (MJO) and convectively coupled equatorial wave (CCEW) activity during wintertime is examined by analyzing precipitation from 26 general circulation models (GCMs) participating in the MJO Task Force/Global Energy and Water Cycle Experiment (GEWEX) Atmospheric System Study (GASS) MJO model intercomparison project as well as observations based on the Tropical Rainfall Measuring Mission (TRMM). A model's performance in simulating the MJO is determined by how faithfully it reproduces the eastward propagation of the large-scale intraseasonal variability (ISV) compared to TRMM observations. Results suggest that models that simulate a better MJO tend to 1) have higher fractional variances for various high-frequency wave modes (Kelvin, mixed Rossby-gravity, and westward and eastward inertio-gravity waves), which are defined by the ratios of wave variances of specific wave modes to the "total" variance, and 2) exhibit stronger CCEW variances in association with the eastward-propagating ISV precipitation anomalies for these high-frequency wave modes. The former result is illustrative of an alleviation in the good MJO models of the widely reported GCM deficiency in simulating the correct distribution of variance in tropical convection [i.e., typically too weak (strong) variance in the high- (low-) frequency spectrum of the precipitation]. The latter suggests better coherence and stronger interactions between these aforementioned high-frequency CCEWs and the ISV envelope in good MJ0 models. Both factors likely contribute to the improved simulation of the MJO in a GCM.
C1 [Guo, Yanjuan; Waliser, Duane E.; Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Guo, YJ (reprint author), CALTECH, Jet Prop Lab, M-S 233-304,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yguo@jifresse.ucla.edu
FU Marine Meteorology Program of the Office of Naval Research
[ONRBAA12-001]; NSF Climate and Large-Scale Dynamics Program
[AGS-1221013, AGS-1228302]; NOAA MAPP Program [NA12OAR4310075]
FX The authors thank three anonymous reviewers for their helpful comments
on earlier versions of this paper. This work was supported by the Marine
Meteorology Program of the Office of Naval Research under Project
ONRBAA12-001, the NSF Climate and Large-Scale Dynamics Program under
Awards AGS-1221013 and AGS-1228302, and the NOAA MAPP Program under
Award NA12OAR4310075. The contribution from DEW to this study was
performed on behalf of the Joint Institute for Regional Earth Science
and Engineering (JIFRESSE) at the University of California, Los Angeles,
and the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 81
TC 2
Z9 2
U1 0
U2 11
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 MAR 1
PY 2015
VL 28
IS 5
BP 1881
EP 1904
DI 10.1175/JCLI-D-14-00485.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD1MP
UT WOS:000350839300009
ER
PT J
AU Coats, S
Cook, BI
Smerdon, JE
Seager, R
AF Coats, Sloan
Cook, Benjamin I.
Smerdon, Jason E.
Seager, Richard
TI North American Pancontinental Droughts in Model Simulations of the Last
Millennium
SO JOURNAL OF CLIMATE
LA English
DT Article
ID UNITED-STATES; GREAT-PLAINS; CLIMATE; PACIFIC; VARIABILITY; ATLANTIC;
US; RECONSTRUCTIONS; OSCILLATION; CMIP5
AB Pancontinental droughts in North America, or droughts that simultaneously affect a large percentage of the geographically and climatically distinct regions of the continent, present significant on-the-ground management challenges and, as such, are an important target for scientific research. The methodology of paleoclimate-model data comparisons is used herein to provide a more comprehensive understanding of pancontinental drought dynamics. Models are found to simulate pancontinental drought with the frequency and spatial patterns exhibited by the paleoclimate record. They do not, however, agree on the modes of atmosphere ocean variability that produce pancontinental droughts because simulated El Nino-Southern Oscillation (ENSO), Pacific decadal oscillation (PDO), and Atlantic multidecadal oscillation (AMO) dynamics, and their teleconnections to North America, are different between models and observations. Despite these dynamical differences, models are able to reproduce large-magnitude centennial-scale variability in the frequency of pancontinental drought occurrence an important feature of the paleoclimate record. These changes do not appear to be tied to exogenous forcing, suggesting that simulated internal hydroclimate variability on these time scales is large in magnitude. Results clarify our understanding of the dynamics that produce real-world pancontinental droughts while assessing the ability of models to accurately characterize future drought risks.
C1 [Coats, Sloan; Cook, Benjamin I.; Smerdon, Jason E.; Seager, Richard] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Coats, Sloan] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Coats, S (reprint author), Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10964 USA.
EM sjc2164@columbia.edu
RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012
FU NOAA [NA10OAR4310137, NA11OAR4310166]; NSF [AGS-1243204, AGS-1401400]
FX This work was supported by NOAA Awards NA10OAR4310137 (Global Decadal
Hydroclimate Variability and Change, GloDecH) and NA11OAR4310166, as
well as NSF Awards AGS-1243204 and AGS-1401400. We acknowledge the World
Climate Research Programme's Working Group on Coupled Modelling, which
is responsible for CMIP, and we thank the climate modeling groups
(listed in Table 1) for producing and making available their model
output. For CMIP, the Department of Energy's Program for Climate Model
Diagnosis and Intercomparison provides coordinating support and led the
development of the software infrastructure in partnership with the
Global Organization for Earth System Science Portal. We also thank Haibo
Liu and Naomi Henderson for their considerable computational and data
management support.
NR 57
TC 10
Z9 10
U1 4
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAR 1
PY 2015
VL 28
IS 5
BP 2025
EP 2043
DI 10.1175/JCLI-D-14-00634.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD1MP
UT WOS:000350839300016
ER
PT J
AU Loikith, PC
Broccoli, AJ
AF Loikith, Paul C.
Broccoli, Anthony J.
TI Comparison between Observed and Model-Simulated Atmospheric Circulation
Patterns Associated with Extreme Temperature Days over North America
Using CMIP5 Historical Simulations
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SELF-ORGANIZING MAPS; UNITED-STATES; HEAT WAVES; PRECIPITATION;
20TH-CENTURY; EVENTS; 21ST-CENTURY; VARIABILITY; 2ND-HALF; ENSEMBLE
AB Circulation patterns associated with extreme temperature days over North America, as simulated by a suite of climate models, are compared with those obtained from observations. The authors analyze 17 coupled atmosphere ocean general circulation models contributing to the fifth phase of the Coupled Model Intercomparison Project. Circulation patterns are defined as composites of anomalies in sea level pressure and 500-hPa geopotential height concurrent with days in the tails of temperature distribution. Several metrics used to systematically describe circulation patterns associated with extreme temperature days are applied to both the observed and model-simulated data. Additionally, self-organizing maps are employed as a means of comparing observed and model-simulated circulation patterns across the North American domain. In general, the multimodel ensemble resembles the observed patterns well, especially in areas removed from complex geographic features (e.g., mountains and coastlines). Individual model results vary; however, the majority of models capture the major features observed. The multimodel ensemble captures several key features, including regional variations in the strength and orientation of atmospheric circulation patterns associated with extreme temperatures, both near the surface and aloft, as well as variations with latitude and season. The results from this work suggest that these models can be used to comprehensively examine the role that changes in atmospheric circulation will play in projected changes in temperature extremes because of future anthropogenic climate warming.
C1 [Loikith, Paul C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Broccoli, Anthony J.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
RP Loikith, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-233, Pasadena, CA 91109 USA.
EM paul.c.loikith@jpl.nasa.gov
RI Broccoli, Anthony/D-9186-2014
OI Broccoli, Anthony/0000-0003-2619-1434
FU Office of Science (BER), U.S. Department of Energy [DE-SC0005467]
FX This study was supported by the Office of Science (BER), U.S. Department
of Energy, Award DE-SC0005467. This work was done as a private venture
and not in the author's capacity as an employee of the Jet Propulsion
Laboratory, California Institute of Technology.
NR 40
TC 2
Z9 2
U1 3
U2 10
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 MAR 1
PY 2015
VL 28
IS 5
BP 2063
EP 2079
DI 10.1175/JCLI-D-13-00544.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD1MP
UT WOS:000350839300018
ER
PT J
AU Garrabos, Y
Lecoutre, C
Marre, S
Guillaument, R
Beysens, D
Hahn, I
AF Garrabos, Y.
Lecoutre, C.
Marre, S.
Guillaument, R.
Beysens, D.
Hahn, I.
TI Crossover Equation of State Models Applied to the Critical Behavior of
Xenon
SO JOURNAL OF STATISTICAL PHYSICS
LA English
DT Article
DE Critical crossover function; Parametric equation of state; Turbidity;
Xenon
ID LIQUID CRITICAL-POINT; THERMODYNAMIC BEHAVIOR; CRITICAL EXPONENTS;
CORRELATION RANGE; CRITICAL REGION; FLUIDS; DENSITY; FLUCTUATIONS;
SCATTERING; XE
AB The turbidity () measurements of Guttinger and Cannell (Phys Rev A 24:3188-3201, 1981) in the temperature range along the critical isochore of homogeneous xenon are reanalyzed. The singular behaviors of the isothermal compressibility () and the correlation length () predicted from the master crossover functions are introduced in the turbidity functional form derived by Puglielli and Ford (Phys Rev Lett 25:143-146, 1970). We show that the turbidity data are thus well represented by the Ornstein-Zernike approximant, within 1 % precision. We also introduce a new crossover master model (CMM) of the parametric equation of state for a simple fluid system with no adjustable parameter. The CMM model and the phenomenological crossover parametric model are compared with the turbidity data and the coexisting liquid-gas density difference (). The excellent agreement observed for , , , and in a finite temperature range well beyond the Ising-like preasymptotic domain confirms that the Ising-like critical crossover behavior of xenon can be described in conformity with the universal features estimated by the renormalization-group methods. Only 4 critical coordinates of the vapor-liquid critical point are needed in the (pressure, temperature, molecular volume) phase surface of xenon.
C1 [Garrabos, Y.; Lecoutre, C.; Marre, S.; Guillaument, R.] CNRS, ICMCB ESEME, UPR 9048, F-33600 Pessac, France.
[Garrabos, Y.; Lecoutre, C.; Marre, S.; Guillaument, R.] Univ Bordeaux, ICMCB, UPR 9048, F-33600 Pessac, France.
[Beysens, D.] Univ Paris Diderot, Univ Paris 06, Phys & Mecan Milieux Heterogenes, ESEME CEA,ESPCI,UMR CNRS 7636, F-75005 Paris, France.
[Beysens, D.] UJF Grenoble 1, INAC, UMR E CEA, Serv Basses Temp, Grenoble, France.
[Hahn, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Garrabos, Y (reprint author), Univ Bordeaux, ICMCB, UPR 9048, F-33600 Pessac, France.
EM garrabos@icmcb-bordeaux.cnrs.fr; dbeysens@cea.fr;
inseob.hahn@jpl.nasa.gov
RI Lecoutre, Carole/H-3367-2013; Garrabos, Yves/H-5404-2013; Marre,
Samuel/H-3377-2013
FU CNRS; CNES; NASA
FX We acknowledge discussions and helpful comments from M. A. Anisimov. YG
acknowledges F. Palencia for its contribution in the data analyses using
Mathematica. The research at ICMCB and PMMH was supported by CNRS and
CNES, and at the Jet Propulsion Laboratory, California Institute of
Techology, by NASA.
NR 72
TC 4
Z9 4
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-4715
EI 1572-9613
J9 J STAT PHYS
JI J. Stat. Phys.
PD MAR
PY 2015
VL 158
IS 6
BP 1379
EP 1412
DI 10.1007/s10955-014-1157-x
PG 34
WC Physics, Mathematical
SC Physics
GA CD1IC
UT WOS:000350827300008
ER
PT J
AU Strom, RG
Malhotra, R
Xiao, ZY
Ito, T
Yoshida, F
Ostrach, LR
AF Strom, Robert G.
Malhotra, Renu
Xiao, Zhi-Yong
Ito, Takashi
Yoshida, Fumi
Ostrach, Lillian R.
TI The inner solar system cratering record and the evolution of impactor
populations
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE solar system: formation; minor planets, asteroids; Earth; Moon
ID MAIN-BELT ASTEROIDS; LUNAR CATACLYSM IMPACTORS; LATE HEAVY BOMBARDMENT;
NEAR-EARTH ASTEROIDS; COLLISIONAL EVOLUTION; TERRESTRIAL PLANETS; GLOBAL
DISTRIBUTION; SIZE DISTRIBUTION; MELT BRECCIAS; MARE BASALTS
AB We review previously published and newly obtained crater size-frequency distributions in the inner solar system. These data indicate that the Moon and the terrestrial planets have been bombarded by two populations of objects. Population 1, dominating at early times, had nearly the same size distribution as the present-day asteroid belt, and produced heavily cratered surfaces with a complex, multi-sloped crater size-frequency distribution. Population 2, dominating since about 3.8-3.7 Gyr, had the same size distribution as near-Earth objects (NEOs) and a much lower impact flux, and produced a crater size distribution characterized by a differential -3 single-slope power law in the crater diameter range 0.02 km to 100 km. Taken together with the results from a large body of work on age-dating of lunar and meteorite samples and theoretical work in solar system dynamics, a plausible interpretation of these data is as follows. The NEO population is the source of Population 2 and it has been in near-steady state over the past similar to 3.7-3.8 Gyr; these objects are derived from the main asteroid belt by size-dependent non-gravitational effects that favor the ejection of smaller asteroids. However, Population 1 was composed of main belt asteroids ejected from their source region in a size-independent manner, possibly by means of gravitational resonance sweeping during orbit migration of giant planets; this caused the so-called Late Heavy Bombardment (LHB). The LHB began some time before similar to 3.9 Gyr, peaked and declined rapidly over the next similar to 100 to 300 Myr, and possibly more slowly from about 3.8-3.7 Gyr to similar to 2 Gyr. A third crater population (Population S) consisted of secondary impact craters that can dominate the cratering record at small diameters.
C1 [Strom, Robert G.; Malhotra, Renu] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Xiao, Zhi-Yong] China Univ Geosci, Planetary Sci Inst, Wuhan 430074, Peoples R China.
[Ito, Takashi; Yoshida, Fumi] Natl Astron Observ, Tokyo 1818588, Japan.
[Ostrach, Lillian R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Strom, RG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM rstrom@lpl.arizona.edu
RI Yoshida, Fumi/I-6389-2016; Ito, Takashi/E-5270-2013
OI Yoshida, Fumi/0000-0002-3286-911X; Ito, Takashi/0000-0002-0549-9002
FU NSF [AST-1312498]
FX We thank Z. Ivezic and J. S. Stuart for providing us with digital
versions of their published data. RM acknowledges research support from
NSF grant #AST-1312498. We also thank the anonymous referee for their
comments which improved the quality of this paper.
NR 109
TC 10
Z9 11
U1 1
U2 11
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD MAR
PY 2015
VL 15
IS 3
BP 407
EP 434
DI 10.1088/1674-4527/15/3/009
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC9HY
UT WOS:000350680800009
ER
PT J
AU Kanan, C
Bseiso, DNF
Ray, NA
Hsiao, JH
Cottrell, GW
AF Kanan, Christopher
Bseiso, Dina N. F.
Ray, Nicholas A.
Hsiao, Janet H.
Cottrell, Garrison W.
TI Humans have idiosyncratic and task-specific scanpaths for judging faces
SO VISION RESEARCH
LA English
DT Article
DE Eye movements; Machine learning; Scanpath routines; Face perception
ID SACCADIC EYE-MOVEMENTS; PSYCHOPHYSICS TOOLBOX; RECOGNITION TASKS;
OBSERVERS TASK; INFORMATION; PATTERNS; YARBUS; CLASSIFICATION;
IDENTIFICATION; VALIDATION
AB Since Yarbus's seminal work, vision scientists have argued that our eye movement patterns differ depending upon our task. This has recently motivated the creation of multi-fixation pattern analysis algorithms that try to infer a person's task (or mental state) from their eye movements alone. Here, we introduce new algorithms for multi-fixation pattern analysis, and we use them to argue that people have scanpath routines for judging faces. We tested our methods on the eye movements of subjects as they made six distinct judgments about faces. We found that our algorithms could detect whether a participant is trying to distinguish angriness, happiness, trustworthiness, tiredness, attractiveness, or age. However, our algorithms were more accurate at inferring a subject's task when only trained on data from that subject than when trained on data gathered from other subjects, and we were able to infer the identity of our subjects using the same algorithms. These results suggest that (1) individuals have scanpath routines for judging faces, and that (2) these are diagnostic of that subject, but that (3) at least for the tasks we used, subjects do not converge on the same "ideal" scanpath pattern. Whether universal scanpath patterns exist for a task, we suggest, depends on the task's constraints and the level of expertise of the subject. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Kanan, Christopher] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Bseiso, Dina N. F.; Ray, Nicholas A.; Cottrell, Garrison W.] Univ Calif San Diego, Dept Comp Sci & Engn, La Jolla, CA 92093 USA.
[Hsiao, Janet H.] Univ Hong Kong, Dept Psychol, Hong Kong, Hong Kong, Peoples R China.
RP Kanan, C (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM ckanan@caltech.edu; dbseiso@ucsd.edu; niray@ucsd.edu; jhsiao@hku.hk;
gary@ucsd.edu
FU NSF REU Site grant [SMA-1005256]; NSF Science of Learning Center
[SBE-0542013, SMA-1041755]
FX We thank the reviewers for their valuable comments, which substantially
improved the manuscript. C.K. was affiliated with UC San Diego when this
project was completed. This work was supported in part by NSF REU Site
grant SMA-1005256 and NSF Science of Learning Center grants SBE-0542013
and SMA-1041755 to the Temporal Dynamics of Learning Center.
NR 49
TC 3
Z9 3
U1 2
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0042-6989
EI 1878-5646
J9 VISION RES
JI Vision Res.
PD MAR
PY 2015
VL 108
BP 67
EP 76
DI 10.1016/j.visres.2015.01.013
PG 10
WC Neurosciences; Ophthalmology
SC Neurosciences & Neurology; Ophthalmology
GA CD0RH
UT WOS:000350781100008
PM 25641371
ER
PT J
AU Borish, HJ
Huang, CL
Chevalier, RA
Breslauer, BM
Kingery, AM
Privon, GC
AF Borish, H. Jacob
Huang, Chenliang
Chevalier, Roger A.
Breslauer, Benjamin M.
Kingery, Aaron M.
Privon, George C.
TI NEAR-INFRARED SPECTROSCOPY OF THE TYPE IIn SN 2010jl: EVIDENCE FOR HIGH
VELOCITY EJECTA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; supernovae: general; supernovae: individual (SN
2010jl)
ID CIRCUMSTELLAR INTERACTION; SUPERNOVA 2010JL; DUST GRAINS; EVOLUTION;
PROGENITOR; SPECTROGRAPH; ENVIRONMENT; EXPLOSION; EMISSION; SN1998S
AB The Type IIn supernova SN 2010jl was relatively nearby and luminous, allowing detailed studies of the near-infrared (NIR) emission. We present 1-2.4 mu m spectroscopy over the age range of 36-565 days from the earliest detection of the supernova. On day 36, the H lines show an unresolved narrow emission component along with a symmetric broad component that can be modeled as the result of electron scattering by a thermal distribution of electrons. Over the next hundreds of days, the broad components of the H lines shift to the blue by 700 km s(-1), as is also observed in optical lines. The narrow lines do not show a shift, indicating they originate in a different region. He I lambda 10830 and lambda 20587 lines both show an asymmetric broad emission component, with a shoulder on the blue side that varies in prominence and velocity from -5500 km s(-1) on day 108 to -4000 km s(-1) on day 219. This component may be associated with the higher velocity flow indicated by X-ray observations of the supernova. The absence of the feature in the H lines suggests that this is from a He-rich ejecta flow. The He I lambda 10830 feature has a narrow P Cygni line, with absorption extending to similar to 100 km s(-1) and strengthening over the first 200 days, and an emission component which weakens with time. At day 403, the continuum emission becomes dominated by a blackbody spectrum with a temperature of similar to 1900 K, suggestive of dust emission.
C1 [Borish, H. Jacob; Huang, Chenliang; Chevalier, Roger A.; Breslauer, Benjamin M.; Kingery, Aaron M.; Privon, George C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Breslauer, Benjamin M.] Google, Mountain View, CA 94043 USA.
[Kingery, Aaron M.] NASA, George C Marshall Space Flight Ctr, ERC Inc, Jacobs ESSSA Grp, Huntsville, AL 35812 USA.
[Privon, George C.] Univ Concepcion, Dept Astron, Concepcion, Chile.
RP Borish, HJ (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
EM hjborish@virginia.edu
OI Privon, George/0000-0003-3474-1125
FU NSF grant [AST-0807727]; NASA grant [NNX12AF90G]; National Aeronautics
and Space Administration
FX We are grateful to Ori Fox for help with the observations as well as
discussion of the results. We thank Claes Fransson for fruitful
discussions and correspondence on SN 2010jl, and the referee who
provided detailed comments that led to significant improvement of the
paper. Thanks are also due to Meredith Drosback, Sarah Schmidt, and Yue
Shen, who very graciously donated telescope time for our observations of
SN 2010jl. We also wish to thank Mike Skrutskie for his help with
gathering, reducing, and interpreting the spectra. This research was
supported in part by NSF grant AST-0807727 and NASA grant NNX12AF90G.
The research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France, 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 37
TC 4
Z9 4
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2015
VL 801
IS 1
AR 7
DI 10.1088/0004-637X/801/1/7
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700007
ER
PT J
AU Lanz, L
Ogle, PM
Evans, D
Appleton, PN
Guillard, P
Emonts, B
AF Lanz, L.
Ogle, P. M.
Evans, D.
Appleton, P. N.
Guillard, P.
Emonts, B.
TI JET-ISM INTERACTION IN THE RADIO GALAXY 3C 293: JET-DRIVEN SHOCKS HEAT
ISM TO POWER X-RAY AND MOLECULAR H-2 EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (3C 293); galaxies: ISM;
galaxies: jets; X-rays: galaxies; X-rays: ISM
ID SPITZER-SPACE-TELESCOPE; POLYCYCLIC AROMATIC-HYDROCARBONS; BRIGHTEST
CLUSTER GALAXIES; NEARBY SEYFERT-GALAXIES; HYDROGEN EMISSION; CHANDRA
OBSERVATIONS; BLACK-HOLES; XMM-NEWTON; HOT-SPOTS; INFRARED SPECTROGRAPH
AB We present a 70 ks Chandra observation of the radio galaxy 3C 293. This galaxy belongs to the class of molecular hydrogen emission galaxies (MOHEGs) that have very luminous emission from warm molecular hydrogen. In radio galaxies, the molecular gas appears to be heated by jet-driven shocks, but exactly how this mechanism works is still poorly understood. With Chandra, we observe X-ray emission from the jets within the host galaxy and along the 100 kpc radio jets. We model the X-ray spectra of the nucleus, the inner jets, and the X-ray features along the extended radio jets. Both the nucleus and the inner jets show evidence of 10(7) K shock-heated gas. The kinetic power of the jets is more than sufficient to heat the X-ray emitting gas within the host galaxy. The thermal X-ray and warm H-2 luminosities of 3C 293 are similar, indicating similar masses of X-ray hot gas and warm molecular gas. This is consistent with a picture where both derive from a multiphase, shocked interstellar medium (ISM). We find that radio-loud MOHEGs that are not brightest cluster galaxies (BCGs), like 3C 293, typically have L-H2/L-X similar to 1 and M-H2/M-X similar to 1, whereas MOHEGs that are BCGs have L-H2/L-X similar to 0.01 and M-H2/M-X similar to 0.01. The more massive, virialized, hot atmosphere in BCGs overwhelms any direct X-ray emission from current jet-ISM interaction. On the other hand, L-H2/L-X similar to 1 in the Spiderweb BCG at z = 2, which resides in an unvirialized protocluster and hosts a powerful radio source. Over time, jet-ISM interaction may contribute to the establishment of a hot atmosphere in BCGs and other massive elliptical galaxies.
C1 [Lanz, L.; Ogle, P. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Evans, D.] Natl Sci Fdn, Arlington, VA 22230 USA.
[Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA.
[Guillard, P.] Univ Paris 06, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Emonts, B.] CSIC, INTA, Ctr Astrobiol, E-28850 Madrid, Spain.
RP Lanz, L (reprint author), CALTECH, Infrared Proc & Anal Ctr, MC100-22, Pasadena, CA 91125 USA.
EM llanz@ipac.caltech.edu
OI Lanz, Lauranne/0000-0002-3249-8224; Appleton, Philip/0000-0002-7607-8766
FU National Aeronautics and Space Administration through Chandra Award
[GO1-12122X]
FX L.L. thanks Aneta Siemiginowska and Katherine Alatalo for insightful
discussions. We also thank Alvaro Labiano for sharing the CO data from
his paper. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO1-12122X issued by the Chandra X-Ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060. The scientific results reported in this article are based on
observations made by the Chandra X-Ray Observatory and data obtained
from the Chandra Data Archive, some of which was published previously in
cited articles. This work also used archival data obtained from the
Spitzer Science Archive, the Mikulski Archive for Space Telescopes
(MAST), and the NASA/ IPAC Infrared Science Archive (IRSA). Spitzer is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. GALEX is operated for NASA by the
California Institute of Technology under NASA contract NAS5-98034. This
research has made use of the NASA/ IPAC Extragalactic Database (NED),
which along with IRSA, is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. B.E. acknowledges funding through
the European Union FP7 IEF grant No. 624351.
NR 106
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2015
VL 801
IS 1
AR 17
DI 10.1088/0004-637X/801/1/17
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700017
ER
PT J
AU Madsen, KK
Reynolds, S
Harrison, F
An, HJ
Boggs, S
Christensen, FE
Craig, WW
Fryer, CL
Grefenstette, BW
Hailey, CJ
Markwardt, C
Nynka, M
Stern, D
Zoglauer, A
Zhang, W
AF Madsen, Kristin K.
Reynolds, Stephen
Harrison, Fiona
An, Hongjun
Boggs, Steven
Christensen, Finn E.
Craig, William W.
Fryer, Chris L.
Grefenstette, Brian W.
Hailey, Charles J.
Markwardt, Craig
Nynka, Melania
Stern, Daniel
Zoglauer, Andreas
Zhang, William
TI BROADBAND X-RAY IMAGING AND SPECTROSCOPY OF THE CRAB NEBULA AND PULSAR
WITH NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (Crab); stars: neutron; X-rays: individual (Crab)
ID SPATIAL-DISTRIBUTION; SUPERNOVA REMNANT; LUNAR OCCULTATION; STANDARD
CANDLE; WIND; EMISSION; CONSTRAINTS; SPECTRUM; CHANDRA; FLARE
AB We present broadband (3-78 keV) NuSTAR X-ray imaging and spectroscopy of the Crab nebula and pulsar. We show that while the phase-averaged and spatially integrated nebula + pulsar spectrum is a power law in this energy band, spatially resolved spectroscopy of the nebula finds a break at similar to 9 keV in the spectral photon index of the torus structure with a steepening characterized by Delta Gamma similar to 0.25. We also confirm a previously reported steepening in the pulsed spectrum, and quantify it with a broken power law with break energy at similar to 12 keV and Delta Gamma similar to 0.27. We present spectral maps of the inner 100 '' the remnant and measure the size of the nebula as a function of energy in seven bands. These results find that the rate of shrinkage with energy of the torus size can be fitted by a power law with an index of gamma = 0.094 +/- 0.018, consistent with the predictions of Kennel and Coroniti. The change in size is more rapid in the NW direction, coinciding with the counter-jet where we find the index to be a factor of two larger. NuSTAR observed the Crab during the latter part of a gamma-ray flare, but found no increase in flux in the 3-78 keV energy band.
C1 [Madsen, Kristin K.; Harrison, Fiona; Grefenstette, Brian W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Reynolds, Stephen] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Boggs, Steven] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Livermore, CA 94550 USA.
[Hailey, Charles J.; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Markwardt, Craig; Zhang, William] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Madsen, KK (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012;
Madsen, Kristin/0000-0003-1252-4891
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 (NuSTAR-DAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA).
NR 50
TC 9
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2015
VL 801
IS 1
AR 66
DI 10.1088/0004-637X/801/1/66
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700066
ER
PT J
AU Montgomery, CG
Swank, JH
AF Montgomery, C. G.
Swank, J. H.
TI STATISTICS OF X-RAY POLARIZATION MEASUREMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; polarization; X-rays:
general
ID LINEAR-POLARIZATION; STOKES PARAMETERS; NOISE
AB The polarization of an X-ray beam that produces electrons with velocity components perpendicular to the beam generates an azimuthal distribution of the ejected electrons. We present methods for simulating and for analyzing the angular dependence of electron detections which enable us to derive simple analytical expressions for useful statistical properties of observable data. The derivations are verified by simulations. While we confirm the results of previous work on this topic, we provide an extension needed for analytical treatment of the full range of possible polarization amplitudes.
C1 [Swank, J. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Montgomery, CG (reprint author), 42 Blueberry Lane, Peterborough, NH 03458 USA.
EM jean.swank@nasa.gov
NR 15
TC 2
Z9 2
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2015
VL 801
IS 1
AR 21
DI 10.1088/0004-637X/801/1/21
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700021
ER
PT J
AU Rigliaco, E
Pascucci, I
Duchene, G
Edwards, S
Ardila, DR
Grady, C
Mendigutia, I
Montesinos, B
Mulders, GD
Najita, JR
Carpenter, J
Furlan, E
Gorti, U
Meijerink, R
Meyer, MR
AF Rigliaco, Elisabetta
Pascucci, I.
Duchene, G.
Edwards, S.
Ardila, D. R.
Grady, C.
Mendigutia, I.
Montesinos, B.
Mulders, G. D.
Najita, J. R.
Carpenter, J.
Furlan, E.
Gorti, U.
Meijerink, R.
Meyer, M. R.
TI PROBING STELLAR ACCRETION WITH MID-INFRARED HYDROGEN LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; infrared: stars; line:
identification; stars: activity
ID T-TAURI STARS; MAIN-SEQUENCE STARS; NE-II EMISSION; SUN-LIKE STARS;
YOUNG CIRCUMSTELLAR DISKS; SPITZER-SPACE-TELESCOPE; H ALPHA-EMISSION;
LOW-MASS STARS; INFRARED SPECTROGRAPH; PLANETARY SYSTEMS
AB In this paper we investigate the origin of the mid-infrared (IR) hydrogen recombination lines for a sample of 114 disks in different evolutionary stages (full, transitional, and debris disks) collected from the Spitzer archive. We focus on the two brighter H I lines observed in the Spitzer spectra, the H I (7-6) at 12.37 mu m and the H I (9-7) at 11.32 mu m. We detect the H I (7-6) line in 46 objects, and the H I (9-7) in 11. We compare these lines with the other most common gas line detected in Spitzer spectra, the [Ne II] at 12.81 mu m. We argue that it is unlikely that the H I emission originates from the photoevaporating upper surface layers of the disk, as has been found for the [Ne II] lines toward low-accreting stars. Using the H I (9-7)/H I (7-6) line ratios we find these gas lines are likely probing gas with hydrogen column densities of 10(10)-10(11) cm(-3). The subsample of objects surrounded by full and transitional disks show a positive correlation between the accretion luminosity and the H I line luminosity. These two results suggest that the observed mid-IR H I lines trace gas accreting onto the star in the same way as other hydrogen recombination lines at shorter wavelengths. A pure chromospheric origin of these lines can be excluded for the vast majority of full and transitional disks. We report for the first time the detection of the H I (7-6) line in eight young (<20 Myr) debris disks. A pure chromospheric origin cannot be ruled out in these objects. If the H I (7-6) line traces accretion in these older systems, as in the case of full and transitional disks, the strength of the emission implies accretion rates lower than 10(-10) M-circle dot yr(-1). We discuss some advantages of extending accretion indicators to longer wavelengths, and the next steps required pinning down the origin of mid-IR hydrogen lines.
C1 [Rigliaco, Elisabetta; Pascucci, I.; Mulders, G. D.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85719 USA.
[Rigliaco, Elisabetta; Meyer, M. R.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, G.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Duchene, G.] CNRS, IPAG, F-38000 Grenoble, France.
[Edwards, S.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA.
[Ardila, D. R.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Ardila, D. R.] Aerosp Corp, El Segundo, CA 90245 USA.
[Grady, C.] Eureka Sci, Oakland, CA 94602 USA.
[Grady, C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Mendigutia, I.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Montesinos, B.] Ctr Astrobiol, Dept Astrofis, E-28691 Madrid, Spain.
[Najita, J. R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Carpenter, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Furlan, E.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gorti, U.] SETI Inst, Mountain View, CA 94043 USA.
[Meijerink, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Rigliaco, E (reprint author), Univ Arizona, Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85719 USA.
EM rigliaco@lpl.arizona.edu
RI Montesinos, Benjamin/C-3493-2017;
OI Montesinos, Benjamin/0000-0002-7982-2095; Mendigutia,
Ignacio/0000-0002-0233-5328; Furlan, Elise/0000-0001-9800-6248
FU NASA's Astrophysics Data Analysis Program research grant [ID:
NNX11AG60G]
FX The authors thank Catherine Espaillat and Lynne Hillenbrand for
providing the optical spectra and physical parameters of a few objects,
and John Kwan for providing the mid-IR hydrogen line ratios. E.R. is
supported by the NASA's Astrophysics Data Analysis Program research
grant to I.P. (ID: NNX11AG60G).
NR 132
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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 MAR 1
PY 2015
VL 801
IS 1
AR 31
DI 10.1088/0004-637X/801/1/31
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700031
ER
PT J
AU Zitrin, A
Fabris, A
Merten, J
Melchior, P
Meneghetti, M
Koekemoer, A
Coe, D
Maturi, M
Bartelmann, M
Postman, M
Umetsu, K
Seidel, G
Sendra, I
Broadhurst, T
Balestra, I
Biviano, A
Grillo, C
Mercurio, A
Nonino, M
Rosati, P
Bradley, L
Carrasco, M
Donahue, M
Ford, H
Frye, BL
Moustakas, J
AF Zitrin, Adi
Fabris, Agnese
Merten, Julian
Melchior, Peter
Meneghetti, Massimo
Koekemoer, Anton
Coe, Dan
Maturi, Matteo
Bartelmann, Matthias
Postman, Marc
Umetsu, Keiichi
Seidel, Gregor
Sendra, Irene
Broadhurst, Tom
Balestra, Italo
Biviano, Andrea
Grillo, Claudio
Mercurio, Amata
Nonino, Mario
Rosati, Piero
Bradley, Larry
Carrasco, Mauricio
Donahue, Megan
Ford, Holland
Frye, Brenda L.
Moustakas, John
TI HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE
CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: high-redshift; gravitational
lensing: strong; gravitational lensing: weak
ID LUMINOUS GALAXY CLUSTERS; STAR-FORMING GALAXIES; FRONTIER FIELDS
CLUSTERS; DARK-MATTER DISTRIBUTION; LINE-OF-SIGHT; X-RAY; MACS
J0717.5+3745; RXC J2248.7-4431; MULTIPLE IMAGES; YOUNG GALAXY
AB We present results from a comprehensive lensing analysis in Hubble Space Telescope (HST) data of the complete Cluster Lensing And Supernova survey with Hubble cluster sample. We identify previously undiscovered multiple images, allowing improved or first constraints on the cluster inner mass distributions and profiles. We combine these strong lensing constraints with weak lensing shape measurements within the HST field of view (FOV) to jointly constrain the mass distributions. The analysis is performed in two different common parameterizations (one adopts light-traces-mass for both galaxies and dark matter while the other adopts an analytical, elliptical Navarro-Frenk-White form for the dark matter) to provide a better assessment of the underlying systematics-which is most important for deep, cluster-lensing surveys, especially when studying magnified high-redshift objects. We find that the typical (median), relative systematic differences throughout the central FOV are similar to 40% in the (dimensionless) mass density, kappa, and similar to 20% in the magnification, mu. We show maps of these differences for each cluster, as well as the mass distributions, critical curves, and two-dimensional (2D)-integrated mass profiles. For the Einstein radii (z(s) = 2) we find that all typically agree within 10% between the two models, and Einstein masses agree, typically, within similar to 15%. At larger radii, the total projected, 2D-integrated mass profiles of the two models, within r similar to 2', differ by similar to 30%. Stacking the surface-density profiles of the sample from the two methods together, we obtain an average slope of d log(Sigma)/d log(r) similar to -0.64 +/- 0.1, in the radial range [5350] kpc. Last, we also characterize the behavior of the average magnification, surface density, and shear differences between the two models as a function of both the radius from the center and the best-fit values of these quantities. All mass models and magnification maps are made publicly available for the community.
C1 [Zitrin, Adi; Merten, Julian] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Fabris, Agnese; Maturi, Matteo; Bartelmann, Matthias; Carrasco, Mauricio] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Merten, Julian; Meneghetti, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Koekemoer, Anton; Coe, Dan; Bradley, Larry] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Seidel, Gregor] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Sendra, Irene; Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, E-48080 Bilbao, Spain.
[Broadhurst, Tom] Ikerbasque, Basque Fdn Sci, E-48011 Bilbao, Spain.
[Biviano, Andrea; Nonino, Mario] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Mercurio, Amata] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Rosati, Piero] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Ford, Holland] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Frye, Brenda L.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
RP Zitrin, A (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, MC 249-17, Pasadena, CA 91125 USA.
EM adizitrin@gmail.com
RI Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015;
OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Balestra, Italo/0000-0001-9660-894X;
Nonino, Mario/0000-0001-6342-9662; Umetsu, Keiichi/0000-0002-7196-4822;
Biviano, Andrea/0000-0002-0857-0732; Koekemoer,
Anton/0000-0002-6610-2048
FU NASA from Space Telescope Science Institute (STScI) [12065]; Association
of Universities for Research in Astronomy, Inc., under NASA [NAS
5-26555]; NASA [HST-HF2-51334.001-A]; STScI; Ministry of Science and
Technology of Taiwan [MOST 103-2112-M-001-030-MY3]
FX We thank the reviewer of this work for valuable comments. A.Z. is
grateful for useful discussions with Carrie Bridge and Drew Newman. This
work is based on observations made with the NASA/ESA Hubble Space
Telescope. Support for Program 12065 was provided by NASA from 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. Support for this work was provided by NASA through
Hubble Fellowship Grant HST-HF2-51334.001-A awarded by STScI. K.U.
acknowledges support from the Ministry of Science and Technology of
Taiwan through Grant MOST 103-2112-M-001-030-MY3. The research was in
part carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA.
NR 138
TC 41
Z9 41
U1 3
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2015
VL 801
IS 1
AR 44
DI 10.1088/0004-637X/801/1/44
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC6PR
UT WOS:000350488700044
ER
PT J
AU Adriani, O
Barbarino, GC
Bazilevskaya, GA
Bellotti, R
Boezio, M
Bogomolov, EA
Bongi, M
Bonvicini, V
Bottai, S
Bravar, U
Bruno, A
Cafagna, F
Campana, D
Carbone, R
Carlson, P
Casolino, M
Castellini, G
Christian, ER
De Donato, C
de Nolfo, GA
De Santis, C
De Simone, N
Di Felice, V
Formato, V
Galper, AM
Karelin, AV
Koldashov, SV
Koldobskiy, S
Krutkov, SY
Kvashnin, AN
Lee, M
Leonov, A
Malakhov, V
Marcelli, L
Martucci, M
Mayorov, AG
Menn, W
Merge, M
Mikhailov, VV
Mocchiutti, E
Monaco, A
Mori, N
Munini, R
Osteria, G
Palma, F
Panico, B
Papini, P
Pearce, M
Picozza, P
Ricci, M
Ricciarini, SB
Ryan, JM
Sarkar, R
Scotti, V
Simon, M
Sparvoli, R
Spillantini, P
Stochaj, S
Stozhkov, YI
Thakur, N
Vacchi, A
Vannuccini, E
Vasilyev, GI
Voronov, SA
Yurkin, YT
Zampa, G
Zampa, N
AF Adriani, O.
Barbarino, G. C.
Bazilevskaya, G. A.
Bellotti, R.
Boezio, M.
Bogomolov, E. A.
Bongi, M.
Bonvicini, V.
Bottai, S.
Bravar, U.
Bruno, A.
Cafagna, F.
Campana, D.
Carbone, R.
Carlson, P.
Casolino, M.
Castellini, G.
Christian, E. R.
De Donato, C.
de Nolfo, G. A.
De Santis, C.
De Simone, N.
Di Felice, V.
Formato, V.
Galper, A. M.
Karelin, A. V.
Koldashov, S. V.
Koldobskiy, S.
Krutkov, S. Y.
Kvashnin, A. N.
Lee, M.
Leonov, A.
Malakhov, V.
Marcelli, L.
Martucci, M.
Mayorov, A. G.
Menn, W.
Merge, M.
Mikhailov, V. V.
Mocchiutti, E.
Monaco, A.
Mori, N.
Munini, R.
Osteria, G.
Palma, F.
Panico, B.
Papini, P.
Pearce, M.
Picozza, P.
Ricci, M.
Ricciarini, S. B.
Ryan, J. M.
Sarkar, R.
Scotti, V.
Simon, M.
Sparvoli, R.
Spillantini, P.
Stochaj, S.
Stozhkov, Y. I.
Thakur, N.
Vacchi, A.
Vannuccini, E.
Vasilyev, G. I.
Voronov, S. A.
Yurkin, Y. T.
Zampa, G.
Zampa, N.
TI PAMELA'S MEASUREMENTS OF MAGNETOSPHERIC EFFECTS ON HIGH-ENERGY SOLAR
PARTICLES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Earth; Sun: coronal mass ejections (CMEs); Sun: flares; Sun:
heliosphere; Sun: particle emission
ID GROUND-LEVEL ENHANCEMENT; COSMIC-RAYS; OCTOBER 22; CYCLE 24; EVENT;
PROTONS
AB The nature of particle acceleration at the Sun, whether through flare reconnection processes or through shocks driven by coronal mass ejections, is still under scrutiny despite decades of research. The measured properties of solar energetic particles (SEPs) have long been modeled in different particle-acceleration scenarios. The challenge has been to disentangle the effects of transport from those of acceleration. The Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) instrument enables unique observations of SEPs including the composition and angular distribution of the particles about the magnetic field, i.e., pitch angle distribution, over a broad energy range (>80 MeV)-bridging a critical gap between space-based and ground-based measurements. We present high-energy SEP data from PAMELA acquired during the 2012 May 17 SEP event. These data exhibit differential anisotropies and thus transport features over the instrument rigidity range. SEP protons exhibit two distinct pitch angle distributions: a low-energy population that extends to 90 degrees and a population that is beamed at high energies (>1 GeV), consistent with neutron monitor measurements. To explain a low-energy SEP population that exhibits significant scattering or redistribution accompanied by a high-energy population that reaches the Earth relatively unaffected by dispersive transport effects, we postulate that the scattering or redistribution takes place locally. We believe that these are the first comprehensive measurements of the effects of solar energetic particle transport in the Earth's magnetosheath.
C1 [Adriani, O.; Bongi, M.; Mori, N.; Spillantini, P.] Univ Florence, Dept Phys & Astron, I-50019 Florence, Italy.
[Adriani, O.; Bongi, M.; Bottai, S.; Mori, N.; Papini, P.; Ricciarini, S. B.; Spillantini, P.; Vannuccini, E.] Ist Nazl Fis Nucl, Sez Florence, I-50019 Florence, Italy.
[Barbarino, G. C.; Scotti, V.] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy.
[Barbarino, G. C.; Campana, D.; Osteria, G.; Panico, B.; Scotti, V.] Ist Nazl Fis Nucl, Sez Naples, I-80126 Naples, Italy.
[Bazilevskaya, G. A.; Kvashnin, A. N.; Stozhkov, Y. I.] PN Lebedev Phys Inst, RU-119991 Moscow, Russia.
[Bellotti, R.; Bruno, A.; Monaco, A.] Univ Bari, I-70126 Bari, Italy.
[Bellotti, R.; Cafagna, F.; Monaco, A.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Boezio, M.; Bonvicini, V.; Carbone, R.; Formato, V.; Mocchiutti, E.; Munini, R.; Zampa, G.; Zampa, N.] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy.
[Bogomolov, E. A.; Krutkov, S. Y.; Vasilyev, G. I.] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia.
[Bravar, U.; Lee, M.; Ryan, J. M.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Casolino, M.; De Donato, C.; De Santis, C.; De Simone, N.; Di Felice, V.; Merge, M.; Palma, F.; Picozza, P.; Sparvoli, R.] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, I-00133 Rome, Italy.
[De Donato, C.; Marcelli, L.; Martucci, M.; Merge, M.; Palma, F.; Picozza, P.; Sparvoli, R.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy.
[Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Leonov, A.; Malakhov, V.; Mayorov, A. G.; Mikhailov, V. V.; Voronov, S. A.; Yurkin, Y. T.] Natl Res Nucl Univ MEPhI, RU-115409 Moscow, Russia.
[Carlson, P.; Pearce, M.] KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Carlson, P.; Pearce, M.] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Casolino, M.] RIKEN, Adv Sci Inst, Wako, Saitama, Japan.
[Castellini, G.; Ricciarini, S. B.] IFAC, I-50019 Florence, Italy.
[Christian, E. R.; de Nolfo, G. A.; Thakur, N.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
[Formato, V.; Munini, R.] Univ Trieste, Dept Phys, I-34147 Trieste, Italy.
[Menn, W.; Simon, M.] Univ Siegen, Dept Phys, D-57068 Siegen, Germany.
[Di Felice, V.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Martucci, M.; Ricci, M.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy.
[Sarkar, R.] Indian Ctr Space Phys, Kolkata 700084, W Bengal, India.
[Stochaj, S.] New Mexico State Univ, Elect & Comp Engn, Las Cruces, NM 88003 USA.
[Vacchi, A.] Udini Univ, Dept Math & Informat, Trieste, Italy.
[Vacchi, A.] Ist Nazl Fis Nucl, Trieste, Italy.
[Sarkar, R.] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy.
RP Adriani, O (reprint author), Univ Florence, Dept Phys & Astron, I-50019 Florence, Italy.
EM georgia.a.denolfo@nasa.gov
RI Cafagna, Francesco/A-9299-2010; marcelli, laura/K-8860-2016; Di Felice,
Valeria/L-2989-2016; Mori, Nicola/D-9459-2016; Karelin,
Alexander/O-6576-2016; Mayorov, Andrey/M-1207-2016; Voronov,
Sergey/P-9654-2016; Malakhov, Vitaly/Q-6730-2016; Panico,
Beatrice/F-1137-2017; Kvashnin, Aleksandr/M-8673-2015; Galper,
Arkady/M-9610-2015; Koldobskiy, Sergey/K-6507-2015; Krutkov,
Sergey/E-7561-2014; Vasilyev, Gennady/E-4843-2014; De Santis,
Cristian/C-1210-2011; De Donato, Cinzia/J-9132-2015; Palma,
Francesco/K-3224-2015; Barbarino, Giancarlo/L-2559-2015; Bazilevskaya,
Galina/M-6175-2015; Stozhkov, Yuri/M-7433-2015; Mikhailov,
Vladimir/B-5368-2014; Bongi, Massimo/L-9417-2015; Leonov,
Alexey/E-4698-2016; Vacchi, Andrea/C-1291-2010;
OI Cafagna, Francesco/0000-0002-7450-4784; marcelli,
laura/0000-0002-3180-1228; Mori, Nicola/0000-0003-2138-3787; Voronov,
Sergey/0000-0002-9209-0618; Panico, Beatrice/0000-0003-1063-6961;
Monaco, Alfonso/0000-0002-5968-8642; Kvashnin,
Aleksandr/0000-0001-7218-6738; casolino, marco/0000-0001-6067-5104;
Papini, Paolo/0000-0003-4718-2895; Koldobskiy,
Sergey/0000-0001-9187-0383; De Santis, Cristian/0000-0002-7280-2446; De
Donato, Cinzia/0000-0002-9725-1281; Palma,
Francesco/0000-0001-7076-8830; Barbarino, Giancarlo/0000-0001-9253-3397;
Mikhailov, Vladimir/0000-0003-3851-2901; Bongi,
Massimo/0000-0002-6050-1937; Ricciarini, Sergio
Bruno/0000-0001-6176-3368; Sparvoli, Roberta/0000-0002-6314-6117;
Picozza, Piergiorgio/0000-0002-7986-3321; Bellotti,
Roberto/0000-0003-3198-2708; Vacchi, Andrea/0000-0003-3855-5856; Boezio,
Mirko/0000-0002-8015-2981
FU NASA Heliophysics and Solar Research grant; National Science Foundation
(SHINE); Italian Space Agency (ASI); Deutsches Zentrum fur Luft-und
Raumfahrt (DLR); Swedish National Space Board; Swedish Research Council;
Russian Space Agency (Roscosmos); Russian Science Foundation
FX The authors acknowledge support from a NASA Heliophysics and Solar
Research grant, the National Science Foundation (SHINE), the Italian
Space Agency (ASI), Deutsches Zentrum fur Luft-und Raumfahrt (DLR), the
Swedish National Space Board, the Swedish Research Council, the Russian
Space Agency (Roscosmos), and the Russian Science Foundation. We
gratefully thank N. Tsyganenko and Dr. Charlie Farrugia for helpful
discussions, and Drs. M. I. Sitnov and G. K. Stephens for support in the
use of the TS07D model.
NR 31
TC 5
Z9 5
U1 3
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2015
VL 801
IS 1
AR L3
DI 10.1088/2041-8205/801/1/L3
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3QB
UT WOS:000350262900003
ER
PT J
AU France, K
McCray, R
Fransson, C
Larsson, J
Frank, KA
Burrows, DN
Challis, P
Kirshner, RP
Chevalier, RA
Garnavich, P
Heng, K
Lawrence, SS
Lundqvist, P
Smith, N
Sonneborn, G
AF France, Kevin
McCray, Richard
Fransson, Claes
Larsson, Josefin
Frank, Kari A.
Burrows, David N.
Challis, Peter
Kirshner, Robert P.
Chevalier, Roger A.
Garnavich, Peter
Heng, Kevin
Lawrence, Stephen S.
Lundqvist, Peter
Smith, Nathan
Sonneborn, George
TI MAPPING HIGH-VELOCITY H alpha AND Ly alpha EMISSION FROM SUPERNOVA 1987A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; shock waves; supernovae: individual (SN 1987A)
ID SN 1987A; REMNANT 1987A; SN-1987A; RING; NEBULA; SHOCK; TWIN; GAS
AB We present new Hubble Space Telescope images of high-velocity H alpha and Ly alpha emission in the outer debris of SN 1987 A. The Ha images are dominated by emission from hydrogen atoms crossing the reverse shock (RS). For the first time we observe emission from the RS surface well above and below the equatorial. ring (ER), suggesting a bipolar or conical structure perpendicular to the ring plane. Using the H alpha imaging, we measure the mass flux of hydrogen atoms crossing the RS front, in the velocity intervals (-7500 < V-obs < -2800 km s(-1)) and (1000 < V-obs < 7500 km s(-1)), (M)(H) over dot = 1.2 x 10(-3) M-circle dot yr(-1). We also present the first Ly alpha imaging of the whole remnant and new Chandra X-ray observations. Comparing the spatial distribution of the Ly alpha and X-ray emission, we observe that the majority of the high-velocity Ly alpha emission originates interior to the ER. The observed Ly alpha/H alpha photon ratio, < R(L alpha/H alpha)> approximate to 17, is significantly higher than the theoretically predicted ratio of approximate to 5 for neutral atoms crossing the RS front. We attribute this excess to Ly alpha emission produced by X-ray heating of the outer debris. The spatial orientation of the Ly alpha and X-ray emission suggests that X-ray heating of the outer debris is the dominant Ly alpha production mechanism in SN 1987 A at this phase in its evolution.
C1 [France, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[McCray, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fransson, Claes; Lundqvist, Peter] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Larsson, Josefin] KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Frank, Kari A.; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Garnavich, Peter] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland.
[Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP France, K (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 392 UCB, Boulder, CO 80309 USA.
EM kevin.france@colorado.edu
FU Cycle SAINTS program [13401, 13405]
FX The HST observations presented here were acquired as part of the Cycle
SAINTS program (13401 and 13405).
NR 16
TC 5
Z9 5
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2015
VL 801
IS 1
AR L16
DI 10.1088/2041-8205/801/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3QB
UT WOS:000350262900016
ER
PT J
AU Venemans, BP
Banados, E
Decarli, R
Farina, EP
Walter, F
Chambers, KC
Fan, X
Rix, HW
Schlafly, E
McMahon, RG
Simcoe, R
Stern, D
Burgett, WS
Draper, PW
Flewelling, H
Hodapp, KW
Kaiser, N
Magnier, EA
Metcalfe, N
Morgan, JS
Price, PA
Tonry, JL
Waters, C
AlSayyad, Y
Banerji, M
Chen, SS
Gonzalez-Solares, EA
Greiner, J
Mazzucchelli, C
McGreer, I
Miller, DR
Reed, S
Sullivan, PW
AF Venemans, B. P.
Banados, E.
Decarli, R.
Farina, E. P.
Walter, F.
Chambers, K. C.
Fan, X.
Rix, H-W.
Schlafly, E.
McMahon, R. G.
Simcoe, R.
Stern, D.
Burgett, W. S.
Draper, P. W.
Flewelling, H.
Hodapp, K. W.
Kaiser, N.
Magnier, E. A.
Metcalfe, N.
Morgan, J. S.
Price, P. A.
Tonry, J. L.
Waters, C.
AlSayyad, Y.
Banerji, M.
Chen, S. S.
Gonzalez-Solares, E. A.
Greiner, J.
Mazzucchelli, C.
McGreer, I.
Miller, D. R.
Reed, S.
Sullivan, P. W.
TI THE IDENTIFICATION OF z-DROPOUTS IN PAN-STARRS1: THREE QUASARS AT 6.5 <
z < 6.7
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: active; galaxies: individual (PSO
J036.5078+03.0498, PSO J167.6415-13.4960, PSO J338.2298+29.5089);
quasars: general
ID DIGITAL SKY SURVEY; SIMILAR-TO 6; Z-GREATER-THAN-5.7 QUASARS;
INTERGALACTIC MEDIUM; ADDITIONAL QUASARS; STAR-FORMATION; HOST GALAXIES;
BLACK-HOLES; PAN-STARRS; REDSHIFT
AB Luminous distant quasars are unique probes of the high-redshift intergalactic medium (IGM) and of the growth of massive galaxies and black holes in the early universe. Absorption due to neutral hydrogen in the IGM makes quasars beyond a redshift of z similar or equal to 6.5 very faint in the optical z band, thus locating quasars at higher redshifts requires large surveys that are sensitive above 1 micron. We report the discovery of three new z > 6.5 quasars, corresponding to an age of the universe of <850 Myr, selected as z-band dropouts in the Pan-STARRS1 survey. This increases the number of known z > 6.5 quasars from four to seven. The quasars have redshifts of z = 6.50, 6.52, and 6.66, and include the brightest z-dropout quasar reported to date, PSO J036.5078 + 03.0498 with M-1450 = -27.4. We obtained near-infrared spectroscopy for the quasars, and from the Mg II line, we estimate that the central black holes have masses between 5 x 10(8) and 4 x 10(9) M-circle dot and are accreting close to the Eddington limit (L-Bol/L-Edd = 0.13 - 1.2). We investigate the ionized regions around the quasars and find near-zone radii of R-NZ = 1.5 - 5.2 proper Mpc, confirming the trend of decreasing near-zone sizes with increasing redshift found for quasars at 5.7 < z < 6.4. By combining R-NZ of the PS1 quasars with those of 5.7 < z < 7.1 quasars in the literature, we derive a luminosity-corrected redshift evolution of R-NZ,R-corrected = (7.2 +/- 0.2) - (6.1 +/- 0.7) x (z - 6) Mpc. However, the large spread in R-NZ in the new quasars implies a wide range in quasar ages and/or a large variation in the neutral hydrogen fraction along different lines of sight.
C1 [Venemans, B. P.; Banados, E.; Decarli, R.; Farina, E. P.; Walter, F.; Rix, H-W.; Schlafly, E.; Mazzucchelli, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Chambers, K. C.; Flewelling, H.; Hodapp, K. W.; Kaiser, N.; Magnier, E. A.; Morgan, J. S.; Tonry, J. L.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Fan, X.; McGreer, I.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, R. G.; Banerji, M.; Gonzalez-Solares, E. A.; Reed, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[McMahon, R. G.; Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Simcoe, R.; Chen, S. S.; Miller, D. R.; Sullivan, P. W.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Burgett, W. S.] GMTO Corp, Pasadena, CA 91101 USA.
[Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[AlSayyad, Y.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Venemans, BP (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM venemans@mpia.de
OI Farina, Emanuele Paolo/0000-0002-6822-2254; Flewelling,
Heather/0000-0002-1050-4056; Reed, Sophie/0000-0002-4422-0553; McMahon,
Richard/0000-0001-8447-8869; Schlafly, Edward Ford/0000-0002-3569-7421;
Banados, Eduardo/0000-0002-2931-7824; Banerji,
Manda/0000-0002-0639-5141; Chambers, Kenneth /0000-0001-6965-7789
FU ERC grant "Cosmic Dawn"; US NSF [AST 11-07682, AST-1109915]; National
Aeronautics and Space Administration through the Planetary Science
Division of the NASA Science Mission Directorate [NNX08AR22G]; National
Science Foundation [AST-1238877]; Leibniz-Prize; DFG [HA 1850/28-1];
University of California, Los Angeles; Jet Propulsion
Laboratory/California Institute of Technology - National Aeronautics and
Space Administration
FX B.P.V., E.P.F., and F.W. acknowledge funding through ERC grant "Cosmic
Dawn." E.B. thanks the IMPRS for Astronomy & Cosmic Physics at the
University of Heidelberg. X.F. and I. D.M. acknowledge support from US
NSF grant AST 11-07682, and R.S. and D.M. from US NSF grant
AST-1109915.; The Pan-STARRS1 Surveys have been made possible through
contributions of the Institute for Astronomy, University of Hawaii, the
Pan-STARRS Project Office, the Max-Planck Society and its participating
institutes, Max-Planck-Institute for Astronomy, Heidelberg and
Max-Planck-Institute for Extraterrestrial Physics, Garching, The Johns
Hopkins University, Durham University, University of Edinburgh, Queens
University Belfast, Harvard-Smithsonian Center for Astrophysics, the Las
Cumbres Observatory Global Telescope Network Incorporated, the National
Central University of Taiwan, the Space Telescope Science Institute, the
National Aeronautics and Space Administration under grant No. NNX08AR22G
issued through the Planetary Science Division of the NASA Science
Mission Directorate, the National Science Foundation under grant
AST-1238877, the University of Maryland, and Eotvos Lorand University
(ELTE).; Part of the funding for GROND was granted from the
Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).; This
publication makes use of data products from the Wide-field Infrared
Survey Explorer, a joint project of the University of California, Los
Angeles, and the Jet Propulsion Laboratory/California Institute of
Technology, funded by the National Aeronautics and Space Administration.
The LBT is an international collaboration among institutions in the USA,
Italy, and Germany. The partners are The University of Arizona; Istituto
Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany,
representing the Max-Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; The Ohio State University; The
Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota, and University of Virginia.
NR 36
TC 24
Z9 24
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2015
VL 801
IS 1
AR L11
DI 10.1088/2041-8205/801/1/L11
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3QB
UT WOS:000350262900011
ER
PT J
AU Kassie, BT
Asseng, S
Rotter, RP
Hengsdijk, H
Ruane, AC
Van Ittersum, MK
AF Kassie, Belay T.
Asseng, Senthold
Rotter, Reimund P.
Hengsdijk, Huib
Ruane, Alex C.
Van Ittersum, Martin K.
TI Exploring climate change impacts and adaptation options for maize
production in the Central Rift Valley of Ethiopia using different
climate change scenarios and crop models
SO CLIMATIC CHANGE
LA English
DT Article
ID AFRICA; YIELD; AGRICULTURE; RISKS; OPPORTUNITIES; VULNERABILITY;
TEMPERATURES; UNCERTAINTY; VARIABILITY; PROJECTIONS
AB Exploring adaptation strategies for different climate change scenarios to support agricultural production and food security is a major concern to vulnerable regions, including Ethiopia. This study assesses the potential impacts of climate change on maize yield and explores specific adaptation options under climate change scenarios for the Central Rift Valley of Ethiopia by mid-century. Impacts and adaptation options were evaluated using three General Circulation Models (GCMs) in combination with two Representative Concentration Pathways (RCPs) and two crop models. Results indicate that maize yield decreases on average by 20 % in 2050s relative to the baseline (1980-2009) due to climate change. A negative impact on yield is very likely, while the extent of impact is more uncertain. The share in uncertainties of impact projections was higher for the three GCMs than it was for the two RCPs and two crop models used in this study. Increasing nitrogen fertilization and use of irrigation were assessed as potentially effective adaptation options, which would offset negative impacts. However, the response of yields to increased fertilizer and irrigation will be less for climate change scenarios than under the baseline. Changes in planting dates also reduced negative impacts, while changing the maturity type of maize cultivars was not effective in most scenarios. The multi-model based analysis allowed estimating climate change impact and adaptation uncertainties, which can provide valuable insights and guidance for adaptation planning.
C1 [Kassie, Belay T.; Asseng, Senthold] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA.
[Rotter, Reimund P.] MTT Agrifood Res Finland, Plant Prod Res, Mikkeli 50100, Finland.
[Hengsdijk, Huib] Wageningen Univ, Plant Res Int, NL-6708 PB Wageningen, Netherlands.
[Ruane, Alex C.] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Van Ittersum, Martin K.] Wageningen Univ, Plant Prod Syst Grp, NL-6708 PB Wageningen, Netherlands.
RP Kassie, BT (reprint author), Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA.
EM belay_tsega@yahoo.com
RI van Ittersum, Martin/J-8024-2014
OI van Ittersum, Martin/0000-0001-8611-6781
FU Academy of Finland through the AlterCLIMA project [127405]
FX We are grateful to the Academy of Finland for funding this research
through the AlterCLIMA project (decision no. 127405). We thank Marcel
Lubbers, Mink Zijlstra and Joost Wolf (Plant Production Systems group of
Wageningen University) for their help in model input data management. We
acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
output.
NR 47
TC 4
Z9 4
U1 7
U2 48
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 MAR
PY 2015
VL 129
IS 1-2
BP 145
EP 158
DI 10.1007/s10584-014-1322-x
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CC4VP
UT WOS:000350352800012
ER
PT J
AU Keller, AA
Ciannelli, L
Wakefield, WW
Simon, V
Barth, JA
Pierce, SD
AF Keller, Aimee A.
Ciannelli, Lorenzo
Wakefield, W. Waldo
Simon, Victor
Barth, John A.
Pierce, Stephen D.
TI Occurrence of demersal fishes in relation to near-bottom oxygen levels
within the California Current large marine ecosystem
SO FISHERIES OCEANOGRAPHY
LA English
DT Article
DE bottom dissolved oxygen; demersal fish catch; Dover sole; greenstriped
rockfish; Northeast Pacific; petrale sole; probability of occurrence;
species richness; spotted ratfish
ID MINIMUM ZONE; NORTHEAST PACIFIC; DECLINING OXYGEN; HYPOXIA; WASHINGTON;
TRAWL; SLOPE; SHELF; WATER; VARIABILITY
AB Various ocean-climate models driven by increased greenhouse gases and higher temperatures predict a decline in oceanic dissolved oxygen (DO) as a result of greater stratification, reduced ventilation below the thermocline, and decreased solubility at higher temperatures. Since spreading of low oxygen waters is underway and predicted to increase, understanding impacts on higher trophic levels is essential. Within the California Current System, shoaling of the oxygen minimum zone (OMZ) is expected to produce complex changes. Onshore movement of the OMZ could lead to habitat compression for species with higher oxygen requirements while allowing expansion of species tolerant of low bottom DO. As part of annual groundfish surveys, we sampled catch across a range of conditions from the upper to the lower limit of the OMZ and shoreward across the continental shelf of the US west coast. DO ranged from 0.02 to 4.25mLL(-1) with 642 stations (of 1020 sampled) experiencing hypoxic conditions in 2008-2010. Catch and species richness exhibited significant and positive relationships with near-bottom oxygen concentration. The probability of occurrence was estimated for four species (spotted ratfish, petrale sole, greenstriped rockfish and Dover sole) using a binomial Generalized Additive Model. The models for each species included terms for position, day of the year, salinity, near-bottom temperature and the interaction term between depth and near-bottom DO. Spotted ratfish and petrale sole were sensitive to changes in near-bottom oxygen, while greenstriped rockfish and Dover sole show no changes in probability of occurrence in relation to changes in oxygen concentration.
C1 [Keller, Aimee A.; Simon, Victor] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA.
[Ciannelli, Lorenzo; Barth, John A.; Pierce, Stephen D.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci CEOAS, Corvallis, OR 97331 USA.
[Wakefield, W. Waldo] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Keller, AA (reprint author), NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Ctr, Natl Marine Fisheries Serv, 2725 Montlake Blvd East, Seattle, WA 98112 USA.
EM Aimee.Keller@noaa.gov
FU West Coast & Polar Regions Undersea Research Center of NOAA's Office of
Ocean Exploration and Research; NSF-SEES-RCN [1140207]
FX We thank the NWFSC bottom trawl survey group (Keith Bosley, John
Buchanan, Mark Bradburn, Doug Draper, Melissa Head, John Harms, Dan
Kamikawa, and Vanessa Tuttle), associated participants, and Beth
Horness. Funding was provided from the West Coast & Polar Regions
Undersea Research Center of NOAA's Office of Ocean Exploration and
Research and from NSF-SEES-RCN grant number: 1140207.
NR 53
TC 6
Z9 6
U1 6
U2 25
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1054-6006
EI 1365-2419
J9 FISH OCEANOGR
JI Fish Oceanogr.
PD MAR
PY 2015
VL 24
IS 2
BP 162
EP 176
DI 10.1111/fog.12100
PG 15
WC Fisheries; Oceanography
SC Fisheries; Oceanography
GA CC7KE
UT WOS:000350545400005
ER
PT J
AU Trautman, P
Ma, J
Murray, RM
Krause, A
AF Trautman, Pete
Ma, Jeremy
Murray, Richard M.
Krause, Andreas
TI Robot navigation in dense human crowds: Statistical models and
experimental studies of human-robot cooperation
SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH
LA English
DT Article
DE Learning and adaptive systems; cognitive robotics; social human-robot
interaction; human-centered and life-like robotics; adaptive control;
mechanics; design and control
ID MOTION; ENVIRONMENTS; UNCERTAIN
AB We consider the problem of navigating a mobile robot through dense human crowds. We begin by exploring a fundamental impediment to classical motion planning algorithms called the freezing robot problem: once the environment surpasses a certain level of dynamic complexity, the planner decides that all forward paths are unsafe, and the robot freezes in place (or performs unnecessary maneuvers) to avoid collisions. We argue that this problem can be avoided if the robot anticipates human cooperation, and accordingly we develop interacting Gaussian processes, a prediction density that captures cooperative collision avoidance, and a multiple goal extension that models the goal-driven nature of human decision making. We validate this model with an empirical study of robot navigation in dense human crowds (488 runs), specifically testing how cooperation models effect navigation performance. The multiple goal interacting Gaussian processes algorithm performs comparably with human teleoperators in crowd densities nearing 0.8 humans/m(2), while a state-of-the-art non-cooperative planner exhibits unsafe behavior more than three times as often as the multiple goal extension, and twice as often as the basic interacting Gaussian process approach. Furthermore, a reactive planner based on the widely used dynamic window approach proves insufficient for crowd densities above 0.55 people/m(2). We also show that our non-cooperative planner or our reactive planner capture the salient characteristics of nearly any dynamic navigation algorithm. Based on these experimental results and theoretical observations, we conclude that a cooperation model is critical for safe and efficient robot navigation in dense human crowds.
C1 [Trautman, Pete] Matrix Res Inc, Dayton, OH USA.
[Ma, Jeremy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Murray, Richard M.] CALTECH, Pasadena, CA 91125 USA.
[Krause, Andreas] ETH, Zurich, Switzerland.
RP Trautman, P (reprint author), 472 Irving Ave, Dayton, OH 45409 USA.
EM peter.trautman@gmail.com
OI Murray, Richard/0000-0002-5785-7481
FU Boeing company
FX This work was supported in part by the Boeing company through a grant to
the California Institute of Technology.
NR 73
TC 11
Z9 11
U1 6
U2 22
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 MAR
PY 2015
VL 34
IS 3
BP 335
EP 356
DI 10.1177/0278364914557874
PG 22
WC Robotics
SC Robotics
GA CC6KC
UT WOS:000350472800006
ER
PT J
AU Siskind, DE
Mlynczak, MG
Marshall, T
Friedrich, M
Gumbel, J
AF Siskind, David E.
Mlynczak, Martin G.
Marshall, Tom
Friedrich, Martin
Gumbel, Joerg
TI Implications of odd oxygen observations by the TIMED/SABER instrument
for lower D region ionospheric modeling
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Mesosphere; Ionosphere; D region
ID ELECTRON-DENSITY PROFILES; LOWER THERMOSPHERE; ION CHEMISTRY;
NITRIC-OXIDE; MESOSPHERE; OZONE; TIME
AB We document the variability in atomic oxygen inferred by the Sounding of the Atmosphere with Broadband Emission Radiometry (SABER) instrument on the NASA/TIMED satellite in the lower mesosphere (50-80 km altitude) according to its diurnal, latitudinal, seasonal and solar cycle components. The dominant variation is diurnal and latitudinal. Below 75 km, seasonal and solar cycle effects are less than 5%. Accordingly, we have developed a simple climatology that depends upon local time and latitude and applied it to a model of the D region of the ionosphere. Between 60 and 70 km, atomic oxygen is important in governing the ratio of negative ions to electrons. Using the SABER O climatology along with a previously published climatology of nitric oxide based upon UARS/HALOE data, we compare our model results both to previous calculations and to a profile of electron density [e(-)] acquired by a rocket launched from Kwajalein Atoll. The model results are shown to be consistent with previously published calculations, but the comparison with the data reveals a dramatic discrepancy whereby the calculated [e(-)] is over an order of magnitude less than the observations below 65 km. The most plausible explanation involves changing the partition of negative charge between molecules such as O-2 which rapidly dissociate in sunlight versus heavier, more stable negative ions. Although observations of [e(-)] below 70 km are difficult and infrequent, more research should be invested to evaluate the pervasiveness and the seasonal, latitudinal and diurnal morphology of this model [e(-)] deficit. This may have practical implications as empirical models of the ionosphere predict a secondary maximum in HF radio absorption in the 70 km altitude region. Published by Elsevier Ltd.
C1 [Siskind, David E.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Marshall, Tom] GATS Inc, Hampton, VA USA.
[Friedrich, Martin] Graz Univ Technol, A-8010 Graz, Austria.
[Gumbel, Joerg] Stockholm Univ, MISU, S-10691 Stockholm, Sweden.
RP Siskind, DE (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM david.siskind@nrl.navy.mil
FU Chief of Naval Research; NASA/TIMED SABER project [NNG11PX00I]
FX This work was sponsored by the Chief of Naval Research and the
NASA/TIMED SABER project through Interagency Purchase Request
NNG11PX00I.
NR 29
TC 1
Z9 1
U1 1
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD MAR
PY 2015
VL 124
BP 63
EP 70
DI 10.1016/j.jastp.2015.01.014
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA CC7EF
UT WOS:000350529800008
ER
PT J
AU Cowling, RM
Potts, AJ
Bradshaw, PL
Colville, J
Arianoutsou, M
Ferrier, S
Forest, F
Fyllas, NM
Hopper, SD
Ojeda, F
Proches, S
Smith, RJ
Rundel, PW
Vassilakis, E
Zutta, BR
AF Cowling, Richard M.
Potts, Alastair J.
Bradshaw, Peter L.
Colville, Jonathan
Arianoutsou, Margarita
Ferrier, Simon
Forest, Felix
Fyllas, Nikolaos M.
Hopper, Stephen D.
Ojeda, Fernando
Proches, Serban
Smith, Rhian J.
Rundel, Philip W.
Vassilakis, Emmanuel
Zutta, Brian R.
TI Variation in plant diversity in mediterranean-climate ecosystems: the
role of climatic and topographical stability
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE California; Cape Floristic Region; central Chile; diversification rate;
mature radiation; Mediterranean Basin; OCBIL; recent radiation;
south-western Australia; YODFEL
ID CAPE FLORISTIC REGION; SOUTH-AFRICA; BIODIVERSITY HOTSPOT;
WESTERN-AUSTRALIA; CALIFORNIA FLORA; BETIC CORDILLERA; GLOBAL PATTERNS;
NON-CONVERGENCE; ROCK UPLIFT; EVOLUTION
AB AimAlthough all five of the major mediterranean-climate ecosystems (MCEs) of the world are recognized as loci of high plant species diversity and endemism, they show considerable variation in regional-scale richness. Here, we assess the role of stable Pleistocene climate and Cenozoic topography in explaining variation in regional richness of the globe's MCEs. We hypothesize that older, more climatically stable MCEs would support more species, because they have had more time for species to accumulate than MCEs that were historically subject to greater topographic upheavals and fluctuating climates.
LocationSouth-western Africa (Cape), south-western Australia, California, central Chile and the eastern (Greece) and western (Spain) Mediterranean Basin.
MethodsWe estimated plant diversity for each MCE as the intercepts of species-area curves that are homogeneous in slope across all regions. We used two down-scaled global circulation models of the Last Glacial Maximum (LGM) to quantify climate stability by comparing the change in the location of MCEs between the LGM and present. We quantified the Cenozoic topographic stability of each MCE by comparing contemporary topographic profiles with those present in the late Oligocene and the early Pliocene.
ResultsThe most diverse MCEs - Cape and Australia - had the highest Cenozoic environmental stability, and the least diverse - Chile and California - had the lowest stability.
Main conclusionsVariation in plant diversity in MCEs is likely to be a consequence not of differences in diversification rates, but rather the persistence of numerous pre-Pliocene clades in the more stable MCEs. The extraordinary plant diversity of the Cape is a consequence of the combined effects of both mature and recent radiations, the latter associated with increased habitat heterogeneity produced by mild tectonic uplift in the Neogene.
C1 [Cowling, Richard M.; Potts, Alastair J.; Bradshaw, Peter L.] Nelson Mandela Metropolitan Univ, Dept Bot, ZA-6032 Port Elizabeth, South Africa.
[Bradshaw, Peter L.] Nelson Mandela Metropolitan Univ, South African Natl Pk, ZA-6031 Port Elizabeth, South Africa.
[Colville, Jonathan] South African Natl Biodivers Inst, Appl Biodivers Res Div, ZA-7735 Claremont, South Africa.
[Arianoutsou, Margarita; Fyllas, Nikolaos M.] Univ Athens, Fac Biol, Dept Systemat & Ecol, Athens 15784, Greece.
[Ferrier, Simon] CSIRO Ecosyst Sci, Canberra, ACT 2601, Australia.
[Forest, Felix; Hopper, Stephen D.; Smith, Rhian J.] Royal Bot Gardens, Richmond TW9 3DS, Surrey, England.
[Hopper, Stephen D.] Univ Western Australia, Ctr Excellence Nat Resource Management, Albany 6330, Australia.
[Hopper, Stephen D.] Univ Western Australia, Sch Plant Biol, Albany 6330, Australia.
[Ojeda, Fernando] Univ Cadiz, Dept Biol, Puerto Real 11510, Spain.
[Proches, Serban] Univ KwaZulu Natal, Sch Biol & Conservat Sci, ZA-3209 Scottsville, South Africa.
[Rundel, Philip W.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Vassilakis, Emmanuel] Univ Athens, Fac Geol & Geoenvironm, Dept Dynam, Athens 15784, Greece.
[Zutta, Brian R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cowling, RM (reprint author), Nelson Mandela Metropolitan Univ, Dept Bot, POB 77000, ZA-6031 Port Elizabeth, South Africa.
EM richard.cowling@nmmu.ac.za
RI Ferrier, Simon/C-1490-2009; Proches, Serban/A-2044-2008; Ojeda,
Fernando/L-1626-2014; Hopper, Stephen/G-4222-2012;
OI Ferrier, Simon/0000-0001-7884-2388; Ojeda, Fernando/0000-0001-5480-0925;
Vassilakis, Emmanuel/0000-0002-1175-3628; Fyllas,
Nikolaos/0000-0002-5651-5578
FU National Research Foundation; Nelson Mandela Metropolitan University;
Claude Leon Foundation; Stunt Ranch Santa Monica Mountains Reserve
FX We thank the South African National Biodiversity Institute for hosting
the workshop on which this contribution is based. R.M.C. acknowledges
the National Research Foundation and Nelson Mandela Metropolitan
University for funding; A.J.P. was supported by funding from the Claude
Leon Foundation; P.W.R. was supported by funding from the Stunt Ranch
Santa Monica Mountains Reserve; M.A. thanks M. Panitsa and I. Bazos for
providing references for the flora of the Aegean islands.
NR 100
TC 17
Z9 17
U1 8
U2 69
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0305-0270
EI 1365-2699
J9 J BIOGEOGR
JI J. Biogeogr.
PD MAR
PY 2015
VL 42
IS 3
BP 552
EP 564
DI 10.1111/jbi.12429
PG 13
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA CC7PG
UT WOS:000350559900013
ER
PT J
AU Jiang, JH
Su, H
Zhai, CX
Shen, TJ
Wu, TW
Zhang, J
Cole, JNS
von Salzen, K
Donner, LJ
Seman, C
Del Genio, A
Nazarenko, LS
Dufresne, JL
Watanabe, M
Morcrette, C
Koshiro, T
Kawai, H
Gettelman, A
Millan, L
Read, WG
Livesey, NJ
Kasai, Y
Shiotani, M
AF Jiang, Jonathan H.
Su, Hui
Zhai, Chengxing
Shen, T. Janice
Wu, Tongwen
Zhang, Jie
Cole, Jason N. S.
von Salzen, Knut
Donner, Leo J.
Seman, Charles
Del Genio, Anthony
Nazarenko, Larissa S.
Dufresne, Jean-Louis
Watanabe, Masahiro
Morcrette, Cyril
Koshiro, Tsuyoshi
Kawai, Hideaki
Gettelman, Andrew
Millan, Luis
Read, William G.
Livesey, Nathaniel J.
Kasai, Yasko
Shiotani, Masato
TI Evaluating the Diurnal Cycle of Upper-Tropospheric Ice Clouds in Climate
Models Using SMILES Observations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; TROPICAL OCEANIC CONVECTION; SYSTEM MODEL;
CUMULUS CONVECTION; ATMOSPHERE MODEL; UNITED-STATES; WATER-VAPOR;
PRECIPITATION; SCHEME; CMIP5
AB Upper-tropospheric ice cloud measurements from the Superconducting Submillimeter Limb Emission Sounder (SMILES) on the International Space Station (ISS) are used to study the diurnal cycle of upper-tropospheric ice cloud in the tropics and midlatitudes (40 degrees S-40 degrees N) and to quantitatively evaluate ice cloud diurnal variability simulated by 10 climatemodels. Over land, the SMILES-observed diurnal cycle has a maximum around 1800 local solar time (LST), while the model-simulated diurnal cycles have phases differing from the observed cycle by -4 to 12 h. Over ocean, the observations show much smaller diurnal cycle amplitudes than over land with a peak at 1200 LST, while the modeled diurnal cycle phases are widely distributed throughout the 24-h period. Most models show smaller diurnal cycle amplitudes over ocean than over land, which is in agreement with the observations. However, there is a large spread of modeled diurnal cycle amplitudes ranging from 20% to more than 300% of the observed over both land and ocean. Empirical orthogonal function (EOF) analysis on the observed and model-simulated variations of ice clouds finds that the first EOF modes over land from both observation and model simulations explain more than 70% of the ice cloud diurnal variations and they have similar spatial and temporal patterns. Over ocean, the first EOF from observation explains 26.4% of the variance, while the first EOF from most models explains more than 70%. The modeled spatial and temporal patterns of the leading EOFs over ocean show large differences from observations, indicating that the physical mechanisms governing the diurnal cycle of oceanic ice clouds are more complicated and not well simulated by the current climate models.
C1 [Jiang, Jonathan H.; Su, Hui; Zhai, Chengxing; Shen, T. Janice; Millan, Luis; Read, William G.; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wu, Tongwen; Zhang, Jie] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China.
[Cole, Jason N. S.; von Salzen, Knut] Environm Canada, Canadian Ctr Climate Modeling & Anal, Victoria, BC, Canada.
[Donner, Leo J.; Seman, Charles] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Del Genio, Anthony; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dufresne, Jean-Louis] Inst Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France.
[Watanabe, Masahiro] Univ Tokyo, Atmosphere & Ocean Res Inst, Model Interdisciplinary Res Climate, Kashiwa, Chiba, Japan.
[Morcrette, Cyril] Met Off Hadley Ctr, Exeter, Devon, England.
[Koshiro, Tsuyoshi; Kawai, Hideaki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
[Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Kasai, Yasko] Natl Inst Informat & Commun Technol, Tokyo, Japan.
[Shiotani, Masato] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto, Japan.
RP Jiang, JH (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91011 USA.
EM jonathan.h.jiang@jpl.nasa.gov
RI Morcrette, Cyril/H-7282-2012; Dufresne, Jean-Louis/I-5616-2015; Millan,
Luis/J-2759-2015; Koshiro, Tsuyoshi/O-7183-2016;
OI Morcrette, Cyril/0000-0002-4240-8472; Dufresne,
Jean-Louis/0000-0003-4764-9600; Koshiro, Tsuyoshi/0000-0003-2971-7446;
Cole, Jason/0000-0003-0450-2748
FU NASA [ROSES08-USPI, ROSES12-MAP, ROSES13-NDOA]; NASA; BCC; CCCma; GFDL;
GISS; IPSL; MIROC; MOHC; MRI; NCAR; MERRA
FX The authors appreciate the funding support by the NASA ROSES08-USPI,
ROSES12-MAP, and ROSES13-NDOA programs. This work was performed at the
NASA-sponsored Jet Propulsion Laboratory, California Institute of
Technology. We are also very thankful for the support from climate
modeling centers across the globe, including BCC, CCCma, GFDL, GISS,
IPSL, MIROC, MOHC, MRI, NCAR, and MERRA.
NR 98
TC 8
Z9 8
U1 3
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAR
PY 2015
VL 72
IS 3
BP 1022
EP 1044
DI 10.1175/JAS-D-14-0124.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC4OQ
UT WOS:000350333100004
ER
PT J
AU Venter, C
Kopp, A
Harding, AK
Gonthier, PL
Busching, I
AF Venter, Christo
Kopp, Andreas
Harding, Alice K.
Gonthier, Peter L.
Buesching, Ingo
TI The contribution of millisecond pulsars to the Galactic cosmic-ray
lepton spectrum
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Cosmic rays; Pulsars; Electrons; Positrons
ID INTERSTELLAR RADIATION-FIELD; POSITRON EXCESS; NEARBY PULSARS; AREA
TELESCOPE; MILKY-WAY; ELECTRONS; EMISSION; ORIGIN; PROPAGATION; MODELS
AB Pulsars are believed to be sources of relativistic electrons and positrons. The abundance of detections of gamma-ray millisecond pulsars by Fermi Large Area Telescope coupled with their light curve characteristics that imply copious pair production in their magnetospheres, motivated us to investigate this old pulsar population as a source of Galactic electrons and positrons and their contribution to the enhancement in cosmic-ray positron flux at GeV energies. We use a population synthesis code to predict the source properties (number, position, and power) of the present-day Galactic millisecond pulsars, taking into account the latest Fermi and radio observations to calibrate the model output. Next, we simulate pair cascade spectra from these pulsars using a model that invokes an offset-dipole magnetic field. We assume free escape of the pairs from the pulsar environment. We then compute the cumulative spectrum of transported electrons and positrons at Earth, following their diffusion and energy losses as they propagate through the Galaxy. Our results indicate that the predicted particle flux increases for non-zero offsets of the magnetic polar caps. Comparing our predicted local interstellar spectrum and positron fraction to measurements by AMS-02, PAMELA, and Fermi, we find that millisecond pulsars are only modest contributors at a few tens of GeV, after which this leptonic spectral component cuts off. The positron fraction is therefore only slightly enhanced above 10 GeV relative to a background flux model. This implies that alternative sources such as young, nearby pulsars and supernova remnants should contribute additional primary positrons within the astrophysical scenario.
C1 [Venter, Christo; Kopp, Andreas; Buesching, Ingo] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Harding, Alice K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Gonthier, Peter L.] Hope Coll, Dept Phys, Holland, MI 49423 USA.
RP Venter, C (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa.
EM Christo.Venter@nwu.ac.za
NR 50
TC 3
Z9 3
U1 0
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD MAR 1
PY 2015
VL 55
IS 5
BP 1529
EP 1536
DI 10.1016/j.asr.2014.12.022
PG 8
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CB6HJ
UT WOS:000349727800022
ER
PT J
AU Duncan, C
Chauvenet, ALM
Brown, ME
Pettorelli, N
AF Duncan, Clare
Chauvenet, Alienor L. M.
Brown, Molly E.
Pettorelli, Nathalie
TI Energy availability, spatio-temporal variability and implications for
animal ecology
SO DIVERSITY AND DISTRIBUTIONS
LA English
DT Article
DE Body mass; energy; interannual variability; macro-ecology; NDVI; trophic
level
ID LARGE HERBIVORES; HOME-RANGE; PRIMARY PRODUCTIVITY; TEMPORAL VARIATION;
SPECIES RICHNESS; BODY-SIZE; BIODIVERSITY; PATTERNS; COMMUNITIES;
DIVERSITY
AB AimGlobal environmental change, through anthropogenic activities and climatic changes, is promoting broad-scale alterations to energy availability across the world's ecosystems. However, spatio-temporal variation in available energy is a key driver of animals' life histories, movement patterns and abundance, thus shaping the global distribution of individuals and species. As such, there is an increasing need to understand how and where changes to energy availability will produce the greatest impacts on animal ecology, and ultimately on the distribution of biodiversity.
LocationGlobal.
MethodsWe compiled data from the published literature where attempts (n=171) have been made to find linkages between prevailing energy availability (primary productivity, indexed by the Normalized Difference Vegetation Index; NDVI) and ecological parameters (abundance, distribution and life histories) for bird and mammal species. We extracted information on trophic level (diet) and body mass for the species considered in these studies, as well as long-term site-specific average energy availability, and levels of seasonality and interannual stability (all indexed using NDVI-based metrics as proxies). We conducted a GLMM analysis to assess how these variables may structure the variability in the reported linkages between prevailing energy availability and the considered ecological parameters.
ResultsOur analysis revealed that the strength of the reported relationships between metrics of prevailing energy availability and ecological parameters was highest in environments with high long-term interannual stability in available energy, and for larger, non-carnivorous animals. Importantly, we found no support for an influence of long-term site-specific average energy availability on the strength of these relationships.
Main conclusionsOverall, our results support the hypothesis that temporal stability in energy availability is a key factor controlling animal ecology over total available energy itself. These results may have some important implications for the future health and conservation requirements of currently largely stable regions under global environmental change.
C1 [Duncan, Clare; Chauvenet, Alienor L. M.; Pettorelli, Nathalie] Zool Soc London, Inst Zool, London NW1 4RY, England.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pettorelli, N (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England.
EM nathalie.pettorelli@ioz.ac.uk
RI Chauvenet, Alienor/L-9135-2015; Brown, Molly/E-2724-2010
OI Chauvenet, Alienor/0000-0002-3743-7375; Brown, Molly/0000-0001-7384-3314
NR 71
TC 1
Z9 1
U1 6
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1366-9516
EI 1472-4642
J9 DIVERS DISTRIB
JI Divers. Distrib.
PD MAR
PY 2015
VL 21
IS 3
BP 290
EP 301
DI 10.1111/ddi.12270
PG 12
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CB9RN
UT WOS:000349970100005
ER
PT J
AU Carnevali, PBM
Rohrssen, M
Williams, MR
Michaud, AB
Adams, H
Berisford, D
Love, GD
Priscu, JC
Rassuchine, O
Hand, KP
Murray, AE
AF Carnevali, P. B. Matheus
Rohrssen, M.
Williams, M. R.
Michaud, A. B.
Adams, H.
Berisford, D.
Love, G. D.
Priscu, J. C.
Rassuchine, O.
Hand, K. P.
Murray, A. E.
TI Methane sources in arctic thermokarst lake sediments on the North Slope
of Alaska
SO GEOBIOLOGY
LA English
DT Article
ID ORGANIC-CARBON; ISOTOPE FRACTIONATION; COMMUNITY COMPOSITION;
SEASONAL-VARIATION; MARINE-SEDIMENTS; WATER INTERFACE; PERMAFROST THAW;
OXYGEN-UPTAKE; TEMPERATURE; OXIDATION
AB The permafrost on the North Slope of Alaska is densely populated by shallow lakes that result from thermokarst erosion. These lakes release methane (CH4) derived from a combination of ancient thermogenic pools and contemporary biogenic production. Despite the potential importance of CH4 as a greenhouse gas, the contribution of biogenic CH4 production in arctic thermokarst lakes in Alaska is not currently well understood. To further advance our knowledge of CH4 dynamics in these lakes, we focused our study on (i) the potential for microbial CH4 production in lake sediments, (ii) the role of sediment geochemistry in controlling biogenic CH4 production, and (iii) the temperature dependence of this process. Sediment cores were collected from one site in Siqlukaq Lake and two sites in Sukok Lake in late October to early November. Analyses of pore water geochemistry, sedimentary organic matter and lipid biomarkers, stable carbon isotopes, results from CH4 production experiments, and copy number of a methanogenic pathway-specific gene (mcrA) indicated the existence of different sources of CH4 in each of the lakes chosen for the study. Analysis of this integrated data set revealed that there is biological CH4 production in Siqlukaq at moderate levels, while the very low levels of CH4 detected in Sukok had a mixed origin, with little to no biological CH4 production. Furthermore, methanogenic archaea exhibited temperature-dependent use of in situ substrates for methanogenesis, and the amount of CH4 produced was directly related to the amount of labile organic matter in the sediments. This study constitutes an important first step in better understanding the actual contribution of biogenic CH4 from thermokarst lakes on the coastal plain of Alaska to the current CH4 budgets.
C1 [Carnevali, P. B. Matheus; Rassuchine, O.; Murray, A. E.] Univ Nevada, Desert Res Inst, Div Earth & Ecosyst Sci, Reno, NV 89506 USA.
[Carnevali, P. B. Matheus; Rassuchine, O.] Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA.
[Rohrssen, M.; Williams, M. R.; Love, G. D.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Michaud, A. B.; Adams, H.; Priscu, J. C.] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA.
[Berisford, D.; Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Murray, AE (reprint author), Univ Nevada, Desert Res Inst, Div Earth & Ecosyst Sci, Reno, NV 89506 USA.
EM kevin.p.hand@jpl.nasa.gov; alison.murray@dri.edu
FU Division of Earth and Ecosystem Sciences, DRI; NSF IGERT Program in
Geobiological Systems [DGE 0654336]; Jet Propulsion Laboratory (JPL),
California Institute of Technology, under National Aeronautics and Space
Administration (NASA); NASA Astrobiology Institute; Astrobiology of Icy
Worlds program at JPL; NASA Astrobiology Science and Technology for
Exploring Planets (ASTEP) award (Project Narvak) [NNN13D036T]
FX We especially thank A. Klesh, J. Leichty, and P. Santibanez, for
assistance in the field; K. Walter Anthony for sharing her observations
about the study area; and Frank Loffler for analyses of pore waters in
the University of Tennessee. We are very grateful to N. Riedinger, J.
Memmott, G. Miller, E. Ulrich, M. Miller, G. Trubl, J. Dodsworth, B.
Hedlund, and J. Qualls for invaluable technical support. Likewise, we
appreciate the efforts of the Barrow Arctic Science Consortium (BASC)
and the UMIAQ Corporation in Barrow, AK, for providing logistical
support and insight into the local region. Special thanks to the
anonymous reviewers of the manuscript and to Life Technologies for use
of the Applied Biosystems 7500 Fast system to conduct qPCR. PMC was
supported in part by the Division of Earth and Ecosystem Sciences, DRI.
Funding for ABM was provided in part by NSF IGERT Program in
Geobiological Systems (DGE 0654336). KPH and DB acknowledge support
through the Jet Propulsion Laboratory (JPL), California Institute of
Technology, under contract with the National Aeronautics and Space
Administration (NASA). Financial support for this work was provided in
part by the NASA Astrobiology Institute, Astrobiology of Icy Worlds
program at JPL, and a NASA Astrobiology Science and Technology for
Exploring Planets (ASTEP) award (Project Narvak, NNN13D036T). Support
from these programs is gratefully acknowledged.
NR 89
TC 2
Z9 2
U1 6
U2 44
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD MAR
PY 2015
VL 13
IS 2
BP 181
EP 197
DI 10.1111/gbi.12124
PG 17
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA CC0UR
UT WOS:000350053400007
ER
PT J
AU Sabaka, TJ
Olsen, N
Tyler, RH
Kuvshinov, A
AF Sabaka, Terence J.
Olsen, Nils
Tyler, Robert H.
Kuvshinov, Alexey
TI CM5, a pre-Swarm comprehensive geomagnetic field model derived from over
12 yr of CHAMP, Orsted, SAC-C and observatory data
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Geomagnetic induction; Magnetic anomalies: modelling and interpretation;
Magnetic field; Satellite magnetics
ID EARTHS MAGNETIC-FIELD; SECULAR VARIATION; GLOBAL INDUCTION; SATELLITE
DATA; CONSTELLATION; RESPONSES; PRODUCTS; SPHERE
AB A comprehensive magnetic field model named CM5 has been derived from CHAMP, Orsted and SAC-C satellite and observatory hourly-means data from 2000 August to 2013 January using the Swarm Level-2 Comprehensive Inversion (CI) algorithm. Swarm is a recently launched constellation of three satellites to map the Earth's magnetic field. The CI technique includes several interesting features such as the bias mitigation scheme known as Selective Infinite Variance Weighting (SIVW), a new treatment for attitude error in satellite vector measurements, and the inclusion of 3-D conductivity for ionospheric induction. SIVW has allowed for a much improved lithospheric field recovery over CM4 by exploiting CHAMP along-track difference data yielding resolution levels up to spherical harmonic degree 107, and has allowed for the successful extraction of the oceanic M-2 tidal magnetic field from quiet, nightside data. The 3-D induction now captures anomalous Solar-quiet features in coastal observatory daily records. CM5 provides a satisfactory, continuous description of the major magnetic fields in the near-Earth region over this time span, and its lithospheric, ionospheric and oceanic M-2 tidal constituents may be used as validation tools for future Swarm Level-2 products coming from the CI algorithm and other dedicated product algorithms.
C1 [Sabaka, Terence J.; Tyler, Robert H.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Olsen, Nils] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Tyler, Robert H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kuvshinov, Alexey] ETH, Inst Geophys, CH-8092 Zurich, Switzerland.
RP Sabaka, TJ (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM Terence.J.Sabaka@nasa.gov
RI Olsen, Nils/H-1822-2011
OI Olsen, Nils/0000-0003-1132-6113
FU NASA Earth Surface and Interior program
FX We thank Vincent Lesur and an anonymous reviewer for valuable comments
that improved the quality of the paper. The NASA Center for Climate
Simulation at Goddard Space Flight Center provided computational
resources. TJS and RHT are supported by the NASA Earth Surface and
Interior program.
NR 61
TC 31
Z9 33
U1 5
U2 20
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD MAR
PY 2015
VL 200
IS 3
BP 1596
EP 1626
DI 10.1093/gji/ggu493
PG 31
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CC0RG
UT WOS:000350042800022
ER
PT J
AU Li, T
Hasegawa, T
Yin, XY
Zhu, Y
Boote, K
Adam, M
Bregaglio, S
Buis, S
Confalonieri, R
Fumoto, T
Gaydon, D
Marcaida, M
Nakagawa, H
Oriol, P
Ruane, AC
Ruget, F
Singh, B
Singh, U
Tang, L
Tao, FL
Wilkens, P
Yoshida, H
Zhang, Z
Bouman, B
AF Li, Tao
Hasegawa, Toshihiro
Yin, Xinyou
Zhu, Yan
Boote, Kenneth
Adam, Myriam
Bregaglio, Simone
Buis, Samuel
Confalonieri, Roberto
Fumoto, Tamon
Gaydon, Donald
Marcaida, Manuel, III
Nakagawa, Hiroshi
Oriol, Philippe
Ruane, Alex C.
Ruget, Francoise
Singh, Balwinder-
Singh, Upendra
Tang, Liang
Tao, Fulu
Wilkens, Paul
Yoshida, Hiroe
Zhang, Zhao
Bouman, Bas
TI Uncertainties in predicting rice yield by current crop models under a
wide range of climatic conditions
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE AgMIP; climate change; crop-model ensembles; Oryza sativa; yield
prediction uncertainty
ID AIR CO2 ENRICHMENT; HIGH-TEMPERATURE STRESS; ELEVATED CO2; SPIKELET
FERTILITY; NIGHT TEMPERATURE; CARBON-DIOXIDE; GROWTH; STERILITY; FACE;
PRODUCTIVITY
AB Predicting rice (Oryza sativa) productivity under future climates is important for global food security. Ecophysiological crop models in combination with climate model outputs are commonly used in yield prediction, but uncertainties associated with crop models remain largely unquantified. We evaluated 13 rice models against multi-year experimental yield data at four sites with diverse climatic conditions in Asia and examined whether different modeling approaches on major physiological processes attribute to the uncertainties of prediction to field measured yields and to the uncertainties of sensitivity to changes in temperature and CO2 concentration [CO2]. We also examined whether a use of an ensemble of crop models can reduce the uncertainties. Individual models did not consistently reproduce both experimental and regional yields well, and uncertainty was larger at the warmest and coolest sites. The variation in yield projections was larger among crop models than variation resulting from 16 global climate model-based scenarios. However, the mean of predictions of all crop models reproduced experimental data, with an uncertainty of less than 10% of measured yields. Using an ensemble of eight models calibrated only for phenology or five models calibrated in detail resulted in the uncertainty equivalent to that of the measured yield in well-controlled agronomic field experiments. Sensitivity analysis indicates the necessity to improve the accuracy in predicting both biomass and harvest index in response to increasing [CO2] and temperature.
C1 [Li, Tao; Marcaida, Manuel, III; Bouman, Bas] Int Rice Res Inst, Los Banos, Philippines.
[Hasegawa, Toshihiro; Fumoto, Tamon] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 305, Japan.
[Yin, Xinyou] Wageningen Univ, Ctr Crop Syst Anal, NL-6700 AP Wageningen, Netherlands.
[Zhu, Yan; Tang, Liang] Nanjing Agr Univ, Natl Engn & Technol Ctr Informat Agr, Nanjing, Jiangsu, Peoples R China.
[Boote, Kenneth] Univ Florida, Gainesville, FL USA.
[Adam, Myriam; Oriol, Philippe] CIRAD, UMR AGAP, Montpellier, France.
[Bregaglio, Simone; Confalonieri, Roberto] Univ Milan, DiSAA, Cassandra Lab, Milan, Italy.
[Buis, Samuel; Ruget, Francoise] INRA, EMMAH UMR1114, F-84914 Avignon, France.
[Gaydon, Donald] CSIRO Agr Flagship, Brisbane, Qld, Australia.
[Nakagawa, Hiroshi; Yoshida, Hiroe] Natl Agr & Food Res Org, Tsukuba, Ibaraki, Japan.
[Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Singh, Balwinder-] CIMMYT, New Delhi 110008, India.
[Singh, Upendra; Wilkens, Paul] Int Fertilizer Dev Ctr, Muscle Shoals, AL 35662 USA.
[Tao, Fulu] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing, Peoples R China.
[Zhang, Zhao] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China.
[Ruget, Francoise] UAPV, EMMAH UMR1114, F-84914 Avignon, France.
RP Hasegawa, T (reprint author), Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 305, Japan.
EM thase@affrc.go.jp; Xinyou.Yin@wur.nl
RI Gaydon, Donald /F-4608-2012; YADAV, SUDHIR/K-7110-2012; Singh,
Balwinder/F-3063-2011;
OI YADAV, SUDHIR/0000-0001-7658-8144; Singh, Balwinder/0000-0002-6715-2207;
Gaydon, Donald/0000-0002-0078-4154; Boote, Kenneth/0000-0002-1358-5496
FU International Rice Research Institute (IRRI) through the Global Rice
Science Partnership (GRiSP); NASA Modeling, Analysis, and Prediction
Program
FX This study was partly financed by the International Rice Research
Institute (IRRI) through the Global Rice Science Partnership (GRiSP). We
are grateful to the members of the AgMIP Leadership team for their
support and to Senthold Asseng and Frank Ewert for sharing their
insights in the AgMIP Wheat team. IRRI (via Dr. Sudhir Yadav and Dr.
Roland Buresh), Nanjing Agricultural University (China), and the
National Institute for Agro-Environmental Sciences (Japan) kindly
provided the experimental data used in this study. We acknowledge the
global climate modeling groups, the Program for Climate Model Diagnosis
and Intercomparison (PCMDI), and the WCRP's Working Group on Coupled
Modelling (WGCM) for making the WCRP CMIP3 multi-model dataset
available. Support for this dataset is provided by the Office of
Science, U.S. Department of Energy. Dr. Ruane's participation in the
study was supported by the NASA Modeling, Analysis, and Prediction
Program.
NR 42
TC 41
Z9 41
U1 11
U2 98
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD MAR
PY 2015
VL 21
IS 3
BP 1328
EP 1341
DI 10.1111/gcb.12758
PG 14
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CB8QS
UT WOS:000349896400025
PM 25294087
ER
PT J
AU Li, YR
Zeng, XW
Agui, J
AF Li, Yuru
Zeng, Xiangwu
Agui, Juan
TI Developing a Lightweight
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Geotechnical; Mobility; Simulant; Sinkage
ID MARTIAN ATMOSPHERE; MARS; PATHFINDER; SIMULANT; DEPOSITS; ROVER
AB The geotechnical properties of Martian soils are critical parameters in predicting and simulating soil behavior with regard to vehicle performance on Mars. In preparation for manned or robotic missions to Mars, surface vehicles must be tested on terrains that represent the mechanical characteristics of the Martian ground. This paper presents the development of a lightweight simulant and its preparation method to emulate the mechanical properties of Martian soil for high sinkage mobility tests. A geotechnical testing program was developed to measure specific gravity, particle size distribution, bulk density, compression indices and shear strength. The simulant can achieve the typical Martian regolith density range, which is approximately 38% of that on earth. This is of particular importance because strength parameters of granular materials, which characterize the plastic behavior of soil samples in sinkage tests, are controlled by the effective confining pressure, which itself is induced by gravity. (C) 2014 American Society of Civil Engineers.
C1 [Li, Yuru; Zeng, Xiangwu] Case Western Reserve Univ, Dept Civil Engn, Cleveland, OH 44106 USA.
[Agui, Juan] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Zeng, XW (reprint author), Case Western Reserve Univ, Dept Civil Engn, 10900 Euclid Ave, Cleveland, OH 44106 USA.
EM xxz16@cwru.edu
FU NASA Glenn Research Center
FX The first two authors would like to thank the financial support provided
by NASA Glenn Research Center through a research grant for the work
reported in this paper.
NR 33
TC 2
Z9 2
U1 3
U2 13
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 MAR
PY 2015
VL 28
IS 2
AR 04014058
DI 10.1061/(ASCE)AS.1943-5525.0000377
PG 7
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA CB8CK
UT WOS:000349855800002
ER
PT J
AU Hebert, P
Bajracharya, M
Ma, J
Hudson, N
Aydemir, A
Reid, J
Bergh, C
Borders, J
Frost, M
Hagman, M
Leichty, J
Backes, P
Kennedy, B
Karplus, P
Satzinger, B
Byl, K
Shankar, K
Burdick, J
AF Hebert, Paul
Bajracharya, Max
Ma, Jeremy
Hudson, Nicolas
Aydemir, Alper
Reid, Jason
Bergh, Charles
Borders, James
Frost, Matthew
Hagman, Michael
Leichty, John
Backes, Paul
Kennedy, Brett
Karplus, Paul
Satzinger, Brian
Byl, Katie
Shankar, Krishna
Burdick, Joel
TI Mobile Manipulation and Mobility as Manipulation-Design and Algorithms
of RoboSimian
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
AB This article presents the hardware design and software algorithms of RoboSimian, a statically stable quadrupedal robot capable of both dexterous manipulation and versatile mobility in difficult terrain. The robot has generalized limbs and hands capable of mobility and manipulation, along with almost fully hemispherical three-dimensional sensing with passive stereo cameras. The system is semiautonomous, enabling low-bandwidth, high latency control operated from a standard laptop. Because limbs are used for mobility and manipulation, a single unified mobile manipulation planner is used to generate autonomous behaviors, including walking, sitting, climbing, grasping, and manipulating. The remote operator interface is optimized to designate, parametrize, sequence, and preview behaviors, which are then executed by the robot. RoboSimian placed fifth in the DARPA Robotics Challenge Trials, demonstrating its ability to perform disaster recovery tasks in degraded human environments.
C1 [Hebert, Paul; Bajracharya, Max; Ma, Jeremy; Hudson, Nicolas; Aydemir, Alper; Reid, Jason; Bergh, Charles; Borders, James; Frost, Matthew; Hagman, Michael; Leichty, John; Backes, Paul; Kennedy, Brett] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Karplus, Paul] Stanford Univ, Palo Alto, CA 94305 USA.
[Satzinger, Brian; Byl, Katie] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Shankar, Krishna; Burdick, Joel] CALTECH, Pasadena, CA 91125 USA.
RP Hebert, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paul.Hebert@jpl.nasa.gov
FU DARPA Robotics Challenge Track A program; NASA
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, with funding
from the DARPA Robotics Challenge Track A program through an agreement
with NASA.
NR 15
TC 13
Z9 13
U1 0
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD MAR
PY 2015
VL 32
IS 2
SI SI
BP 255
EP 274
DI 10.1002/rob.21566
PG 20
WC Robotics
SC Robotics
GA CC0BI
UT WOS:000349999600006
ER
PT J
AU Raj, SV
AF Raj, S. V.
TI Comparison of the Thermal Expansion Behavior of Several Intermetallic
Silicide Alloys Between 293 and 1523 K
SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE
LA English
DT Article
DE CTE; disilicides; intermetallic alloys; thermal expansion
ID COMPOSITES
AB Thermal expansion measurements were conducted on hot-pressed CrSi2, TiSi2, WSi2 and a two-phase Cr-Mo-Si intermetallic alloy between 303 and 1523 K during three heat-cool cycles. The corrected thermal expansion, (Delta L/L-0)(thermal), varied with the absolute temperature, T, as
(Delta L/L-0)(thermal) = A(T - 293)(3) + B(T - 293)(2) + C(T - 293) + D
where, A, B, C, and D are regression constants. Excellent reproducibility was observed for most of the materials after the first heat-up cycle. In some cases, the data from first heat-up cycle deviated from those determined in the subsequent cycles. This deviation was attributed to the presence of residual stresses developed during processing, which are relieved after the first heat-up cycle.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Raj, SV (reprint author), NASA, Glenn Res Ctr, MS 106-5,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sai.v.raj@nasa.gov
FU NASA's ARMD Seedling Fund Program
FX The author thanks the late Ms. Anna Palczer for conducting the thermal
expansion measurements. This research was supported by a generous Grant
from NASA's ARMD Seedling Fund Program, and this is gratefully
acknowledged.
NR 20
TC 2
Z9 2
U1 1
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1059-9495
EI 1544-1024
J9 J MATER ENG PERFORM
JI J. Mater. Eng. Perform.
PD MAR
PY 2015
VL 24
IS 3
BP 1199
EP 1205
DI 10.1007/s11665-015-1390-8
PG 7
WC Materials Science, Multidisciplinary
SC Materials Science
GA CC0WE
UT WOS:000350058600013
ER
PT J
AU Perrin, A
Toon, G
Orphal, J
AF Perrin, Agnes
Toon, Geoffrey
Orphal, Johannes
TI Detection of atmospheric (NO2)-N-15 in the nu(3) spectral region (6.3 mu
m)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Nitrogen dioxide; (NO2)-N-15; nu(3) band; MkIV; 6.3 mu m
ID FAR-INFRARED-SPECTRUM; LINE POSITIONS; STRATOSPHERE; INTENSITIES;
VALIDATION; ISOTOPOMER; TRANSPORT; BANDS; NO2
AB A reinvestigation of the nu(3) band of (NO2)-N-15 has been performed using experimental data acquired in 2000 [Orphal J, Perrin A, Flaud JM, Smimov M, Himmelmann, Voigt S, Burrows JP. J Mol Spec 2000;204:72-9]. The linelist generated in this way during this study was used to detect this isotopologue in the atmosphere for the first time, using balloon-borne solar occultation spectra measured by the JPL MkIV Fourier transform spectrometer. It is shown that over the 15-35 km altitude range where (NO2)-N-15 can be detected, the retrieved 15/14 NO2 ratio is within 5% of the expected value (0.00364), implying that the absolute line intensities in the new linelist are accurate. Over the same altitude range the RMS spectral fitting residuals reduce significantly as a result of including the new (NO2)-N-15 linelist, improving the accuracy of retrievals of all gases that absorb in the 1550-1650 cm(-1) region (e.g., (NO2)-N-14, H2O, HOD, O-2). (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Perrin, Agnes] CNRS, UMR 7583, Lab Interuniv Syst Atmospher, F-94010 Creteil, France.
[Perrin, Agnes] Univ Paris Est Creteil, F-94010 Creteil, France.
[Perrin, Agnes] Univ Paris 07, Inst Paul Simon Laplace, F-94010 Creteil, France.
[Toon, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Orphal, Johannes] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Eggenstein Leopoldshafen, Germany.
RP Perrin, A (reprint author), CNRS, UMR 7583, Lab Interuniv Syst Atmospher, 61 Ave Gen Gaulle, F-94010 Creteil, France.
EM Agnes.Perrin@lisa.u-pec.fr
FU French national program LEFE/INSU (Institut National des Sciences de l'
Univers) of the CNRS (Centre National de la Recherche Scientifique);
NASA
FX Agnes Perrin gratefully acknowledges financial support from the French
national program LEFE/INSU (Institut National des Sciences de l'
Univers) of the CNRS (Centre National de la Recherche Scientifique).
Part of this work was performed within the "Groupement de Recherche
International" (GDRI) "HiResMIR" of the CNRS. Part of this work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. We thank the Columbia Scientific
Ballooning Facility (CSBF) who performed the MkIV balloon launches.
NR 20
TC 0
Z9 0
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 154
BP 91
EP 97
DI 10.1016/j.jqsrt.2014.12.006
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8JY
UT WOS:000349877000010
ER
PT J
AU Videen, G
Sun, WB
Kocifaj, M
Kai, KJ
Kawamoto, K
Horvath, H
Mishchenko, M
AF Videen, Gorden
Sun, Wenbo
Kocifaj, Miroslav
Kai, Kenji
Kawamoto, Kazuaki
Horvath, Helmuth
Mishchenko, Michael
TI Topical issue on optical particle characterization and remote sensing of
the atmosphere: Part II
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
ID 3-DIMENSIONAL DATA ASSIMILATION; SURFACE PRESSURE MEASUREMENTS;
ABSORPTION RADAR SYSTEM; LIGHT-SCATTERING; VALIDATION; MORPHOLOGY;
AEROSOLS; IMPACT; LIDAR; DUST
C1 [Videen, Gorden] INTA, Madrid 28850, Spain.
[Videen, Gorden] Univ Cantabria, Fac Ciencias, Dept Fis Aplicada, Grp Opt, E-39005 Santander, Spain.
[Videen, Gorden] US Army Res Lab, Adelphi, MD 20783 USA.
[Videen, Gorden] Space Sci Inst, Boulder, CO 80301 USA.
[Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Kocifaj, Miroslav] Slovak Acad Sci, Bratislava 84503, Slovakia.
[Kai, Kenji] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Kawamoto, Kazuaki] Nagasaki Univ, Fac Environm Studies, Nagasaki 852, Japan.
[Horvath, Helmuth] Univ Vienna, Dept Phys, A-1090 Vienna, Austria.
[Mishchenko, Michael] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Videen, G (reprint author), INTA, Ctra Ajalvir Km 4, Madrid 28850, Spain.
EM gorden.w.videen.civ@mail.mil
RI Mishchenko, Michael/D-4426-2012
NR 31
TC 1
Z9 1
U1 5
U2 20
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 153
SI SI
BP 1
EP 3
DI 10.1016/j.jqsrt.2015.01.005
PG 3
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8MH
UT WOS:000349883200001
ER
PT J
AU Kawamoto, K
Suzuki, K
AF Kawamoto, Kazuaki
Suzuki, Kentaroh
TI Distributional correspondence of 94-GHz radar reflectivity with the
variation in water cloud properties over the northwestern Pacific and
China
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Cloud microphysics; Drizzle; Precipitation; Vertical profile; CloudSat
ID MICROPHYSICAL PROPERTIES; NOAA AVHRR; MODIS OBSERVATIONS; SATELLITE;
RAIN; LIQUID; OCEANS; PRECIPITATION; MICROWAVE; POLLUTION
AB This paper studied the behavior of 94-GHz radar reflectivity (Z(e)) with variation in the properties of low-level water clouds, such as the effective droplet radius (r(e)), geometrical thickness (D-cld), and liquid water path (LWP), over the northwest Pacific and China. The changes in the distribution of maxZ(e) (the largest Z(e) within a cloud layer) were examined in terms of variation in the cloud parameters such as small, mid and large categories, while maxZ(e) had monomodal distributions regarding variation in r(e) and D-cld, that appeared bimodal in the small category of LWP. It was confirmed that the small category of LWP contained both non-precipitating clouds in the incipient stage and raining clouds in the dissipating stage. Next, optically measured particle size was combined with LWP derived from the microwave measurement to classify the precipitation type. Applying maxZ(e) and D-cld to the analysis of classified precipitation types corroborated the importance of D-cld for examining the occurrence of precipitation. Finally, the position of maxZ(e), relative to the cloud top was investigated using a measure of the probability of precipitation (POP) according to variation in r(e). The results showed that the Pacific and China had 'bow' and 'funnel' shapes, respectively. The emergence of these shapes according to the variation in r(e) was interpreted as the enhancement of Z(e), due to droplet collisional growth and the attenuation of Z(e), by the presence of large particles. Furthermore, a detailed analysis of smaller particles ( <10 mu m in radius) reinforced the idea of rapid, efficient particle growth in the lower part of the cloud. (c) 2014 Elsevier Ltd. All rights reserved.
C1 [Kawamoto, Kazuaki] Nagasaki Univ, Grad Sch Fisheries Sci & Environm Studies, Nagasaki 8528521, Japan.
[Suzuki, Kentaroh] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kawamoto, K (reprint author), Nagasaki Univ, Grad Sch Fisheries Sci & Environm Studies, 1-14 Bunkyo Machi, Nagasaki 8528521, Japan.
EM kazukawa@nagasaki-u.ac.jp
RI Suzuki, Kentaroh/C-3624-2011
FU National Aeronautics and Space Administration
FX K. Kawamoto is supported by Grant-in aid for Scientific Research (B),
Grant-in aid for Challenging Exploratory Research and Grant-in aid for
Scientific Research on Innovative Areas. The CloudSat data products of
2B-GEO-PROF, 2B-TAU, 2C-PRECIP-COLUMN and ECMWF-AUX were provided by the
CloudSat Data Processing Center at CIRA/Colorado State University. Part
of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 42
TC 2
Z9 2
U1 1
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 153
SI SI
BP 38
EP 48
DI 10.1016/j.jqsrt.2014.10.012
PG 11
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8MH
UT WOS:000349883200005
ER
PT J
AU Yan, HR
Huang, JP
Minnis, P
Yi, YH
Sun-Mack, S
Wang, TH
Nakajima, TY
AF Yan, Hongru
Huang, Jianping
Minnis, Patrick
Yi, Yuhong
Sun-Mack, Sunny
Wang, Tianhe
Nakajima, Takashi Y.
TI Comparison of CERES-MODIS cloud microphysical properties with surface
observations over Loess Plateau
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Validation; Cloud microphysical properties; Satellite
ID GENERAL-CIRCULATION MODELS; DROPLET EFFECTIVE RADIUS; ENERGY SYSTEM
CERES; ARM SGP SITE; SATELLITE MEASUREMENTS; FEEDBACK PROCESSES; CLIMATE
FEEDBACK; RADIATION; SENSITIVITY; GROWTH
AB To enhance the utility of satellite-derived cloud properties for studying the role of clouds in climate change and the hydrological cycle in semi-arid areas, it is necessary to know their uncertainties. This paper estimates the uncertainties of several cloud properties by comparing those derived over the China Loess Plateau from the MODerate-resolution Imaging Spectroradiometer (MODIS) on Terra and Aqua by the Clouds and Earth's Radiant Energy System (CERES) with surface observations at the Semi-Arid Climate and Environment Observatory of Lanzhou University (SACOL). The comparisons use data from January 2008 to June 2010 limited to single layer and overcast stratus conditions during daytime. Cloud optical depths (tau) and liquid water paths (LWP) from both Terra and Aqua generally track the variation of the surface counterparts with modest correlation, while cloud effective radius (r(e)) is only weakly correlated with the surface retrievals. The mean differences between Terra and the SACOL retrievals are -4.7 +/- 12.9, 2.1 +/- 3.2 mu m and 30.2 +/- 85.3 g m(-2) for tau, r(e) and LWP, respectively. The corresponding differences for Aqua are 2.1 +/- 8.4, 1.2 +/- 2.9 mu m and 47.4 +/- 79.6 g m(-2), respectively. Possible causes for biases of satellite retrievals are discussed through statistical analysis and case studies. Generally, the CERES-MODIS cloud properties have a bit larger biases over the Loess Plateau than those in previous studies over other locations. (c) 2014 Elsevier Ltd. All rights reserved.
C1 [Yan, Hongru; Huang, Jianping; Wang, Tianhe] Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Sun-Mack, Sunny] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Nakajima, Takashi Y.] Tokai Univ, Res & Informat Ctr, Tokyo 151, Japan.
[Yi, Yuhong] Lanzhou Univ, Res Sch Arid Environm & Climate Change, Minist Educ, Key Lab Western Chinas Environm Syst, Lanzhou 730000, Peoples R China.
RP Huang, JP (reprint author), Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
EM hjp@lzu.edu.cn
RI Wang, Tianhe/F-8236-2012
FU Lanzhou University through the 985 Program; National Basic Research
Program of China [2013CB955802, 2012CB955301]; National Natural Science
Foundation of China [41375031]; Program for Changjiang Scholars and
Innovative Research Team in University [IRT1018]; China 111 Project
[B13045]; NASA CERES Project
FX SACOL was sponsored by the Lanzhou University through the 985 Program.
This study is supported by the National Basic Research Program of China
(2013CB955802 and 2012CB955301), National Natural Science Foundation of
China (41375031), the Program for Changjiang Scholars and Innovative
Research Team in University (IRT1018), and China 111 Project (No.
B13045). Support for Yuhong Yi and Sunny Sun-Mack was provided by the
NASA CERES Project. Thanks to Tian Zhou, Beidou Zhang and Jianrong Bi
for their efforts in providing ground-based observations.
NR 57
TC 2
Z9 2
U1 2
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 153
SI SI
BP 65
EP 76
DI 10.1016/j.jqsrt.2014.09.009
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8MH
UT WOS:000349883200008
ER
PT J
AU Kiemle, C
Ehret, G
Kawa, SR
Browell, EV
AF Kiemle, C.
Ehret, G.
Kawa, S. R.
Browell, E. V.
TI The global distribution of cloud gaps in CALIPSO data
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE CALIPSO; Cloud-free regions; Space lidar missions; Cloud length
distribution
ID LIDAR MISSION; CO2; METHANE
AB Future space-borne lidar missions are foreseen to measure global concentrations of methane, carbon dioxide and aerosols with high sensitivity and to relate the concentrations to their surface sources and sinks. Therefore, full visibility down to the surface is required. We use Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) level-2 total atmosphere cloud optical depths for the full year 2007 to assess the global and seasonal variability of such cloud-free regions with high accuracy and spatial resolution (5 km), both to contribute to an improved scientific understanding of their distribution and to identify clear regions where the above missions are expected to significantly add to the current global observation system. The global length distribution of cloudy and of cloud-free regions is strongly skewed towards a high probability of occurrence of small lengths and roughly follows a power law with exponent -5/3 up to scales of about 1000 km. Belts with extended cloud-free regions span along the subtropics, seasonally interrupted by monsoon systems. In winter large parts of the Arctic are less cloudy than in summer. Over regions with intense anthropogenic or biogenic aerosol and greenhouse gas emissions, low cloud cover is found in India and Northeast China in winter and in Amazonia, the USA, and Central Asia in summer. Here, favorable conditions for key contributions by the next generation of remote sensing missions are encountered. (c) 2014 Elsevier Ltd. All rights reserved.
C1 [Kiemle, C.; Ehret, G.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
[Kawa, S. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Browell, E. V.] NASA, Langley Res Ctr, STARSS Affiliate 2, Hampton, VA 23665 USA.
RP Kiemle, C (reprint author), DLR Inst Phys Atmosphare, D-82234 Oberpfaffenhofen, Germany.
EM Christoph.Kiemle@dlr.de; stephan.r.kawa@nasa.gov;
edward.v.browell@nasa.gov
NR 19
TC 2
Z9 2
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 153
SI SI
BP 95
EP 101
DI 10.1016/j.jqsrt.2014.12.001
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8MH
UT WOS:000349883200011
ER
PT J
AU Brown, AJ
Michaels, TI
Byrne, S
Sun, WB
Titus, TN
Colaprete, A
Wolff, MJ
Videen, G
Grund, CJ
AF Brown, Adrian J.
Michaels, Timothy I.
Byrne, Shane
Sun, Wenbo
Titus, Timothy N.
Colaprete, Anthony
Wolff, Michael J.
Videen, Gorden
Grund, Christian J.
TI The case for a modern multiwavelength, polarization-sensitive LIDAR in
orbit around Mars
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Mars; LIDAR; Polarization; Muller matrix; Symmetry; Light scattering
ID CARBON-DIOXIDE CLOUDS; MARTIAN POLAR CAPS; WATER-ICE CLOUDS;
DIFFERENTIAL ABSORPTION LIDAR; CO2 ICE; MULTIPLE-SCATTERING;
OPTICAL-PROPERTIES; VERTICAL STRUCTURE; ATMOSPHERIC DUST; LASER
ALTIMETER
AB We present the scientific case to build a multiple-wavelength, active, near-infrared (NIR) instrument to measure the reflected intensity and polarization characteristics of back-scattered radiation from planetary surfaces and atmospheres. We focus on the ability of such an instrument to enhance, potentially revolutionize, our understanding of climate, volatiles and astrobiological potential of modern-day Mars.
Such an instrument will address the following three major science themes, which we address in this paper:
Science Theme I. Surface. This would include global, night and day mapping of H2O and CO2 surface ice properties.
Science Theme 2. Ice Clouds. This would including unambiguous discrimination and seasonal mapping of CO2 and H2O ice clouds.
Science Theme 3. Dust Aerosols. This theme would include multiwavelength polarization measurements to infer dust grain shapes and size distributions. (c) 2014 Elsevier Ltd. All rights reserved.
C1 [Brown, Adrian J.; Michaels, Timothy I.] SETI Inst, Mountain View, CA 94043 USA.
[Byrne, Shane] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Sun, Wenbo] Sci Syst & Applicat Inc, Washington, DC USA.
[Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Colaprete, Anthony] NASA, Ames Res Ctr, Div Space Sci, Mountain View, CA USA.
[Wolff, Michael J.; Videen, Gorden] Space Sci Inst, Boulder, CO 80301 USA.
[Grund, Christian J.] Lightworks LLC, Boulder, CO 80301 USA.
RP Brown, AJ (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM abrown@seti.org
RI Richards, Amber/K-8203-2015
FU NASA Planetary Geology and Geophysics [NNX11AP23G, NNX13AN21G]; NASA
Mars Data Analysis Program [NNX11AN41G, NNX13AJ73G]
FX AJB acknowledges support from two grants (NNX11AP23G and NNX13AN21G)
from the NASA Planetary Geology and Geophysics program run by Dr. Mike
Kelley and two grants from the NASA Mars Data Analysis Program
(NNX11AN41G and NNX13AJ73G) administered by Dr. Mitch Schulte. We would
also like to thank Jeff Applegate, Rich Dissly, Sara Tucker, Jonathan
Weinberg and Carl Weimer at Ball Aerospace for their invaluable efforts
on this project.
NR 119
TC 9
Z9 9
U1 0
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2015
VL 153
SI SI
BP 131
EP 143
DI 10.1016/j.jqsrt.2014.10.021
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CB8MH
UT WOS:000349883200015
ER
PT J
AU Martin, N
Monnier, J
AF Martin, N.
Monnier, J.
TI Inverse rheometry and basal properties inference for pseudoplastic
geophysical flows
SO EUROPEAN JOURNAL OF MECHANICS B-FLUIDS
LA English
DT Article
DE Power-law fluid; Non-linear sliding; Sensitivity analysis; Parameter
identification; Augmented Lagrangian; Automatic differentiation
ID QUASI-NEWTONIAN FLOWS; ICE-SHEET; LAVA FLOWS; POWER-LAW; RHEOLOGY;
SURFACE; IDENTIFICATION; PARAMETERS; DYNAMICS; GLACIERS
AB The present work addresses the question of performing inverse rheometry and basal properties inference for pseudoplastic gravity-driven free-surface flows at low Reynolds' number. The modeling of these flows involves several parameters, such as the rheological ones or the state of the basal boundary (modeling an interface between the base and the fluid). The issues of inverse rheometry are addressed in a general laboratory flow context using surface velocity data. The inverse characterization of the basal boundary is proposed in a geophysical flow context where the parameters involved in the empirical effective sliding law are particularly difficult to estimate. Using an accurate direct and inverse model based on the adjoint method combined with an original efficient solver, sensitivity analyses and parameter identification are performed for a wide range of flow regimes, defined by the degree of slip and the non-linearity of the viscous sliding law considered at the bottom.
The first result is the numerical assessment of the passive aspect of the viscosity singularity inherent to a power-law pseudoplastic (shear-thinning) description in terms of surface velocities. From this result, identification of the two parameters of the constitutive law, namely the power-law exponent and the consistency, are performed. These numerical experiments provide, on the one hand, a very robust identification of the power-law exponent, even for very noisy surface velocity observations and on the other hand, a strong equifinality problem on the identification of the consistency. This parameter has a minor influence on the flow, in terms of surface velocities. Typically for temperature-dependent geophysical fluids, a law describing a priori its spatial variability is then sufficient (e.g. based on a temperature vertical profile).
This study then focuses on the basal properties interacting with the fluid rheology. An accurate joint identification of the scalar valued triple (n, m; beta) (respectively the rheological exponent, the non linear friction exponent and the friction coefficient) is achieved for any degree of slip, allowing to completely infer the flow regime. Next, in a geophysical flow context, identifications of a spatially varying friction coefficient are performed for various perturbed bedrock topography. The (2D-vertical) results demonstrate a severely ill-posed problem that allows to compute a given set of surface velocity data with different topography/friction pairs. Published by Elsevier Masson SAS.
C1 [Martin, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Monnier, J.] Math Inst Toulouse, Inst Natl Sci Appl, F-31077 Toulouse 4, France.
RP Martin, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nathan.mar7in@gmail.com
FU Agence Nationale de la Recherche through ADAGe project
[ANR-09-SYSC-001]; PRES Toulouse
FX This work was partially supported by PRES Toulouse, with the Ph.D. fund
of the first author. It was carried on at the Jet Propulsion Laboratory
and the California Institute of Technology under a contract with the
National Aeronautics and Space Administration through the President's
and Director's Fund Program. The authors want to thank Eric Larour (Jet
Propulsion Laboratory) as the project lead for the Ice Sheet System
Model (ISSM) and Ronan Madec (Toulouse Institute of Mathematics) for his
help on the development of the adjoint model of DassFlow-Ice. The
authors also thank Jean-Paul Vila (Mathematics Institute of Toulouse)
for fruitful discussions related to the singularity existence at free
surface. This work was also supported by Agence Nationale de la
Recherche through ADAGe project No. ANR-09-SYSC-001. Finally, the
authors want to thank two anonymous reviewers for their helpful and
encouraging remarks.
NR 37
TC 3
Z9 3
U1 1
U2 5
PU GAUTHIER-VILLARS/EDITIONS ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75015 PARIS, FRANCE
SN 0997-7546
EI 1873-7390
J9 EUR J MECH B-FLUID
JI Eur. J. Mech. B-Fluids
PD MAR-APR
PY 2015
VL 50
BP 110
EP 126
DI 10.1016/j.euromechflu.2014.11.011
PG 17
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA CB4CZ
UT WOS:000349577100011
ER
PT J
AU Wouters, J
McDermott, HJ
Francart, T
AF Wouters, Jan
McDermott, Hugh J.
Francart, Tom
TI Sound Coding in Cochlear Implants
SO IEEE SIGNAL PROCESSING MAGAZINE
LA English
DT Article
ID PROCESSING STRATEGIES; SPEECH RECOGNITION; PERCEPTION; STIMULATION;
SENSITIVITY; SITES
AB Cochlear implantation is a life-changing intervention for people with a severe hearing impairment [1]. For most cochlear implant (CI) users, speech intelligibility is satisfactory in quiet environments. Although modern CIs provide up to 22 stimulation channels, information transfer is still limited for the perception of fine spectrotemporal details in many types of sound. These details contribute to the perception of music and speech in common listening situations, such as where background noise is present. Over the past several decades, many different sound processing strategies have been developed to provide more details about acoustic signals to CI users. In this article, progress in sound coding for CIs is reviewed. Starting from a basic strategy, the current commercially most-used signal processing schemes are discussed, as well as recent developments in coding strategies that aim to improve auditory perception. This article focuses particularly on the stimulation strategies, which convert sound signals into patterns of nerve stimulation. The neurophysiological rationale behind some of these strategies is discussed and aspects of CI performance that require further improvement are identified.
C1 [Wouters, Jan] UCL Louvain la Neuve, Inst Nucl Phys, Natl Fund Sci Res FWO, Louvain, Belgium.
[Wouters, Jan] NASA, Goddard Space Flight Ctr, Washington, DC USA.
[Wouters, Jan] Katholieke Univ Leuven, Dept Neurosci, Louvain, Belgium.
[McDermott, Hugh J.] Bion Inst Australia, Melbourne, Vic, Australia.
[McDermott, Hugh J.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[McDermott, Hugh J.] IEEE, New York, NY USA.
[McDermott, Hugh J.] Acoust Soc Amer, Louvain, Belgium.
[Francart, Tom] Katholieke Univ Leuven, Dept Neurosci, Res Grp ExpORL, Louvain, Belgium.
RP Wouters, J (reprint author), Katholieke Univ Leuven, Dept Neurosci, Louvain, Belgium.
EM jan.wouters@med.kuleuven.be; hmcdermott@bionicsinstitute.org;
tom.francart@med.kuleuven.be
RI Wouters, Jan/D-1800-2015; Magazine, Signal Processing/E-9947-2015
OI Wouters, Jan/0000-0002-0093-698X;
FU Victorian Government, Australia
FX We thank Bas van Dijk (Cochlear), Leonid Litvak (Advanced Bionics),
Peter Nopp (Med-El), and Dirk Meister (Med-El) for providing the data
used to generate the electrodogram plots, information on the strategies,
and insightful comments on the respective parts of the manuscript. We
apologize for not being able to include all significant references that
we wanted due to space constraints. We are grateful to Jonas
Vanthornhout for his assistance with the figures. The Bionics Institute
acknowledges the support it receives from the Victorian Government,
Australia, through its Operational Infrastructure Support Program.
NR 30
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U1 4
U2 14
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1053-5888
EI 1558-0792
J9 IEEE SIGNAL PROC MAG
JI IEEE Signal Process. Mag.
PD MAR
PY 2015
VL 32
IS 2
BP 67
EP 80
DI 10.1109/MSP.2014.2371671
PG 14
WC Engineering, Electrical & Electronic
SC Engineering
GA CB6XX
UT WOS:000349771400010
ER
PT J
AU Michalek, G
Gopalswamy, N
Yashiro, S
Bronarska, K
AF Michalek, G.
Gopalswamy, N.
Yashiro, S.
Bronarska, K.
TI Dynamics of CMEs in the LASCO Field of View
SO SOLAR PHYSICS
LA English
DT Article
DE Sun: solar activity; Sun: coronal mass ejections
ID CORONAL MASS EJECTIONS; ACCELERATION; FLARES; MODEL
AB A large set (16 000) of coronal mass ejections (CMEs) observed during 1996 2011 was selected to study their dynamics in the LASCO field of view (LFOV). These events were selected based on the criterion that at least three height-time measurements were available for each CME. The height-time measurements included in the SOHO/LASCO catalog were used to determine velocities and accelerations of the respective CMEs at successive distances from the Sun. Next, these parameters were sorted into 30 subsamples depending on the distance from the Sun at which they were determined. The mean velocities and accelerations calculated for the successive distance-dependent subsamples of CMEs were used to study their dynamics. We demonstrate that CMEs in the LFOV manifest three distinct phases of propagation: (i) The propelling Lorentz force dominates the dynamics of CMEs in the inner (C2 LASCO) FOV, (ii) a stable propagation occurs as a result of the balance between the propelling and drag forces, (iii) the drag force dominates at the outer edge of the LFOV. When we considered different categories of CME separately, we found different acceleration-distance profiles for different categories.
C1 [Michalek, G.; Bronarska, K.] Jagiellonian Univ, Astron Observ, Krakow, Poland.
[Gopalswamy, N.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Michalek, G (reprint author), Jagiellonian Univ, Astron Observ, Krakow, Poland.
EM michalek@oa.uj.edu.pl
NR 28
TC 2
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U1 1
U2 2
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 MAR
PY 2015
VL 290
IS 3
BP 903
EP 917
DI 10.1007/s11207-015-0653-8
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB8TF
UT WOS:000349903300015
ER
PT J
AU Le Chat, G
Issautier, K
Zaslavsky, A
Pantellini, F
Meyer-Vernet, N
Belheouane, S
Maksimovic, M
AF Le Chat, G.
Issautier, K.
Zaslavsky, A.
Pantellini, F.
Meyer-Vernet, N.
Belheouane, S.
Maksimovic, M.
TI Effect of the Interplanetary Medium on Nanodust Observations by the
Solar Terrestrial Relations Observatory
SO SOLAR PHYSICS
LA English
DT Article
DE Interplanetary dust; Nanodust; In situ dust detection; Radio antennas;
STEREO/WAVES; Solar wind; Coronal mass ejections
ID SPACED DATA; DUST; SPACECRAFT; ANTENNAS
AB Dust particles provide an important part of the matter composing the interplanetary medium; their mass flux at 1 AU is similar to that of the solar wind. Dust grains of nanometer size-scale can be detected using radio and plasma wave instruments because they move at roughly the solar wind speed. The high-velocity impact of a dust particle generates a small crater on the spacecraft: the dust particle and the crater material are vaporized. This produces a plasma cloud whose associated electrical charge induces an electric pulse measured with radio and plasma instruments. Since their first detection in the interplanetary medium, nanodust particles have been routinely measured using the Solar Terrestrial Relations Observatory/WAVES experiment [S/WAVES]. We present the nanodust properties measured using S/WAVES/Low Frequency Receiver [LFR] observations between 2007 and 2013, and for the first time present evidence of coronal mass ejection interaction with the nanodust, leading to a higher nanodust flux measured at 1 AU. Finally, possible influences of the inner planets on the nanodust flux are presented and discussed.
C1 [Le Chat, G.; Issautier, K.; Zaslavsky, A.; Pantellini, F.; Meyer-Vernet, N.; Belheouane, S.; Maksimovic, M.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, F-92195 Meudon, France.
[Le Chat, G.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
[Le Chat, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MD USA.
RP Le Chat, G (reprint author), Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM gaetan.lechat@obspm.fr
FU CNES; CNRS; NASA [NAS5-00132]
FX We thank the team who designed and built the S/WAVES instrument. The
S/WAVES data used here are produced by an international consortium of
the Observatoire de Paris (France), the University of Minnesota (USA),
the University of California Berkeley (USA), and NASA Goddard Space
Flight Center (USA). The French contribution is funded by CNES and CNRS,
and the USA institutions are funded by NASA. We thank the STEREO PLASTIC
Investigation (A.B. Galvin, PI) and NASA Contract NAS5-00132 for
providing the proton data, and the STEREO IMPACT (J. Luhman, PI) for
providing the magnetic field data.
NR 23
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U1 3
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD MAR
PY 2015
VL 290
IS 3
BP 933
EP 942
DI 10.1007/s11207-015-0651-x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB8TF
UT WOS:000349903300017
ER
PT J
AU Balla, RJ
AF Balla, R. Jeffrey
TI Mach 10 Rayleigh Scattering Gas-Cap Density, Pressure, and Shock-Jump
Measurements
SO AIAA JOURNAL
LA English
DT Article
ID WIND-TUNNEL; ARF LASER; AIR; TEMPERATURE
AB Laser Rayleigh scattering measurements were performed along a 38.7mm line in the gas cap created by a multipurpose crew vehicle model in the NASA Langley Research Center's 31in. Mach 10 air wind tunnel. Data were acquired at a fixed stagnation temperature near 990K, and five stagnation pressures spanning 2.41 to 10.0MPa (350-1454psi). Data averaged over 371 images and 210 pixels per line produced measured gas-cap densities that agree with computed densities using the GASPROPS code within 1-5%. Gas-cap pressures calculated using measured offbody densities and computed gas-cap temperatures agree with onbody surface-pressure measurements within 5 to 15%. A line-averaged shock-density ratio of 5.92 based on four stagnation pressures agrees with the expected value of 5.97 to approximate to 1%.
C1 NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
RP Balla, RJ (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
EM robert.j.balla@nasa.gov
NR 11
TC 3
Z9 3
U1 1
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD MAR
PY 2015
VL 53
IS 3
BP 756
EP 762
DI 10.2514/1.J053698
PG 7
WC Engineering, Aerospace
SC Engineering
GA CB1PI
UT WOS:000349399700019
ER
PT J
AU Grajewski, B
Whelan, EA
Lawson, CC
Hein, MJ
Waters, MA
Anderson, JL
MacDonald, LA
Mertens, CJ
Tseng, CY
Cassinelli, RT
Luo, L
AF Grajewski, Barbara
Whelan, Elizabeth A.
Lawson, Christina C.
Hein, Misty J.
Waters, Martha A.
Anderson, Jeri L.
MacDonald, Leslie A.
Mertens, Christopher J.
Tseng, Chih-Yu
Cassinelli, Rick T., II
Luo, Lian
TI Miscarriage Among Flight Attendants
SO EPIDEMIOLOGY
LA English
DT Article
ID SPONTANEOUS-ABORTION; COSMIC-RADIATION; PREGNANCY OUTCOMES; EXPOSURE;
DISRUPTION; EVENTS; RISK
AB Background: Cosmic radiation and circadian disruption are potential reproductive hazards for flight attendants.
Methods: Flight attendants from 3 US airlines in 3 cities were interviewed for pregnancy histories and lifestyle, medical, and occupational covariates. We assessed cosmic radiation and circadian disruption from company records of 2 million individual flights. Using Cox regression models, we compared respondents (1) by levels of flight exposures and (2) to teachers from the same cities, to evaluate whether these exposures were associated with miscarriage.
Results: Of 2654 women interviewed (2273 flight attendants and 381 teachers), 958 pregnancies among 764 women met study criteria. A hypothetical pregnant flight attendant with median first-trimester exposures flew 130 hours in 53 flight segments, crossed 34 time zones, and flew 15 hours during her home-base sleep hours (10 pm-8 am), incurring 0.13 mGy absorbed dose (0.36 mSv effective dose) of cosmic radiation. About 2% of flight attendant pregnancies were likely exposed to a solar particle event, but doses varied widely. Analyses suggested that cosmic radiation exposure of 0.1 mGy or more may be associated with increased risk of miscarriage in weeks 9-13 (odds ratio = 1.7 [95% confidence interval = 0.95-3.2]). Risk of a first-trimester miscarriage with 15 hours or more of flying during home-base sleep hours was increased (1.5 [1.1-2.2]), as was risk with high physical job demands (2.5 [1.5-4.2]). Miscarriage risk was not increased among flight attendants compared with teachers.
Conclusions: Miscarriage was associated with flight attendant work during sleep hours and high physical job demands and may be associated with cosmic radiation exposure.
C1 [Grajewski, Barbara; Whelan, Elizabeth A.; Lawson, Christina C.; Hein, Misty J.; Waters, Martha A.; Anderson, Jeri L.; MacDonald, Leslie A.; Tseng, Chih-Yu; Cassinelli, Rick T., II; Luo, Lian] NIOSH, Cincinnati, OH 45226 USA.
[Mertens, Christopher J.] NASA, Hampton, VA USA.
RP Grajewski, B (reprint author), Ctr Dis Control & Prevent, Natl Inst Occupat Safety & Hlth R15, 1090 Tusculum Ave, Cincinnati, OH 45226 USA.
EM bag2@cdc.gov
FU Federal Aviation Administration; Department of Defense Women's Health
Research Program
FX Supported, in part, by interagency agreements with the Federal Aviation
Administration and the Department of Defense Women's Health Research
Program.
NR 40
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U1 2
U2 12
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1044-3983
EI 1531-5487
J9 EPIDEMIOLOGY
JI Epidemiology
PD MAR
PY 2015
VL 26
IS 2
BP 192
EP 203
DI 10.1097/EDE.0000000000000225
PG 12
WC Public, Environmental & Occupational Health
SC Public, Environmental & Occupational Health
GA CB1PO
UT WOS:000349400300025
PM 25563432
ER
PT J
AU Suvarna, P
Bulmer, J
Leathersich, JM
Marini, J
Mahaboob, I
Hennessy, J
Bell, LD
Nikzad, S
Shahedipour-Sandvik, F
AF Suvarna, Puneet
Bulmer, John
Leathersich, Jeffrey M.
Marini, Jonathan
Mahaboob, Isra
Hennessy, John
Bell, L. Douglas
Nikzad, Shouleh
Shahedipour-Sandvik, F. (Shadi)
TI Ion Implantation-Based Edge Termination to Improve III-N APD Reliability
and Performance
SO IEEE PHOTONICS TECHNOLOGY LETTERS
LA English
DT Article
DE GaN; ultraviolet detector; premature breakdown; APD; avalanche;
photodiode; edge termination; device simulation; reliability
ID GAN SCHOTTKY RECTIFIERS; GROWTH
AB We report on the development of ion implantation-based contact-edge termination technique to improve the reliability and performance of p-i-n and p-i-n-i-n GaN ultraviolet avalanche photodiode structures. The GaN photodiode structures were grown on sapphire substrates and implanted along the edge of the p-contact. The implanted devices show an absence of premature breakdown and demonstrate a lower dark-current with reliable ultraviolet photoresponse, compared with the standard unimplanted devices. Device simulations of the implanted structures at the breakdown voltage, show a reduction in crowding and spiking of the electric field along the perimeter of the contact by a factor of similar to 7, compared with the unimplanted structures.
C1 [Suvarna, Puneet; Bulmer, John; Leathersich, Jeffrey M.; Marini, Jonathan; Mahaboob, Isra; Shahedipour-Sandvik, F. (Shadi)] SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12222 USA.
[Hennessy, John; Bell, L. Douglas; Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Suvarna, P (reprint author), SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12222 USA.
EM psuvarna@albany.edu; jbulmer@albany.edu; jleathersich@albany.edu;
jmarini@albany.edu; imahaboob@albany.edu; hennessy@caltech.edu;
lloyddoug.bell@jpl.nasa.gov; shouleh.nikzad@jpl.nasa.gov;
sshahedipour-sandvik@albany.edu
OI Marini, Jonathan/0000-0002-9994-0144
FU Planetary Instrument Definition and Development Program, National
Aeronautics and Space Administration
FX This work was supported by the Planetary Instrument Definition and
Development Program, National Aeronautics and Space Administration.
NR 15
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U1 6
U2 30
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1041-1135
EI 1941-0174
J9 IEEE PHOTONIC TECH L
JI IEEE Photonics Technol. Lett.
PD MAR 1
PY 2015
VL 27
IS 5
BP 498
EP 501
DI 10.1109/LPT.2014.2382611
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA CB4TM
UT WOS:000349621100012
ER
PT J
AU Glass, JR
Kruse, GH
Miller, SA
AF Glass, Jessica R.
Kruse, Gordon H.
Miller, Scott A.
TI Socioeconomic considerations of the commercial weathervane scallop
fishery off Alaska using SWOT analysis
SO OCEAN & COASTAL MANAGEMENT
LA English
DT Article
DE weathervane scallops; bycatch; SWOT analysis; Alaska; fishery
stakeholders
ID MANAGEMENT; ACIDIFICATION; STAKEHOLDERS; COOPERATIVES; COMMUNITIES;
AQUACULTURE; EASTERN; OCEAN; GULF
AB We conducted a socioeconomic assessment of the commercial weathervane scallop (Patinopecten caurinus) fishery off Alaska. The research was structured within the framework of an SWOT (strengths, weaknesses, opportunities, threats) analysis, a strategy commonly used to analyze the internal (strengths, weaknesses) and external (opportunities, threats) components of an industry. Specifically, we focused on five categories: social, technological, economic, environmental, and regulatory. Semistructured interviews were conducted with 27 participants who had detailed knowledge of the fishery, including industry members, fishery managers, biologists, and members of coastal communities who interact with the fishery. We addressed topics such as attitudes of the Alaskan public towards scallop dredging, impacts of the scallop industry on Alaskan coastal communities, market influences of U.S. east coast and imported scallops, changes in the management of the fishery, and a number of environmental considerations. Several unifying opinions emerged from this study, including a lack of awareness of the fishery in many Alaskan communities and fears about rising fuel costs and diminishing harvest levels. Whereas the data-poor status of the stock appears to be the fishery's biggest weakness, the greatest strengths come in the form of conservative management, industry self-regulation, and the small footprint of the fishery. Impending threats include stock decline, unknown long-term detrimental effects of dredging, and changes in the management and structure of the fishery with the sunset of the State of Alaska's limited entry permit program. Most participants consider the fishery to be managed sustainably, although lack of data on scallop recruitment and abundance is a large concern. This analysis provides relevant information to both fishery managers and scallop industry members to contribute to the environmental, economic, and social sustainability of the scallop fishery. (C) 2015 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license.
C1 [Glass, Jessica R.; Kruse, Gordon H.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Miller, Scott A.] Natl Marine Fisheries Serv, Alaska Reg Off, Juneau, AK 99802 USA.
RP Glass, JR (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, POB 208106, New Haven, CT 06520 USA.
EM jessica.glass@yale.edu
OI Glass, Jessica/0000-0002-9843-1786
FU National Science Foundation Marine Ecosystem Sustainability in the
Arctic and Subarctic (MESAS) IGERT [DGE-0801720]; National Science
Foundation Graduate Research Fellowship Program; Northern Gulf of Alaska
Applied Research Award; H. Richard Carlson Fellowship; North Pacific
Research Board (NPRB) [519]; University of Alaska Coastal Marine
Institute; US Department of the Interior, Bureau of Ocean Energy
Management (BOEM), Environmental Studies Program, Washington, D.C.
[M13AC00004]
FX We thank Dr. Stephen Jewett and Dr. Franz Mueter for their helpful
reviews and suggestions. This study was carried out with approval of the
University of Alaska Fairbanks Institutional Review Board (IRB#
474118-1). This project was supported by the National Science Foundation
Marine Ecosystem Sustainability in the Arctic and Subarctic (MESAS)
IGERT (Award DGE-0801720), the National Science Foundation Graduate
Research Fellowship Program, the Northern Gulf of Alaska Applied
Research Award, the H. Richard Carlson Fellowship, the North Pacific
Research Board (NPRB publication no. 519), and the University of Alaska
Coastal Marine Institute with funding from the US Department of the
Interior, Bureau of Ocean Energy Management (BOEM), Environmental
Studies Program, Washington, D.C., Cooperative Agreement Award No.
M13AC00004. The views and conclusions contained in this document are
those of the authors and should not be interpreted as representing the
opinions or policies of the U.S. Government. Mention of trade names or
commercial products does not constitute their endorsement by the U.S.
Government.
NR 59
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U1 5
U2 28
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0964-5691
EI 1873-524X
J9 OCEAN COAST MANAGE
JI Ocean Coastal Manage.
PD MAR
PY 2015
VL 105
BP 154
EP 165
DI 10.1016/j.ocecoaman.2015.01.005
PG 12
WC Oceanography; Water Resources
SC Oceanography; Water Resources
GA CB1ZS
UT WOS:000349427100016
ER
PT J
AU Halbig, MC
Asthana, R
Singh, M
AF Halbig, M. C.
Asthana, R.
Singh, M.
TI Diffusion bonding of SiC fiber-bonded ceramics using Ti/Mo and Ti/Cu
interlayers
SO CERAMICS INTERNATIONAL
LA English
DT Article
DE Electron microscopy; Diffusion bonding; Silicon carbide; Knoop hardness;
Reaction layers
ID CARBIDE-BASED CERAMICS; SILICON-CARBIDE; INTEGRATION TECHNOLOGIES;
MECHANICAL-PROPERTIES; PHASE REACTION; DEGREES-C; JOINTS;
MICROSTRUCTURE; SYSTEM; PATH
AB A SiC fiber-bonded ceramic (SA-Tyrannohex (TM)) was diffusion bonded using Ti/Mo and Ti/Cu interlayers. The influence of metallic interlayers and SiC fiber orientation in the ceramic substrate with respect to the interlayers on joint microstructure, elemental composition, and microhardness in diffusion bonds was investigated using Optical Microscopy (OM), Field Emission Scanning Electron Microscopy (FE-SEM), Energy Dispersive Spectroscopy (EDS), and Knoop microhardness test. Compared to the Ti/Mo bilayers, the Ti/Cu bilayers yielded higher quality joints. The reaction products distributed more homogeneously across the joint thickness in Ti/Cu bonds than in Ti/Mo bonds. The reaction layers adjacent to the SiC substrate in both parallel and perpendicular SA-THX/Mo/Ti/SA-THX joints were twice as hard as the joint center where the Mo interlayer had remained untransformed during diffusion bonding. In SA-THX/Cu/Ti joints, hardness distribution was uniform across the joint thickness consistent with a more homogeneous reaction phase distribution across the joint. (C) 2014 Elsevier Ltd and Techna Group S.r.l. All rights reserved.
C1 [Asthana, R.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Asthana, R.] Univ Wisconsin Stout, Menomonie, WI 54751 USA.
[Singh, M.] Ohio Aerosp Inst, Cleveland, OH USA.
RP Asthana, R (reprint author), Univ Wisconsin Stout, 326 Ftyklund Hall, Menomonie, WI 54751 USA.
EM asthanar@uwstout.edu
NR 34
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U1 1
U2 25
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0272-8842
EI 1873-3956
J9 CERAM INT
JI Ceram. Int.
PD MAR
PY 2015
VL 41
IS 2
BP 2140
EP 2149
DI 10.1016/j.ceramint.2014.10.014
PN A
PG 10
WC Materials Science, Ceramics
SC Materials Science
GA CA5PX
UT WOS:000348961400027
ER
PT J
AU Sippel, T
Eveson, JP
Galuardi, B
Lam, C
Hoyle, S
Maunder, M
Kleiber, P
Carvalho, F
Tsontos, V
Teo, SLH
Aires-da-Silva, A
Nicol, S
AF Sippel, Tim
Eveson, J. Paige
Galuardi, Benjamin
Lam, Chi
Hoyle, Simon
Maunder, Mark
Kleiber, Pierre
Carvalho, Felipe
Tsontos, Vardis
Teo, Steven L. H.
Aires-da-Silva, Alexandre
Nicol, Simon
TI Using movement data from electronic tags in fisheries stock assessment:
A review of models, technology and experimental design
SO FISHERIES RESEARCH
LA English
DT Article
DE Spatial stock assessment; Fish movement; Electronic tags; Experimental
design
ID ATLANTIC BLUEFIN TUNA; SATELLITE ARCHIVAL TAGS; CENTRAL PACIFIC-OCEAN;
CATCH-AT-AGE; TAGGING DATA; MORTALITY-RATES; HORIZONTAL MOVEMENTS;
POPULATION-STRUCTURE; KATSUWONUS-PELAMIS; THUNNUS-ALBACARES
AB Tag-recapture data have long been important data sources for fisheries management, with the capacity to inform abundance, mortality, growth and movement within stock assessments. Historically, this role has been fulfilled with low-tech conventional tags, but the relatively recent and rapid development of electronic tags has dramatically increased the potential to collect more high quality data. Stock assessment models have also been evolving in power and complexity recently, with the ability to integrate multiple data sources into unified spatially explicit frameworks. However, electronic tag technologies and stock assessment models have developed largely independently, and frameworks for incorporating these valuable data in contemporary stock assessments are nascent, at best. Movement dynamics of large pelagic species have been problematic to resolve in modern assessments, and electronic tags offer new opportunities to resolve some of these issues. Pragmatic ways of modeling movement are often not obvious, and basic research into discrete and continuous processes, for example, is ongoing. Experimental design of electronic tagging research has been driven mostly by ecological and biological questions, rather than optimized for stock assessment, and this is probably a complicating factor in integration of the data into assessment models. A holistic overview of the current state of assessment models, electronic tag technologies, and experimental design is provided here, with the aim to provide insight into how stock assessment and electronic tagging research can be conducted most effectively together. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Sippel, Tim; Teo, Steven L. H.] Southwest Fisheries Sci Ctr, NOAA Fisheries, La Jolla, CA 92037 USA.
[Eveson, J. Paige] CSIRO Marine & Atmospher Res, Hobart, Tas, Australia.
[Galuardi, Benjamin; Lam, Chi] UMass Amherst, Large Pelag Res Ctr, Gloucester, MA 01930 USA.
[Hoyle, Simon; Nicol, Simon] Secretariat Pacific Community, Noumea 98848, New Caledonia.
[Maunder, Mark; Aires-da-Silva, Alexandre] Inter Amer Trop Tuna Commiss, Santa Clara, CA 92037 USA.
[Kleiber, Pierre] NOAA, Pacific Islands Fisheries Sci Ctr, Honolulu, HI 96822 USA.
[Carvalho, Felipe] Univ Florida, Program Fisheries & Aquat Sci, Gainesville, FL 32653 USA.
[Tsontos, Vardis] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sippel, T (reprint author), Southwest Fisheries Sci Ctr, NOAA Fisheries, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM tim.sippel@noaa.gov
FU Pelagic Fisheries Research Program at the University of Hawaii through
the project titled "Integrating Electronic and Conventional Tagging Data
into Modern Stock Assessment Models" [661550]
FX This paper is a culmination of a scientific meeting held during October
2011 in La Jolla, CA, which was funded by the Pelagic Fisheries Research
Program at the University of Hawaii through the project titled
"Integrating Electronic and Conventional Tagging Data into Modern Stock
Assessment Models" (Project Number 661550). Attendees at the workshop
included Mark Maunder, Alex Aires Da Silva, Michael Hinton, Rick Deriso,
Steve Teo, Suzanne Kohin, Tim Sippel, Ian Taylor, Pierre Kleiber, Simon
Nicol, Simon Hoyle, Karine Briand, Tim Lam, Ben Galuardi, Francois
Royer, Eunjung Kim, Irina Senina, Felipe Carvalho, Juan Valero, Yukio
Takeuchi, Shiga Iwata and Mark Fitchett. Thanks to the Inter American
Tropical Tuna Commission for convening the meeting, to Jeff Laake, Kevin
Hill, Guest Editor Hilario Murua and two anonymous reviewers for their
helpful reviews of this manuscript.
NR 106
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Z9 10
U1 3
U2 32
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 MAR
PY 2015
VL 163
SI SI
BP 152
EP 160
DI 10.1016/j.fishres.2014.04.006
PG 9
WC Fisheries
SC Fisheries
GA CA5TS
UT WOS:000348971300014
ER
PT J
AU Maltagliati, L
Bezard, B
Vinatier, S
Hedman, MM
Lellouch, E
Nicholson, PD
Sotin, C
de Kok, RJ
Sicardy, B
AF Maltagliati, Luca
Bezard, Bruno
Vinatier, Sandrine
Hedman, Matthew M.
Lellouch, Emmanuel
Nicholson, Philip D.
Sotin, Christophe
de Kok, Remco J.
Sicardy, Bruno
TI Titan's atmosphere as observed by Cassini/VIMS solar occultations: CH4,
CO and evidence for C2H6 absorption
SO ICARUS
LA English
DT Article
DE Atmospheres, composition; Infrared observations; Occultations;
Spectroscopy; Titan, atmosphere
ID METHANE (CH4)-C-12; GLOBAL ANALYSIS; WATER-VAPOR; SPECTRA; CM(-1);
STRATOSPHERE; ABUNDANCES; SPECTROSCOPY; PROFILES; DATABASE
AB We present an analysis of the VIMS solar occultations dataset, which allows us to extract vertically resolved information on the characteristics of Titan's atmosphere between similar to 100 and 700 km with a vertical resolution of similar to 10 km. After a series of data treatment procedures to correct problems in pointing stability and parasitic light, 4 occultations out of 10 are retained. This sample covers different seasons and latitudes of Titan. The transmittances show clearly the evolution of the haze, with the detection of the detached layer at similar to 310 km in September 2011 at mid-northern latitudes. Through the inversion of the transmission spectra with a line-by-line radiative transfer code we retrieve the vertical distribution of CH4 and CO mixing ratio. For methane inversion we use its 1.4, 1.7 and 2.3 gm bands. The first two bands are always in good agreement and yield an average stratospheric abundance of 1.28 +/- 0.08%, after correcting for forward-scattering effects, with no significant differences between the occultations. This is significantly less than the value of 1.48% obtained by the GCMS/Huygens instrument. We find that the 2.3 gm band cannot be used for the extraction of methane abundance because it is blended with other absorptions, not included in our atmospheric model. The analysis of the residual spectra after the inversion shows that such additional absorptions are present through a great part of the VIMS wavelength range. We attribute many of these bands, including the one at 2.3 mu m, to gaseous ethane, whose near infrared spectrum is not well modeled yet. Ethane also contributes significantly to the strong absorption at 3.2-3.5 mu m that was previously attributed only to C-H stretching bands from aerosols. Ethane bands may affect the surface windows too, especially at 2.7 mu m. Other residual bands are generated by stretching modes of C-H, C-C and C-N bonds. In addition to the C-H stretch from aliphatic hydrocarbons at 3.4 mu m, we detect a strong and narrow absorption at 3.28 mu m which we tentatively attribute to the presence of PAHs in the stratosphere. C-C and C-N stretching bands are possibly present between 4.3 and 4.5 mu m. Finally, we obtain the CO mixing ratio between 70 and 170 km, through the inversion of its 4.7 mu m band. The average result of 46 +/- 16 ppm is in good agreement with previous studies. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Maltagliati, Luca; Bezard, Bruno; Vinatier, Sandrine; Lellouch, Emmanuel; Sicardy, Bruno] Univ Paris 07, LESIA Observ Paris, CNRS, Univ Paris 06, F-92195 Meudon, France.
[Hedman, Matthew M.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[Nicholson, Philip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Kok, Remco J.] SRON, NL-3584 CA Utrecht, Netherlands.
RP Maltagliati, L (reprint author), CEA Saclay, DSM IRFU Serv Astrophys, Ctr Orme Merisiers, Bat 709, F-91191 Gif Sur Yvette, France.
EM luca.maltagliati@obspm.fr
FU Agence Nationale de la Recherche (ANR Project "APOSTIC", France)
[11BS56002]; French Space Agency (CNES); NASA Cassini Data Analysis
Program (CDAP)
FX We thank P. Lavvas, D.F. Strobel and P. Rannou for their interesting and
useful insights, and the two anonymous reviewers whose suggestions
helped to improve significantly the content and the readability of the
paper. We thank the Agence Nationale de la Recherche (ANR Project
"APOSTIC" no11BS56002, France) and the French Space Agency (CNES) for
their support. CS acknowledges support by the NASA Cassini Data Analysis
Program (CDAP).
NR 54
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Z9 9
U1 1
U2 18
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 MAR 1
PY 2015
VL 248
BP 1
EP 24
DI 10.1016/j.icarus.2014.10.004
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000001
ER
PT J
AU Johnson, JR
Grundy, WM
Lemmon, MT
Bell, JF
Deen, RG
AF Johnson, Jeffrey R.
Grundy, William M.
Lemmon, Mark T.
Bell, James F., III
Deen, R. G.
TI Spectrophotometric properties of materials observed by Pancam on the
Mars Exploration Rovers: 3. Sols 500-1525
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Spectrophotometry; Spectroscopy
ID MERIDIANI-PLANUM; PHOTOMETRIC PROPERTIES; SPECTRAL REFLECTANCE; GUSEV
CRATER; SCATTERING PROPERTIES; SURFACE REFLECTANCE; MARTIAN ATMOSPHERE;
BURNS FORMATION; HOME PLATE; OPPORTUNITY
AB The Panoramic Camera (Pancam) on the Mars Exploration Rovers Spirit and Opportunity acquired visible/near-infrared (432-1009 nm) multispectral observations of soils and rocks under varying viewing and illumination geometries. Data retrieved from these images were modeled using radiative transfer theory to study the microphysical and surface scattering nature of materials at both sites. Nearly 57,000 individual measurements from 1900 images were collected of rock and soil units identified by their color and morphologic properties over a wide range of phase angles (0-150 degrees). Images were acquired between Sols 500 and 1525 in the Columbia Hills and regions around Home Plate in Gusev Crater and in the plains and craters between Erebus and Victoria Craters in Meridiani Planum. Corrections for diffuse skylight incorporated sky models based on observations of atmospheric opacity throughout the mission. Disparity maps created from Pancam stereo images allowed estimates of local facet orientations. For Spirit, soils at lower elevations near Home Plate were modeled with lower single scattering albedo (w) values than those on the summit of Husband Hill, but otherwise soils exhibited similar scattering properties to previous Gusev soils. Dark ripple sands at the El Dorado dunes were among the most forward-scattering materials modeled. Silica-rich soils and nodules near Home Plate were analyzed for the first time, and exhibited increased forward scattering behavior with increasing wavelength, consistent with microporosity inferred from previous high resolution images and thermal infrared spectroscopy. For Opportunity, the opposition effect width parameter for sandstone outcrop rocks was modeled for the first time, and demonstrated average values consistent with surfaces of intermediate porosity and/or grain size distribution between those modeled for spherule-rich soils and darker, clast-poor soils. Soils outside a wind streak emanating from the northern rim of Victoria Crater exhibited w values similar to 16% higher than soils inside the streak. Overall, w values and scattering properties for outcrop rocks, spherule-rich soils, and rover tracks were similar to previous Meridiani Planum analyses, emphasizing the homogeneity of these materials across nearly 12 km of rover odometry. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Johnson, Jeffrey R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Grundy, William M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Lemmon, Mark T.] Texas A&M Univ, College Stn, TX 77843 USA.
[Bell, James F., III] Arizona State Univ, Tempe, AZ 85287 USA.
[Deen, R. G.] Jet Prop Lab, Pasadena, CA 91011 USA.
RP Johnson, JR (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Jeffrey.R.Johnson@jhuapl.edu
RI Lemmon, Mark/E-9983-2010; Johnson, Jeffrey/F-3972-2015
OI Lemmon, Mark/0000-0002-4504-5136;
FU NASA through the Mars Data Analysis Program [NNX11AL76G]; APL; NASA
Planetary Geology and Geophysics [NNG04G172G]
FX We thank all members of the Mars Exploration Rover operations and
support teams in providing the data sets used here, in particular the
Pancam Payload Uplink Leads for their expert planning in the acquisition
of the Pancam sequences (E. McCartney, J. Proton, E. Dean, D.
Savransky). This work was funded by NASA through the Mars Data Analysis
Program Grant NNX11AL76G; administrative support from APL and S. Murchie
is appreciated. W. Grundy gratefully acknowledges partial support from
NASA Planetary Geology and Geophysics Grant NNG04G172G to Lowell
Observatory. A portion of the research described in the paper was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Valuable reviews were provide by
M. Shepard and an anonymous reviewer that helped clarify aspects of the
manuscript. Editorial handling by O. Aharonson is appreciated.
NR 85
TC 3
Z9 3
U1 4
U2 13
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 25
EP 71
DI 10.1016/j.icarus.2014.10.026
PG 47
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000002
ER
PT J
AU Panning, MP
Beucler, E
Drilleau, M
Mocquet, A
Lognonne, P
Banerdt, WB
AF Panning, Mark P.
Beucler, Eric
Drilleau, Melanie
Mocquet, Antoine
Lognonne, Philippe
Banerdt, W. Bruce
TI Verifying single-station seismic approaches using Earth-based data:
Preparation for data return from the InSight mission to Mars
SO ICARUS
LA English
DT Article
DE Mars; Interior; Geophysics; Earth
ID SURFACE-WAVE DISPERSION; INTERIOR STRUCTURE; RECEIVER FUNCTIONS; CRUSTAL
THICKNESS; JOINT INVERSION; UPPER-MANTLE; THERMAL EVOLUTION; TRANSITION
ZONE; SNC METEORITES; LUNAR MANTLE
AB The planned InSight mission will deliver a single seismic station containing 3-component broadband and short-period sensors to the surface of Mars in 2016. While much of the progress in understanding the Earth and Moon's interior has relied on the use of seismic networks for accurate location of sources, single station approaches can be applied to data returned from Mars in order to locate events and determine interior structure. In preparation for the data return from Insight, we use a terrestrial dataset recorded at the Global Seismic Network station BFO, located at the Black Forest Observatory in Germany, to verify an approach for event location and structure determination based on recordings of multiple orbit surface waves, which will be more favorable to record on Mars than Earth due to smaller planetary radius and potentially lower background noise. With this approach applied to events near the threshold of observability on Earth, we are able to determine epicentral distance within approximately 1 degrees (corresponding to similar to 60 km on Mars), and origin time within similar to 30 s. With back azimuth determined from Rayleigh wave polarization, absolute locations are determined generally within an aperture of 10 degrees, allowing for localization within large tectonic regions on Mars. With these locations, we are able to recover Earth mantle structure within +/- 5% (the InSight mission requirements for martian mantle structure) using ID travel time inversions of P and S travel times for datasets of only 7 events. The location algorithm also allows for the measurement of great-circle averaged group velocity dispersion, which we measure between 40 and 200 s to scale the expected reliable frequency range of the InSight data from Earth to Mars data. Using the terrestrial data, we are able to resolve structure down to similar to 200 km, but synthetic tests demonstrate we should be able to resolve martian structure to similar to 400 km with the same frequency content given the smaller planetary size. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Panning, Mark P.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA.
[Beucler, Eric; Drilleau, Melanie; Mocquet, Antoine] Univ Nantes, Fac Sci & Tech, Lab Planetol & Geodynam, UMR CNRS 6112, F-44322 Nantes 3, France.
[Drilleau, Melanie; Lognonne, Philippe] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, F-75205 Paris 13, France.
[Banerdt, W. Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Panning, MP (reprint author), Univ Florida, Dept Geol Sci, 241 Williamson Hall,Box 112120, Gainesville, FL 32611 USA.
RI Panning, Mark/B-3805-2011; Lognonne, Philippe/F-8846-2010
OI Panning, Mark/0000-0002-2041-3190;
FU NASA/JPL as part of the InSight mission; CNES
FX This work was undertaken during the preparation phase of the SEIS
experiment on InSight mission. M.P. and W.B.B. were supported by funds
from NASA/JPL as part of the InSight mission, and E.B., M.D., A.M., and
P.L. acknowledge the financial support of CNES. The Bayesian inversions
of group velocity dispersion diagrams were performed using HPC resources
of CINES (Centre Informatique National de l'Enseignement Suprieur) under
the allocation 2014047062 made by GENCI (Grand Equipement National de
Calcul Intensif). The authors also thank the editor and the reviewers
for their constructive remarks.
NR 75
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U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 230
EP 242
DI 10.1016/j.icarus.2014.10.035
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000015
ER
PT J
AU Quarles, BL
Lissauer, JJ
AF Quarles, Billy L.
Lissauer, Jack J.
TI Dynamical evolution of the Earth-Moon progenitors - Whence Theia?
SO ICARUS
LA English
DT Article
DE Moon; Planetary dynamics; Origin, Solar System; Resonances, orbital
ID TERRESTRIAL PLANET FORMATION; LATE HEAVY BOMBARDMENT; FORMING GIANT
IMPACT; SOLAR-SYSTEM; LATE-STAGE; ORBITAL ARCHITECTURE; PROTOPLANETARY
DISK; RESONANCE OVERLAP; V HYPOTHESIS; ORIGIN
AB We present integrations of a model Solar System with five terrestrial planets (beginning,similar to 30-50 Myr after the formation of primitive Solar System bodies) in order to determine the preferred regions of parameter space leading to a Giant Impact that resulted in the formation of the Moon. Our results indicate which choices of semimajor axes and eccentricities for Theia (the proto-Moon) at this epoch can produce a late Giant Impact, assuming that Mercury, Venus, and Mars are near the current orbits. We find that the likely semimajor axis of Theia, at the epoch when our simulations begin, depends on the assumed mass ratio of Earth-Moon progenitors (8/1,4/1, or 1/1). The low eccentricities of the terrestrial planets are most commonly produced when the progenitors have similar semimajor axes at the epoch when our integrations commence. Additionally, we show that mean motion resonances among the terrestrial planets and perturbations from the giant planets can affect the dynamical evolution of the system leading to a late Giant Impact. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Quarles, Billy L.; Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Quarles, BL (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
FU NASA
FX B.Q. gratefully acknowledges a Fellowship from the NASA Postdoctoral
Program. The authors thank N. Haghighipour for stimulating conversations
over the course of this work. B.Q. acknowledges S. Satyal for his
assistance with computational resources. We thank T. Dobrovolskis, D.
Jontof-Hutter, and A. Morbidelli for helpful comments on the manuscript.
NR 73
TC 1
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U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 318
EP 339
DI 10.1016/j.icarus.2014.10.044
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000021
ER
PT J
AU Jolly, A
Cottini, V
Fayt, A
Manceron, L
Kwabia-Tchana, F
Benilan, Y
Guillemin, JC
Nixon, C
Irwin, P
AF Jolly, A.
Cottini, V.
Fayt, A.
Manceron, L.
Kwabia-Tchana, F.
Benilan, Y.
Guillemin, J. -C
Nixon, C.
Irwin, P.
TI Gas phase dicyanoacetylene (C4N2) on Titan: New experimental and
theoretical spectroscopy results applied to Cassini CIRS data
SO ICARUS
LA English
DT Article
DE Titan; Abundance, atmosphere; IR spectroscopy; IR observations
ID GLOBAL ROVIBRATIONAL ANALYSIS; FAR-INFRARED SPECTRA; BAND INTENSITIES;
ATMOSPHERE; STRATOSPHERE; SYSTEM; NORTH; VAPOR; C2N2; HC3N
AB Dicyanoacetylene has not been observed so far in the gas phase in Titan's atmosphere but this molecule is still on the list of the detected species, on the basis of the correspondence between a solid phase feature measured at 478 cm(-1) in the laboratory and a spectral feature observed by Voyager. In this work, the infrared spectrum of gaseous C4N2 has been investigated to improve our knowledge of the band intensities and the line parameters for this molecule. Results of previously investigated bands have been revised and the intensity of the v(9) band at 107 cm(-1), measured for the first time, was found to be the strongest absorption in the whole infrared domain. We have also improved the analysis of the complex rotational and hot band structure of C4N2 in order to obtain the first line lists for both bending modes v(8) and v(9). Using our radiative transfer code including the new line list of the strong v(9) band, we have searched for the signature of C4N2 at 107 cm(-1) in the atmosphere of Titan utilizing Titan CIRS far infrared spectra. Despite averaging a large number of CIRS spectra at northern latitudes during the very favorable Titan winter, no gaseous C4N2 could be detected. At the 1-sigma level we obtain an abundance upper limit of 5.3 x 10(-10) for the limb average which is lower than or comparable to previously inferred values. As a consequence, the absence or very low amount of gaseous C4N2 makes quite puzzling its presence in the solid phase with an abundance compatible with the observed spectral feature at 478 cm(-1). (C) 2014 Elsevier Inc. All rights reserved.
C1 [Jolly, A.; Kwabia-Tchana, F.; Benilan, Y.] Univ Paris Diderot, LISA, UMR CNRS 7583, Creteil, France.
[Jolly, A.; Kwabia-Tchana, F.; Benilan, Y.] Univ Paris Est Creteil, IPSL, Creteil, France.
[Cottini, V.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cottini, V.; Nixon, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fayt, A.] Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain La Neuve, Belgium.
[Manceron, L.] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France.
[Manceron, L.] UPMC, MONARIS, UMR 8233, F-75252 Paris 05, France.
[Guillemin, J. -C] Ecole Natl Super Chim Rennes, Inst Sci Chim Rennes, CNRS, UMR6226, F-35708 Rennes 7, France.
[Irwin, P.] Univ Oxford, Oxford OX1 3PU, England.
RP Jolly, A (reprint author), Univ Paris Diderot, LISA, UMR CNRS 7583, Creteil, France.
EM jolly@lisa.u-pec.fr
RI Nixon, Conor/A-8531-2009;
OI Nixon, Conor/0000-0001-9540-9121; Guillemin,
Jean-Claude/0000-0002-2929-057X; Irwin, Patrick/0000-0002-6772-384X
NR 30
TC 8
Z9 8
U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 340
EP 346
DI 10.1016/j.icarus.2014.10.049
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000022
ER
PT J
AU Bandfield, JL
Hayne, P
Williams, JP
Greenhagen, BT
Paige, DA
AF Bandfield, Joshua L.
Hayne, Paul
Williams, Jean-Pierre
Greenhagen, Benjamin T.
Paige, David A.
TI Lunar surface roughness derived from LRO Diviner Radiometer observations
SO ICARUS
LA English
DT Article
DE Moon, surface; Regoliths; Infrared observations
ID THERMAL INFRARED-SPECTRA; THERMOPHYSICAL MODEL; PLANETARY REGOLITHS;
SCALE TOPOGRAPHY; EMISSION-SPECTRA; 9P/TEMPEL 1; MOON; SCATTERING;
INERTIA; ASTEROIDS
AB Sunlit and shaded slopes have a variety of temperatures based on their orientation with respect to the Sun. Generally, greater slope angles lead to higher anisothermality within the field of view. This anisothermality is detected by measuring changing emitted radiance as a function of viewing angle or by measuring the difference in brightness temperatures with respect to observation wavelength. Thermal infrared measurements from the Lunar Reconnaissance Orbiter Diviner Radiometer were used to derive lunar surface roughness via two observation types: (1) nadir multispectral observations with full diurnal coverage and (2) multiple emission angle targeted observations. Measurements were compared to simulated radiance from a radiative equilibrium thermal model and Gaussian slope distribution model. Nadir observations most closely match a 20 degrees RMS slope distribution, and multiple emission angle observations can be modeled using 20-35 degrees RMS slope distributions. Limited sampling of the lunar surface did not show any clear variation in roughness among surface units. Two-dimensional modeling shows that surfaces separated by distances greater than 0.5-5 mm can remain thermally isolated in the lunar environment, indicating the length scale of the roughness features. Non-equilibrium conditions are prevalent at night and near sunrise and sunset, preventing the use of the equilibrium thermal model for roughness derivations using data acquired at these local times. Multiple emission angle observations also show a significant decrease in radiance at high emission angles in both daytime and nighttime observations, and hemispherical emissivity is lower than is apparent from nadir observations. These observations and models serve as a basis for comparison with similar measurements of other airless bodies and as an initial template for the interpretation of TIR measurements acquired under a variety of geometric conditions. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Bandfield, Joshua L.] Space Sci Inst, Boulder, CO 80301 USA.
[Hayne, Paul; Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Williams, Jean-Pierre; Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Bandfield, JL (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
EM jbandfield@spacescience.org
RI Williams, Jean-Pierre/C-3531-2009; Greenhagen, Benjamin/C-3760-2016
OI Williams, Jean-Pierre/0000-0003-4163-2760;
FU Lunar Reconnaissance Orbiter program; NASA Planetary Geology and
Geophysics program [NNX12A046G]; International Space Science Institute
(ISSI); National Aeronautics and Space Administration
FX We would like to thank the LRO, LROC, LOLA, and Diviner operations teams
for the collection of high quality datasets used in this work. Ian
Thomas provided validation for the initial Diviner multiple emission
angle observations. Bjorn Davidsson and an anonymous reviewer provided
kind and constructive comments that improved both the clarity and
content of the manuscript. Support for this work was provided by the
Lunar Reconnaissance Orbiter program and NASA Planetary Geology and
Geophysics program grant NNX12A046G. This work also benefited from
discussions at meetings supported by the International Space Science
Institute (ISSI). Part of this work was carried out at the Jet
Propulsion Laboratory, under contract with the National Aeronautics and
Space Administration.
NR 73
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Z9 14
U1 2
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 357
EP 372
DI 10.1016/j.icarus.2014.11.009
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000024
ER
PT J
AU De Sanctis, MC
Frigeri, A
Ammannito, E
Tosi, F
Marchi, S
Zambon, F
Raymond, CA
Russell, CT
AF De Sanctis, M. C.
Frigeri, A.
Ammannito, E.
Tosi, F.
Marchi, S.
Zambon, F.
Raymond, C. A.
Russell, C. T.
TI Mineralogy of Marcia, the youngest large crater of Vesta: Character and
distribution of pyroxenes and hydrated material
SO ICARUS
LA English
DT Article
DE Asteroids, composition; Asteroid Vesta; Spectroscopy
ID ASTEROID 4 VESTA; DARK MATERIAL; IMAGING SPECTROMETER; REFLECTANCE
SPECTRA; HED METEORITES; DAWN MISSION; GRAIN-SIZE; SURFACE;
SPECTROSCOPY; REGOLITH
AB The young Marcia crater on Vesta displays several interesting features, including pitted and smooth terrains, exposure of relatively bright and dark material, and enrichments of hydrated material in the ejecta. Several questions arise about the origin of Marcia and of the dark material (exogenic material vs volcanic or impact melts) and the smooth and pitted terrains. Here we describe the results of the spectral and thermal analysis of the Marcia crater, with a particular effort to assess the composition of the different units, identifying the presence of OH and its correlation with dark material. Detailed studies of the Marcia crater wall, smooth and floor units reveal a compositional rich terrain with small areas enriched in diogenites with respect to the general eucritic regolith dominating the equatorial region of Vesta. The signature of OH is particularly clear in the pitted floor, dark material, smooth unit, and ejecta. The pitted terrains, beside their appearance, also show thermal anomalies, being colder with respect to the surrounding terrains. The presence of OH, concentrated in darker layers, and the pitted crater floor indicate that the area where the Marcia impact event occurred was rich in volatiles. The results show how the relatively young impact events have modified the surface of Vesta, disrupting a layer of dark material once present on Vesta's equatorial terrain and exposing fresh, bright material rich in pyroxene. (C) 2014 Elsevier Inc. All rights reserved.
C1 [De Sanctis, M. C.; Frigeri, A.; Ammannito, E.; Tosi, F.; Marchi, S.; Zambon, F.] Ist Astrofis & Planetol Spaziali, INAF, Area Ric Tor Vergata, I-00133 Rome, Italy.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Marchi, S.] SSERVI Southwest Res Inst, Boulder, CO 80302 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP De Sanctis, MC (reprint author), Ist Astrofis & Planetol Spaziali, INAF, Area Ric Tor Vergata, I-00133 Rome, Italy.
EM mariacristina.desanctis@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Tosi, Federico/0000-0003-4002-2434;
Zambon, Francesca/0000-0002-4190-6592
FU Italian Space Agency Italy; Italian Space Agency; Dawn Science,
Instrument, and Operations Teams
FX VIR is funded by the Italian Space Agency Italy and was developed under
the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali,
Rome, Italy. The instrument was built by Selex-ES, Florence, Italy. The
authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams. This work was supported by the Italian Space Agency. A
portion of this work was performed at the Jet Propulsion Laboratory
under contract with NASA.
NR 64
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 392
EP 406
DI 10.1016/j.icarus.2014.10.051
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000027
ER
PT J
AU Rodriguez, JAP
Leonard, GJ
Platz, T
Tanaka, KL
Kargel, JS
Fairen, AG
Gulick, V
Baker, VR
Glines, N
Miyamoto, H
Jianguo, Y
Oguma, M
AF Rodriguez, J. Alexis P.
Leonard, Gregory J.
Platz, Thomas
Tanaka, Kenneth L.
Kargel, Jeffrey S.
Fairen, Alberto G.
Gulick, Virginia
Baker, Victor R.
Glines, Natalie
Miyamoto, Hideaki
Jianguo, Yan
Oguma, Midori
TI New insights into the Late Amazonian zonal shrinkage of the martian
south polar plateau
SO ICARUS
LA English
DT Article
DE Mars; Polar caps; Polar geology; Ices
ID GLOBAL SURVEYOR DATA; LAYERED DEPOSITS; GEOLOGIC HISTORY; MARS; REGIONS;
FLOW; ACCUMULATION; TOPOGRAPHY; MECHANISMS; ORIGIN
AB The martian south polar plateau, Planum Australe, comprises the largest known water-ice surface deposit on the planet. Here, we present evidence for an episode of extensive polar plateau retreat during the Late Amazonian, which affected regions flanking circum-polar terrains located between Cavi Angusti and Sisyphi Montes. (C) 2014 Published by Elsevier Inc.
C1 [Rodriguez, J. Alexis P.; Gulick, Virginia; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rodriguez, J. Alexis P.; Platz, Thomas] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Leonard, Gregory J.; Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Platz, Thomas] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany.
[Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Gulick, Virginia] SETI Inst, Mountain View, CA 94043 USA.
[Miyamoto, Hideaki; Oguma, Midori] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
[Jianguo, Yan] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
RP Rodriguez, JAP (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
RI Platz, Thomas/F-7539-2013; Miyamoto, Hideaki/B-9666-2008
OI Platz, Thomas/0000-0002-1253-2034;
FU DFG grant [PL613/2-1]; Helmholtz association; KAKENHI [23340126]
FX Funding provided by NASA's NPP program to J. Alexis P. Rodriguez and by
MRO HiRISE Co-Investigator funds to V.C. Gulick. T. Platz was supported
by a DFG grant (PL613/2-1) and the Helmholtz association through the
research alliance "Planetary Evolution and Life". HiRISE images were
analyzed using HiView developed by the Lunar and Planetary Laboratory at
the University of Arizona. The participation of Hideaki Miyamoto was
supported by grant KAKENHI 23340126.
NR 42
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U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 407
EP 411
DI 10.1016/j.icarus.2014.08.047
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000028
ER
PT J
AU Romero-Wolf, A
Vance, S
Maiwald, F
Heggy, E
Ries, P
Liewer, K
AF Romero-Wolf, Andrew
Vance, Steve
Maiwald, Frank
Heggy, Essam
Ries, Paul
Liewer, Kurt
TI A passive probe for subsurface oceans and liquid water in Jupiter's icy
moons
SO ICARUS
LA English
DT Article
DE Jupiter; Europa; Ganymede; Ices; Radar observations
ID JOVIAN S-BURSTS; INTERNAL STRUCTURE; EUROPAS OCEAN; CONSTRAINTS; SHELL;
SATELLITES; THICKNESS; MODELS; STATE
AB We describe an interferometric reflectometer method for passive detection of subsurface oceans and liquid water in jovian icy moons using Jupiter's decametric radio emission (DAM). The DAM flux density exceeds 3000 times the galactic background in the neighborhood of the jovian icy moons, providing a signal that could be used for passive radio sounding. An instrument located between the icy moon and Jupiter could sample the DAM emission along with its echoes reflected in the ice layer of the target moon. Cross-correlating the direct emission with the echoes would provide a measurement of the ice shell thickness along with its dielectric properties. The interferometric reflectometer provides a simple solution to sub-jovian radio sounding of ice shells that is complementary to ice penetrating radar measurements better suited to measurements in the anti-jovian hemisphere that shadows Jupiter's strong decametric emission. The passive nature of this technique also serves as risk reduction in case of radar transmitter failure. The interferometric reflectometer could operate with electrically short antennas, thus extending ice depth measurements to lower frequencies, and potentially providing a deeper view into the ice shells of jovian moons. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Romero-Wolf, Andrew; Vance, Steve; Maiwald, Frank; Heggy, Essam; Ries, Paul; Liewer, Kurt] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
RP Romero-Wolf, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM Andrew.Romero-Wolf@jpl.nasa.gov
FU Internal Research and Technology Development program
FX We would like to thank Mike Janssen, Sam Gulkis, Steve Levin, Chuck
Naudet, Charley Dunn, Jim Zumberge, Luis Amaro, and William Smythe at
the Jet Propulsion Laboratory for their helpful and encouraging
discussions on this idea. We would also like to thank Imke de Pater at
UC Berkeley for her helpful advice. This research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and
funded through the Internal Research and Technology Development program.
Copyright 2014 California Institute of Technology. Government
sponsorship acknowledged.
NR 43
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 463
EP 477
DI 10.1016/j.icarus.2014.10.043
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000032
ER
PT J
AU Gilli, G
Lopez-Valverde, MA
Peralta, J
Bougher, S
Brecht, A
Drossartd, P
Piccioni, G
AF Gilli, G.
Lopez-Valverde, M. A.
Peralta, J.
Bougher, S.
Brecht, A.
Drossartd, P.
Piccioni, G.
TI Carbon monoxide and temperature in the upper atmosphere of Venus from
VIRTIS/Venus Express non-LTE limb measurements
SO ICARUS
LA English
DT Article
DE Venus atmosphere; Radiative transfer; Infrared observations; Terrestrial
planets
ID NONLOCAL THERMODYNAMIC-EQUILIBRIUM; MU-M WAVELENGTH; MIDDLE ATMOSPHERE;
LINE OBSERVATIONS; HETERODYNE SPECTROSCOPY; INFRARED EMISSIONS; THERMAL
STRUCTURE; CO; MODEL; WINDS
AB The upper mesosphere and the lower thermosphere of Venus (from 90 to 150 km altitude) seems to play a transition region in photochemistry, dynamics and radiation, but is still very poorly constrained observationally. Since 2006 VIRTIS on board Venus Express has been obtaining limb observations of CO fluorescent infrared emissions in a systematic manner. This study represents the scientific exploitation of this dataset and reports new information on the composition and temperature at those altitudes. This work is focused on the 4.7 mu m emission of CO as observed by VIRTIS, which contains two emission bands, the fundamental and the first hot of the main CO isotope. A specific scheme for a simultaneous retrieval of CO and temperature is proposed, based on results of a comprehensive non-LTE model of these molecular emissions. A forward model containing such non-LTE model is used at the core of an inversion scheme that consists of two steps: (i) a minimization procedure of model-data differences and (ii) a linear inversion around the solution of the first step. A thorough error analysis is presented, which shows that the retrievals of CO and temperature are very noisy but can be improved by suitable averaging of data. These averages need to be consistent with the non-LTE nature of the emissions. Unfortunately, the data binning process reduced the geographical coverage of the results. The obtained retrieval results indicate a global distribution of the CO in the Venus dayside with a maximum around the sub-solar point, and a decrease of a factor 2 towards high latitudes. Also a gradient from noon to the morning and evening sides is evident in the equator, this being smaller at high latitudes. No morning-afternoon differences in the CO concentration are observed, or are comparable to our retrieval errors. All this argues for a CO distribution controlled by dynamics in the lower thermosphere, with a dominant sub-solar to anti-solar gradient. Similar variations are found with the Venus Thermospheric General Circulation Model (VTGCM), but the VIRTIS CO is systematically larger than in the model. The thermal structure obtained by VIRTIS presents a hint of local maximum around 115 km near the terminator at equatorial latitudes, but not at noon, in clear contrast to VTGCM predictions and to an upper mesosphere in pure radiative balance. A few tentative ideas to explain these model-data discrepancies are discussed. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Gilli, G.; Lopez-Valverde, M. A.; Peralta, J.] Inst Astrofis Andalucia CSIC, Granada, Spain.
[Bougher, S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Brecht, A.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Drossartd, P.] Observ Paris, LESIA, Meudon, France.
[Piccioni, G.] IAPS INAF, Rome, Italy.
[Gilli, G.] CNRS, Meteorol Dynam Lab, Paris, France.
RP Gilli, G (reprint author), CNRS, Meteorol Dynam Lab, Paris, France.
OI Piccioni, Giuseppe/0000-0002-7893-6808; Lopez-Valverde, M.
A./0000-0002-7989-4267; Peralta, Javier/0000-0002-6823-1695
FU Spanish MINECO [AYA2008-03498/ESP]; CONSOLIDER program [CSD2009-00038];
EC FEDER funds; panish National Research Council (CSIC) JAE-Predoc
grant; European Social Fund (ESF); MINECO 'Ramon y Cajal' project
[RYC-2011-08269]; CNES postdoc contract
FX The IAA-CSIC team was supported by the Spanish MINECO under Project
AYA2008-03498/ESP and the CONSOLIDER program CSD2009-00038 and EC FEDER
funds. GG has been funded by a Spanish National Research Council (CSIC)
JAE-Predoc grant, co-funded by the European Social Fund (ESF). GG has
also been financially supported by a Grant associated to the MINECO
'Ramon y Cajal' project RYC-2011-08269, and by a CNES postdoc contract
during 2014.
NR 58
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Z9 7
U1 3
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 478
EP 498
DI 10.1016/j.icarus.2014.10.047
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000033
ER
PT J
AU Becker, TM
Howell, ES
Nolan, MC
Magri, C
Pravec, P
Taylor, PA
Oey, J
Higgins, D
Vilagi, J
Kornos, L
Galad, A
Gajdos, S
Gaftonyuk, NM
Krugly, YN
Molotov, IE
Hicks, MD
Carbognani, A
Warner, BD
Vachier, F
Marchis, F
Pollock, JT
AF Becker, Tracy M.
Howell, Ellen S.
Nolan, Michael C.
Magri, Christopher
Pravec, Petr
Taylor, Patrick A.
Oey, Julian
Higgins, David
Vilagi, Jozef
Kornos, Leonard
Galad, Adrian
Gajdos, Stefan
Gaftonyuk, Ninel M.
Krugly, Yurij N.
Molotov, Igor E.
Hicks, Michael D.
Carbognani, Albino
Warner, Brian D.
Vachier, Frederic
Marchis, Franck
Pollock, Joseph T.
TI Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from
radar and optical light curve observations
SO ICARUS
LA English
DT Article
DE Asteroid; Near-Earth objects; Satellites of asteroids; Radar
observations; Photometry; Asteroids, rotation
ID SMALL BINARY ASTEROIDS; 1999 KW4; ROTATIONAL FISSION; ANGULAR-MOMENTUM;
TIDAL EVOLUTION; SHAPE MODELS; RUBBLE PILES; POPULATION; SYSTEMS;
OBJECTS
AB We report radar observations (2380-MHz, 13-cm) by the Arecibo Observatory and optical light curves observed from eight different observatories and collected at the Ondrejov Observatory of the triple near-Earth asteroid system (153591) 2001 SN263. The radar observations were obtained over the course of ten nights spanning February 12-26, 2008 and the light curve observations were made throughout January 12 - March 31, 2008. Both data sets include observations during the object's close approach of 0.06558 AU on February 20th, 2008. The delay-Doppler images revealed the asteroid to be comprised of three components, making it the first known triple near-Earth asteroid. Only one other object, (136617) 1994 CC is a confirmed triple near-Earth asteroid.
We present physical models of the three components of the asteroid system. We constrain the primary's pole direction to an ecliptic longitude and latitude of (309, 80) 15. We find that the primary rotates with a period 3.4256 +/- 0.0002 h and that the larger satellite has a rotation period of 13.43 +/- 0.01 h, considerably shorter than its orbital period of approximately 6 days. We find that the rotation period of the smaller satellite is consistent with a tidally locked state and therefore rotates with a period of 0.686 +/- 0.002 days (Fang et al. [2011]. Astron. J. 141, 154-168). The primary, the larger satellite, and the smaller satellite have equivalent diameters of 2.5 +/- 0.3 km, 0.77 +/- 0.12 km, 0.43 +/- 0.14 km and densities of 1.1 +/- 0.2 g/cm(3), 1.0 +/- 0.4 g/cm(3), 2.3 +/- 1.3 g/cm(3), respectively. (C) 2014 The Authors. Published by Elsevier Inc.
C1 [Becker, Tracy M.] Univ Cent Florida, Orlando, FL 32816 USA.
[Howell, Ellen S.; Nolan, Michael C.; Taylor, Patrick A.] Univ Space Res Assoc, Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA.
[Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
[Pravec, Petr] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic.
[Oey, Julian] Leura Observ, Leura, NSW, Australia.
[Higgins, David] Hunters Hill Observ, Ngunnawal, ACT 2913, Australia.
[Vilagi, Jozef; Kornos, Leonard; Galad, Adrian; Gajdos, Stefan] FMFI UK, Modra Observ, Dept Astron Phys Earth & Meteool, SK-84248 Bratislava, Slovakia.
[Gaftonyuk, Ninel M.] Crimean Astrophys Observ, Simeiz Dept, UA-98680 Simeiz, Crimea, Ukraine.
[Krugly, Yurij N.] Kharkov Natl Univ, Inst Astron, UA-61022 Kharkov, Ukraine.
[Hicks, Michael D.] CALTECH, Jet Prop Lab, La Canada Flintridge, CA 91011 USA.
[Molotov, Igor E.] MV Keldysh Appl Math Inst, Moscow 125047, Russia.
[Carbognani, Albino] Astron Observ Autonomous Reg Aosta Valley OAVdA, I-11020 Nus, Aosta, Italy.
[Warner, Brian D.] Ctr Solar Syst Studies, Eaton, CO 80615 USA.
[Vachier, Frederic] Univ Paris 06, IMCEE, Observ Paris, Sorbonne Univ,CNRS UMR8028, F-75014 Paris, France.
[Marchis, Franck] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Pollock, Joseph T.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
RP Becker, TM (reprint author), Univ Cent Florida, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
EM tbecker@knights.ucf.edu
RI Pravec, Petr/G-9037-2014; Galad, Adrian/G-9011-2014;
OI Nolan, Michael/0000-0001-8316-0680
FU Arecibo Observatory; National Science Foundation Research Experience for
Undergraduates (REU) program; NSF [AST-0808064]; National Aeronautics
and Space Administration through the Near Earth Object Observations
Program [NNX10AP64G, NNX12AF24G]; Grant Agency of the Czech Republic
[P209/12/0229]; Slovak Grant Agency for Science VEGA [1/0670/13];
Florida Space Grant Consortium; [RVO 67985815]
FX The authors thank the reviewers for their useful comments which helped
improve the content of this paper. The Arecibo Observatory is part of
the National Astronomy and Ionosphere Center, which at the time of
observation was operated by Cornell University for the National Science
Foundation. This research was supported by the Arecibo Observatory and
the National Science Foundation Research Experience for Undergraduates
(REU) program. This work was partially supported by NSF AST-0808064.
This material is based upon work supported by the National Aeronautics
and Space Administration under Grant Nos. NNX10AP64G and NNX12AF24G
issued through the Near Earth Object Observations Program. The work done
at the Ondrejov Observatory was supported by the Grant Agency of the
Czech Republic, Grant P209/12/0229, and by Program RVO 67985815. The
work done at the Modra Observatory was supported by the Slovak Grant
Agency for Science VEGA (Grant 1/0670/13). TMB would like to thank the
Florida Space Grant Consortium and also Dr. Joshua Colwell for his
support of this work.
NR 71
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U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 499
EP 515
DI 10.1016/j.icarus.2014.10.048
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000034
ER
PT J
AU Cassidy, TA
Merkel, AW
Burger, MH
Sarantos, M
Killen, RM
McClintock, WE
Vervack, RJ
AF Cassidy, Timothy A.
Merkel, Aimee W.
Burger, Matthew H.
Sarantos, Menelaos
Killen, Rosemary M.
McClintock, William E.
Vervack, Ronald J., Jr.
TI Mercury's seasonal sodium exosphere: MESSENGER orbital observations
SO ICARUS
LA English
DT Article
DE Mercury, atmosphere; Atmospheres, structure; Atmospheres, dynamics;
Spectroscopy
ID PHOTON-STIMULATED DESORPTION; RADIATION PRESSURE; NEUTRAL SODIUM; LUNAR
SAMPLE; ATMOSPHERE; SURFACE; TEMPERATURE; MODEL; MAGNETOSPHERE; EMISSION
AB The Mercury Atmospheric and Surface Composition Spectrometer (MASCS) Ultraviolet and Visible Spectrometer (UVVS) on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft now orbiting Mercury provides the first close-up look at the planet's sodium exosphere. UVVS has observed the exosphere from orbit almost daily for over 10 Mercury years. In this paper we describe and analyze a subset of these data: altitude profiles taken above the low-latitude dayside and south pole. The observations show spatial and temporal variation but there is little or no year-to-year variation; we do not see the episodic variability reported by ground-based observers. We used these altitude profiles to make estimates of sodium density and temperature. The bulk of the exosphere is about 1200 K, much warmer than Mercury's surface. This value is consistent with some ground-based measurements and suggests that photon-stimulated desorption is the primary ejection process. We also observe a tenuous energetic component but do not see evidence of the predicted thermalized (or partially thermalized) sodium near Mercury's surface temperature. Overall we do not see the variable mixture of temperatures predicted by most Monte Carlo models of the exosphere. (C) 2014 Published by Elsevier Inc.
C1 [Cassidy, Timothy A.; Merkel, Aimee W.; McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Burger, Matthew H.] Morgan State Univ, Baltimore, MD 21251 USA.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21250 USA.
[Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Cassidy, TA (reprint author), 3665 Discovery Dr, Boulder, CO 80303 USA.
EM timothy.cassidy@lasp.colorado.edu
RI Vervack, Ronald/C-2702-2016
OI Vervack, Ronald/0000-0002-8227-9564
FU NASA Discovery Program [NAS5-97271]; MESSENGER Participating Scientist
Program; [NASW-00002]
FX The visualization of UVVS observations shown in Fig. 1 was developed at
the Laboratory for Atmospheric and Space Physics by Jay Kominek, Ken
Griest, and Dane Larsen. The MESSENGER project is supported by the NASA
Discovery Program under contracts NAS5-97271 to The Johns Hopkins
University Applied Physics Laboratory and NASW-00002 to the Carnegie
Institution of Washington. RJV and RMK are supported by the MESSENGER
Participating Scientist Program.
NR 67
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U1 2
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2015
VL 248
BP 547
EP 559
DI 10.1016/j.icarus.2014.10.037
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ7PR
UT WOS:000348411000038
ER
PT J
AU Neel, J
Cook, P
Mellen, N
Akbar, I
Devasirvatham, D
Sheehe, C
Schutz, B
AF Neel, James
Cook, Peter
Mellen, Neal
Akbar, Ihsan
Devasirvatham, Daniel
Sheehe, Charles
Schutz, Bob
TI The Role of Context in Cognitive Systems
SO JOURNAL OF SIGNAL PROCESSING SYSTEMS FOR SIGNAL IMAGE AND VIDEO
TECHNOLOGY
LA English
DT Article
DE Context; Cognitive Radio; WISDM; Big RF
AB To make effective decisions, a cognitive radio needs to understand its operating context. Over the past several months, the Wireless Innovation Forum's Cognitive Radio Work Group has been exploring how to enable a cognitive radio to represent, understand, and share its context. Material to be covered in this paper includes the following:
What exactly is meant by "context" in varying published existing context-aware applications
The role of context in communications and information systems
A survey of tools and software for developing context-aware applications
A new model of the interactions of the real world, symbolic reasoning and representation, and acting on the reasoning
Relating the components of a key context-aware tool to the new model
Initial work coding a java-based context-aware application for a cognitive radio to reason and act on its context
This paper provides greater detail and context to a presentation given at WinnComm 2013 and reviews work performed on the subject since the earlier presentation.
C1 [Neel, James] Cognit Radio Technol LLC, Lynchburg, VA 24502 USA.
[Cook, Peter] Peter G Cook Consultancy, Macdonald Mesa, AZ 85201 USA.
[Mellen, Neal] Wireless Spectrum Management LLC, Tempe, AZ 85283 USA.
[Akbar, Ihsan] Harris Corp, Lynchburg, VA 24501 USA.
[Devasirvatham, Daniel] Wi Plan Wireless Consulting, Idaho Falls, ID 83415 USA.
[Sheehe, Charles] NASA, Cleveland, OH 44135 USA.
[Schutz, Bob] Artisan Wireless Solut, Carlsbad, CA 92009 USA.
RP Neel, J (reprint author), Cognit Radio Technol LLC, 147 Mill Ridge Rd STE 212, Lynchburg, VA 24502 USA.
EM james.neel@crtwireless.com; pgcook@pgcook.com; neal@wsmgmnt.com;
iakbar@harris.com; Charles.J.Sheehe@NASA.GOV;
bschutz@artisanwireless.com
NR 24
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U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1939-8018
EI 1939-8115
J9 J SIGNAL PROCESS SYS
JI J. Signal Process. Syst. Signal Image Video Technol.
PD MAR
PY 2015
VL 78
IS 3
BP 243
EP 256
DI 10.1007/s11265-014-0885-0
PG 14
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA CA6HN
UT WOS:000349011900002
ER
PT J
AU Montesano, PM
Rosette, J
Sun, G
North, P
Nelson, RF
Dubayah, RO
Ranson, KJ
Kharuk, V
AF Montesano, P. M.
Rosette, J.
Sun, G.
North, P.
Nelson, R. F.
Dubayah, R. O.
Ranson, K. J.
Kharuk, V.
TI The uncertainty of biomass estimates from modeled ICESat-2 returns
across a boreal forest gradient
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ecotone; LiDAR; Radiative transfer model; Forest biomass; Uncertainty;
Spaceboume
ID RADIATIVE-TRANSFER MODEL; WAVE-FORM LIDAR; SIBERIAN LARCH;
CLIMATE-CHANGE; VEGETATION HEIGHT; LASER ALTIMETRY; POLAR URALS;
AIRBORNE; CARBON; PERMAFROST
AB The Forest Light (FLIGHT) radiative transfer model was used to examine the uncertainty of vegetation structure measurements from NASA's planned ICESat-2 photon counting light detection and ranging (LiDAR) instrument across a synthetic Larix forest gradient in the taiga-tundra ecotone. The simulations demonstrate how measurements from the planned spaceborne mission, which differ from those of previous LiDAR systems, may perform across a boreal forest to non-forest structure gradient in globally important ecological region of northern Siberia. We used a modified version of FLIGHT to simulate the acquisition parameters of ICESat-2. Modeled returns were analyzed from collections of sequential footprints along LiDAR tracks (link-scales) of lengths ranging from 20 m-90 m. These link-scales traversed synthetic forest stands that were initialized with parameters drawn from field surveys in Siberian Larix forests. LiDAR returns from vegetation were compiled for 100 simulated LiDAR collections for each 10 Mg . ha(-1) interval in the 0-100 Mg . ha-1 above-ground biomass density (AGB) forest gradient. Canopy height metrics were computed and AGB was inferred from empirical models. The root mean square error (RMSE) and RMSE uncertainty associated with the distribution of inferred AGB within each AGB interval across the gradient was examined.
Simulation results of the bright daylight and low vegetation reflectivity conditions for collecting photon counting LiDAR with no topographic relief show that 1-2 photons are returned for 79%-88% of LiDAR shots. Signal photons account for similar to 67% of all LiDAR returns, while similar to 50% of shots result in 1 signal photon returned. The proportion of these signal photon returns do not differ significantly (p > 0.05) for AGB intervals >20 Mg . ha(-1). The 50 m link-scale approximates the finest horizontal resolution (length) at which photon counting LiDAR collection provides strong model fits and minimizes forest structure uncertainty in the synthetic Larix stands. At this link-scale AGB >20 Mg . ha(-1) has AGB error from 20-50% at the 95% confidence level. These results suggest that the theoretical sensitivity of ICESat-2 photon counting LiDAR measurements alone lack the ability to consistently discern differences in inferred AGB at 10 Mg . ha-1 intervals in sparse forests characteristic of the taiga-tundra ecotone. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Montesano, P. M.; Sun, G.; Dubayah, R. O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Montesano, P. M.] Sigma Space Corp, Lanham, MD 20706 USA.
[Montesano, P. M.; Sun, G.; Nelson, R. F.; Ranson, K. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Rosette, J.; North, P.] Swansea Univ, Dept Geog, Swansea SA2 8PP, W Glam, Wales.
[Rosette, J.] No Res Stn, Roslin EH26 9SY, Midlothian, Scotland.
[Kharuk, V.] Russian Acad Sci, Sukachev Inst Forest, Siberian Branch, Krasnoyarsk 660036, Russia.
RP Montesano, PM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20771 USA.
EM paul.m.montesano@nasa.gov
RI North, Peter/A-1616-2009; Ranson, Kenneth/G-2446-2012
OI North, Peter/0000-0001-9933-6935; Ranson, Kenneth/0000-0003-3806-7270
FU NASA Terrestrial Ecology Program
FX This work was supported by the NASA Terrestrial Ecology Program. We
acknowledge the expertise of Sergey Im, Pasha Oskorbin and Mukhtar
Naurzbaev that was critical to the success of various field expeditions
in remote areas of northern Siberia. We also acknowledge the importance
of the constructive criticism provided by the anonymous reviewers who
helped improve this manuscript.
NR 90
TC 9
Z9 9
U1 9
U2 59
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 MAR 1
PY 2015
VL 158
BP 95
EP 109
DI 10.1016/j.rse.2014.10.029
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CA4MR
UT WOS:000348879100008
ER
PT J
AU Schaepman, ME
Jehle, M
Hueni, A
D'Odorico, P
Damm, A
Weyerrnann, J
Schneider, FD
Laurent, V
Popp, C
Seidel, FC
Lenhard, K
Gege, P
Kuchler, C
Brazile, J
Kohler, P
De Vos, L
Meuleman, K
Meynart, R
Schlapfer, D
Kneubuhler, M
Itten, KI
AF Schaepman, Michael E.
Jehle, Michael
Hueni, Andreas
D'Odorico, Petra
Damm, Alexander
Weyerrnann, Jurg
Schneider, Fabian D.
Laurent, Valerie
Popp, Christoph
Seidel, Felix C.
Lenhard, Karim
Gege, Peter
Kuechler, Christoph
Brazile, Jason
Kohler, Peter
De Vos, Lieve
Meuleman, Koen
Meynart, Roland
Schlaepfer, Daniel
Kneubuhler, Mathias
Itten, Klaus I.
TI Advanced radiometry measurements and Earth science applications with the
Airborne Prism Experiment (APEX)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Imaging spectroscopy; Earth observation; APEX; Calibration; Processing;
Validation; Earth science applications
ID PUSHBROOM IMAGING SPECTROMETER; INDUCED CHLOROPHYLL FLUORESCENCE;
REMOTELY-SENSED DATA; RADIANCE DATA; VEGETATION INDEXES; SPECTROSCOPY
DATA; SURFACE ALBEDO; LAND-COVER; PERFORMANCE; RETRIEVAL
AB We present the Airborne Prism Experiment (APEX), its calibration and subsequent radiometric measurements as well as Earth science applications derived from this data. APEX is a dispersive pushbroom imaging spectrometer covering the solar reflected wavelength range between 372 and 2540 nm with nominal 312 (max. 532) spectral bands. APEX is calibrated using a combination of laboratory, in-flight and vicarious calibration approaches. These are complemented by using a forward and inverse radiative transfer modeling approach, suitable to further validate APEX data. We establish traceability of APEX radiances to a primary calibration standard, including uncertainty analysis. We also discuss the instrument simulation process ranging from initial specifications to performance validation. In a second part, we present Earth science applications using APEX. They include geometric and atmospheric compensated as well as reflectance anisotropy minimized Level 2 data. Further, we discuss retrieval of aerosol optical depth as well as vertical column density of NOx, a radiance data-based coupled canopy atmosphere model, and finally measuring sun-induced chlorophyll fluorescence (Fs) and infer plant pigment content. The results report on all APEX specifications including validation. APEX radiances are traceable to a primary standard with <4% uncertainty and with an average SNR of >625 for all spectral bands. Radiance based vicarious calibration is traceable to a secondary standard with <= 65% uncertainty. Except for inferring plant pigment content, all applications are validated using in-situ measurement approaches and modeling. Even relatively broad APEX bands (FWHM of 6 nm at 760 nm) can assess Fs with modeling agreements as high as R-2 = 0.87 (relative RMSE = 27.76%). We conclude on the use of high resolution imaging spectrometers and suggest further development of imaging spectrometers supporting science grade spectroscopy measurements. (C) 2014 The Authors. Published by Elsevier Inc.
C1 [Schaepman, Michael E.] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland.
[Schaepman, Michael E.; Jehle, Michael; Hueni, Andreas; D'Odorico, Petra; Damm, Alexander; Weyerrnann, Jurg; Schneider, Fabian D.; Laurent, Valerie; Kneubuhler, Mathias; Itten, Klaus I.] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland.
[Popp, Christoph] Smithsonian Inst, NMNH, Washington, DC 20013 USA.
[Seidel, Felix C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lenhard, Karim; Gege, Peter] Earth Observat Ctr, German Aerosp Ctr, D-82234 Oberpfaffenhofen, Wessling, Germany.
[Kuechler, Christoph] RUAG Schweiz AG, RUAG Aviat, CH-6032 Emmenbrucke, Switzerland.
[Brazile, Jason; Kohler, Peter] Netcetera AG, CH-8004 Zurich, Switzerland.
[De Vos, Lieve] OIP Sensor Syst, B-9700 Oudenaarde, Belgium.
[Meuleman, Koen] VITO, B-2400 Mol, Belgium.
[Meynart, Roland] ESA ESTEC, NL-2201 AZ Noordwijk, Netherlands.
[Schlaepfer, Daniel] ReSe Applicat Schlapfer, CH-9500 Wil, Switzerland.
RP Schaepman, ME (reprint author), Univ Zurich, Remote Sensing Labs, Winterthurerstr 190, CH-8057 Zurich, Switzerland.
EM michael.schaepman@geo.uzh.ch
RI Kneubuehler, Mathias/D-1153-2010; Damm, Alexander/D-1160-2010;
Schaepman, Michael/B-9213-2009;
OI Kneubuehler, Mathias/0000-0002-6716-585X; Schaepman,
Michael/0000-0002-9627-9565; Seidel, Felix/0000-0002-4282-2198; Hueni,
Andreas/0000-0002-4283-2484
FU University of Zurich; ESA PRODEX [16298/02/NL/US, 15449/01/NL/Sfe];
Swiss National Science Foundation (SNSF); Belgian Science Policy Office
(BELSPO); Swiss University Conference (SUK, KIP-SEON); University of
Zurich Research Priority Program on 'Global Change and Biodiversity'
(URPP GCB); Swiss Space Office (SSO); European Metrology Research
Programme (EMRP) - EMRP within EURAMET; European Metrology Research
Programme (EMRP) - European Union; ESA; German Aerospace Center (DLR)
FX We thank the University of Zurich for continued funding and support to
APEX. APEX is further supported through ESA, ESA PRODEX (16298/02/NL/US
and 15449/01/NL/Sfe), the Swiss National Science Foundation (SNSF), the
Belgian Science Policy Office (BELSPO), the Swiss University Conference
(SUK, KIP-SEON), the University of Zurich Research Priority Program on
'Global Change and Biodiversity' (URPP GCB), the Swiss Space Office
(SSO), the European Metrology Research Programme (EMRP, which is jointly
funded by the EMRP participating countries within EURAMET and the
European Union), and the German Aerospace Center (DLR). We thank former
UZH APEX project managers Jens Nieke and Edoardo Alberti and former ESA
APEX project managers Gerd Ulbrich, Jose Gaviras, and Hilde
Schroeven-Deceuninck for their support. We thank the reviewers for
helpful comments, allowing us to improve the manuscript
NR 108
TC 27
Z9 27
U1 4
U2 31
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 1
PY 2015
VL 158
BP 207
EP 219
DI 10.1016/j.rse.2014.11.014
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CA4MR
UT WOS:000348879100016
ER
PT J
AU Mertes, CM
Schneider, A
Sulla-Menashe, D
Tatem, AJ
Tan, B
AF Mertes, C. M.
Schneider, A.
Sulla-Menashe, D.
Tatem, A. J.
Tan, B.
TI Detecting change in urban areas at continental scales with MODIS data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Urban areas; Urbanization; Cities; Land cover; Change detection;
Classification; Machine learning; Decision trees; Data fusion; Decision
fusion
ID LAND-COVER CLASSIFICATION; NIGHTTIME LIGHT DATA; REMOTELY-SENSED DATA;
TIME-SERIES; UNITED-STATES; URBANIZATION DYNAMICS; SURFACE-TEMPERATURE;
SATELLITE DATA; RESOLUTION; IMAGERY
AB Urbanization is one of the most important components of global environmental change, yet most of what we know about urban areas is at the local scale. Remote sensing of urban expansion across large areas provides information on the spatial and temporal patterns of growth that are essential for understanding differences in socioeconomic and political factors that spur different forms of development, as well the social, environmental, and climatic impacts that result. However, mapping urban expansion globally is challenging: urban areas have a small footprint compared to other land cover types, their features are small, they are heterogeneous in both material composition and configuration, and the form and rates of new development are often highly variable across locations. Here we demonstrate a methodology for monitoring urban land expansion at continental to global scales using Moderate Resolution Imaging Spectroradiometer (MODIS) data. The new method focuses on resolving the spectral and temporal ambiguities between urban/non-urban land and stable/changed areas by: (1) spatially constraining the study extent to known locations of urban land; (2) integrating multi-temporal data from multiple satellite data sources to classify c. 2010 urban extent; and (3) mapping newly built areas (2000-2010) within the 2010 urban land extent using a multi-temporal composite change detection approach based on MODIS 250 m annual maximum enhanced vegetation index (EVI). We test the method in 15 countries in East-Southeast Asia experiencing different rates and manifestations of urban expansion. A two-tiered accuracy assessment shows that the approach characterizes urban change across a variety of socioeconomic/political and ecological/climatic conditions with good accuracy (70-91% overall accuracy by country, 69-89% by biome). The 250 m EVI data not only improve the classification results, but are capable of distinguishing between change and no-change areas in urban areas. Over 80% of the error in the change detection can be related to definitional issues or error propagation, rather than algorithm error. As such, these methods hold great potential for routine monitoring of urban change, as well as for providing a consistent and up-todate dataset on urban extent and expansion for a rapidly evolving region. (C) 2014 Published by Elsevier Inc.
C1 [Mertes, C. M.; Schneider, A.] Ctr Sustainabil & Global Environm, Nelson Inst Environm Studies, Madison, WI 53726 USA.
[Mertes, C. M.; Schneider, A.] Univ Wisconsin, Dept Geog, Madison, WI 53726 USA.
[Sulla-Menashe, D.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Tatem, A. J.] Univ Southampton, Dept Geog & Environm, Southampton SO17 1BJ, Hants, England.
[Tatem, A. J.] NIH, Fogarty Int Ctr, Bethesda, MD 20892 USA.
[Tan, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mertes, CM (reprint author), Ctr Sustainabil & Global Environm, Nelson Inst Environm Studies, Madison, WI 53726 USA.
EM cmertes@wisc.edu
FU World Bank
FX The authors wish to thank Phil Townsend, Mutlu Ozdogan, Caitlin Kontgis,
and two anonymous reviewers for comments on an earlier draft of this
manuscript. The authors are grateful to Sarah Graves, Jo Horton, James
Rollo, and Ian Schelly for technical support, assistance in data
collection, and cartographic expertise. This work was funded in part by
support from the World Bank. The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 101
TC 21
Z9 21
U1 15
U2 112
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 MAR 1
PY 2015
VL 158
BP 331
EP 347
DI 10.1016/j.rse.2014.09.023
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CA4MR
UT WOS:000348879100024
ER
PT J
AU Harter, TS
Morrison, PR
Mandelman, JW
Rummer, JL
Farrell, AP
Brill, RW
Brauner, CJ
AF Harter, T. S.
Morrison, P. R.
Mandelman, J. W.
Rummer, J. L.
Farrell, A. P.
Brill, R. W.
Brauner, C. J.
TI Validation of the i-STAT system for the analysis of blood gases and
acid-base status in juvenile sandbar shark (Carcharhinus plumbeus)
SO CONSERVATION PHYSIOLOGY
LA English
DT Article
DE Carbon dioxide tension; elasmobranch; oxygen tension; pH; portable
clinical analyser
ID DOGFISH SQUALUS-ACANTHIAS; SCYLIORHINUS-STELLARIS; EXHAUSTING ACTIVITY;
LONGLINE CAPTURE; ELASMOBRANCH; ANALYZER; EXERCISE; PARAMETERS;
PHYSIOLOGY; MORTALITY
AB Accurate measurements of blood gases and acid-base status require an array of sophisticated laboratory equipment that is typically not available during field research; such is the case for many studies on the stress physiology, ecology and conservation of elasmobranch fish species. Consequently, researchers have adopted portable clinical analysers that were developed for the analysis of human blood characteristics, but often without thoroughly validating these systems for their use on fish. The aim of our study was to test the suitability of the i-STAT system, the most commonly used portable clinical analyser in studies on fish, for analysing blood gases and acid-base status in elasmobranchs, over a broad range of conditions and using the sandbar shark (Carcharhinus plumbeus) as a model organism. Our results indicate that the i-STAT system can generate useful measurements of whole blood pH, and the use of appropriate correction factors may increase the accuracy of results. The i-STAT system was, however, unable to generate reliable results for measurements of partial pressure of oxygen (PO2) and the derived parameter of haemoglobin O-2 saturation. This is probably due to the effect of a closed-system temperature change on PO2 within the i-STAT cartridge and the fact that the temperature correction algorithms used by i-STAT assume a human temperature dependency of haemoglobin-O-2 binding; in many ectotherms, this assumption will lead to equivocal i-STAT PO2 results. The in vivo partial pressure of CO2 (PCO2) in resting sandbar sharks is probably below the detection limit for PCO2 in the i-STAT system, and the measurement of higher PCO2 tensions was associated with a large measurement error. In agreement with previous work, our results indicate that the i-STAT system can generate useful data on whole blood pH in fishes, but not blood gases.
C1 [Harter, T. S.; Morrison, P. R.; Farrell, A. P.; Brauner, C. J.] Univ British Columbia, Dept Zool, 6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada.
[Mandelman, J. W.] New England Aquarium, John H Prescott Marine Lab, Boston, MA 02110 USA.
[Rummer, J. L.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia.
[Farrell, A. P.] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada.
[Brill, R. W.] James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Highlands, NJ 07732 USA.
RP Harter, TS (reprint author), Univ British Columbia, Dept Zool, 6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada.
EM harter@zoology.ubc.ca
OI Morrison, Phillip/0000-0001-9470-4540
FU Natural Sciences and Engineering Research Council (NSERC) of Canada
Discovery Grant; NSERC Accelerator Supplement
FX This study was supported by a Natural Sciences and Engineering Research
Council (NSERC) of Canada Discovery Grant to C.J.B. and A.P.F. and an
NSERC Accelerator Supplement to C.J.B. A.P.F. holds a Canada Research
Chair. This is contribution number 3433 from the Virginia Institute of
Marine Science, College of William & Mary. Funding for some of the study
supplies, including cartridges, was provided by an anonymous donor
supporting J.W.M.'s work.
NR 28
TC 4
Z9 4
U1 4
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 2051-1434
J9 CONSERV PHYSIOL
JI Conserv. Physiol.
PD MAR 1
PY 2015
VL 3
AR cov002
DI 10.1093/conphys/cov002
PG 10
WC Biodiversity Conservation; Ecology; Environmental Sciences; Physiology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Physiology
GA DK8RB
UT WOS:000375194900001
PM 27293687
ER
PT J
AU Fischman, M
Chan, S
Huang, N
Pak, K
AF Fischman, Mark
Chan, Samuel
Huang, Nelson
Pak, Kyung
TI Frequency-Agile Radar Electronics for the Soil Moisture Active/Passive
(SMAP) Mission
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
AB The radar aboard the Soil Moisture Active/Passive (SMAP) instrument is an L-band scatterometer/ synthetic aperture radar (SAR) with uniquely designed capabilities for global retrieval of surface soil moisture. Several key science requirements have shaped the radar architecture, including requirements on terrestrial radio frequency interference (RFI) mitigation, calibration stability, and on silencing radiated emissions from the electronics in the presence of the sensitive radiometer aboard SMAP. The design uses an unconventional conical scan sequence to collect SAR data over a wide swath while the radar frequency-hops over 1217-1298 MHz in order to avoid RFI from ground sources. In this paper, we discuss: 1) the design trades that led to the choice of a frequency-hopping, "tunable LO" receiver scheme that significantly reduces the SMAP radar susceptibility to RFI; 2) loopback calibration to minimize bias errors in the transmit-power x receiver-gain product; 3) hardware design techniques for decreasing radiated emissions levels in the 1.41-GHz radiometer band; and 4) pre-launch performance results from flight radar environmental testing.
C1 [Fischman, Mark; Chan, Samuel; Huang, Nelson; Pak, Kyung] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fischman, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM mafisch@jpl.nasa.gov
NR 12
TC 1
Z9 1
U1 0
U2 1
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 MAR
PY 2015
VL 3
IS 1
BP 10
EP 19
DI 10.1109/MGRS.2015.2397443
PG 10
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0FI
UT WOS:000390000700003
ER
PT J
AU Jones, CM
Driggers, WB
AF Jones, Christian M.
Driggers, William B., III
TI Clarification on the Fecundity of Rhinoptera bonasus (Mitchill)
SO SOUTHEASTERN NATURALIST
LA English
DT Article
ID CHESAPEAKE BAY; COWNOSE RAY; REPRODUCTIVE-BIOLOGY
AB Accurate fecundity estimates are necessary for the proper assessment of fish stocks. Despite all recent investigations of the reproductive biology of Rhinoptera bonasus (Cownose Ray) indicating a maximum fecundity of 2 embryos per brood, maximum fecundity estimates of 6 per brood persist. All reports of 6 embryos per brood seem to stem from a single account. It is the purpose of this paper to present evidence indicating that the report of 6 embryos is based upon a misidentification in the field, and that maximum fecundity estimates for the Cownose Ray are therefore up to six-fold higher than actually observed.
C1 [Jones, Christian M.; Driggers, William B., III] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
RP Jones, CM (reprint author), Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM christian.jones@noaa.gov
NR 18
TC 0
Z9 0
U1 1
U2 3
PU HUMBOLDT FIELD RESEARCH INST
PI STEUBEN
PA PO BOX 9, STEUBEN, ME 04680-0009 USA
SN 1528-7092
EI 1938-5412
J9 SOUTHEAST NAT
JI Southeast. Nat.
PD MAR
PY 2015
VL 14
IS 1
BP N16
EP N20
DI 10.1656/058.014.0113
PG 5
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DE8NJ
UT WOS:000370892400020
ER
PT J
AU Bednarcyk, BA
Stier, B
Simon, JW
Reese, S
Pineda, EJ
AF Bednarcyk, Brett A.
Stier, Bertram
Simon, Jaan-W.
Reese, Stefanie
Pineda, Evan J.
TI Meso- and micro-scale modeling of damage in plain weave composites
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Damage; Composite materials; Finite element method; Micromechanics;
Woven composites; Simulation
ID FINITE-ELEMENT ANALYSIS; PROGRESSIVE DAMAGE; GENERALIZED-METHOD; LOCAL
DAMAGE; PART I; CELLS; FAILURE; ACCUMULATION; DEFORMATION; BEHAVIOR
AB This paper presents a comparison of meso- and micro-scale approaches to modeling progressive damage in plain weave reinforced polymer matrix composites. The mesa-scale approach treats the woven composite tows as effective materials, utilizing an anisotropic progressive continuum damage model. The micro-scale approach utilizes the Generalized Method of Cells semi-analytical micromechanics theory to represent the nonlinear response of the tows, wherein the same progressive damage model, now specialized to initially isotropic materials, is used to model the matrix material within the tows. For consistency, the micro-scale nonlinear tow predictions were used to characterize the anisotropic damage model for the tows for use in the meso-scale approach. The damage model thus plays a key role in the presented study as it must be three-dimensional to admit the in-situ stress state within the woven composite tows, and it must capture the coupling between directional damage components that is predicted by the microscale model for the tows. The developed three-dimensional, energy based, anisotropic, stiffness reduction damage model was implemented within Abaqus as a user constitutive model and within the Generalized Method of Cells. Hence, the identical plain weave composite geometry, modeled in Abaqus, was used in the mesa-scale approach (with the anisotropic damage model representing the tows) and in the microscale approach (with the Generalized Method of Cells representing the tows). Published by Elsevier Ltd.
C1 [Bednarcyk, Brett A.; Pineda, Evan J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Stier, Bertram; Simon, Jaan-W.; Reese, Stefanie] Rhein Westfal TH Aachen, Inst Appl Mech IFAM, Aachen, Germany.
RP Bednarcyk, BA (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Brett.A.Bednarcyk@nasa.gov
RI Reese, Stefanie/A-8756-2014; Simon, Jaan/J-9114-2014
OI Simon, Jaan/0000-0003-2231-2569
FU NASA Fundamental Aeronautics Program Aero Sciences Project; Deutsche
Forschungsgemeinschaft (DFG); Theodore-von-Karman Fellowship of the
Exploratory Research Space (ERS) of RWTH Aachen University
FX The authors gratefully acknowledge the financial support of the NASA
Fundamental Aeronautics Program Aero Sciences Project, the Deutsche
Forschungsgemeinschaft (DFG), and the Theodore-von-Karman Fellowship of
the Exploratory Research Space (ERS) of RWTH Aachen University, who made
this collaboration possible.
NR 31
TC 5
Z9 5
U1 2
U2 28
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-8223
EI 1879-1085
J9 COMPOS STRUCT
JI Compos. Struct.
PD MAR
PY 2015
VL 121
BP 258
EP 270
DI 10.1016/j.compstruct.2014.11.013
PG 13
WC Materials Science, Composites
SC Materials Science
GA AZ2TP
UT WOS:000348085500025
ER
PT J
AU Rathsam, J
Rafaely, B
AF Rathsam, J.
Rafaely, B.
TI Analysis of absorption in situ with a spherical microphone array
SO APPLIED ACOUSTICS
LA English
DT Article
DE Absorption; In situ; Array processing
ID REFLECTION COEFFICIENTS; ACOUSTIC-IMPEDANCE; SOUND-ABSORPTION; DESIGN
AB Measured values of acoustic absorption often vary between the laboratory and the field due to deficiencies in standard measurement methods. This paper introduces a new method of measuring acoustic absorption in the field using a spherical microphone array. Plane-wave decomposition is used to separate direct energy from reflected energy when the array is placed adjacent to the absorptive sample. Additional signal processing techniques including the Dolph-Chebyshev beampattern and Delay-and-Sum processing are introduced and used to improve the method. The method is verified by simulation for normal and oblique incidence and by experiment for normal incidence. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Rathsam, J.; Rafaely, B.] Ben Gurion Univ Negev, Dept Elect & Comp Engn, IL-84105 Beer Sheva, Israel.
RP Rathsam, J (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Mail Stop 463, Hampton, VA 23681 USA.
EM jonathan.rathsam@nasa.gov
RI RAFAELY, BOAZ/F-2016-2012
FU United States National Science Foundation [0753753]; Israel Science
Foundation [155/06]
FX Work supported by the United States National Science Foundation (Grant
No. 0753753) and the Israel Science Foundation (Grant No. 155/06). The
authors thank Dr. Peter D'Antonio for permitting the first author to use
the impedance tube at RPG Diffusor Systems, Inc. Ran Manor and Yuval
Starky are acknowledged for their assistance during the in situ
measurement.
NR 26
TC 2
Z9 3
U1 0
U2 10
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0003-682X
EI 1872-910X
J9 APPL ACOUST
JI Appl. Acoust.
PD MAR
PY 2015
VL 89
BP 273
EP 280
DI 10.1016/j.apacoust.2014.10.008
PG 8
WC Acoustics
SC Acoustics
GA AW8YY
UT WOS:000346546300029
ER
PT J
AU Abeysekara, AU
Alfaro, R
Alvarez, C
Alvarez, JD
Angeles, F
Arceo, R
Arteaga-Velazquezd, JC
Avila-Aroche, A
Solares, HAA
Badillo, C
Barber, AS
Baughman, BM
Bautista-Elivar, N
Gonzalez, JB
Belmont, E
Benitez, E
BenZvi, SY
Berley, D
Bernal, A
Rosales, MB
Braun, J
Caballero-Lopez, RA
Caballero-More, KS
Cabrera, I
Carraminana, A
Castaneda-Martinez, L
Castillo, M
Cotti, U
Cotzomi, J
de la Fuente, E
De Leon, C
DeYoung, T
Diaz-Azuara, A
Diaz-Cruz, L
Hernandez, RD
Diaz-Velez, JC
Dingus, BL
Dultzin, D
DuVernois, MA
Ellsworth, RW
Fernandez, A
Fiorino, DW
Fraija, N
Galindo, A
Garcia-Torales, G
Garfias, F
Gonzalez, A
Gonzalez, LX
Gonzalez, MM
Goodman, JA
Grabski, V
Gussert, M
Guzman-Ceron, C
Hampel-Arias, Z
Harding, JP
Hernandez-Cervantes, L
Hui, CM
Huntemeyer, P
Imran, A
Iriarte, A
Karn, P
Kieda, D
Kunde, GJ
Langarica, R
Lara, A
Lara, G
Lauer, RJ
Lee, WH
Lennarz, D
Vargas, HL
Linares, EC
Linnemann, JT
Longo, M
Luna-Garcia, R
Marinelli, A
Martinez, LA
Martinez, H
Martinez, O
Martinez-Castro, J
Martos, M
Matthews, JAJ
McEnery, J
Torres, EM
Miranda-Romagnoli, P
Moreno, E
Mostafa, M
Nava, J
Nellen, L
Newbold, M
Noriega-Papaqui, R
Oceguera-Becerra, T
Page, DP
Patricelli, B
Pelayo, R
Perez-Perez, EG
Pretz, J
Ramirez, I
Renteria, A
Riviere, C
Rosa-Gonzalez, D
Ruiz-Sala, F
Ruiz-Velasco, EL
Ryan, J
Sacahui, JR
Salazar, H
Salesa, F
Sandoval, A
Santos, E
Schneider, M
Silich, S
Sinnis, G
Smith, AJ
Woodle, KS
Springer, RW
Suarez, F
Taboada, I
Tepe, A
Toale, PA
Tollefson, K
Torres, I
Tinoco, S
Ukwatta, TN
Galicia, JFV
Vanegas, P
Vazquez, A
Villasenor, L
Wall, W
Weisgarber, T
Westerhoff, S
Wisher, IG
Wood, J
Yodh, GB
Younk, PW
Zaborov, D
Zepeda, A
Zhou, H
AF Abeysekara, A. U.
Alfaro, R.
Alvarez, C.
Alvarez, J. D.
Angeles, F.
Arceo, R.
Arteaga-Velazquezd, J. C.
Avila-Aroche, A.
Solares, H. A. Ayala
Badillo, C.
Barber, A. S.
Baughman, B. M.
Bautista-Elivar, N.
Gonzalez, J. Becerra
Belmont, E.
Benitez, E.
BenZvi, S. Y.
Berley, D.
Bernal, A.
Rosales, M. Bonilla
Braun, J.
Caballero-Lopez, R. A.
Caballero-More, K. S.
Cabrera, I.
Carraminana, A.
Castaneda-Martinez, L.
Castillo, M.
Cotti, U.
Cotzomi, J.
de la Fuente, E.
De Leon, C.
DeYoung, T.
Diaz-Azuara, A.
Diaz-Cruz, L.
Hernandez, R. Diaz
Diaz-Velez, J. C.
Dingus, B. L.
Dultzin, D.
DuVernois, M. A.
Ellsworth, R. W.
Fernandez, A.
Fiorino, D. W.
Fraija, N.
Galindo, A.
Garcia-Torales, G.
Garfias, F.
Gonzalez, A.
Gonzalez, L. X.
Gonzalez, M. M.
Goodman, J. A.
Grabski, V.
Gussert, M.
Guzman-Ceron, C.
Hampel-Arias, Z.
Harding, J. P.
Hernandez-Cervantes, L.
Hui, C. M.
Huentemeyer, P.
Imran, A.
Iriarte, A.
Karn, P.
Kieda, D.
Kunde, G. J.
Langarica, R.
Lara, A.
Lara, G.
Lauer, R. J.
Lee, W. H.
Lennarz, D.
Vargas, H. Leon
Linares, E. C.
Linnemann, J. T.
Longo, M.
Luna-Garcia, R.
Marinelli, A.
Martinez, L. A.
Martinez, H.
Martinez, O.
Martinez-Castro, J.
Martos, M.
Matthews, J. A. J.
McEnery, J.
Torres, E. Mendoza
Miranda-Romagnoli, P.
Moreno, E.
Mostafa, M.
Nava, J.
Nellen, L.
Newbold, M.
Noriega-Papaqui, R.
Oceguera-Becerra, T.
Page, D. P.
Patricelli, B.
Pelayo, R.
Perez-Perez, E. G.
Pretz, J.
Ramirez, I.
Renteria, A.
Riviere, C.
Rosa-Gonzalez, D.
Ruiz-Sala, F.
Ruiz-Velasco, E. L.
Ryan, J.
Sacahui, J. R.
Salazar, H.
Salesa, F.
Sandoval, A.
Santos, E.
Schneider, M.
Silich, S.
Sinnis, G.
Smith, A. J.
Woodle, K. Sparks
Springer, R. W.
Suarez, F.
Taboada, I.
Tepe, A.
Toale, P. A.
Tollefson, K.
Torres, I.
Tinoco, S.
Ukwatta, T. N.
Galicia, J. F. Valdes
Vanegas, P.
Vazquez, A.
Villasenor, L.
Wall, W.
Weisgarber, T.
Westerhoff, S.
Wisher, I. G.
Wood, J.
Yodh, G. B.
Younk, P. W.
Zaborov, D.
Zepeda, A.
Zhou, H.
TI VAMOS: A pathfinder for the HAWC gamma-ray observatory
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Detector prototype; Scientific verification; TeV cosmic rays
ID FORBUSH DECREASES
AB VAMOS(1) was a prototype detector built in 2011 at an altitude of 4100 m a.s.l. in the state of Puebla, Mexico. The aim of VAMOS was to finalize the design, construction techniques and data acquisition system of the HAWC observatory. HAWC is an air-shower array currently under construction at the same site of VAMOS with the purpose to study the TeV sky. The VAMOS setup included six water Cherenkov detectors and two different data acquisition systems. It was in operation between October 2011 and May 2012 with an average live time of 30%. Besides the scientific verification purposes, the eight months of data were used to obtain the results presented in this paper: the detector response to the Forbush decrease of March 2012, and the analysis of possible emission, at energies above 30 GeV, for long gamma-ray bursts GRB111016B and GRB120328B. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Abeysekara, A. U.; Langarica, R.; Linnemann, J. T.; Tollefson, K.; Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Alfaro, R.; Badillo, C.; Belmont, E.; Cabrera, I.; Gonzalez, A.; Grabski, V.; Vargas, H. Leon; Marinelli, A.; Ramirez, I.; Renteria, A.; Sandoval, A.; Suarez, F.; Vanegas, P.; Vazquez, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City, DF, Mexico.
[Alvarez, C.; Arceo, R.; Santos, E.] Univ Autonoma Chiapas, CEFyMAP, Tuxtla Gutierrez, Chiapas, Mexico.
[Alvarez, J. D.; Arteaga-Velazquezd, J. C.; Cotti, U.; De Leon, C.; Linares, E. C.; Villasenor, L.] Univ Michoacana, Morelia, Michoacan, Mexico.
[Angeles, F.; Avila-Aroche, A.; Benitez, E.; Bernal, A.; Castaneda-Martinez, L.; Diaz-Azuara, A.; Dultzin, D.; Fraija, N.; Garfias, F.; Gonzalez, M. M.; Guzman-Ceron, C.; Hernandez-Cervantes, L.; Iriarte, A.; Lara, G.; Lee, W. H.; Martinez, L. A.; Martos, M.; Page, D. P.; Patricelli, B.; Riviere, C.; Ruiz-Sala, F.; Ruiz-Velasco, E. L.; Sacahui, J. R.; Tinoco, S.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Solares, H. A. Ayala; Hui, C. M.; Huentemeyer, P.; Zhou, H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA.
[Barber, A. S.; Kieda, D.; Newbold, M.; Springer, R. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT USA.
[Baughman, B. M.; Gonzalez, J. Becerra; Berley, D.; Braun, J.; Ellsworth, R. W.; Goodman, J. A.; Smith, A. J.; Wood, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Bautista-Elivar, N.; Perez-Perez, E. G.] Univ Politecn Pachuca, Pachuca, Hidalgo, Mexico.
[Gonzalez, J. Becerra; McEnery, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[BenZvi, S. Y.; Diaz-Velez, J. C.; DuVernois, M. A.; Fiorino, D. W.; Hampel-Arias, Z.; Imran, A.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Rosales, M. Bonilla; Carraminana, A.; Hernandez, R. Diaz; Galindo, A.; Torres, E. Mendoza; Nava, J.; Rosa-Gonzalez, D.; Silich, S.; Torres, I.; Wall, W.] Inst Nacl Astrofis Opt & Electr, Tonantzintla, Puebla, Mexico.
[Caballero-Lopez, R. A.; Gonzalez, L. X.; Lara, A.; Galicia, J. F. Valdes] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico.
[Caballero-Lopez, R. A.; Gonzalez, L. X.; Lara, A.; Galicia, J. F. Valdes] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico.
[Caballero-More, K. S.; Martinez, H.; Zepeda, A.] IPN, Ctr Invest & Estudios Avanzados, Dept Phys, Mexico City 07738, DF, Mexico.
[Castillo, M.; Cotzomi, J.; Diaz-Cruz, L.; Fernandez, A.; Martinez, O.; Moreno, E.; Salazar, H.] Benemerita Univ Autonoma Puebla, Fac Ciencias Fis Matemat, Puebla, Mexico.
[de la Fuente, E.; Garcia-Torales, G.; Oceguera-Becerra, T.] Univ Guadalajara, Dept Fis ITPhd CUCEA, Phys Mat Phd CUVALLES, Guadalajara, Jalisco, Mexico.
[de la Fuente, E.; Garcia-Torales, G.; Oceguera-Becerra, T.] Univ Guadalajara, Dept Elect CUCEI, IT Phd CUCEA, Phys Mat Phd CUVALLES, Guadalajara, Jalisco, Mexico.
[DeYoung, T.; Mostafa, M.; Pretz, J.; Salesa, F.; Woodle, K. Sparks; Zaborov, D.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Dingus, B. L.; Harding, J. P.; Kunde, G. J.; Sinnis, G.; Younk, P. W.] Los Alamos Natl Lab, Div Phys, Los Alamos, NM USA.
[Ellsworth, R. W.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Gussert, M.; Longo, M.] Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA.
[Karn, P.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Lauer, R. J.; Matthews, J. A. J.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Lennarz, D.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys & Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Luna-Garcia, R.; Martinez-Castro, J.; Pelayo, R.] Inst Politecn Nacl, Ctr Invest Computac, Mexico City, DF, Mexico.
[Miranda-Romagnoli, P.; Noriega-Papaqui, R.] Univ Autonoma Estado Hidalgo, Pachuca, Hidalgo, Mexico.
[Nellen, L.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Ryan, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Schneider, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Toale, P. A.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Marinelli, A (reprint author), Univ Nacl Autonoma Mexico, Inst Fis, Mexico City, DF, Mexico.
EM antonio.marinelli@fisica.unam.mx; zaborov@phys.psu.edu
OI Lara, Alejandro/0000-0001-6336-5291; Dingus, Brenda/0000-0001-8451-7450;
Lauer, Robert/0000-0003-1933-7861; Becerra Gonzalez,
Josefa/0000-0002-6729-9022
FU National Science Foundation; US Department of Energy Office of
High-Energy Physics; LDRD program of Los Alamos National Laboratory;
Consejo Nacional de Ciencia y Tecnologia [55155, 103520, 105033, 105666,
122331, 194116, 132197, 179588]; Red de Fisica de Altas Energias;
DGAPA-UNAM [IN110212, IN105211, IN108713, IN121309, IN115409, IN111612,
IN112412, IG100414-3]; VIEP-BUAP [161-EXC-2011]; Luc-Binette Foundation
UNAM Postdoctoral Fellowship; University of Wisconsin Alumni Research
Foundation; Institute of Geophysics and Planetary Physics at Los Alamos
National Lab
FX We gratefully acknowledge Scott DeLay and Federico Bareilles for their
dedicated efforts in the construction and maintenance of the VAMOS
prototype. This work has been supported by: the National Science
Foundation, the US Department of Energy Office of High-Energy Physics,
the LDRD program of Los Alamos National Laboratory, Consejo Nacional de
Ciencia y Tecnologia (Grants 55155, 103520, 105033, 105666, 122331,
194116, 132197 and 179588), Red de Fisica de Altas Energias, DGAPA-UNAM
(Grants IN110212, IN105211, IN108713, IN121309, IN115409, IN111612,
IN112412 and IG100414-3), VIEP-BUAP (Grant 161-EXC-2011), Luc-Binette
Foundation UNAM Postdoctoral Fellowship, the University of Wisconsin
Alumni Research Foundation, and the Institute of Geophysics and
Planetary Physics at Los Alamos National Lab.
NR 31
TC 3
Z9 3
U1 0
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD MAR
PY 2015
VL 62
BP 125
EP 133
DI 10.1016/j.astropartphys.2014.08.004
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AW8ZR
UT WOS:000346548200015
ER
PT J
AU Yi, BQ
Yang, P
Dessler, A
da Silva, AM
AF Yi, Bingqi
Yang, Ping
Dessler, Andrew
da Silva, Arlindo M.
TI Response of Aerosol Direct Radiative Effect to the East Asian Summer
Monsoon
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Aerosol direct radiative forcing; Clouds and Earth's Radiant Energy
System (CERES) observations; East Asian summer monsoon; MERRAero
reanalysis
ID ATMOSPHERE; TOP; INSTRUMENT; SATELLITE; OCEANS; CLOUDS
AB Asian summer monsoon and atmospheric aerosol simultaneously influence the climate in the East Asian region. However, substantial uncertainties exist in the current understanding of the interactions between monsoon and aerosol and their combined effects. Previous studies have shown that aerosols influence the strength of monsoon and monsoon-related water cycles; however, monsoon strongly regulates the aerosol spatial distribution. This letter investigates the radiative flux response at the top of the atmosphere to the Asian summer monsoon by using observations made by the Clouds and Earth's Radiant Energy System and the Moderate Resolution Imaging Spectroradiometer. In comparison with the ten-year (2002-2011) mean climatology, the aerosol radiative effect is estimated over two eastern Asia regions for the months of July in 2002 and 2003, corresponding to a weak and a strong summer monsoon event, respectively. The dramatically different influences show the aerosol radiative forcing over land to be strongly responsive to Asian summer monsoon. Furthermore, the reanalysis-based estimate of the aerosol radiative effect is consistent with its observation-only counterpart.
C1 [Yi, Bingqi; Yang, Ping; Dessler, Andrew] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Natl Aeronaut & Space Adm, Greenbelt, MD 20771 USA.
RP Yi, BQ (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM bingqi.yi@tamu.edu
RI Yi, Bingqi/E-4076-2012; Yang, Ping/B-4590-2011; Dessler,
Andrew/G-8852-2012
OI Yi, Bingqi/0000-0002-1437-8376; Dessler, Andrew/0000-0003-3939-4820
FU David Bullock Harris Chair in Geosciences; College of Geosciences at
Texas AM University; National Science Foundation Grant [ATM-0803779]
FX This work was supported in part by the endowment funds associated with
the David Bullock Harris Chair in Geosciences, the College of
Geosciences at Texas A&M University, and National Science Foundation
Grant ATM-0803779.
NR 16
TC 2
Z9 2
U1 0
U2 32
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 MAR
PY 2015
VL 12
IS 3
BP 597
EP 600
DI 10.1109/LGRS.2014.2352630
PG 4
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AT5NE
UT WOS:000344988800032
ER
PT J
AU Yi, DH
Harbeck, JP
Manizade, SS
Kurtz, NT
Studinger, M
Hofton, M
AF Yi, Donghui
Harbeck, Jeremy P.
Manizade, Serdar S.
Kurtz, Nathan T.
Studinger, Michael
Hofton, Michelle
TI Arctic Sea Ice Freeboard Retrieval With Waveform Characteristics for
NASA's Airborne Topographic Mapper (ATM) and Land, Vegetation, and Ice
Sensor (LVIS)
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Algorithms; altimetry; arctic region; remote sensing; sea ice
ID THICKNESS
AB Data from an IceBridge Arctic campaign on April 20, 2010 with the Airborne Topographic Mapper (ATM) and the Land, Vegetation, and Ice Sensor (LVIS) in operation on the same airplane were used in this study. ATM and LVIS lidar waveforms were fitted with Gaussian curves to calculate pulsewidth, peak location, pulse amplitude, and signal baseline. For each waveform, the centroid, skewness, kurtosis, and pulse area were also calculated. Received waveform parameters, such as pulsewidth, pulse amplitude, pulse area, skewness, and kurtosis, show coherent response to variations of geophysical features along an ATM or LVIS profile. These parameters, combined with elevation, were used to identify leads in sea-ice freeboard calculation. The relationship between these parameters and sea-ice freeboard and surface features were studied by comparing the parameters with ATM and LVIS-derived freeboard and coincident Digital Mapping System images which have been used to classify sea-ice surface types such as leads, thin ice, gray ice, and thick ice. An elevation bias of more than 16 cm (peak-to-peak) as a function of laser scanner azimuth was found in the ATM data, and an empirical correction was applied; this correction will improve the ATM shot-to-shot freeboard significantly. The newly derived ATM freeboard was compared with the current IceBridge IDCSI2 freeboard product at National Snow and Ice Data Center (NSIDC) and the freeboard derived from LVIS data. Over the studied area, the mean freeboard is 0.540 +/- 0.091 m for the IDCSI2 at NSIDC, 0.496 +/- 0.062 m for the ATM after empirical elevation correction, and 0.509 +/- 0.048 m for the LVIS.
C1 [Yi, Donghui] NASA, Stinger Ghaffarian Technol Inc, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Harbeck, Jeremy P.] NASA, ADNET Syst Inc, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Manizade, Serdar S.] NASA, URS Corp, Cryospher Sci Lab, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Kurtz, Nathan T.; Studinger, Michael] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hofton, Michelle] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Yi, DH (reprint author), NASA, Stinger Ghaffarian Technol Inc, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
EM donghui.yi@nasa.gov
RI Beckley, Matthew/D-4547-2013
FU National Aeronautics and Space Administration's Operation IceBridge
project
FX This work was supported by the National Aeronautics and Space
Administration's Operation IceBridge project.
NR 17
TC 2
Z9 2
U1 1
U2 26
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 MAR
PY 2015
VL 53
IS 3
BP 1403
EP 1410
DI 10.1109/TGRS.2014.2339737
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 AR9MZ
UT WOS:000343900600023
ER
PT J
AU Khlopenkov, KV
Doelling, DR
Okuyama, A
AF Khlopenkov, Konstantin V.
Doelling, David R.
Okuyama, Arata
TI MTSAT-1R Visible Imager Point Spread Function Correction, Part II:
Theory
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; deconvolution; image restoration; multi-functional
transport satellite (MTSAT-1R); point spread function (PSF)
ID SYSTEM; CERES
AB An image processing methodology is presented to recover the quality of the Multifunctional Transport Satellite (MTSAT)-1R visible channel data affected by spatial crosstalk. The slight blurring of the visible optical path is attributed to an imperfection in the mirror surface caused either by flawed polishing or a dust contaminant. The methodology assumes that the dispersed portion of the signal is small and distributed randomly around the optical axis, which allows the image to be deconvolved using an inverted point spread function (PSF). The PSF is described by four parameters, which are solved using a maximum-likelihood estimator using coincident collocated MTSAT-2 images as truth. A subpixel image matching technique is used to align the MTSAT-2 pixels into the MTSAT-1R projection and to correct for navigation errors and cloud displacement due to the time and viewing geometry differences between the two satellite observations. An optimal set of the PSF parameters is derived by an iterative routine based on the 4-D Powell's conjugate direction method that minimizes the difference between the PSF-corrected MTSAT-1R and the collocated MTSAT-2 images. The PSF parameters were found to be consistent over the 5 days of available daytime coincident and MTSAT-1R and MTSAT-2 images. After applying the PSF parameters, the visible sensor response is nearly linear, and the space count is close to zero. The overall linear regression standard error was reduced by 52%. Users can easily apply the PSF parameter coefficients to the MTSAT-1R imager pixel level counts to restore the original quality of the entire MTSAT-1R record.
C1 [Khlopenkov, Konstantin V.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Doelling, David R.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Okuyama, Arata] Japan Meteorol Agcy, Meteorol Satellite Ctr, Tokyo 2040012, Japan.
RP Khlopenkov, KV (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM konstantin.khlopenkov@nasa.gov; david.r.doelling@nasa.gov;
okuyama.arata@met.kishou.go.jp
RI Richards, Amber/K-8203-2015
FU National Aeronautics and Space Administration Earth Science Enterprise
Office through the Clouds and the Earth's Radiant Energy System
FX This work was supported by the National Aeronautics and Space
Administration Earth Science Enterprise Office through the Clouds and
the Earth's Radiant Energy System.
NR 13
TC 3
Z9 3
U1 1
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2015
VL 53
IS 3
BP 1504
EP 1512
DI 10.1109/TGRS.2014.2344627
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 AR9MZ
UT WOS:000343900600031
ER
PT J
AU Doelling, DR
Khlopenkov, KV
Okuyama, A
Haney, CO
Gopalan, A
Scarino, BR
Nordeen, M
Bhatt, R
Avey, L
AF Doelling, David R.
Khlopenkov, Konstantin V.
Okuyama, Arata
Haney, Conor O.
Gopalan, Arun
Scarino, Benjamin R.
Nordeen, Michele
Bhatt, Rajendra
Avey, Lance
TI MTSAT-1R Visible Imager Point Spread Correction Function, Part I: The
Need for, Validation of, and Calibration With
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Geostationary visible imager calibration; multifunctional transport
satellite (MTSAT)-1R; point-spread function (PSF)
ID PATHFINDER BENCHMARK PERIOD; METEOROLOGICAL SATELLITE;
INTER-CALIBRATION; SOLAR CHANNELS; TARGETS; SYSTEM; DESERT; GMS-5; CERES
AB The multifunctional transport satellite (MTSAT)-1R imager was launched in 2005 and is operated by the Japan Meteorological Agency (JMA). A nonlinear behavior in the MTSAT-1R visible sensor response is observed when the instrument is intercalibrated with coincident moderate resolution imaging spectroradiometer (MODIS) ray-matched radiances. Analysis reveals that the nonlinear behavior is not a result of imager navigation, sensor spectral response difference, nor scan pattern. Examination of coincident MTSAT-1R and MTSAT-2 images reveals that MTSAT-1R dark ocean radiances are affected by neighboring bright clouds, whereas large regions of dark ocean radiances are not impacted. Although the IR and visible optical paths are shared, the MTSAT-1R brightness temperatures are not affected. A dust contaminant coating the mirror, which only affects certain wavelengths, may be one explanation. To address the nonlinearity, a pixel point spread function (PSF) correction algorithm is implemented, wherein most of the radiance contribution is from the pixel field of view itself, as well as including a small contribution from all pixels within a radii of several hundred kilometers. The application of the PSF-corrected similar to 80% of the affected pixel radiances. After application, a near linear response is observed between the coincident MTSAT-1R and Aqua-MODIS ray-matched radiances, and the intercept is now near the predicted space count of zero. The monthly calibration gain noise is reduced by one-third when compared with the non-PSF-corrected gains. The monthly gains are the most erratic during the first two years of operation, and the MTSAT-1R visible sensor is degrading at similar to 1.9% decade.
C1 [Doelling, David R.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Khlopenkov, Konstantin V.; Haney, Conor O.; Gopalan, Arun; Scarino, Benjamin R.; Nordeen, Michele; Bhatt, Rajendra] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Okuyama, Arata] Japan Meteorol Agcy, Meteorol Satellite Ctr, Tokyo 2040012, Japan.
[Avey, Lance] Utah Dept Environm Qual, Div Air Qual, Salt Lake City, UT 84114 USA.
RP Doelling, DR (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
EM david.r.doelling@nasa.gov; konstantin.khlopenkov@nasa.gov;
okuyama.arata@met.kishou.go.jp; conor.o.haney@nasa.gov;
arun.gopalan-1@nasa.gov; Benjamin.r.scarino@nasa.gov;
michele.l.nordeen@nasa.gov; rajendra.bhatt@nasa.gov; lavey@utah.gov
RI Richards, Amber/K-8203-2015
FU National Aeronautics and Space Administration Earth Science Enterprise
Office through the Clouds and the Earth's Radiant Energy System
FX This work was supported by the National Aeronautics and Space
Administration Earth Science Enterprise Office through the Clouds and
the Earth's Radiant Energy System.
NR 37
TC 3
Z9 3
U1 1
U2 29
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 MAR
PY 2015
VL 53
IS 3
BP 1513
EP 1526
DI 10.1109/TGRS.2014.2344678
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AR9MZ
UT WOS:000343900600032
ER
PT J
AU Lei, N
Xiong, XX
Guenther, B
AF Lei, Ning
Xiong, Xiaoxiong
Guenther, Bruce
TI Modeling the Detector Radiometric Gains of the Suomi NPP VIIRS
Reflective Solar Bands
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; degradation modeling; optical throughput; relative spectral
response (RSR); Suomi National Polar-orbiting Partnership (SNPP) Visible
Infrared Imaging Radiometer Suite (VIIRS)
AB Right after the opening of the nadir door of the Visible Infrared Imaging Radiometer Suite (VIIRS) aboard the Suomi National Polar-orbiting Partnership satellite, the detector gains of the near-infrared bands had decreased much faster than expected, indicating large degradation of the VIIRS optical system. To help determine the root cause and to access the potential outcome of the degradation, we developed a mathematical model based on a physical hypothesis that the observed degradation was due to the sensor Rotating Telescope Assembly (RTA) mirror surface contamination. To date, the detector gains have been consistent with a physical model of a thin contaminant layer of material on each of the four RTA reflective mirrors. The contaminated material, after exposure to solar radiation, reduces the mirror reflectance over the reflective solar band (RSB) wavelength region. We describe the mathematical model and apply the model to predict the RSB detector gains at the end of seven-year mission operation. The model also projects that the signal-to-noise ratios of the RSB will all be larger than the design requirements with a margin of at least 25% at the end of seven years of mission operation. In addition, the detector relative spectral response (RSR) is modulated by the wavelength-dependent optical throughput degradation. We compute the modulated RSR and its impacts on sensor radiometric calibration and the computed top-of-the-atmosphere spectral reflectance at the Sensor Data Record level.
C1 [Lei, Ning] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD USA.
[Guenther, Bruce] Stellar Solut Inc, Chantilly, VA 20151 USA.
RP Lei, N (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM ning.lei@sigmaspace.com
NR 18
TC 15
Z9 15
U1 2
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2015
VL 53
IS 3
BP 1565
EP 1573
DI 10.1109/TGRS.2014.2345481
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 AR9MZ
UT WOS:000343900600037
ER
PT J
AU Smith, GL
Wong, TM
Bush, KA
AF Smith, G. Louis
Wong, Takmeng
Bush, Kathryn A.
TI Time-Sampling Errors of Earth Radiation From Satellites: Theory for
Outgoing Longwave Radiation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Earth Radiation Budget Experiment (ERBE); error analysis; time-sampling
error
ID BUDGET EXPERIMENT; DIURNAL VARIABILITY; SPATIAL VARIABILITY; ALGORITHMS;
RESOLUTION; SPECTRA; CLOUD; ERBE
AB The measurements of radiation budget by satellites in low Earth orbit provide limited sampling of the diurnal cycle. Thus, maps of monthly mean radiation fluxes contain errors due to this limitation. The Earth Radiation Budget Experiment reduced these errors in the data products by using a half-sine fit to account for regional diurnal cycles. An algorithm is presented to compute errors that are created when one computes the average value of outgoing longwave radiative flux (OLR) for a month based on the half-sine fit. Details of the temporal sampling are described by a sampling matrix that gives the number of OLR measurements in each local hour and each day of the month. The error analysis must take into account the correlation in time between irregularly spaced data due to synoptic variations, the weighting of measurements to accommodate the half-sine fit and deviations of the regional diurnal cycle from the half-sine. Using these ingredients, a closed-form expression is presented for the standard deviation of the temporal-sampling errors of the monthly mean OLR as computed from satellite measurements. The method is demonstrated for a well-sampled case and a poorly sampled case. This approach can be used to evaluate data products for existing measurements and for future mission design, or evaluating measurements of other atmospheric parameters.
C1 [Smith, G. Louis; Bush, Kathryn A.] Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Wong, Takmeng] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
RP Smith, GL (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
EM george.l.smith@nasa.gov
FU Science Systems Applications, Inc.; Clouds and Earth's Radiant Energy
System (CERES) Program in the Science Directorate of the Langley
Research Centre; Earth Sciences Enterprise of NASA as a part of the
Earth Observation System
FX This work was supported by the Science Systems Applications, Inc., by
the Clouds and Earth's Radiant Energy System (CERES) Program in the
Science Directorate of the Langley Research Centre, and by the Earth
Sciences Enterprise of NASA as a part of the Earth Observation System.
NR 23
TC 1
Z9 1
U1 0
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 MAR
PY 2015
VL 53
IS 3
BP 1656
EP 1665
DI 10.1109/TGRS.2014.2338793
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AR9MZ
UT WOS:000343900600045
ER
PT J
AU Park, J
Stolle, C
Xiong, C
Luhr, H
Pfaff, RF
Buchert, S
Martinis, CR
AF Park, Jaeheung
Stolle, Claudia
Xiong, Chao
Luehr, Hermann
Pfaff, Robert F.
Buchert, Stephan
Martinis, Carlos R.
TI A dayside plasma depletion observed at midlatitudes during quiet
geomagnetic conditions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LOW LATITUDE IONOSPHERE; F-LIKE IRREGULARITIES; SPREAD-F; EQUATORIAL
IONOSPHERE; TOPSIDE IONOSPHERE; SATELLITE; BUBBLES; DAYTIME; JICAMARCA;
ALTITUDE
AB In this study we investigate a dayside, midlatitude plasma depletion (DMLPD) encountered on 22 May 2014 by the Swarm and GRACE satellites, as well as ground-based instruments. The DMLPD was observed near Puerto Rico by Swarm near 10 LT under quiet geomagnetic conditions at altitudes of 475-520 km and magnetic latitudes of similar to 25 degrees-30 degrees. The DMLPD was also revealed in total electron content observations by the Saint Croix station and by the GRACE satellites (430 km) near 16 LT and near the same geographic location. The unique Swarm constellation enables the horizontal tilt of the DMLPD to be measured (35 degrees clockwise from the geomagnetic east-west direction). Ground-based airglow images at Arecibo showed no evidence for plasma density depletions during the night prior to this dayside event. The C/NOFS equatorial satellite showed evidence for very modest plasma density depletions that had rotated into the morningside from nightside. However, the equatorial depletions do not appear related to the DMLPD, for which the magnetic apex height is about 2500 km. The origins of the DMLPD are unknown, but may be related to gravity waves.
C1 [Park, Jaeheung; Stolle, Claudia; Xiong, Chao; Luehr, Hermann] German Res Ctr Geosci, GFZ, Helmholtz Ctr Potsdam, Potsdam, Germany.
[Stolle, Claudia] Univ Potsdam, Fac Sci, Potsdam, Germany.
[Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Buchert, Stephan] Swedish Inst Space Phys, Uppsala, Sweden.
[Martinis, Carlos R.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
RP Park, J (reprint author), Korea Astron & Space Sci Inst, Taejon, South Korea.
EM park@gfz-potsdam.de
FU ESA/ESTEC [4000102140/10/NL/JA]; USAF Space Test Program; KASI; Air
Force Research Laboratory [FA2386-14-1-4004]
FX The authors gratefully acknowledge OMNI data obtained from the GSFC/SPDF
OMNI Web interface at http://omniweb.gsfc.nasa.gov. The Swarm data have
been provided under the ESA/ESTEC contract 4000102140/10/NL/JA. We
acknowledge the use of GRACE and C/NOFS data. The GRACE data have been
provided after requests to GFZ. The Communication/Navigation Outage
Forecast System (C/NOFS) mission, conceived and developed by the Air
Force Research Laboratory, is sponsored and executed by the USAF Space
Test Program. The Arecibo airglow images are available at
http://www.buimaging.com. The ground-based GNSS observation data have
been downloaded from the IGS SOPAC website. J. Park was partially
supported by the "Planetary system research for space exploration"
project, the basic research funding from KASI, and the Air Force
Research Laboratory, under agreement FA2386-14-1-4004.
NR 23
TC 4
Z9 4
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 28
PY 2015
VL 42
IS 4
BP 967
EP 974
DI 10.1002/2014GL062655
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900001
ER
PT J
AU Olsen, N
Hulot, G
Lesur, V
Finlay, CC
Beggan, C
Chulliat, A
Sabaka, TJ
Floberghagen, R
Friis-Christensen, E
Haagmans, R
Kotsiaros, S
Luhr, H
Toffner-Clausen, L
Vigneron, P
AF Olsen, Nils
Hulot, Gauthier
Lesur, Vincent
Finlay, Christopher C.
Beggan, Ciaran
Chulliat, Arnaud
Sabaka, Terence J.
Floberghagen, Rune
Friis-Christensen, Eigil
Haagmans, Roger
Kotsiaros, Stavros
Luehr, Hermann
Toffner-Clausen, Lars
Vigneron, Pierre
TI The Swarm Initial Field Model for the 2014 geomagnetic field
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EARTHS MAGNETIC-FIELD; CONSTELLATION; SCARF; CORE
AB Data from the first year of ESA's Swarm constellation mission are used to derive the Swarm Initial Field Model (SIFM), a new model of the Earth's magnetic field and its time variation. In addition to the conventional magnetic field observations provided by each of the three Swarm satellites, explicit advantage is taken of the constellation aspect by including east-west magnetic intensity gradient information from the lower satellite pair. Along-track differences in magnetic intensity provide further information concerning the north-south gradient. The SIFM static field shows excellent agreement (up to at least degree 60) with recent field models derived from CHAMP data, providing an initial validation of the quality of the Swarm magnetic measurements. Use of gradient data improves the determination of both the static field and its secular variation, with the mean misfit for east-west intensity differences between the lower satellite pair being only 0.12 nT.
C1 [Olsen, Nils; Finlay, Christopher C.; Friis-Christensen, Eigil; Kotsiaros, Stavros; Toffner-Clausen, Lars] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Hulot, Gauthier; Vigneron, Pierre] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, Equipe Geomagnetisme,UMR CNRS INSU 7154, Paris, France.
[Lesur, Vincent; Luehr, Hermann] Deutsch GeoForschungsZentrum, Helmholtz Zentrum Potsdam, Potsdam, Germany.
[Beggan, Ciaran] British Geol Survey, Edinburgh, Midlothian, Scotland.
[Chulliat, Arnaud] NOAA, Natl Geophys Data Ctr, Boulder, CO USA.
[Sabaka, Terence J.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
[Floberghagen, Rune] ESRIN, Directorate Earth Observat Programmes, Frascati, Italy.
[Haagmans, Roger] ESA ESTEC, Noordwijk, Netherlands.
RP Olsen, N (reprint author), Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
EM nio@space.dtu.dk
RI Hulot, Gauthier/A-5627-2011; Chulliat, Arnaud/A-5747-2011; Olsen,
Nils/H-1822-2011; Finlay, Christopher/B-5062-2014; Lesur,
Vincent/H-1031-2012;
OI Chulliat, Arnaud/0000-0001-7414-9631; Olsen, Nils/0000-0003-1132-6113;
Finlay, Christopher/0000-0002-4592-2290; Lesur,
Vincent/0000-0003-2568-320X; Toffner-Clausen, Lars/0000-0003-4314-3776
FU European Space Agency (ESA) through ESRIN [4000109587/13/I-NB]
FX We would like to thank the European Space Agency (ESA) for providing
prompt access to the Swarm L1b data, and for support through ESRIN
contract 4000109587/13/I-NB "SWARM ESL". Swarm Level 1b data are
available from ESA at http://earth.esa.int/swarm.
NR 23
TC 14
Z9 15
U1 3
U2 20
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 FEB 28
PY 2015
VL 42
IS 4
BP 1092
EP 1098
DI 10.1002/2014GL062659
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900017
ER
PT J
AU Llovel, W
Lee, T
AF Llovel, William
Lee, Tong
TI Importance and origin of halosteric contribution to sea level change in
the southeast Indian Ocean during 2005-2013
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INDONESIAN THROUGHFLOW; ROSSBY WAVES; VARIABILITY; RISE; CIRCULATION;
IMPACT; BUDGET; FLOW
AB Steric sea level change has been identified as one of the major contributors to the regional variability of sea level trends observed by satellite altimetry for the past two decades. This contribution varies in space and time. The temperature (thermosteric) contribution to sea level has generally been found to be more important than the salinity (halosteric) effect. Based on sea level measurements from satellite altimetry and temperature and salinity data from Argo floats during 2005-2013, we found that the southeast Indian Ocean experiences a large halosteric contribution to sea level change. The conspicuously large halosteric contribution is associated with a freshening in the upper 300 m. Neither local atmospheric forcing such as Ekman pumping and E - P nor halosteric signal transmitted from the western tropical Pacific can explain this freshening. An enhanced precipitation in the Maritime Continent region and the observed strengthening of the Indonesian throughflow are the likely causes.
C1 [Llovel, William; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Llovel, William] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Llovel, W (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM william.llovel@cerfacs.fr
RI LLOVEL, William/G-6930-2016
FU University of California at Los Angeles, Joint Institute for Regional
Earth System Science and Engineering (JIFRESSE), Los Angeles, CA, USA;
NOAA Climate Observations and Monitoring (COM) program
FX William Llovel was supported by University of California at Los Angeles,
Joint Institute for Regional Earth System Science and Engineering
(JIFRESSE), Los Angeles, CA 90024, USA. We sincerely thank Arnold Gordon
for his insight in estimating the advective time scales associated with
the ITF based on the pathway of the ITF and related velocity
measurements. The altimeter products were produced by Ssalto/Duacs and
distributed by AVISO, with support from CNES
(http://www.aviso.altimetry.fr/duacs/). The Argo data were collected and
made freely available by the International Argo Program and the national
programs that contribute to it (http://www.argo.ucsd.edu and
http://argo.jcommops.org). The Argo Program is part of the Global Ocean
Observing System. NCEP_Reanalysis 2 and GPCP data provided by the
NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at
http://www.esrl.noaa.gov/psd/. The global ocean evaporation products
were provided by the WHOI OAFlux project (http://oaflux.whoi.edu) funded
by the NOAA Climate Observations and Monitoring (COM) program. We also
thank Paul Durack and an anonymous reviewer for their time and helpful
suggestions. The relevant research conducted by Tong Lee was carried out
at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with the National Aeronautics and Space Administration.
NR 45
TC 9
Z9 9
U1 0
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 FEB 28
PY 2015
VL 42
IS 4
BP 1148
EP 1157
DI 10.1002/2014GL062611
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900024
ER
PT J
AU Smith, DM
Allan, RP
Coward, AC
Eade, R
Hyder, P
Liu, CL
Loeb, NG
Palmer, MD
Roberts, CD
Scaife, AA
AF Smith, Doug M.
Allan, Richard P.
Coward, Andrew C.
Eade, Rosie
Hyder, Patrick
Liu, Chunlei
Loeb, Norman G.
Palmer, Matthew D.
Roberts, Chris D.
Scaife, Adam A.
TI Earth's energy imbalance since 1960 in observations and CMIP5 models
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OCEAN HEAT-CONTENT; GLOBAL UPPER-OCEAN; SEA-LEVEL RISE; CLIMATE-CHANGE;
MASS-BALANCE; TEMPERATURE; SYSTEM; HIATUS; VARIABILITY; REANALYSIS
AB Observational analyses of running 5 year ocean heat content trends (H-t) and net downward top of atmosphere radiation (N) are significantly correlated (r similar to 0.6) from 1960 to 1999, but a spike in Ht in the early 2000s is likely spurious since it is inconsistent with estimates of N from both satellite observations and climate model simulations. Variations in N between 1960 and 2000 were dominated by volcanic eruptions and are well simulated by the ensemble mean of coupled models from the Fifth Coupled Model Intercomparison Project (CMIP5). We find an observation-based reduction in N of -0.31 +/- 0.21 W m(-2) between 1999 and 2005 that potentially contributed to the recent warming slowdown, but the relative roles of external forcing and internal variability remain unclear. While present-day anomalies of N in the CMIP5 ensemble mean and observations agree, this may be due to a cancelation of errors in outgoing longwave and absorbed solar radiation.
C1 [Smith, Doug M.; Eade, Rosie; Hyder, Patrick; Palmer, Matthew D.; Roberts, Chris D.; Scaife, Adam A.] Met Off Hadley Ctr, Exeter, Devon, England.
[Allan, Richard P.; Liu, Chunlei] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Coward, Andrew C.] Natl Oceanog Ctr, Southampton, Hants, England.
[Loeb, Norman G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Smith, DM (reprint author), Met Off Hadley Ctr, Exeter, Devon, England.
EM doug.smith@metoffice.gov.uk
RI Allan, Richard/B-5782-2008
OI Allan, Richard/0000-0003-0264-9447
FU joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101];
FP7 SPECS project; Natural Environment Research Council (NERC) DEEP-C
grant [NE/K005480/1]
FX This work was supported by the joint DECC/Defra Met Office Hadley Centre
Climate Programme (GA01101), the EU FP7 SPECS project, and the Natural
Environment Research Council (NERC) DEEP-C grant NE/K005480/1. Thanks to
Jeff Knight for supplying the C20C data. Thanks to Magdalena Balmaseda
for supplying ORA-S4 data and for comments on the manuscript. We
acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
outputs. For CMIP, the U.S. Department of Energy's PCMDI provided
coordinating support and led development of software infrastructure in
partnership with the Global Organization for Earth System Science
Portals. The authors thank two anonymous referees for their thoughtful
comments.
NR 58
TC 18
Z9 18
U1 1
U2 28
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 FEB 28
PY 2015
VL 42
IS 4
BP 1205
EP 1213
DI 10.1002/2014GL062669
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900031
ER
PT J
AU Lubin, D
Kahn, BH
Lazzara, MA
Rowe, P
Walden, V
AF Lubin, Dan
Kahn, Brian H.
Lazzara, Matthew A.
Rowe, Penny
Walden, Von P.
TI Variability in AIRS-retrieved cloud amount and thermodynamic phase over
west versus east Antarctica influenced by the SAM
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID REFRACTIVE-INDEXES; ANNULAR MODE; SURFACE; CLIMATE; TEMPERATURE; SYSTEM;
WATER
AB In a sample of summertime cloud retrievals from the NASA Atmospheric Infrared Sounder (AIRS), a positive Southern Annular Mode (SAM) index polarity is associated with greater cloud frequency and larger effective cloud fraction over West Antarctica compared with a negative SAM index polarity. The opposite result appears over the high East Antarctic Plateau. Comparing AIRS-retrieved cloud fraction with Antarctic Automatic Weather Station 2 m air temperature data, a positive and significant correlation is found over most of West Antarctica, signifying a longwave heating effect of clouds. Over East Antarctica correlations between Sun elevation and 2 m air temperature are strongest, consistent with lower cloud amount.
C1 [Lubin, Dan] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Kahn, Brian H.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Lazzara, Matthew A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Lazzara, Matthew A.] Madison Area Tech Coll, Dept Phys Sci, Madison, WI USA.
[Rowe, Penny] Univ Idaho, Dept Geog, Moscow, ID 83843 USA.
[Rowe, Penny] Univ Santiago Chile, Dept Fis, Santiago, Chile.
[Walden, Von P.] Washington State Univ, Dept Civil & Environm Engn, Lab Atmospher Res, Pullman, WA 99164 USA.
RP Lubin, D (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM dlubin@ucsd.edu
FU NASA Radiation Sciences Program [NNX08AF79G]; NSF [ARC-1108451];
USACH-DICYT Postdoc; AIRS project at JPL; U.S. National Science
Foundation [ANT-0944018, ANT-1245663]
FX The AIRS version 6 data sets were processed and obtained from the
Goddard Earth Services Data and Information Services Center
(http://daac.gsfc.nasa.gov) and the AIRS Project Science and Computing
Facility at JPL. ERA-Interim data were obtained from the University
Corporation for Atmospheric Research (UCAR) CISL Research Data Archive
(http://rda.ucar.edu). D. Lubin, P. Rowe, and V.P. Walden were supported
by the NASA Radiation Sciences Program under grant NNX08AF79G. P. Rowe
also received support from NSF award ARC-1108451 and from USACH-DICYT
Postdoc. B. H. Kahn was supported by the AIRS project at JPL. 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 Linda Keller of the
University of Wisconsin for timely processing of the Antarctic Automatic
Weather Station (AWS) data. The AWS program appreciates the support of
the U.S. National Science Foundation under ANT-0944018 and ANT-1245663.
NR 27
TC 2
Z9 2
U1 3
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 FEB 28
PY 2015
VL 42
IS 4
BP 1259
EP 1267
DI 10.1002/2014GL062285
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900037
ER
PT J
AU Bloom, AA
Worden, J
Jiang, Z
Worden, H
Kurosu, T
Frankenberg, C
Schimel, D
AF Bloom, A. Anthony
Worden, John
Jiang, Zhe
Worden, Helen
Kurosu, Thomas
Frankenberg, Christian
Schimel, David
TI Remote-sensing constraints on South America fire traits by Bayesian
fusion of atmospheric and surface data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EMISSION FACTORS; BIOMASS; DROUGHT; AMAZON; FOREST; SAVANNA; CO
AB Satellite observations reveal substantial burning during the 2007 and 2010 tropical South America fire season, with both years exhibiting similar total burned area. However, 2010 CO fire emissions, based on satellite CO concentration measurements, were substantially lower (-28%), despite the once-in-a-century drought in 2010. We use Bayesian inference with satellite measurements of CH4 and CO concentrations and burned area to quantify shifts in combustion characteristics in 2010 relative to 2007. We find an 88% probability in reduced combusted biomass density associated with the 2010 fires and an 82% probability of lower fire carbon losses in 2010 relative to 2007. Higher combustion efficiency was a smaller contributing factor to the reduced 2010 CO emissions. The reduction in combusted biomass density is consistent with a reduction (4-6%) in Global Ozone Monitoring Experiment 2 solar-induced fluorescence ( a proxy for gross primary production) during the preceding months and a potential reduction in biomass (<= 8.3%) due to repeat fires.
C1 [Bloom, A. Anthony; Worden, John; Jiang, Zhe; Kurosu, Thomas; Frankenberg, Christian; Schimel, David] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Worden, Helen] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
RP Bloom, AA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM abloom@jpl.nasa.gov
RI Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
FU National Aeronautics and Space Administration (NASA) Earth Observing
System(EOS) Program; NASA ROSES CSS [13-CARBON13_2-0071]
FX Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. TES CH4 and CO data
products are available at tes.jpl.nasa.gov. The MODIS burned area
product was obtained from modis-fire.umd.edu. The NCAR MOPITT project is
supported by the National Aeronautics and Space Administration (NASA)
Earth Observing System(EOS) Program. We are grateful for feedback from
F. Landerer and J. Joiner on our use of GRACE and GOME-2 data. This
research was funded by NASA ROSES CSS proposal 13-CARBON13_2-0071.
NR 31
TC 9
Z9 9
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 28
PY 2015
VL 42
IS 4
BP 1268
EP 1274
DI 10.1002/2014GL062584
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CE5DY
UT WOS:000351851900038
ER
PT J
AU Xia, YL
Peter-Lidard, CD
Huang, MY
Wei, HL
Ek, M
AF Xia, Youlong
Peter-Lidard, Christa D.
Huang, Maoyi
Wei, Helin
Ek, Mike
TI Improved NLDAS-2 Noah-simulated hydrometeorological products with an
interim run
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE NLDAS-2; Noah land surface model; hydrometeorological products; snow
hydrology
ID DATA ASSIMILATION SYSTEM; MESOSCALE ETA-MODEL; LAND-SURFACE; OKLAHOMA
MESONET; EVAPOTRANSPIRATION; EVAPORATION; MOISTURE; GCIP
AB In North American Land Data Assimilation System Phase 2 (NLDAS-2) Noah simulation, the NLDAS team introduced an intermediate 'fix' to constrain the surface exchange coefficient when the atmospheric boundary layer is stable. In the current NLDAS-2 Noah version, this fix is used for all stable cases including snow-free grid cells. In this study, we simply apply this fix to the grid cells in which both stable atmospheric boundary layer and snow exist simultaneously, excluding the snow-free grid cells as we recognize that the fix in NLDAS-2 is too strong. We conduct a 31-year (1979-2009) NLDAS-2 Noah interim (Noah-I) run and use observed streamflow, evapotranspiration, land surface temperature, soil temperature, and ground heat flux to evaluate the results, including comparisons with the original NLDAS-2 Noah run. The results show that Noah-I has the same performance as NLDAS-2 Noah for snow water equivalent; however, Noah-I significantly improved the simulation of other hydrometeorological products as noted earlier when compared with NLDAS-2 Noah and the observations. This simple modification is being included in the next Noah version used in NLDAS. The hydrometeorological products from the improved NLDAS-2 Noah-I are being staged on the National Centers for Environmental Prediction public server. Copyright (C) 2014 John Wiley & Sons, Ltd.
C1 [Xia, Youlong; Wei, Helin; Ek, Mike] NOAA, EMC, NCEP, College Pk, MD 20740 USA.
[Xia, Youlong; Wei, Helin] NOAA, IMSG, EMC, NCEP, College Pk, MD 20740 USA.
[Peter-Lidard, Christa D.] NASA, Hydrol Sci Lab, Goddard Fight Space Ctr, Green Belt, MD USA.
[Huang, Maoyi] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Xia, YL (reprint author), NOAA, IMSG, EMC, NCEP, College Pk, MD 20740 USA.
EM youlong.xia@noaa.gov
RI Huang, Maoyi/I-8599-2012
OI Huang, Maoyi/0000-0001-9154-9485
FU NOAA Climate Program Office (CPO) Modeling, Analysis, Predictions and
Projections (MAPP) programme; Department of Energy (DOE)'s Atmospheric
System Research (ASR) programme
FX Y. X. and C. P. L. were supported by NOAA Climate Program Office (CPO)
Modeling, Analysis, Predictions and Projections (MAPP) programme. M. H.
is supported by Department of Energy (DOE)'s Atmospheric System Research
(ASR) programme. In addition, the authors thank two anonymous reviewers
whose comments greatly improved the quality of this manuscript.
NR 35
TC 8
Z9 8
U1 0
U2 5
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 FEB 28
PY 2015
VL 29
IS 5
BP 780
EP 792
DI 10.1002/hyp.10190
PG 13
WC Water Resources
SC Water Resources
GA CC7LF
UT WOS:000350548300010
ER
PT J
AU Zhang, ZQ
Xue, YK
MacDonald, G
Cox, PM
Collatz, GJ
AF Zhang, Zhengqiu
Xue, Yongkang
MacDonald, Glen
Cox, Peter M.
Collatz, G. James
TI Investigation of North American vegetation variability under recent
climate: A study using the SSiB4/TRIFFID biophysical/dynamic vegetation
model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LEAF-AREA INDEX; ATMOSPHERE-BIOSPHERE MODEL; TREE-GRASS INTERACTIONS;
LAND-SURFACE MODELS; UNITED-STATES; COMMUNITY LAND; GLOBAL CLIMATE;
TEMPERATURE; FEEDBACKS; IMPACT
AB Recent studies have shown that current dynamic vegetation models have serious weaknesses in reproducing the observed vegetation dynamics and contribute to bias in climate simulations. This study intends to identify the major factors that underlie the connections between vegetation dynamics and climate variability and investigates vegetation spatial distribution and temporal variability at seasonal to decadal scales over North America (NA) to assess a 2-D biophysical model/dynamic vegetation model's (Simplified Simple Biosphere Model version 4, coupled with the Top-down Representation of Interactive Foliage and Flora Including Dynamics Model (SSiB4/TRIFFID)) ability to simulate these characteristics for the past 60 years (1948 through 2008). Satellite data are employed as constraints for the study and to compare the relationships between vegetation and climate from the observational and the simulation data sets. Trends in NA vegetation over this period are examined. The optimum temperature for photosynthesis, leaf drop threshold temperatures, and competition coefficients in the Lotka-Volterra equation, which describes the population dynamics of species competing for some common resource, have been identified as having major impacts on vegetation spatial distribution and obtaining proper initial vegetation conditions in SSiB4/TRIFFID. The finding that vegetation competition coefficients significantly affect vegetation distribution suggests the importance of including biotic effects in dynamical vegetation modeling. The improved SSiB4/TRIFFID can reproduce the main features of the NA distributions of dominant vegetation types, the vegetation fraction, and leaf area index (LAI), including its seasonal, interannual, and decadal variabilities. The simulated NA LAI also shows a general increasing trend after the 1970s in responding to warming. Both simulation and satellite observations reveal that LAI increased substantially in the southeastern U. S. starting from the 1980s. The effects of the severe drought during 1987-1992 and the last decade in the southwestern U. S. on vegetation are also evident from decreases in the simulated and satellite-derived LAIs. Both simulated and satellite-derived LAIs have the strongest correlations with air temperature at northern middle to high latitudes in spring reflecting the effect of these climatic variables on photosynthesis and phenological processes. Meanwhile, in southwestern dry lands, negative correlations appear due to the heat and moisture stress there during the summer. Furthermore, there are also positive correlations between soil wetness and LAI, which increases from spring to summer. The present study shows both the current improvements and remaining weaknesses in dynamical vegetation models. It also highlights large continental-scale variations that have occurred in NA vegetation over the past six decades and their potential relations to climate. With more observational data availability, more studies with different models and focusing on different regions will be possible and are necessary to achieve comprehensive understanding of the vegetation dynamics and climate interactions.
C1 [Zhang, Zhengqiu; Xue, Yongkang; MacDonald, Glen] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
[Zhang, Zhengqiu] Chinese Acad Meteorol Sci, Beijing, Peoples R China.
[Zhang, Zhengqiu] China Meteorol Adm, Inst Atmospher Environm, Shenyang, Peoples R China.
[Xue, Yongkang] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90024 USA.
[Cox, Peter M.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England.
[Collatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Xue, YK (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
EM yxue@geog.ucla.edu
RI collatz, george/D-5381-2012; Cox, Peter/B-3299-2012
FU NOAA [NA07OAR4310226]; U.S., NSF [AGS-1115506, AGS-1419526]; NASA
[NNX10AO97G]; China CMA [GYHY201406019]; Department of the Interior
Southwest Climate Science Center Contribution
FX This research was supported by NOAA grant NA07OAR4310226 U.S., NSF
grants AGS-1115506 and AGS-1419526, NASA grant NNX10AO97G, China CMA
grant GYHY201406019 and a Department of the Interior Southwest Climate
Science Center Contribution. The authors thank Sam Shen of SDSU for his
help in statistical analysis. We also appreciate two anonymous
reviewers' detailed and very constructive comments/suggestions. The data
for this paper are available at
http://www.sscnet.ucla.edu/geog/wamme/NA_ClimVeg/NA_ClimVeg1948_0
8.tar.gz.
NR 88
TC 4
Z9 4
U1 2
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 27
PY 2015
VL 120
IS 4
BP 1300
EP 1321
DI 10.1002/2014JD021963
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD6EN
UT WOS:000351182400005
ER
PT J
AU Vernier, JP
Fairlie, TD
Natarajan, M
Wienhold, FG
Bian, J
Martinsson, BG
Crumeyrolle, S
Thomason, LW
Bedka, KM
AF Vernier, J. -P.
Fairlie, T. D.
Natarajan, M.
Wienhold, F. G.
Bian, J.
Martinsson, B. G.
Crumeyrolle, S.
Thomason, L. W.
Bedka, K. M.
TI Increase in upper tropospheric and lower stratospheric aerosol levels
and its potential connection with Asian pollution
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SUMMER MONSOON; CLOUDS; TRANSPORT; OUTFLOW; BACKSCATTER; SIMULATION;
LAYER
AB Satellite observations have shown that the Asian Summer Monsoon strongly influences the upper troposphere and lower stratosphere (UTLS) aerosol morphology through its role in the formation of the Asian Tropopause Aerosol Layer (ATAL). Stratospheric Aerosol and Gas Experiment II solar occultation and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) lidar observations show that summertime UTLS Aerosol Optical Depth (AOD) between 13 and 18 km over Asia has increased by three times since the late 1990s. Here we present the first in situ balloon measurements of aerosol backscatter in the UTLS from Western China, which confirm high aerosol levels observed by CALIPSO since 2006. Aircraft in situ measurements suggest that aerosols at lower altitudes of the ATAL are largely composed of carbonaceous and sulfate materials (carbon/sulfur elemental ratio ranging from 2 to 10). Back trajectory analysis from Cloud-Aerosol Lidar with Orthogonal Polarization observations indicates that deep convection over the Indian subcontinent supplies the ATAL through the transport of pollution into the UTLS. Time series of deep convection occurrence, carbon monoxide, aerosol, temperature, and relative humidity suggest that secondary aerosol formation and growth in a cold, moist convective environment could play an important role in the formation of ATAL. Finally, radiative calculations show that the ATAL layer has exerted a short-term regional forcing at the top of the atmosphere of -0.1 W/m(2) in the past 18 years.
C1 [Vernier, J. -P.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Vernier, J. -P.; Fairlie, T. D.; Natarajan, M.; Thomason, L. W.; Bedka, K. M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Wienhold, F. G.] Swiss Fed Inst Technol, Zurich, Switzerland.
[Bian, J.] Chinese Acad Sci, Inst Atmospher Phys, LAGEO, Beijing, Peoples R China.
[Martinsson, B. G.] Lund Univ, Dept Phys, S-22362 Lund, Sweden.
[Crumeyrolle, S.] Univ Lille1, LOA, CNRS, Villeneuve Dascq, France.
RP Vernier, JP (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM jeanpaul.vernier@nasa.gov
OI Thomason, Larry/0000-0002-1902-0840
FU National Natural Science Foundation of China [91337214, 41175040]
FX All data and codes used to produce this study can be obtained by
contacting Jean-Paul Vernier (jeanpaul.vernier@nasa.gov) and will be
shared through a dropbox system (https://www.dropbox.com/home) under the
folder JGR-ATAL-2014
(https://www.dropbox.com/sh/k3vim6ocl3tipzb/AAC25oBOkjYE_3cxedZ
S7mTAa?dl=0). We thank Mian Chin for the discussion on the comparison
between CALIPSO and the GOCART model (not shown in this paper). We also
thank Robaidek from the University of Wisconsin and ISRO for making
available the KALPANA satellite data via the McIDAS-V system
(http://www.ssec.wisc.edu/data/). The following satellite data used in
this study are publically available at CALIPSO,
https://eosweb.larc.nasa.gov/project/calipso/calipso_table; SAGE,
https://eosweb.larc.nasa.gov/project/sage2/sage2_table; MLS,
http://mirador.gsfc.nasa.gov/cgibin/mirador/homepageAlt.pl?keyword=MLS;
TRMM,
http://mirador.gsfc.nasa.gov/cgibin/mirador/homepageAlt.pl?keyword=TR
MM; and Cosmic GPS: http://www.cosmic.ucar.edu/data.html. The COBALD
balloon campaign in Lhasa was supported by National Natural Science
Foundation of China (grants 91337214 and 41175040).
NR 33
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Z9 14
U1 3
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 27
PY 2015
VL 120
IS 4
BP 1608
EP 1619
DI 10.1002/2014JD022372
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CD6EN
UT WOS:000351182400023
ER
PT J
AU Chamberlin, SJ
Creighton, JDE
Siemens, X
Demorest, P
Ellis, J
Price, LR
Romano, JD
AF Chamberlin, Sydney J.
Creighton, Jolien D. E.
Siemens, Xavier
Demorest, Paul
Ellis, Justin
Price, Larry R.
Romano, Joseph D.
TI Time-domain implementation of the optimal cross-correlation statistic
for stochastic gravitational-wave background searches in pulsar timing
data
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLE BINARIES; GALAXY FORMATION; ARRAY DATA; LIMITS; RADIATION;
MEMORY; COALESCENCE; SIGNALS; SYSTEMS; BURSTS
AB Supermassive black hole binaries, cosmic strings, relic gravitational waves from inflation, and first-order phase transitions in the early Universe are expected to contribute to a stochastic background of gravitational waves in the 10(-9)-10(-7) Hz frequency band. Pulsar timing arrays (PTAs) exploit the high-precision timing of radio pulsars to detect signals at such frequencies. Here we present a time-domain implementation of the optimal cross-correlation statistic for stochastic background searches in PTA data. Due to the irregular sampling typical of PTA data as well as the use of a timing model to predict the times of arrival of radio pulses, time-domain methods are better-suited for gravitational-wave data analysis of such data. We present a derivation of the optimal cross-correlation statistic starting from the likelihood function, a method to produce simulated stochastic background signals, and a rigorous derivation of the scaling laws for the signal-to-noise ratio of the cross-correlation statistic in the two relevant PTA regimes: the weak-signal limit where instrumental noise dominates over the gravitational-wave signal at all frequencies, and a second regime where the gravitational-wave signal dominates at the lowest frequencies.
C1 [Chamberlin, Sydney J.; Creighton, Jolien D. E.; Siemens, Xavier] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Demorest, Paul] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ellis, Justin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Price, Larry R.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Romano, Joseph D.] Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA.
[Romano, Joseph D.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
RP Chamberlin, SJ (reprint author), Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
EM sydc@gravity.phys.uwm.edu; jolien@gravity.phys.uwm.edu;
siemens@gravity.phys.uwm.edu; pdemores@nrao.edu;
Justin.A.Ellis@jpl.nasa.gov; larryp@caltech.edu; joe@phys.utb.edu
FU National Science Foundation (NSF) through CAREER Grant [0955929];
Partnerships for International Research and Education (PIRE) [0968126,
0970074]; Wisconsin Space Grant Consortium; National Aeronautics and
Space Administration (NASA) through Einstein Fellowship [PF4-150120];
NSF [HRD-0734800, HRD-1242090, PHY-1205585]
FX We thank Eanna Flanagan for pointing out a sign error in [31], which has
been corrected here. We also thank Chris Pankow and Madeline Wade for
many useful comments and suggestions. We extend our gratitude to the
members of the NANOGrav Data Analysis Working Group. The work of S. J.
C., X. S., and J. A. E. was partially funded by the National Science
Foundation (NSF) through CAREER Grant No. 0955929, Partnerships for
International Research and Education (PIRE) Grant No. 0968126, Grant No.
0970074, and the Wisconsin Space Grant Consortium. J. A. E. acknowledges
support by National Aeronautics and Space Administration (NASA) through
Einstein Fellowship Grant No. PF4-150120. J. D. R. would like to
acknowledge support from NSF Gants No. HRD-0734800, No. HRD-1242090, and
No. PHY-1205585.
NR 68
TC 7
Z9 7
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD FEB 27
PY 2015
VL 91
IS 4
AR 044048
DI 10.1103/PhysRevD.91.044048
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CC4KH
UT WOS:000350321800008
ER
PT J
AU Zhao, MH
Ming, B
Kim, JW
Gibbons, LJ
Gu, XH
Nguyen, T
Park, C
Lillehei, PT
Villarrubia, JS
Vladar, AE
Liddle, JA
AF Zhao, Minhua
Ming, Bin
Kim, Jae-Woo
Gibbons, Luke J.
Gu, Xiaohong
Nguyen, Tinh
Park, Cheol
Lillehei, Peter T.
Villarrubia, J. S.
Vladar, Andras E.
Liddle, J. Alexander
TI New insights into subsurface imaging of carbon nanotubes in polymer
composites via scanning electron microscopy
SO NANOTECHNOLOGY
LA English
DT Article
DE scanning electron microscopy; subsurface imaging; carbon nanotube
polymer composites
ID STATIC CAPACITANCE CONTRAST; INSULATORS; MECHANISM; NANOCOMPOSITES;
DISPERSION; FILMS; BEAM; TOOL; SEM
AB Despite many studies of subsurface imaging of carbon nanotube (CNT)-polymer composites via scanning electron microscopy (SEM), significant controversy exists concerning the imaging depth and contrast mechanisms. We studied CNT-polyimide composites and, by threedimensional reconstructions of captured stereo-pair images, determined that the maximum SEM imaging depth was typically hundreds of nanometers. The contrast mechanisms were investigated over a broad range of beam accelerating voltages from 0.3 to 30 kV, and ascribed to modulation by embedded CNTs of the effective secondary electron (SE) emission yield at the polymer surface. This modulation of the SE yield is due to non-uniform surface potential distribution resulting from current flows due to leakage and electron beam induced current. The importance of an external electric field on SEM subsurface imaging was also demonstrated. The insights gained from this study can be generally applied to SEM nondestructive subsurface imaging of conducting nanostructures embedded in dielectric matrices such as graphene-polymer composites, silicon-based single electron transistors, high resolution SEM overlay metrology or e-beam lithography, and have significant implications in nanotechnology.
C1 [Zhao, Minhua; Liddle, J. Alexander] NIST, Ctr Nanoscale Sci & Technol, Gaithersburg, MD 20899 USA.
[Ming, Bin; Villarrubia, J. S.; Vladar, Andras E.] NIST, Phys Measurement Lab, Gaithersburg, MD 20899 USA.
[Gu, Xiaohong; Nguyen, Tinh] NIST, Engn Lab, Gaithersburg, MD 20899 USA.
[Kim, Jae-Woo; Park, Cheol; Lillehei, Peter T.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA USA.
[Gibbons, Luke J.] Virginia Polytech Inst & State Univ, Dept Mat Sci & Engn, Blacksburg, VA 24061 USA.
[Zhao, Minhua] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
RP Zhao, MH (reprint author), NIST, Ctr Nanoscale Sci & Technol, Gaithersburg, MD 20899 USA.
EM minhua.zhao@nist.gov; james.liddle@nist.gov
RI Kim, Jae-Woo/A-8314-2008; Liddle, James/A-4867-2013
OI Liddle, James/0000-0002-2508-7910
FU National Science Foundation [CMMI-0928839]; University of Maryland; NIST
FX The work of Dr Minhua Zhao was supported by NIST-ARRA senior fellowship
award in measurement science and technology and Cooperative Research
Program in Nanoscience and Technology between the University of Maryland
and NIST. Luke Gibbons and Cheol Park acknowledge support by National
Science Foundation CMMI-0928839 in part.
NR 37
TC 4
Z9 4
U1 4
U2 43
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 27
PY 2015
VL 26
IS 8
AR 085703
DI 10.1088/0957-4484/26/8/085703
PG 12
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA CA9LH
UT WOS:000349244600020
PM 25649345
ER
PT J
AU Dodson, LG
Shen, LH
Savee, JD
Eddingsaas, NC
Welz, O
Taatjes, CA
Osborn, DL
Sander, SP
Okumura, M
AF Dodson, Leah G.
Shen, Linhan
Savee, John D.
Eddingsaas, Nathan C.
Welz, Oliver
Taatjes, Craig A.
Osborn, David L.
Sander, Stanley P.
Okumura, Mitchio
TI VUV Photoionization Cross Sections of HO2, H2O2, and H2CO
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID GASEOUS-HYDROGEN PEROXIDE; RESOLUTION PHOTOELECTRON-SPECTROSCOPY; FLIGHT
MASS-SPECTROMETRY; VACUUM-ULTRAVIOLET; LOW-PRESSURES; FREE-RADICALS;
RESOLVED PHOTOIONIZATION; COMBUSTION CHEMISTRY; CHEMICAL-DYNAMICS;
MOLECULAR-OXYGEN
C1 [Dodson, Leah G.; Shen, Linhan; Eddingsaas, Nathan C.; Okumura, Mitchio] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Sander, Stanley P.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Savee, John D.; Taatjes, Craig A.; Osborn, David L.] Sandia Natl Labs, Combust Res Facil, Livermore, CA 94551 USA.
RP Dodson, LG (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
EM lgdodson@caltech.edu; cataatj@sandia.gov; dlosbor@sandia.gov;
mo@caltech.edu
RI Okumura, Mitchio/I-3326-2013;
OI Okumura, Mitchio/0000-0001-6874-1137; Dodson, Leah/0000-0001-5960-056X
FU National Science Foundation [CHE-0957490, CHE-1413712]; National
Aeronautics and Space Administration's (NASA) Upper Atmospheric Research
Program [NNX12AI01G]; EPA STAR Fellowship; Sandia Campus Executive
Fellowship; Dreyfus Foundation Postdoctoral Fellowship in Environmental
Chemistry; NASA; U.S. Department of Energy, Office of Science, Office of
Basic Energy Sciences; National Nuclear Security Administration
[DE-AC04-94-AL85000]; DOE Office of Science User Facility at Lawrence
Berkeley National Laboratory [DE-AC02-05CH11231]
FX The Caltech effort was supported by the National Science Foundation
grants CHE-0957490 and CHE-1413712 and the National Aeronautics and
Space Administration's (NASA) Upper Atmospheric Research Program grant
NNX12AI01G. L.G.D. was supported by an EPA STAR Fellowship and a Sandia
Campus Executive Fellowship. N.C.E. was supported in part by a Dreyfus
Foundation Postdoctoral Fellowship in Environmental Chemistry. Part of
this research was carried out by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. The
participation of D.L.O, J.D.S, O.W., and C.A.T. and the development and
maintenance of the MPIMS apparatus are supported by the U.S. Department
of Energy, Office of Science, Office of Basic Energy Sciences. Sandia is
a multiprogram laboratory operated by Sandia Corporation, a Lockheed
Martin Company, for the National Nuclear Security Administration under
contract DE-AC04-94-AL85000. The research conducted used resources of
the Advanced Light Source, which is a DOE Office of Science User
Facility at Lawrence Berkeley National Laboratory under contract
DE-AC02-05CH11231.
NR 94
TC 10
Z9 10
U1 16
U2 75
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 FEB 26
PY 2015
VL 119
IS 8
BP 1279
EP 1291
DI 10.1021/jp508942a
PG 13
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CC4MZ
UT WOS:000350328800006
PM 25621533
ER
PT J
AU Farahmand, A
AghaKouchak, A
Teixeira, J
AF Farahmand, Alireza
AghaKouchak, Amir
Teixeira, Joao
TI A Vantage from Space Can Detect Earlier Drought Onset: An Approach Using
Relative Humidity
SO SCIENTIFIC REPORTS
LA English
DT Article
ID SOIL-MOISTURE; INDEX; PREDICTION; FRAMEWORK; INDICATORS; PRODUCTS;
MISSION; MODEL
AB Each year, droughts cause significant economic and agricultural losses across the world. The early warning and onset detection of drought is of particular importance for effective agriculture and water resource management. Previous studies show that the Standard Precipitation Index (SPI), a measure of precipitation deficit, detects drought onset earlier than other indicators. Here we show that satellite-based near surface air relative humidity data can further improve drought onset detection and early warning. This paper introduces the Standardized Relative Humidity Index (SRHI) based on the NASA Atmospheric Infrared Sounder (AIRS) observations. The results indicate that the SRHI typically detects the drought onset earlier than the SPI. While the AIRS mission was not originally designed for drought monitoring, we show that its relative humidity data offers a new and unique avenue for drought monitoring and early warning. We conclude that the early warning aspects of SRHI may have merit for integration into current drought monitoring systems.
C1 [Farahmand, Alireza; AghaKouchak, Amir] Univ Calif Irvine, Irvine, CA 92697 USA.
[Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP AghaKouchak, A (reprint author), Univ Calif Irvine, Irvine, CA 92697 USA.
EM amir.a@uci.edu
FU National Aeronautics and Space Administration (NASA) [NNX15AC27G]
FX This study is supported by the National Aeronautics and Space
Administration (NASA) Award No. NNX15AC27G.
NR 37
TC 6
Z9 6
U1 4
U2 17
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 FEB 25
PY 2015
VL 5
AR 8553
DI 10.1038/srep08553
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CB8QC
UT WOS:000349894700003
PM 25711500
ER
PT J
AU Sidoli, L
Paizis, A
Furst, F
Torrejon, JM
Kretschmar, P
Bozzo, E
Pottschmidt, K
AF Sidoli, L.
Paizis, A.
Fuerst, F.
Torrejon, J. M.
Kretschmar, P.
Bozzo, E.
Pottschmidt, K.
TI Probing large-scale wind structures in Vela X-1 using off-states with
INTEGRAL
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: neutron; X-rays: binaries; X-rays: individual: Vela X-1
ID X-RAY BINARIES; STELLAR WIND; CIRCUMSTELLAR MATTER; XMM-NEWTON; 3U
0900-40; SUPERGIANT; ACCRETION; MASS; VARIABILITY; TRANSIENTS
AB Vela X-1 is the prototype of the class of wind-fed accreting pulsars in high-mass X-ray binaries hosting a supergiant donor. We have analysed in a systematic way 10 years of INTEGRAL data of Vela X-1 (22-50 keV) and we found that when outside the X-ray eclipse, the source undergoes several luminosity drops where the hard X-rays luminosity goes below similar to 3 x 10(35) erg s(-1), becoming undetected by INTEGRAL. These drops in the X-ray flux are usually referred to as 'off-states' in the literature. We have investigated the distribution of these off-states along the Vela X-1 similar to 8.9 d orbit, finding that their orbital occurrence displays an asymmetric distribution, with a higher probability to observe an off-state near the pre-eclipse than during the post-eclipse. This asymmetry can be explained by scattering of hard X-rays in a region of ionized wind, able to reduce the source hard X-ray brightness preferentially near eclipse ingress. We associate this ionized large-scale wind structure with the photoionization wake produced by the interaction of the supergiant wind with the X-ray emission from the neutron star. We emphasize that this observational result could be obtained thanks to the accumulation of a decade of INTEGRAL data, with observations covering the whole orbit several times, allowing us to detect an asymmetric pattern in the orbital distribution of off-states in Vela X-1.
C1 [Sidoli, L.; Paizis, A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Fuerst, F.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Torrejon, J. M.] Univ Alicante, Inst Univ Fis Aplicada Ciencias & Tecnol, E-03690 Alicante, Spain.
[Kretschmar, P.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Villanueva De La Canada, Madrid, Spain.
[Bozzo, E.] Univ Geneva, INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Sidoli, L (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via E Bassini 15, I-20133 Milan, Italy.
EM sidoli@lambrate.inaf.it
RI Torrejon, Jose /K-6395-2014;
OI Torrejon, Jose /0000-0002-5967-5163; Paizis,
Adamantia/0000-0001-5067-0377; Sidoli, Lara/0000-0001-9705-2883;
Kretschmar, Peter/0000-0001-9840-2048
FU ESA; Italian Space Agency [2013-025.R.0.]; [AYA2010-15431]
FX Based on observations with INTEGRAL, an ESA project with instruments and
science data centre funded by ESA member states (especially the PI
countries: Denmark, France, Germany, Italy, Spain and Switzerland),
Czech Republic and Poland, and with the participation of Russia and the
USA. This work has made use of the INTEGRAL archive developed at
INAF-IASF Milano, http://www.iasf-milano.inaf.it/similar to
ada/GOLIA.html. We acknowledge support from ISSI through funding for the
International Team on 'Unified View of Stellar Winds in Massive X-ray
Binaries' (PI: S. Martinez-Nunez). LS thanks L. Oskinova for interesting
discussions. JMT acknowledges grant AYA2010-15431. LS and AP acknowledge
the Italian Space Agency financial support INTEGRAL ASI/INAF agreement
no. 2013-025.R.0.
NR 38
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2015
VL 447
IS 2
BP 1299
EP 1303
DI 10.1093/mnras/stu2533
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TM
UT WOS:000350272900022
ER
PT J
AU Ford, J
Van Waerbeke, L
Milkeraitis, M
Laigle, C
Hildebrandt, H
Erben, T
Heymans, C
Hoekstra, H
Kitching, T
Mellier, Y
Miller, L
Choi, A
Coupon, J
Fu, LP
Hudson, MJ
Kuijken, K
Robertson, N
Rowe, B
Schrabback, T
Velander, M
AF Ford, Jes
Van Waerbeke, Ludovic
Milkeraitis, Martha
Laigle, Clotilde
Hildebrandt, Hendrik
Erben, Thomas
Heymans, Catherine
Hoekstra, Henk
Kitching, Thomas
Mellier, Yannick
Miller, Lance
Choi, Ami
Coupon, Jean
Fu, Liping
Hudson, Michael J.
Kuijken, Konrad
Robertson, Naomi
Rowe, Barnaby
Schrabback, Tim
Velander, Malin
TI CFHTLenS: a weak lensing shear analysis of the 3D-Matched-Filter galaxy
clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; galaxies: clusters: general; galaxies:
photometry; dark matter
ID DARK-MATTER HALOES; DIGITAL SKY SURVEY; LARGE-SCALE BIAS; MASS-RICHNESS
RELATION; LYMAN-BREAK GALAXIES; PHOTOMETRIC REDSHIFTS; MAXBCG CLUSTERS;
MAGNIFICATION; PROFILES; ALGORITHM
AB We present the cluster mass-richness scaling relation calibrated by a weak lensing analysis of greater than or similar to 18 000 galaxy cluster candidates in the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). Detected using the 3D-Matched-Filter (MF) cluster-finder of Milkeraitis et al., these cluster candidates span a wide range of masses, from the small group scale up to similar to 1015M(circle dot), and redshifts 0.2 less than or similar to z less than or similar to 0.9. The total significance of the stacked shear measurement amounts to 54 sigma. We compare cluster masses determined using weak lensing shear and magnification, finding the measurements in individual richness bins to yield 1 sigma compatibility, but with magnification estimates biased low. This first direct mass comparison yields important insights for improving the systematics handling of future lensing magnification work. In addition, we confirm analyses that suggest cluster miscentring has an important effect on the observed 3D-MF halo profiles, and we quantify this by fitting for projected cluster centroid offsets, which are typically similar to 0.4 arcmin. We bin the cluster candidates as a function of redshift, finding similar cluster masses and richness across the full range up to z similar to 0.9. We measure the 3D-MF mass-richness scaling relation M-200 = M-0(N-200/20)(beta). We find a normalization M-0 similar to (2.7(-0.4)(+0.5)) x 10(13)M(circle dot), and a logarithmic slope of beta similar to 1.4 +/- 0.1, both of which are in 1 sigma agreement with results from the magnification analysis. We find no evidence for a redshift dependence of the normalization. The CFHTLenS 3D-MF cluster catalogue is now available at cfhtlens. org.
C1 [Ford, Jes; Van Waerbeke, Ludovic; Milkeraitis, Martha; Laigle, Clotilde; Hildebrandt, Hendrik] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Laigle, Clotilde; Mellier, Yannick] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Laigle, Clotilde] Ecole Polytech, F-91128 Palaiseau, France.
[Hildebrandt, Hendrik; Erben, Thomas; Schrabback, Tim] Argelander Inst Astron, D-53121 Bonn, Germany.
[Heymans, Catherine; Choi, Ami; Robertson, Naomi] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Hoekstra, Henk; Kuijken, Konrad; Schrabback, Tim; Velander, Malin] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Kitching, Thomas] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Mellier, Yannick] CEA, Irfu, SAp Saclay, Lab AIM, F-91191 Gif Sur Yvette, France.
[Miller, Lance; Velander, Malin] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Coupon, Jean] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Coupon, Jean] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Fu, Liping] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China.
[Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Hudson, Michael J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schrabback, Tim] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Ford, J (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
EM jesford@phas.ubc.ca
RI Hudson, Michael/H-3238-2012; Fu, Liping/B-3051-2012;
OI Hudson, Michael/0000-0002-1437-3786; Ford, Jes/0000-0002-2946-3776;
Rowe, Barnaby/0000-0002-7042-9174
FU UBC Four-Year-Fellowship; NSERC; CIfAR; DFG Emmy Noether grant [Hi
1495/2-1]; Deutsche Forschungsgemeinschaft [ER 327/3-1]; Transregional
Collaborative Research Centre TR 33 - 'The Dark Universe'; European
Research Council under the EC FP7 [240185]; NSFC [11103012, 11333001];
SMEC [12ZZ134]; STCSM [11290706600]; Pujiang Programme [12PJ1406700];
Shanghai Research grant [13JC1404400]
FX The authors would like to thank Jasper Wall for helpful discussions on
statistics, and the referee for providing helpful feedback and
suggestions that greatly improved this work. JF is supported by a UBC
Four-Year-Fellowship and NSERC. LVW is supported by NSERC and CIfAR. HHi
is supported by the DFG Emmy Noether grant Hi 1495/2-1. TE is supported
by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and
the Transregional Collaborative Research Centre TR 33 - 'The Dark
Universe'. CH, AC, and NR acknowledge funding from the European Research
Council under the EC FP7 grant number 240185. LF acknowledges support
from NSFC grants 11103012 & 11333001, Innovation Programme 12ZZ134 of
SMEC, STCSM grant 11290706600, Pujiang Programme 12PJ1406700 and
Shanghai Research grant 13JC1404400. MH is supported by NSERC.; This
work is partly based on observations obtained with MegaPrime/MegaCam, a
joint project of CFHT and CEA/IRFU, at the CFHT which is operated by the
National Research Council (NRC) of Canada, the Institut National des
Sciences de lUnivers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. This research used the
facilities of the Canadian Astronomy Data Centre operated by the NRC of
Canada with the support of the Canadian Space Agency. CFHTLenS data
processing was made possible thanks to significant computing support
from the NSERC Research Tools and Instruments grant programme.
NR 68
TC 10
Z9 10
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2015
VL 447
IS 2
BP 1304
EP 1318
DI 10.1093/mnras/stu2545
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TM
UT WOS:000350272900023
ER
PT J
AU Bauschlicher, CW
AF Bauschlicher, Charles W., Jr.
TI The infrared spectra of nonplanar polycyclic aromatic hydrocarbons with
five- or seven-membered rings
SO CHEMICAL PHYSICS
LA English
DT Article
DE Polycyclic aromatic hydrocarbon; Infrared spectra; DFT; Choice of
functional
ID NONCOVALENT INTERACTIONS; CORRELATION-ENERGY; SYMMETRY-BREAKING;
RAMAN-SPECTRA; EXCHANGE; C-60; C-70; PAHS; APPROXIMATION; MOLECULES
AB The infrared (IR) spectra are computed for compact polycyclic aromatic hydrocarbons (PAHs) with one five-or one seven-membered central ring, which have a bowl and saddle shape, respectively. In spite of the large geometric distortion compared with the planar PAHs with only six-membered rings, the IR spectra are surprisingly similar. Species with more than one five-membered ring show larger difference compared with typical PAHs. The C-C modes in the "ball'' shaped C-60 and C-70 are shifted somewhat from those in typical PAHs. The ions of C-60 and C-70 show the typical enhancement of these modes compared with neutrals. Cases where the B3LYP method fail are discussed as is the choice of functional. Published by Elsevier B.V.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov
NR 42
TC 4
Z9 4
U1 3
U2 19
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 FEB 20
PY 2015
VL 448
BP 43
EP 52
DI 10.1016/j.chemphys.2015.01.002
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CD0FV
UT WOS:000350747000006
ER
PT J
AU Refaat, TF
Singh, UN
Yu, JR
Petros, M
Ismail, S
Kavaya, MJ
Davis, KJ
AF Refaat, Tamer F.
Singh, Upendra N.
Yu, Jirong
Petros, Mulugeta
Ismail, Syed
Kavaya, Michael J.
Davis, Kenneth J.
TI Evaluation of an airborne triple-pulsed 2 mu m IPDA lidar for
simultaneous and independent atmospheric water vapor and carbon dioxide
measurements
SO APPLIED OPTICS
LA English
DT Article
ID DIFFERENTIAL ABSORPTION LIDAR; CO2 COLUMN MEASUREMENTS;
SENSITIVITY-ANALYSIS; LASER; FEEDBACK
AB Water vapor and carbon dioxide are the most dominant greenhouse gases directly contributing to the Earth's radiation budget and global warming. A performance evaluation of an airborne triple-pulsed integrated path differential absorption (IPDA) lidar system for simultaneous and independent monitoring of atmospheric water vapor and carbon dioxide column amounts is presented. This system leverages a state-of-the-art Ho:Tm:YLF triple-pulse laser transmitter operating at 2.05 mu m wavelength. The transmitter provides wavelength tuning and locking capabilities for each pulse. The IPDA lidar system leverages a low risk and technologically mature receiver system based on InGaAs pin detectors. Measurement methodology and wavelength setting are discussed. The IPDA lidar return signals and error budget are analyzed for airborne operation on-board the NASA B-200. Results indicate that the IPDA lidar system is capable of measuring water vapor and carbon dioxide differential optical depth with 0.5% and 0.2% accuracy, respectively, from an altitude of 8 km to the surface and with 10 s averaging. Provided availability of meteorological data, in terms of temperature, pressure, and relative humidity vertical profiles, the differential optical depth conversion into weighted-average column dry-air volume-mixing ratio is also presented. (C) 2015 Optical Society of America
C1 [Refaat, Tamer F.; Singh, Upendra N.; Yu, Jirong; Petros, Mulugeta; Ismail, Syed; Kavaya, Michael J.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Davis, Kenneth J.] Penn State Univ, University Pk, PA 16802 USA.
RP Refaat, TF (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM tamer.f.refaat@nasa.gov
FU NASA Earth Science Technology Office
FX This work is supported by NASA Earth Science Technology Office under the
Instrument Incubator Program (IIP-2013: ESTO Program Director: George
Komar and IIP Program Manager: Parminder Ghuman).
NR 28
TC 12
Z9 12
U1 4
U2 19
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD FEB 20
PY 2015
VL 54
IS 6
BP 1387
EP 1398
DI 10.1364/AO.54.001387
PG 12
WC Optics
SC Optics
GA CB5RR
UT WOS:000349685700023
PM 25968204
ER
PT J
AU Apai, D
Schneider, G
Grady, CA
Wyatt, MC
Lagrange, AM
Kuchner, MJ
Stark, CJ
Lubow, SH
AF Apai, Daniel
Schneider, Glenn
Grady, Carol A.
Wyatt, Mark C.
Lagrange, Anne-Marie
Kuchner, Marc J.
Stark, Christopher J.
Lubow, Stephen H.
TI THE INNER DISK STRUCTURE, DISK-PLANET INTERACTIONS, AND TEMPORAL
EVOLUTION IN THE beta PICTORIS SYSTEM: A TWO-EPOCH HST/STIS
CORONAGRAPHIC STUDY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; planetary systems; planets and
satellites: formation; protoplanetary disks; stars: individual (Beta
Pictoris); techniques: high angular resolution
ID DEBRIS DISK; MOVING GROUP; GIANT PLANETS; DUST DISK; MIDINFRARED IMAGES;
MOLECULAR GAS; ASYMMETRIES; ORBIT; FOMALHAUT; MODELS
AB We present deep Hubble Space Telescope/Space Telescope Imaging Spectrograph coronagraphic images of the beta Pic debris disk obtained at two epochs separated by 15 yr. The new images and the re-reduction of the 1997 data provide the most sensitive and detailed views of the disk at optical wavelengths as well as the yet smallest inner working angle optical coronagraphic image of the disk. Our observations characterize the large-scale and inner-disk asymmetries and we identify multiple breaks in the disk radial surface brightness profile. We study in detail the radial and vertical disk structure and show that the disk is warped. We explore the disk at the location of the beta Pic b super-Jupiter and find that the disk surface brightness slope is continuous between 0 ''.5 and 2 ''.0, arguing for no change at the separations where beta Pic b orbits. The two epoch images constrain the disk's surface brightness evolution on orbital and radiation pressure blow-out timescales. We place an upper limit of 3% on the disk surface brightness change between 3 '' and 5 '', including the locations of the disk warp, and the CO and dust clumps. We discuss the new observations in the context of high-resolution multi-wavelength images and divide the disk asymmetries in two groups: axisymmetric and non-axisymmetric. The axisymmetric structures (warp, large-scale butterfly, etc.) are consistent with disk structure models that include interactions of a planetesimal belt and a non-coplanar giant planet. The non-axisymmetric features, however, require a different explanation.
C1 [Apai, Daniel; Schneider, Glenn] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, Daniel; Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Wyatt, Mark C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Lagrange, Anne-Marie] Univ Grenoble Alpes, F-38000 Grenoble, France.
[Kuchner, Marc J.; Stark, Christopher J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Lubow, Stephen H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Apai, D (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
EM apai@arizona.edu
FU NASA through a grant from the Space Telescope Science Institute [12551];
Association of Universities for Research in Astronomy, Incorporated,
under NASA [NAS5-26555]; EU through ERC [279973]; French National
Research Agency (ANR) [ANR10-BLANC0504-01]
FX We thank STScI program coordinator Tricia Royle, contact scientist John
Debes, and Charles Proffitt for their dedicated support of this program.
We thank Jean-Charles Augereau, Rebecca Dawson, Andras Gaspar, Paul
Kalas, John Debes, Bill Dent, and Kate Su, among others, for valuable
discussions. We thank the anonymous referee, whose timely report has
helped to improve the interpretation of our results and the clarity of
the manuscript. We thank the entire Servicing Mission 4 crew for
restoring HST and STIS operations. The paper also benefitted from the
presentations and discussions at the workshop Beta Pictoris at 30,
Paris. Support for Program number 12551 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. M.C.W. is grateful for support from the
EU through ERC grant number 279973. We acknowledge support from the
French National Research Agency (ANR) through the grant
ANR10-BLANC0504-01.
NR 66
TC 15
Z9 15
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2015
VL 800
IS 2
AR 136
DI 10.1088/0004-637X/800/2/136
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500059
ER
PT J
AU Bachetti, M
Harrison, FA
Cook, R
Tomsick, J
Schmid, C
Grefenstette, BW
Barret, D
Boggs, SE
Christensen, FE
Craig, WW
Fabian, AC
Furst, F
Gandhi, P
Hailey, CJ
Kara, E
Maccarone, TJ
Miller, JM
Pottschmidt, K
Stern, D
Uttley, P
Walton, DJ
Wilms, J
Zhang, WW
AF Bachetti, Matteo
Harrison, Fiona A.
Cook, Rick
Tomsick, John
Schmid, Christian
Grefenstette, Brian W.
Barret, Didier
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Fabian, Andrew C.
Fuerst, Felix
Gandhi, Poshak
Hailey, Charles J.
Kara, Erin
Maccarone, Thomas J.
Miller, Jon M.
Pottschmidt, Katja
Stern, Daniel
Uttley, Phil
Walton, Dominic J.
Wilms, Joern
Zhang, William W.
TI NO TIME FOR DEAD TIME: TIMING ANALYSIS OF BRIGHT BLACK HOLE BINARIES
WITH NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; methods: data analysis;
methods: statistical; X-rays: stars
ID QUASI-PERIODIC OSCILLATIONS; X-RAY VARIABILITY; FREQUENCY-RESOLVED
SPECTROSCOPY; CYGNUS X-1; GRS 1915+105; XMM-NEWTON; GX 339-4; SOFT
STATE; POWER-LAW; TELESCOPE-ARRAY
AB Timing of high-count-rate sources with the NuSTAR Small Explorer Mission requires specialized analysis techniques. NuSTAR was primarily designed for spectroscopic observations of sources with relatively low count rates rather than for timing analysis of bright objects. The instrumental dead time per event is relatively long (similar to 2.5msec) and varies event-to-event by a few percent. The most obvious effect is a distortion of the white noise level in the power density spectrum (PDS) that cannot be easily modeled with standard techniques due to the variable nature of the dead time. In this paper, we show that it is possible to exploit the presence of two completely independent focal planes and use the cospectrum, the real part of the cross PDS, to obtain a good proxy of the white-noise-subtracted PDS. Thereafter, one can use a Monte Carlo approach to estimate the remaining effects of dead time, namely, a frequency-dependent modulation of the variance and a frequency-independent drop of the sensitivity to variability. In this way, most of the standard timing analysis can be performed, albeit with a sacrifice in signal-to-noise ratio relative to what would be achieved using more standard techniques. We apply this technique to NuSTAR observations of the black hole binaries GX 339-4, Cyg X-1, and GRS 1915+105.
C1 [Bachetti, Matteo; Barret, Didier] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bachetti, Matteo; Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Harrison, Fiona A.; Cook, Rick; Grefenstette, Brian W.; Fuerst, Felix; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Tomsick, John; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Schmid, Christian; Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Schmid, Christian; Wilms, Joern] ECAP, D-96049 Bamberg, Germany.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fabian, Andrew C.; Kara, Erin] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Gandhi, Poshak] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Uttley, Phil] Univ Amsterdam, Anton Pannekoek Inst, NL-1098 XH Amsterdam, Netherlands.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bachetti, M (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
EM matteo.bachetti@irap.omp.eu
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015;
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224;
Bachetti, Matteo/0000-0002-4576-9337
NR 77
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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 FEB 20
PY 2015
VL 800
IS 2
AR 109
DI 10.1088/0004-637X/800/2/109
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500032
ER
PT J
AU Gastaldello, F
Wik, DR
Molendi, S
Westergaard, NJ
Hornstrup, A
Madejski, G
Ferreira, DDM
Boggs, SE
Christensen, FE
Craig, WW
Grefenstette, BW
Hailey, CJ
Harrison, FA
Madsen, KK
Stern, D
Zhang, WW
AF Gastaldello, Fabio
Wik, Daniel R.
Molendi, S.
Westergaard, N. J.
Hornstrup, A.
Madejski, G.
Ferreira, D. D. M.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Madsen, K. K.
Stern, D.
Zhang, W. W.
TI A NuSTAR OBSERVATION OF THE CENTER OF THE COMA CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (Coma);
X-rays: galaxies: clusters
ID X-RAY EXCESS; DIFFUSE RADIO-EMISSION; DARK-MATTER SUBHALOS; INTRACLUSTER
MEDIUM; GALAXY CLUSTERS; XMM-NEWTON; RADIATION; CHANDRA; SUBSTRUCTURES;
PROFILES
AB We present the results of a 55 ks NuSTAR observation of the core of the Coma Cluster. The global spectrum can be explained by thermal gas emission, with a conservative 90% upper limit to non-thermal inverse Compton (IC) emission of 5.1x10(-12) erg cm(-2) s(-1) in a 12' x 12' field of view. The brightness of the thermal component in this central region does not allow more stringent upper limits on the IC component when compared with nonimaging instruments with much larger fields of view where claims of detections have been made. Future mosaic NuSTAR observations of Coma will further address this issue. The temperature map shows a relatively uniform temperature distribution with a gradient from the hot northwest side to the cooler southeast, in agreement with previous measurements. The temperature determination is robust given the flat effective area and low background in the 3-20 keV band, making NuSTAR an ideal instrument to measure high temperatures in the intracluster medium.
C1 [Gastaldello, Fabio; Molendi, S.] IASF Milano, INAF, I-20133 Milan, Italy.
[Gastaldello, Fabio] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Wik, Daniel R.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Wik, Daniel R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Westergaard, N. J.; Hornstrup, A.; Ferreira, D. D. M.; Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Madejski, G.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gastaldello, F (reprint author), IASF Milano, INAF, Via Bassini 15, I-20133 Milan, Italy.
EM gasta@lambrate.inaf.it
RI Boggs, Steven/E-4170-2015; Gastaldello, Fabio/N-4226-2015; Ferreira,
Desiree/M-1666-2016;
OI Boggs, Steven/0000-0001-9567-4224; Gastaldello,
Fabio/0000-0002-9112-0184; Ferreira, Desiree/0000-0003-4003-3256;
Molendi, Silvano/0000-0002-2483-278X
FU NASA
FX This research made use of data from the NuSTAR mission, a project led by
the California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by NASA. We thank the NuSTAR Operations,
Software, and Calibration teams for support with the execution and
analysis of these observations. This research has made use of the NuSTAR
Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(USA).
NR 53
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2015
VL 800
IS 2
AR 139
DI 10.1088/0004-637X/800/2/139
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500062
ER
PT J
AU Kuiper, R
Yorke, HW
Turner, NJ
AF Kuiper, Rolf
Yorke, Harold W.
Turner, Neal J.
TI PROTOSTELLAR OUTFLOWS AND RADIATIVE FEEDBACK FROM MASSIVE STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; methods: numerical; stars: formation; stars:
jets; stars: massive; stars: winds, outflows
ID HIGH ACCRETION RATES; MOLECULAR OUTFLOWS; DISK ACCRETION; HYDRODYNAMIC
SIMULATIONS; CLUSTER FORMATION; CORES; EVOLUTION; FRAGMENTATION;
PROTOSTARS; COLLAPSE
AB We carry out radiation hydrodynamical simulations of the formation of massive stars in the super-Eddington regime including both their radiative feedback and protostellar outflows. The calculations start from a prestellar core of dusty gas and continue until the star stops growing. The accretion ends when the remnants of the core are ejected, mostly by the force of the direct stellar radiation in the polar direction and elsewhere by the reradiated thermal infrared radiation. How long the accretion persists depends on whether the protostellar outflows are present. We set the mass outflow rate to 1% of the stellar sink particle's accretion rate. The outflows open a bipolar cavity extending to the core's outer edge, through which the thermal radiation readily escapes. The radiative flux is funneled into the polar directions while the core's collapse proceeds near the equator. The outflow thus extends the "flashlight effect," or anisotropic radiation field, found in previous studies from the few hundred AU scale of the circumstellar disk up to the 0.1 parsec scale of the core. The core's flashlight effect allows core gas to accrete on the disk for longer, in the same way that the disk's flashlight effect allows disk gas to accrete on the star for longer. Thus although the protostellar outflows remove material near the core's poles, causing slower stellar growth over the first few free-fall times, they also enable accretion to go on longer in our calculations. The outflows ultimately lead to stars of somewhat higher mass.
C1 [Kuiper, Rolf] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kuiper, Rolf] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Yorke, Harold W.; Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kuiper, R (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM kuiper@mpia.de; Harold.W.Yorke@jpl.nasa.gov; Neal.J.Turner@jpl.nasa.gov
OI Kuiper, Rolf/0000-0003-2309-8963
FU German Academy of Science Leopoldina within the Leopoldina Fellowship
Programme [LPDS 2011-5]; Max Planck Research Group Star formation
throughout the Milky Way Galaxy at the Max Planck Institute for
Astronomy; National Aeronautics and Space Administration (NASA)
FX We thank Takashi Hosokawa for many critical and fruitful discussions. R.
K. acknowledges financial support by the German Academy of Science
Leopoldina within the Leopoldina Fellowship Programme, grant No. LPDS
2011-5. R.K. further acknowledges funding from the Max Planck Research
Group Star formation throughout the Milky Way Galaxy at the Max Planck
Institute for Astronomy. Major portions of this work were conducted at
the Jet Propulsion Laboratory, California Institute of Technology,
operating under a contract with the National Aeronautics and Space
Administration (NASA).
NR 58
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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 FEB 20
PY 2015
VL 800
IS 2
AR 86
DI 10.1088/0004-637X/800/2/86
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500009
ER
PT J
AU Lurie, JC
Davenport, JRA
Hawley, SL
Wilkinson, TD
Wisniewski, JP
Kowalski, AF
Hebb, L
AF Lurie, John C.
Davenport, James R. A.
Hawley, Suzanne L.
Wilkinson, Tessa D.
Wisniewski, John P.
Kowalski, Adam F.
Hebb, Leslie
TI KEPLER FLARES III: STELLAR ACTIVITY ON GJ 1245A AND B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: low-mass; techniques: image processing
ID WHITE-LIGHT FLARES; M-DWARFS; DIFFERENTIAL ROTATION; MAGNETIC ACTIVITY;
STARS; I.; SAMPLE; ERROR
AB We present the flare occurrence rates and starspot evolution for GJ 1245A and B, two active M5 stars, based on nine months of Kepler short cadence observations, and four years of nearly continuous long cadence observations. The A component is separated from the B component by 7 '', and the stars are not resolved in the Kepler pipeline processing due to Kepler's large plate scale of 4 '' pixel(-1). Analyzing the target pixel data, we have generated separate light curves for components A and B using the PyKE pixel response function modeling procedures, and note the effects of CCD saturation and nonlinear response to high-energy flares. In our sample, GJ 1245A and B exhibit an average of 3.0 and 2.6 flares per day, respectively. We introduce a new metric, L-fl/L-Kp, to compare the flare rates between stars, and discuss this in the context of GJ 1245A and B. Both stars exhibit starspot features that evolve on long timescales, with the slower rotating B component showing evidence of differential rotation. Intriguingly, the angular separation between the A and B component photocenters decreases during the four years of observations in a manner consistent with a shift in the position of the A photocenter due to the orbit of its unseen M8 companion (GJ 1245C), which is similar to 94% less bright. Among the most detailed photometric studies of fully convective M dwarfs in a multiple system, these results provide an important constraint on stellar age-rotation-activity models.
C1 [Lurie, John C.; Davenport, James R. A.; Hawley, Suzanne L.; Wilkinson, Tessa D.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Kowalski, Adam F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hebb, Leslie] Hobart & William Smith Coll, Dept Phys, Geneva, NY 14456 USA.
RP Lurie, JC (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
EM lurie@uw.edu
OI Davenport, James/0000-0002-0637-835X
FU Kepler Cycle 2 GO grant [NNX11AB71G]; Cycle 3 GO grant [NNX12AC79G];
Washington Research Foundation; University of Washington Provost's
Initiative in Data-Intensive Discovery; NASA ADP [NNX09AC77G]; NSF
[AST13-11678, AST08-07205]; NASA Science Mission directorate; NASA
[NAS5-26555]; NASA Office of Space Science [NNX13AC07G]
FX This work was supported by Kepler Cycle 2 GO grant NNX11AB71G and Cycle
3 GO grant NNX12AC79G. J.C.L. acknowledges the support of the Washington
Research Foundation and the University of Washington Provost's
Initiative in Data-Intensive Discovery. J.R.A.D. acknowledges support
from NASA ADP grant NNX09AC77G. J.R.A.D. and S.L.H. acknowledge support
from NSF grant AST13-11678. S.L.H. acknowledges support from NSF grant
AST08-07205.; This paper includes data collected by the Kepler mission.
Funding for the Kepler mission is provided by the NASA Science Mission
directorate. Some of the data presented in this paper were obtained from
the Mikulski Archive for Space Telescopes (MAST). STScI is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. Support for MAST for non-HST data is provided
by the NASA Office of Space Science via grant NNX13AC07G and by other
grants and contracts
NR 39
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2015
VL 800
IS 2
AR 95
DI 10.1088/0004-637X/800/2/95
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500018
ER
PT J
AU Materese, CK
Nuevo, M
Sandford, SA
AF Materese, Christopher K.
Nuevo, Michel
Sandford, Scott A.
TI N- AND O-HETEROCYCLES PRODUCED FROM THE IRRADIATION OF BENZENE AND
NAPHTHALENE IN H2O/NH3-CONTAINING ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; molecular data; molecular processes; solid
state: refractory
ID POLYCYCLIC AROMATIC-HYDROCARBONS; MURCHISON METEORITE; ULTRAVIOLET
PHOTOIRRADIATION; EXTRATERRESTRIAL NUCLEOBASES; CARBONACEOUS METEORITES;
NITROGEN-HETEROCYCLES; INFRARED-SPECTROSCOPY; PREBIOTIC MOLECULES;
UV-IRRADIATION; PYRIMIDINE
AB Aromatic heterocyclic molecules are an important class of molecules of astrophysical and biological significance that include pyridine, pyrimidine, and their derivatives. Such compounds are believed to exist in interstellar and circumstellar environments, though they have never been observed in the gas phase. Regardless of their presence in the gas phase in space, numerous heterocycles have been reported in carbonaceous meteorites, which indicates that they are formed under astrophysical conditions. The experimental work described here shows that N- and O-heterocyclic molecules can form from the ultraviolet (UV) irradiation of the homocyclic aromatic molecules benzene (C6H6) or naphthalene (C10H8) mixed in ices containing H2O and NH3. This represents an alternative way to generate aromatic heterocycles to those considered before and may have important implications for astrochemistry and astrobiology.
C1 [Materese, Christopher K.; Nuevo, Michel; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Materese, Christopher K.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Nuevo, Michel] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Materese, CK (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM christopher.k.materese@nasa.gov
FU NASA's Origins of Solar Systems and Exobiology programs
FX C.K.M. acknowledges R.L. Walker (NASA Ames) for technical support, Drs.
L. Allamandola and A. Mattioda for helpful comments and discussion, and
the NASA Postdoctoral Program (NPP) administered by ORAU. S.A.S.
acknowledges support from NASA's Origins of Solar Systems and Exobiology
programs. We also thank an anonymous reviewer for useful comments and
suggestions.
NR 44
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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 FEB 20
PY 2015
VL 800
IS 2
AR 116
DI 10.1088/0004-637X/800/2/116
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500039
ER
PT J
AU Mazeh, T
Holczer, T
Shporer, A
AF Mazeh, Tsevi
Holczer, Tomer
Shporer, Avi
TI TIME VARIATION OF KEPLER TRANSITS INDUCED BY STELLAR ROTATING SPOTS-A
WAY TO DISTINGUISH BETWEEN PROGRADE AND RETROGRADE MOTION. I. THEORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; starspots; stars: rotation; techniques: photometric
ID SPIN-ORBIT ALIGNMENT; SUN-LIKE STAR; EXOPLANETARY SYSTEM; ECLIPSING
BINARIES; TIMING OBSERVATIONS; PLANETARY ORBITS; RADIAL-VELOCITY; HOT
JUPITERS; LIGHT-CURVE; AXES
AB Some transiting planets discovered by the Kepler mission display transit timing variations (TTVs) induced by stellar spots that rotate on the visible hemisphere of their parent stars. An induced TTV can be observed when a planet crosses a spot and modifies the shape of the transit light curve, even if the time resolution of the data does not allow the detection of the crossing event itself. We present an approach that can, in some cases, use the derived TTVs of a planet to distinguish between a prograde and a retrograde planetary motion with respect to the stellar rotation. Assuming a single spot darker than the stellar disk, spot crossing by the planet can induce measured positive (negative) TTV, if the crossing occurs in the first (second) half of the transit. On the other hand, the motion of the spot toward (away from) the center of the stellar visible disk causes the stellar brightness to decrease (increase). Therefore, for a planet with prograde motion, the induced TTV is positive when the local slope of the stellar flux at the time of transit is negative, and vice versa. Thus, we can expect to observe a negative (positive) correlation between the TTVs and the photometric slopes for prograde (retrograde) motion. Using a simplistic analytical approximation, and also the publicly available SOAP-T tool to produce light curves of transits with spot-crossing events, we show for some cases how the induced TTVs depend on the local stellar photometric slopes at the transit timings. Detecting this correlation in Kepler transiting systems with high enough signal-to-noise ratio can allow us to distinguish between prograde and retrograde planetary motions. In upcoming papers we present analyses of the KOIs and Kepler eclipsing binaries, following the formalism developed here.
C1 [Mazeh, Tsevi; Holczer, Tomer] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Mazeh, Tsevi] Jesus Serra Fdn, Inst Astrofs Canarias, Guest Program, E-38205 Tenerife, Spain.
[Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mazeh, T (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
EM mazeh@post.tau.ac.il
OI Shporer, Avi/0000-0002-1836-3120
FU European Research Council under the EU's Seventh Framework Programme
(FP7)/ ERC Grant [291352]; Israel Science Foundation [1423/11]; Israeli
Centers of Research Excellence (I-CORE) [1829/12]; NASA through the
Sagan Fellowship Program
FX We are grateful to the referee for very helpful comments that helped us
substantially improve the paper. We are thankful to the authors of the
SOAP-T tool that made it publicly available. The research leading to
these results has received funding from the European Research Council
under the EU's Seventh Framework Programme (FP7/(2007-2013)/ ERC Grant
Agreement No. 291352). T. M. also acknowledges support from the Israel
Science Foundation (grant No. 1423/11) and the Israeli Centers of
Research Excellence (I-CORE, grant No. 1829/12). T. M. is grateful to
the Jesus Serra Foundation Guest Program and to Hans Deeg and Rafaelo
Rebolo, that enabled his visit to the Instituto de Astrofsica de
Canarias, where the last stage of this research was completed. This work
was performed in part at the Jet Propulsion Laboratory, under contract
with the California Institute of Technology (Caltech) funded by NASA
through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute.
NR 55
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2015
VL 800
IS 2
AR 142
DI 10.1088/0004-637X/800/2/142
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500065
ER
PT J
AU Nynka, M
Hailey, CJ
Zhang, S
Morris, MM
Zhao, JH
Goss, M
Bauer, FE
Boggs, SE
Craig, WW
Christensen, FE
Gotthelf, EV
Harrison, FA
Mori, K
Perez, KM
Stern, D
Zhang, WW
AF Nynka, Melania
Hailey, Charles J.
Zhang, Shuo
Morris, Mark M.
Zhao, Jun-Hui
Goss, Miller
Bauer, Franz E.
Boggs, Stephen E.
Craig, William W.
Christensen, Finn E.
Gotthelf, Eric V.
Harrison, Fiona A.
Mori, Kaya
Perez, Kerstin M.
Stern, Daniel
Zhang, William W.
TI G359.97-0.038: A HARD X-RAY FILAMENT ASSOCIATED WITH A SUPERNOVA
SHELL-MOLECULAR CLOUD INTERACTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center
ID SAGITTARIUS-A-EAST; PULSAR-WIND NEBULAE; LARGE ARRAY OBSERVATIONS;
GALACTIC-CENTER REGION; HIGH-ENERGY EMISSION; 1720 MHZ MASERS;
NONTHERMAL EMISSION; CIRCUMNUCLEAR DISK; SOURCE CATALOG; COSMIC-RAYS
AB We present the first high-energy X-ray (>10 keV) observations of the non-thermal filament G359.97-0.038 using the Nuclear Spectroscopic Telescope Array (NuSTAR). This filament is one of approximately 20 X-ray filaments of unknown origin located in the central 20 pc region in the Galactic Center near Sgr A*. Its NuSTAR and Chandra broadband spectrum is characterized by a single power law with Gamma = 1.3 +/- 0.3 that extends from 2 to 50 keV, with an unabsorbed luminosity of 1.3 x 10(33) erg s(-1) (d/8 kpc)(2) in the 2-8 keV band. Despite possessing a cometary X-ray morphology that is typical of a pulsar wind nebula (PWN) in high-resolution Chandra imaging, our spatially resolved Chandra spectral analysis found no significant spectral softening along the filament as would be expected from particle synchrotron cooling. Coincident radio emission is detected using the Very Large Array at 5.5 and 8.3 GHz. We examine and subsequently discard a PWN or magnetic flux tube as the origin of G359.97-0.038. We use broadband spectral characteristics and a morphological analysis to show that G359.97-0.038 is likely an interaction site between the shell of Sgr A East and an adjacent molecular cloud. This is supported by CS molecular line spectroscopy and the presence of an OH maser.
C1 [Nynka, Melania; Hailey, Charles J.; Zhang, Shuo; Gotthelf, Eric V.; Mori, Kaya; Perez, Kerstin M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Morris, Mark M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Goss, Miller] NRAO, Socorro, NM 87801 USA.
[Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, Stephen E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nynka, M (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
CONICYT-Chile [Basal-CATA PFB-06/2007, FONDECYT 1141218, "EMBIGGEN"
Anillo ACT1101]; Iniciativa Cientifica Milenio del Ministerio de
Economia, Fomento y Turismo [IC120009]
FX This work was supported under NASA contract No. NNG08FD60C, and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. F.E.B.
acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007,
FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and Project IC120009
"Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa
Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. 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 (NuSTAR-DAS) jointly
developed by the ASI Science Data Center (ASDC, Italy) and the
California Institute of Technology (USA).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2015
VL 800
IS 2
AR 119
DI 10.1088/0004-637X/800/2/119
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500042
ER
PT J
AU Ptak, A
Hornschemeier, A
Zezas, A
Lehmer, B
Yukita, M
Wik, D
Antoniou, V
Argo, MK
Ballo, L
Bechtol, K
Boggs, S
Della Ceca, R
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Krivonos, R
Maccarone, TJ
Stern, D
Tatum, M
Venters, T
Zhang, WW
AF Ptak, A.
Hornschemeier, A.
Zezas, A.
Lehmer, B.
Yukita, M.
Wik, D.
Antoniou, V.
Argo, M. K.
Ballo, L.
Bechtol, K.
Boggs, S.
Della Ceca, R.
Christensen, F. E.
Craig, W. W.
Hailey, C. J.
Harrison, F. A.
Krivonos, R.
Maccarone, T. J.
Stern, D.
Tatum, M.
Venters, T.
Zhang, W. W.
TI A FOCUSED, HARD X-RAY LOOK AT ARP 299 WITH NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (Arp 299); galaxies: starburst;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; INFRARED GALAXIES; NGC
253; EMISSION; CHANDRA; MODEL; CONSTRAINTS; STARBURSTS; DISCOVERY
AB We report on simultaneous observations of the local starburst system Arp 299 with NuSTAR and Chandra, which provides the first resolved images of this galaxy up to energies of similar to 45 keV. Fitting the 3-40 keV spectrum reveals a column density of N-H similar to 4 x 10(24) cm(-2), characteristic of a Compton-thick active galactic nucleus (AGN), and a 10-30 keV luminosity of 1.2 x 1043 erg s(-1). The hard X-rays detected by NuSTAR above 10 keV are centered on the western nucleus, Arp 299-B, which previous X-ray observations have shown to be the primary source of neutral Fe-K emission. Other X-ray sources, including Arp 299-A, the eastern nucleus also thought to harbor an AGN, as well as X-ray binaries, contribute less than or similar to 10% to the 10-20 keV emission from the Arp 299 system. The lack of significant emission above 10 keV other than that attributed to Arp 299-B suggests that: (1) any AGN in Arp 299-A must be heavily obscured (N-H > 10(24) cm(-2)) or have a much lower luminosity than Arp 299-B and (2) the extranuclear X-ray binaries have spectra that cut-off above similar to 10 keV. Such soft spectra are characteristic of ultraluminous X-ray sources observed to date by NuSTAR.
C1 [Ptak, A.; Hornschemeier, A.; Lehmer, B.; Yukita, M.; Wik, D.; Tatum, M.; Venters, T.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ptak, A.; Hornschemeier, A.; Lehmer, B.; Yukita, M.; Wik, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion, Greece.
[Zezas, A.] FORTH, IESL, Iraklion, Crete, Greece.
[Zezas, A.; Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Argo, M. K.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ballo, L.; Della Ceca, R.] Osservatorio Astron Brera INAF, I-20121 Milan, Italy.
[Bechtol, K.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Boggs, S.; Craig, W. W.; Krivonos, R.] UC Berkeley Space Sci Lab, Berkeley, CA USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DK-2100 Copenhagen, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Hailey, C. J.] Columbia Univ, New York, NY USA.
[Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ptak, A (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
RI Boggs, Steven/E-4170-2015; Zezas, Andreas/C-7543-2011; Antoniou,
Vallia/E-3837-2013;
OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X;
Ballo, Lucia/0000-0002-5036-3497; Antoniou, Vallia/0000-0001-7539-1593;
Della Ceca, Roberto/0000-0001-7551-2252; Argo, Megan/0000-0003-3594-0214
FU NuSTAR Data Analysis Software (NUSTARDAS); ASI Science Data Center
(ASDC, Italy); Caltech (USA); NASA [NNX12AN05G]; Chandra grant
[GO3-14124X]; [267251]
FX 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. The
scientific results reported in this article are based in part on
observations made by the Chandra X-ray Observatory. 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 Caltech (USA). We also
made use of the NASA/IPAC Extragalactic Database (NED) and NASA's
Astrophysics Data System. L. B. received financial supports from the
European Commission Seventh Framework Programme (FP7/2007-2013) under
grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt).
A.Z. acknowledges partial support by NASA grant NNX12AN05G and Chandra
grant GO3-14124X. We thank the anonymous referee for suggestions that
improved this paper.
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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 FEB 20
PY 2015
VL 800
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AR 104
DI 10.1088/0004-637X/800/2/104
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500027
ER
PT J
AU Tanner, A
Boyajian, TS
von Braun, K
Kane, S
Brewer, JM
Farrington, C
van Belle, GT
Beichman, CA
Fischer, D
ten Brummelaar, TA
McAlister, HA
Schaefer, G
AF Tanner, Angelle
Boyajian, Tabetha S.
von Braun, Kaspar
Kane, Stephen
Brewer, John M.
Farrington, Chris
van Belle, Gerard T.
Beichman, Charles A.
Fischer, Debra
ten Brummelaar, Theo A.
McAlister, Harold A.
Schaefer, Gail
TI STELLAR PARAMETERS FOR HD 69830, A NEARBY STAR WITH THREE NEPTUNE MASS
PLANETS AND AN ASTEROID BELT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: fundamental parameters; techniques: interferometric
ID MAIN-SEQUENCE STARS; HABITABLE ZONES; Y-2 ISOCHRONES; CHARA ARRAY;
PHOTOMETRY; SYSTEM; DEPENDENCE; DIAMETERS; HD-69830; SEARCH
AB We used the CHARA Array to directly measure the angular diameter of HD 69830, home to three Neptune mass planets and an asteroid belt. Our measurement of 0.674 +/- 0.014 mas for the limb- darkened angular diameter of this star leads to a physical radius of R-* = 0.9058 +/- 0.0190 R-circle dot and luminosity of L-* = 0.622 +/- 0.014 L-circle dot when combined with a fit to the spectral energy distribution of the star. Placing these observed values on a Hertzsprung-Russel diagram along with stellar evolution isochrones produces an age of 10.6 +/- 4 Gyr and mass of 0.863 +/- 0.043 M-circle dot. We use archival optical echelle spectra of HD 69830 along with an iterative spectral fitting technique to measure the iron abundance ([Fe/H] = -0.04 +/- 0.03), effective temperature (5385 +/- 44 K), and surface gravity (log g = 4.49 +/- 0.06). We use these new values for the temperature and luminosity to calculate a more precise age of 7.5 +/- 3 Gyr. Applying the values of stellar luminosity and radius to recent models on the optimistic location of the habitable zone produces a range of 0.61-1.44 AU; partially outside the orbit of the furthest known planet (d) around HD 69830. Finally, we estimate the snow line at a distance of 1.95 +/- 0.19 AU, which is outside the orbit of all three planets and its asteroid belt.
C1 [Tanner, Angelle] Mississippi State Univ, Dept Phys & Astron, Starkville, MS 39762 USA.
[Boyajian, Tabetha S.; Brewer, John M.; Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[von Braun, Kaspar; van Belle, Gerard T.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Kane, Stephen] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Farrington, Chris; ten Brummelaar, Theo A.; McAlister, Harold A.; Schaefer, Gail] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Farrington, Chris; ten Brummelaar, Theo A.; McAlister, Harold A.; Schaefer, Gail] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Tanner, A (reprint author), Mississippi State Univ, Dept Phys & Astron, Hilbun Hall, Starkville, MS 39762 USA.
OI Brewer, John/0000-0002-9873-1471; Boyajian, Tabetha/0000-0001-9879-9313
FU National Science Foundation through NSF [AST-0908253, AST 1211129];
Georgia State University through the College of Arts and Sciences; NASA
[ADAP12-0172]
FX We thank the anonymous referee for insightful comments pertaining to
this manuscript. This research has made use of the JSDC Jean-Marie
Mariotti Center database, available at http://www.jmmc.fr/jsdc. The
CHARA Array is funded by the National Science Foundation through NSF
grants AST-0908253 and AST 1211129, and by Georgia State University
through the College of Arts and Sciences. TSB acknowledges support
provided through NASA grant ADAP12-0172. This research has made use of
the Habitable Zone Gallery at hzgallery. org.
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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 FEB 20
PY 2015
VL 800
IS 2
AR 115
DI 10.1088/0004-637X/800/2/115
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500038
ER
PT J
AU Torres, G
Kipping, DM
Fressin, F
Caldwell, DA
Twicken, JD
Ballard, S
Batalha, NM
Bryson, ST
Ciardi, DR
Henze, CE
Howell, SB
Isaacson, HT
Jenkins, J
Muirhead, PS
Newton, ER
Petigura, EA
Barclay, T
Borucki, WJ
Crepp, JR
Everett, ME
Horch, EP
Howard, AW
Kolbl, R
Marcy, GW
McCauliff, S
Quintana, EV
AF Torres, Guillermo
Kipping, David M.
Fressin, Francois
Caldwell, Douglas A.
Twicken, Joseph D.
Ballard, Sarah
Batalha, Natalie M.
Bryson, Stephen T.
Ciardi, David R.
Henze, Christopher E.
Howell, Steve B.
Isaacson, Howard T.
Jenkins, Jonm.
Muirhead, Philip S.
Newton, Elisabeth R.
Petigura, Erik A.
Barclay, Thomas
Borucki, William J.
Crepp, Justin R.
Everett, Mark E.
Horch, Elliott P.
Howard, Andrew W.
Kolbl, Rea
Marcy, Geoffrey W.
McCauliff, Sean
Quintana, Elisa V.
TI VALIDATION OF 12 SMALL KEPLER TRANSITING PLANETS IN THE HABITABLE ZONE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; planetary systems; stars: individual (KOI-3284
(Kepler-438), KOI-4742 (Kepler-442)); techniques: photometric
ID K-BAND SPECTRA; MAIN-SEQUENCE STARS; M DWARFS; FALSE POSITIVES; BINARY
STARS; LIGHT CURVES; STELLAR EVOLUTION; CANDIDATE PLANETS; BLEND
SCENARIOS; HIPPARCOS STARS
AB We present an investigation of 12 candidate transiting planets from Kepler with orbital periods ranging from 34 to 207 days, selected from initial indications that they are small and potentially in the habitable zone (HZ) of their parent stars. Few of these objects are known. The expected Doppler signals are too small to confirm them by demonstrating that their masses are in the planetary regime. Here we verify their planetary nature by validating them statistically using the BLENDER technique, which simulates large numbers of false positives and compares the resulting light curves with the Kepler photometry. This analysis was supplemented with new follow-up observations (high-resolution optical and near-infrared spectroscopy, adaptive optics imaging, and speckle interferometry), as well as an analysis of the flux centroids. For 11 of them (KOI-0571.05, 1422.04, 1422.05, 2529.02, 3255.01, 3284.01, 4005.01, 4087.01, 4622.01, 4742.01, and 4745.01) we show that the likelihood they are true planets is far greater than that of a false positive, to a confidence level of 99.73% (3 sigma) or higher. For KOI-4427.01 the confidence level is about 99.2% (2.6 sigma). With our accurate characterization of the GKM host stars, the derived planetary radii range from 1.1 to 2.7R(circle plus). All 12 objects are confirmed to be in the HZ, and nine are small enough to be rocky. Excluding three of them that have been previously validated by others, our study doubles the number of known rocky planets in the HZ. KOI-3284.01 (Kepler-438b) and KOI-4742.01 (Kepler-442b) are the planets most similar to the Earth discovered to date when considering their size and incident flux jointly.
C1 [Torres, Guillermo; Kipping, David M.; Fressin, Francois; Newton, Elisabeth R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Caldwell, Douglas A.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA.
[Batalha, Natalie M.; Bryson, Stephen T.; Henze, Christopher E.; Howell, Steve B.; Jenkins, Jonm.; Barclay, Thomas; Borucki, William J.; Quintana, Elisa V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Isaacson, Howard T.; Petigura, Erik A.; Kolbl, Rea; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gtorres@cfa.harvard.edu
RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014;
OI Howard, Andrew/0000-0001-8638-0320; Muirhead,
Philip/0000-0002-0638-8822; Ciardi, David/0000-0002-5741-3047; Newton,
Elisabeth/0000-0003-4150-841X
FU NASA's Science Mission Directorate; NASA [NNX14AB83G]; Harvard College
Observatory Menzel Fellowship
FX We thank the referee for helpful comments on the original manuscript.
This paper includes data collected by the Kepler spacecraft. Funding for
the Kepler Mission is provided by NASA's Science Mission Directorate.
The research has also made use of the Michael Dodds Computing Facility,
of NASA's Astrophysics Data System (ADS), and of data products from the
Mikulski Archive for Space Telescopes (MAST). 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. We extend special thanks to
those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are
privileged to be guests. G.T. acknowledges partial support for this work
from NASA grant NNX14AB83G (Kepler Participating Scientist Program).
D.M.K. is supported by the Harvard College Observatory Menzel
Fellowship.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
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AR 99
DI 10.1088/0004-637X/800/2/99
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500022
ER
PT J
AU Wagner, CR
Brodwin, M
Snyder, GF
Gonzalez, AH
Stanford, SA
Alberts, S
Pope, A
Stern, D
Zeimann, GR
Chary, RR
Dey, A
Eisenhardt, PRM
Mancone, CL
Moustakas, J
AF Wagner, Cory R.
Brodwin, Mark
Snyder, Gregory F.
Gonzalez, Anthony H.
Stanford, S. A.
Alberts, Stacey
Pope, Alexandra
Stern, Daniel
Zeimann, Gregory R.
Chary, Ranga-Ram
Dey, Arjun
Eisenhardt, Peter R. M.
Mancone, Conor L.
Moustakas, John
TI STAR FORMATION IN HIGH-REDSHIFT CLUSTER ELLIPTICALS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD;
galaxies: evolution; galaxies: high-redshift
ID COLOR-MAGNITUDE RELATION; EARLY-TYPE GALAXIES; ACTIVE GALACTIC NUCLEI;
HUBBLE-SPACE-TELESCOPE; IRAC SHALLOW SURVEY; DIGITAL SKY SURVEY;
INFRARED LUMINOUS GALAXIES; EVOLUTION SURVEY COSMOS; EARLY DATA RELEASE;
WIDE-FIELD SURVEY
AB We measure the star formation rates (SFRs) of massive (M-star > 10(10.1)M(circle dot)) early-type galaxies (ETGs) in a sample of 11 high-redshift (1.0 < z < 1.5) galaxy clusters drawn from the IRAC Shallow Cluster Survey (ISCS). We identify ETGs visually from Hubble Space Telescope imaging and select likely cluster members as having either an appropriate spectroscopic redshift or red-sequence color. Mid-infrared SFRs are measured using Spitzer 24 mu m data for isolated cluster galaxies for which contamination by neighbors, and active galactic nuclei, can be ruled out. Cluster ETGs show enhanced specific star formation rates (sSFRs) compared to cluster galaxies in the local universe, but have sSFRs more than four times lower than that of field ETGs at 1 < z < 1.5. Relative to the late-type cluster population, isolated ETGs show substantially quenched mean SFRs, yet still contribute 12% of the overall star formation activity measured in 1 < z < 1.5 clusters. We find that new ETGs are likely being formed in ISCS clusters; the fraction of cluster galaxies identified as ETGs increases from 34% to 56% from z similar to 1.5 -> 1.25. While the fraction of cluster ETGs that are highly star-forming (SFR >= 26 M-circle dot yr(-1)) drops from 27% to 10% over the same period, their sSFRs are roughly constant. All these factors taken together suggest that, particularly at z greater than or similar to 1.25, the events that created these distant cluster ETGs-likely mergers, at least among the most massive-were both recent and gas-rich.
C1 [Wagner, Cory R.; Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Snyder, Gregory F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gonzalez, Anthony H.; Mancone, Conor L.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA.
[Alberts, Stacey; Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Stern, Daniel; Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zeimann, Gregory R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91109 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
RP Wagner, CR (reprint author), Queens Univ, Dept Phys Engn Phys & Astron, Stirling Hall, Kingston, ON K7L 3N6, Canada.
EM cwagner@astro.queensu.ca
FU NASA through Space Telescope Science Institute [10496, 11002, 11597,
11663]; Association of Universities for Research in Astronomy, Inc.,
under NASA [NAS 5-26555]; Chandra X-ray Observatory [SV4-74018, A31];
NASA
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. Support for HST programs 10496, 11002, 11597, and 11663
were provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work
is based in part on observations obtained with the Chandra X-ray
Observatory, under contract SV4-74018, A31 with the Smithsonian
Astrophysical Observatory which operates the Chandra X-Ray Observatory
for NASA.
NR 102
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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 FEB 20
PY 2015
VL 800
IS 2
AR 107
DI 10.1088/0004-637X/800/2/107
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB7CA
UT WOS:000349782500030
ER
PT J
AU Larsson, J
Racusin, JL
Burgess, JM
AF Larsson, J.
Racusin, J. L.
Burgess, J. M.
TI EVIDENCE FOR JET LAUNCHING CLOSE TO THE BLACK HOLE IN GRB 101219B-A
FERMI GRB DOMINATED BY THERMAL EMISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual (GRB 101219B);
radiation mechanisms: thermal
ID GAMMA-RAY BURST; PHOTOSPHERIC EMISSION; PROMPT EMISSION; SIGNATURES;
EVOLUTION; COMPONENT; ENERGY; AFTERGLOWS; GRB090902B; SUPERNOVA
AB We present observations by the Fermi Gamma-Ray Space Telescope Gamma-Ray Burst Monitor (GBM) of the nearby (z = 0.55) GRB 101219B. This burst is a long GRB, with an associated supernova and with a blackbody (BB) component detected in the early afterglow observed by the Swift X-ray Telescope (XRT). Here we show that the prompt gamma-ray emission has a BB spectrum, making this the second such burst observed by Fermi GBM. The properties of the BB, together with the redshift and our estimate of the radiative efficiency makes it possible to calculate the absolute values of the properties of the outflow. We obtain an initial Lorentz factor G = 138 +/- 8, a photospheric radius r(phot) = 4.4 +/- 1.9 x 10(11) cm, and a launch radius r(0) = 2.7 +/- 1.6 x 10(7) cm. The latter value is close to the black hole and suggests that the jet has a relatively unobstructed path through the star. There is no smooth connection between the BB components seen by GBM and XRT, ruling out the scenario that the late emission is due to high-latitude effects. In the interpretation that the XRT BB is prompt emission due to late central engine activity, the jet either has to be very wide or have a clumpy structure where the emission originates from a small patch. Other explanations for this component, such as emission from a cocoon surrounding the jet, are also possible.
C1 [Larsson, J.; Burgess, J. M.] KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, J.; Burgess, J. M.] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Racusin, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Larsson, J (reprint author), KTH, Dept Phys, SE-10691 Stockholm, Sweden.
EM josla@kth.se
OI Burgess, James/0000-0003-3345-9515; /0000-0003-0065-2933
FU Swedish National Space Board
FX This work was supported by the Swedish National Space Board.
NR 37
TC 7
Z9 7
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 FEB 20
PY 2015
VL 800
IS 2
AR L34
DI 10.1088/2041-8205/800/2/L34
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB5UK
UT WOS:000349692900015
ER
PT J
AU Waldron, DL
Preske, A
Zawodny, JM
Krauss, TD
Gupta, MC
AF Waldron, Dennis L.
Preske, Amanda
Zawodny, Joseph M.
Krauss, Todd D.
Gupta, Mool C.
TI Lead selenide quantum dot polymer nanocomposites
SO NANOTECHNOLOGY
LA English
DT Article
DE quantum dots; nanocomposites; optical properties; fluorescence; lead
selenide; PbSe
ID LUMINESCENT SOLAR CONCENTRATORS; SEMICONDUCTOR NANOCRYSTALS; EXTINCTION
COEFFICIENT; RADIATION DETECTION; WAVE-GUIDES; PBSE
AB Optical absorption and fluorescence properties of PbSe quantum dots (QDs) in an Angstrom Bond AB9093 epoxy polymer matrix to form a nanocomposite were investigated. To the authors' knowledge, this is the first reported use of AB9093 as a QD matrix material and it was shown to out-perform the more common poly(methyl methacrylate) matrix in terms of preserving the optical properties of the QD, resulting in the first reported quantum yield (QY) for PbSe QDs in a polymer matrix, 26%. The 1-s first excitonic absorption peak of the QDs in a polymer matrix red shifted 65 nm in wavelength compared to QDs in a hexane solution, while the emission peak in the polymer matrix red shifted by 38 nm. The fluorescence QY dropped from 55% in hexane to 26% in the polymer matrix. A time resolved fluorescence study of the QDs showed single exponential lifetimes of 2.34 and 1.34 mu s in toluene solution and the polymer matrix respectively.
C1 [Waldron, Dennis L.; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Preske, Amanda; Krauss, Todd D.] Univ Rochester, Dept Chem, Rochester, NY 14627 USA.
[Zawodny, Joseph M.] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
RP Waldron, DL (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
OI Waldron, Dennis/0000-0001-9563-5575
FU NASA; NSF I/UCRC
FX We thank the NASA Langley Professor program and NSF I/UCRC for their
support of this project and Dr Jeffrey Peterson of the University of
Rochester for time-resolved photoluminescence measurements and helpful
discussion.
NR 25
TC 2
Z9 2
U1 6
U2 40
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 20
PY 2015
VL 26
IS 7
AR 075705
DI 10.1088/0957-4484/26/7/075705
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA CA9LF
UT WOS:000349244400020
PM 25629463
ER
PT J
AU Nardini, E
Reeves, JN
Gofford, J
Harrison, FA
Risaliti, G
Braito, V
Costa, MT
Matzeu, GA
Walton, DJ
Behar, E
Boggs, SE
Christensen, FE
Craig, WW
Hailey, CJ
Matt, G
Miller, JM
O'Brien, PT
Stern, D
Turner, TJ
Ward, MJ
AF Nardini, E.
Reeves, J. N.
Gofford, J.
Harrison, F. A.
Risaliti, G.
Braito, V.
Costa, M. T.
Matzeu, G. A.
Walton, D. J.
Behar, E.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Hailey, C. J.
Matt, G.
Miller, J. M.
O'Brien, P. T.
Stern, D.
Turner, T. J.
Ward, M. J.
TI Black hole feedback in the luminous quasar PDS 456
SO SCIENCE
LA English
DT Article
ID RADIO-QUIET AGNS; HOST GALAXIES; SIGMA RELATION; OUTFLOWS; WIND;
ABSORBER; LOCATION
AB The evolution of galaxies is connected to the growth of supermassive black holes in their centers. During the quasar phase, a huge luminosity is released as matter falls onto the black hole, and radiation-driven winds can transfer most of this energy back to the host galaxy. Over five different epochs, we detected the signatures of a nearly spherical stream of highly ionized gas in the broadband x-ray spectra of the luminous quasar PDS 456. This persistent wind is expelled at relativistic speeds from the inner accretion disk, and its wide aperture suggests an effective coupling with the ambient gas. The outflow's kinetic power larger than 1046 ergs per second is enough to provide the feedback required by models of black hole and host galaxy coevolution.
C1 [Nardini, E.; Reeves, J. N.; Gofford, J.; Costa, M. T.; Matzeu, G. A.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Reeves, J. N.; Gofford, J.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Risaliti, G.] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Braito, V.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
[Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[O'Brien, P. T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Turner, T. J.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Ward, M. J.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
RP Nardini, E (reprint author), Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
EM e.nardini@keele.ac.uk
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Braito,
Valentina/0000-0002-2629-4989; Risaliti, Guido/0000-0002-3556-977X
FU U.K. Science and Technology Facilities Council [ST/J001384/1]; ESA
member states; National Aeronautics and Space Administration; NASA
[NNX11AJ57G, NNG08FD60C]; Italian Space Agency [ASI-INAF I/037/12/0];
Italian National Institute for Astrophysics [PRIN-INAF 2012]; I-CORE
program of the Planning and Budgeting Committee; Israel Science
Foundation [1937/12, 1163/10]; Israel's Ministry of Science and
Technology
FX This research was supported under the U.K. Science and Technology
Facilities Council grant ST/J001384/1 and is based on x-ray observations
obtained with the XMM-Newton and NuSTAR satellites. XMM-Newton is a
European Space Agency (ESA) science mission with instruments and
contributions directly funded by ESA member states and the National
Aeronautics and Space Administration. The NuSTAR mission is a project
led by the California Institute of Technology, managed by the Jet
Propulsion Laboratory, and funded by NASA. We thank the NuSTAR
Operations, Software, and Calibration teams for support with execution
and analysis of these observations. We also acknowledge financial
support from the Italian Space Agency under grant ASI-INAF I/037/12/0
(G.R. and G.M.); the Italian National Institute for Astrophysics under
grant PRIN-INAF 2012 (G.R.); the I-CORE program of the Planning and
Budgeting Committee, the Israel Science Foundation under grants 1937/12
and 1163/10, Israel's Ministry of Science and Technology (E.B.); and
NASA under grants NNX11AJ57G and NNG08FD60C (T.J.T.). The data are
stored in the science archives of the two x-ray observatories involved
and will become publicly available on 25 March 2015 (XMM-Newton) and
with the upcoming DR6 data release (NuSTAR).
NR 26
TC 30
Z9 30
U1 0
U2 14
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 FEB 20
PY 2015
VL 347
IS 6224
BP 860
EP 863
DI 10.1126/science.1259202
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CB6UB
UT WOS:000349761100040
PM 25700515
ER
PT J
AU Greenberg, JA
Santos, MJ
Dobrowski, SZ
Vanderbilt, VC
Ustin, SL
AF Greenberg, Jonathan A.
Santos, Maria J.
Dobrowski, Solomon Z.
Vanderbilt, Vern C.
Ustin, Susan L.
TI Quantifying Environmental Limiting Factors on Tree Cover Using
Geospatial Data
SO PLOS ONE
LA English
DT Article
ID REGRESSION QUANTILES; CLIMATE-CHANGE; SPECIES DISTRIBUTIONS; ECOSYSTEMS;
ABUNDANCE; DENSITY; USA
AB Environmental limiting factors (ELFs) are the thresholds that determine the maximum or minimum biological response for a given suite of environmental conditions. We asked the following questions: 1) Can we detect ELFs on percent tree cover across the eastern slopes of the Lake Tahoe Basin, NV? 2) How are the ELFs distributed spatially? 3) To what extent are unmeasured environmental factors limiting tree cover? ELFs are difficult to quantify as they require significant sample sizes. We addressed this by using geospatial data over a relatively large spatial extent, where the wall-to-wall sampling ensures the inclusion of rare data points which define the minimum or maximum response to environmental factors. We tested mean temperature, minimum temperature, potential evapotranspiration (PET) and PET minus precipitation (PET-P) as potential limiting factors on percent tree cover. We found that the study area showed system-wide limitations on tree cover, and each of the factors showed evidence of being limiting on tree cover. However, only 1.2% of the total area appeared to be limited by the four (4) environmental factors, suggesting other unmeasured factors are limiting much of the tree cover in the study area. Where sites were near their theoretical maximum, non-forest sites (tree cover <25%) were primarily limited by coldmean temperatures, open-canopy forest sites (tree cover between 25% and 60%) were primarily limited by evaporative demand, and closed-canopy forests were not limited by any particular environmental factor. The detection of ELFs is necessary in order to fully understand the width of limitations that species experience within their geographic range.
C1 [Greenberg, Jonathan A.] Univ Illinois, Dept Geog & Geog Informat Sci, Champaign, IL 61820 USA.
[Santos, Maria J.] Univ Utrecht, Dept Innovat Environm & Energy Sci, Utrecht, Netherlands.
[Dobrowski, Solomon Z.] Univ Montana, Coll Forestry & Conservat, Dept Forest Management, Missoula, MT 59812 USA.
[Vanderbilt, Vern C.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Ustin, Susan L.] Univ Calif Davis, CSTARS, Dept Land Air & Water Resources, Davis, CA 95616 USA.
RP Greenberg, JA (reprint author), Univ Illinois, Dept Geog & Geog Informat Sci, Champaign, IL 61820 USA.
EM jgm@illinois.edu
RI Santos, Maria/H-6391-2015;
OI Santos, Maria/0000-0002-6558-7477; Greenberg,
Jonathan/0000-0001-8435-9077
NR 35
TC 2
Z9 2
U1 1
U2 13
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 FEB 18
PY 2015
VL 10
IS 2
AR e0114648
DI 10.1371/journal.pone.0114648
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CC0WZ
UT WOS:000350061500006
PM 25692604
ER
PT J
AU Schopf, JW
Kudryavtsev, AB
Walter, MR
Van Kranendonk, MJ
Williford, KH
Kozdon, R
Valley, JW
Gallardo, VA
Espinoza, C
Flannery, DT
AF Schopf, J. William
Kudryavtsev, Anatoliy B.
Walter, Malcolm R.
Van Kranendonk, Martin J.
Williford, Kenneth H.
Kozdon, Reinhard
Valley, John W.
Gallardo, Victor A.
Espinoza, Carola
Flannery, David T.
TI Sulfur-cycling fossil bacteria from the 1.8-Ga Duck Creek Formation
provide promising evidence of evolution's null hypothesis
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Great Oxidation Event; microbial evolution; null hypothesis; Precambrian
microorganisms; sulfur bacteria
ID GREAT OXIDATION EVENT; WESTERN-AUSTRALIA; ATMOSPHERIC OXYGEN;
THIOVULUM-MAJUS; IRON-FORMATION; MICROFOSSILS; OCEAN; PHOTOSYNTHESIS;
MICROORGANISMS; DOLOMITE
AB The recent discovery of a deep-water sulfur-cycling microbial biota in the similar to 2.3-Ga Western Australian Turee Creek Group opened a new window to life's early history. We now report a second such subseafloor-inhabiting community from the Western Australian 1.8-Ga Duck Creek Formation. Permineralized in cherts formed during and soon after the 2.4- to 2.2-Ga "Great Oxidation Event," these two biotas may evidence an opportunistic response to the mid-Precambrian increase of environmental oxygen that resulted in increased production of metabolically useable sulfate and nitrate. The marked similarity of microbial morphology, habitat, and organization of these fossil communities to their modern counterparts documents exceptionally slow (hypobradytelic) change that, if paralleled by their molecular biology, would evidence extreme evolutionary stasis.
C1 [Schopf, J. William] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.] Univ Calif Los Angeles, Ctr Study Evolut & Origin Life, Los Angeles, CA 90095 USA.
[Schopf, J. William] Univ Calif Los Angeles, Inst Mol Biol, Los Angeles, CA 90095 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Schopf, J. William; Kudryavtsev, Anatoliy B.; Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Astrobiol Res Consortium, Madison, WI 53706 USA.
[Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Walter, Malcolm R.; Van Kranendonk, Martin J.; Flannery, David T.] Univ New S Wales, Australian Ctr Astrobiol, Randwick, NSW 2052, Australia.
[Walter, Malcolm R.] Univ New S Wales, Sch Biotechnol & Biomol Sci, Randwick, NSW 2052, Australia.
[Van Kranendonk, Martin J.] Univ New S Wales, Sch Biol Earth & Environm Sci, Randwick, NSW 2052, Australia.
[Van Kranendonk, Martin J.] Univ New S Wales, Australian Res Council, Ctr Excellence Core Crust Fluid Syst, Randwick, NSW 2052, Australia.
[Williford, Kenneth H.; Flannery, David T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gallardo, Victor A.; Espinoza, Carola] Univ Concepcion, Fac Ciencias Nat & Oceanog, Dept Oceanog, Concepcion, Chile.
RP Schopf, JW (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
EM schopf@ess.ucla.edu
RI Kozdon, Reinhard/J-9468-2014
OI Kozdon, Reinhard/0000-0001-6347-456X
FU Fondo Nacional de Desarrollo Cientifico y Tecnologico [1070552,
1110786]; International Census of Marine Microbes; UCLA Center for the
Study of Evolution; Origin of Life; Penn State Astrobiology Research
Center; Australian Research Council Discovery [DP1093106]; International
Commission of Stratigraphy; University of New South Wales; University of
Wisconsin Astrobiology Research Consortium; NASA Astrobiology Institute;
NASA
FX We thank J. Shen-Miller, A. K. Garcia, and S. Loyd for reviews of a
draft of this manuscript; Thomas N. Taylor for serving as editor of this
contribution; and Bo Barker Jorgensen, Timothy W. Lyons, and two
anonymous referees for helpful comments on the manuscript submitted.
J.W.S. and M.R.W. thank their colleagues in the Precambrian Paleobiology
Research Group for collection of the samples studied and acknowledge
particularly the late H. J. Hofmann, who, with J.W.S., was first to
investigate fossil-bearing cherts from the studied localities. V.A.G.
and C.E. thank A. Fonseca and N. Ruiz-Tagle for contributing to data
analysis and Fondo Nacional de Desarrollo Cientifico y Tecnologico
(Projects 1070552 and 1110786) and the project International Census of
Marine Microbes. A.B.K. was supported by the UCLA Center for the Study
of Evolution and the Origin of Life and the Penn State Astrobiology
Research Center. M.R.W. acknowledges support by Australian Research
Council Discovery Grant DP1093106. M.J.V.K. acknowledges support by the
International Commission of Stratigraphy and the University of New South
Wales. K.H.W., R.K., and J.W.V. were supported by the University of
Wisconsin Astrobiology Research Consortium, funded by the NASA
Astrobiology Institute. For his current work at Jet Propulsion
Laboratory, K.H.W. acknowledges a grant from NASA.
NR 48
TC 14
Z9 14
U1 0
U2 21
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 FEB 17
PY 2015
VL 112
IS 7
BP 2087
EP 2092
DI 10.1073/pnas.1419241112
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CB2GV
UT WOS:000349446000065
PM 25646436
ER
PT J
AU Shume, EB
Komjathy, A
Langley, RB
Verkhoglyadova, O
Butala, MD
Mannucci, AJ
AF Shume, E. B.
Komjathy, A.
Langley, R. B.
Verkhoglyadova, O.
Butala, M. D.
Mannucci, A. J.
TI Intermediate-scale plasma irregularities in the polar ionosphere
inferred from GPS radio occultation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE polar ionosphere; plasma irregularities; radio occultation; spectral
analysis; scintillation
ID SOLAR MINIMUM; SCINTILLATION; IONIZATION; BOUNDARY; PHASE
AB We report intermediate-scale plasma irregularities in the polar ionosphere inferred from high-resolution radio occultation (RO) measurements using GPS (Global Positioning System) to CASSIOPE (CAScade Smallsat and IOnospheric Polar Explorer) satellite radio links. The high inclination of CASSIOPE and the high rate of signal reception by the GPS Attitude, Positioning, and Profiling RO receiver on CASSIOPE enable a high-resolution investigation of the dynamics of the polar ionosphere with unprecedented detail. Intermediate-scale, scintillation-producing irregularities, which correspond to 1 to 40km scales, were inferred by applying multiscale spectral analysis on the RO phase measurements. Using our multiscale spectral analysis approach and satellite data (Polar Operational Environmental Satellites and Defense Meteorological Satellite Program), we discovered that the irregularity scales and phase scintillations have distinct features in the auroral oval and polar cap. We found that large length scales and more intense phase scintillations are prevalent in the auroral oval compared to the polar cap implying that the irregularity scales and phase scintillation characteristics are a function of the solar wind and magnetospheric forcings.
C1 [Shume, E. B.; Komjathy, A.; Verkhoglyadova, O.; Butala, M. D.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Komjathy, A.; Langley, R. B.] Univ New Brunswick, Geodet Res Lab, Fredericton, NB, Canada.
RP Shume, EB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Esayas.B.Shume@jpl.nasa.gov
RI NASA MMS, Science Team/J-5393-2013;
OI NASA MMS, Science Team/0000-0002-9504-5214; Verkhoglyadova,
Olga/0000-0002-9295-9539
FU NASA; Geodetic Imaging program [NNH10ZDA001N-GEOIM]; Natural Sciences
and Engineering Research Council (NSERC) of Canada
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. The
authors would like to thank NASA Headquarters, the NASA ROSES 2010/A.21
Application of Geodetic Imaging program (NNH10ZDA001N-GEOIM). R.B.L.
acknowledges financial support from the Natural Sciences and Engineering
Research Council (NSERC) of Canada. The Canadian Space Agency, NSERC,
and the University of Calgary supported development of the GAP
instrument and the archiving and distribution of GAP data
(sftpepopdata@esoc-sdpc.phys.ucalgary.ca). The OMNI data (IMF
BZ) were obtained from the GSFC/SPDF
(http://omniweb.gsfc.nasa.gov), and the Dst and AE indices from the
World Data Center for Geomagnetism, Kyoto University
(http://swdcwww.kugi.kyoto-u.ac.jp). The POES particle data were
provided by the NGDC (http://www.ngdc.noaa.gov). The DMSP data for
identification of auroral boundaries were downloaded from
ftp://ghrc.nsstc.nasa.gov/pub/ssmis/.
NR 21
TC 3
Z9 3
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 16
PY 2015
VL 42
IS 3
BP 688
EP 696
DI 10.1002/2014GL062558
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CD8OT
UT WOS:000351355600003
ER
PT J
AU Carn, SA
Yang, K
Prata, AJ
Krotkov, NA
AF Carn, S. A.
Yang, K.
Prata, A. J.
Krotkov, N. A.
TI Extending the long-term record of volcanic SO2 emissions with the Ozone
Mapping and Profiler Suite nadir mapper
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE remote sensing; volcanology; sulfur dioxide; Paluweh volcano
ID STRATOSPHERIC AEROSOL LAYER; SULFUR-DIOXIDE; SPECTROMETER; CLIMATE;
INSTRUMENTS; SATELLITE; CLOUD
AB Uninterrupted, global space-based monitoring of volcanic sulfur dioxide (SO2) emissions is critical for climate modeling and aviation hazard mitigation. We report the first volcanic SO2 measurements using ultraviolet (UV) Ozone Mapping and Profiler Suite (OMPS) nadir mapper data. OMPS was launched on the Suomi National Polar-orbiting Partnership satellite in October 2011. We demonstrate the sensitivity of OMPS SO2 measurements by quantifying SO2 emissions from the modest eruption of Paluweh volcano (Indonesia) in February 2013 and tracking the dispersion of the volcanic SO2 cloud. The OMPS SO2 retrievals are validated using Ozone Monitoring Instrument and Atmospheric Infrared Sounder measurements. The results confirm the ability of OMPS to extend the long-term record of volcanic SO2 emissions based on UV satellite observations. We also show that the Paluweh volcanic SO2 reached the lower stratosphere, further demonstrating the impact of small tropical volcanic eruptions on stratospheric aerosol optical depth and climate.
C1 [Carn, S. A.] Michigan Technol Univ, Dept Geol & Mining Engn & Sci, Houghton, MI 49931 USA.
[Carn, S. A.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Prata, A. J.] Norwegian Inst Air Res, Atmosphere & Climate Dept, Kjeller, Norway.
[Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Armospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
RP Carn, SA (reprint author), Michigan Technol Univ, Dept Geol & Mining Engn & Sci, Houghton, MI 49931 USA.
EM scarn@mtu.edu
RI Krotkov, Nickolay/E-1541-2012
OI Krotkov, Nickolay/0000-0001-6170-6750
FU NASA [NNX11AK95G, NNX13AF50G]
FX We acknowledge NASA's support for this work through grants NNX11AK95G
(Continuation of Long-Term Sulfur Dioxide EDR with the SNPP/OMPS NM) and
NNX13AF50G (Multidecadal Sulfur Dioxide Climatology from Satellite
Instruments). We thank the NASA-funded SNPP Ozone Product Evaluation and
Algorithm Test Element for providing OMPS Level 1B data and gratefully
acknowledge the NOAA Air Resources Laboratory for the provision of the
HYSPLIT transport and dispersion model and/or READY website
(http://www.ready.noaa.gov) used in this publication. Two anonymous
reviewers provided thorough reviews that greatly improved the final
paper. All satellite data used in this paper can either be accessed for
free at the NASA data centers listed herein (AIRS, OMI, CALIOP, and MLS)
or can be obtained from the corresponding author (OMPS-NM).
NR 33
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U1 2
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 16
PY 2015
VL 42
IS 3
BP 925
EP 932
DI 10.1002/2014GL062437
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CD8OT
UT WOS:000351355600032
ER
PT J
AU Saide, PE
Spak, SN
Pierce, RB
Otkin, JA
Schaack, TK
Heidinger, AK
da Silva, AM
Kacenelenbogen, M
Redemann, J
Carmichael, GR
AF Saide, P. E.
Spak, S. N.
Pierce, R. B.
Otkin, J. A.
Schaack, T. K.
Heidinger, A. K.
da Silva, A. M.
Kacenelenbogen, M.
Redemann, J.
Carmichael, G. R.
TI Central American biomass burning smoke can increase tornado severity in
the US
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE aerosol-cloud radiation interactions; severe weather prediction; AOD
data assimilation; WRF-Chem; GSI; smoke
ID RAPID UPDATE CYCLE; BLACK CARBON; ASSIMILATION SYSTEM; CLOUD
MICROPHYSICS; HAILSTORMS REST; AEROSOL IMPACTS; PRECIPITATION; MODEL;
SUPERCELL; ACTIVATION
AB Tornadoes in the Southeast and central U.S. are episodically accompanied by smoke from biomass burning in central America. Analysis of the 27 April 2011 historical tornado outbreak shows that adding smoke to an environment already conducive to severe thunderstorm development can increase the likelihood of significant tornado occurrence. Numerical experiments indicate that the presence of smoke during this event leads to optical thickening of shallow clouds while soot within the smoke enhances the capping inversion through radiation absorption. The smoke effects are consistent with measurements of clouds and radiation before and during the outbreak. These effects result in lower cloud bases and stronger low-level wind shear in the warm sector of the extratropical cyclone generating the outbreak, two indicators of higher probability of tornadogenesis and tornado intensity and longevity. These mechanisms may contribute to tornado modulation by aerosols, highlighting the need to consider aerosol feedbacks in numerical severe weather forecasting.
C1 [Saide, P. E.; Spak, S. N.; Carmichael, G. R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
[Pierce, R. B.; Heidinger, A. K.] NOAA, Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res, Madison, WI USA.
[Otkin, J. A.; Schaack, T. K.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
[da Silva, A. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Data Assimilat Off, Greenbelt, MD 20771 USA.
[Kacenelenbogen, M.] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94035 USA.
[Redemann, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Saide, PE (reprint author), Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
EM pablo-saide@uiowa.edu; gcarmich@engineering.uiowa.edu
RI Spak, Scott/B-7331-2008; Otkin, Jason/D-1737-2012; Pierce, Robert
Bradley/F-5609-2010; Heidinger, Andrew/F-5591-2010
OI Spak, Scott/0000-0002-8545-1411; Otkin, Jason/0000-0003-4034-7845;
Pierce, Robert Bradley/0000-0002-2767-1643; Heidinger,
Andrew/0000-0001-7631-109X
FU NASA [NNX08AL05G, NNX11AI52G]; EPA [83503701]; National Center for
Research Resources (NCRR) [UL1RR024979]; National Institutes of Health
(NIH); Fulbright-CONICYT scholarship [15093810]; NOAA CIMSS under GOES-R
Risk Reduction [NA10NES4400013]; GOES-R Algorithm Working Group program
FX We thank Robert Rabin, Jack Kain, and multiple anonymous reviewers for
their comments that helped improve the study. We also thank Bill Gibson,
Alan Weidemann, and their staff for establishing and maintaining the
WaveCIS AERONET site used in this investigation. CALIPSO and MODIS data
were obtained from the NASA Langley Research Center Atmospheric Science
Data Center. This work was carried out with the aid of NASA grants
NNX08AL05G and NNX11AI52G, EPA grant 83503701, grant UL1RR024979 from
the National Center for Research Resources (NCRR), a part of the
National Institutes of Health (NIH), and Fulbright-CONICYT scholarship
15093810. J.A.O. was supported by NOAA CIMSS grant NA10NES4400013 under
the GOES-R Risk Reduction and GOES-R Algorithm Working Group programs.
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, U.S. Government, and other
funding institutions position, policy, or decision. Contact P.E. Saide
(pablo-saide@uiowa.edu) or G.R. Carmichael
(gregory-carmichael@uiowa.edu) for data and code requests.
NR 66
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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 FEB 16
PY 2015
VL 42
IS 3
BP 956
EP 965
DI 10.1002/2014GL062826
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CD8OT
UT WOS:000351355600036
ER
PT J
AU Tan, J
Jakob, C
Lane, TP
AF Tan, Jackson
Jakob, Christian
Lane, Todd P.
TI The consequences of a local approach in statistical models of convection
on its large-scale coherence
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE convection; organisation; statistical model; cloud regimes; weather
states; coherence
ID TROPICAL WESTERN PACIFIC; CLOUD REGIMES; DEEP CONVECTION; WEATHER
STATES; ENSEMBLE PREDICTION; MULTICLOUD MODEL; CLIMATE MODELS;
PARAMETERIZATION; PRECIPITATION; CIRCULATION
AB Organized tropical convection is a crucial mechanism in the climate system, but its representation in climate models through parametrization schemes has numerous shortcomings. One of these shortcomings is that they are deterministic despite the statistical nature of the relationship they are representing. Several attempts at devising a stochastic parametrization scheme have been made, many of which assume a local approach, that is, one in which the convection in a grid box is determined without consideration of the previous time steps and the surrounding boxes. This study seeks to explore the effect of this assumption on the coherence of convection using cloud regimes, which represent various modes of tropical convection. First, we analyze the coherence of observed convection beyond the typical size of a model grid box and time step. Then, we evaluate the consequences of the local assumption on this coherence in simple statistical models. Cloud regimes in the real world show high degrees of coherence, manifesting in their lifetimes, areas, and inter-regime relationships. However, in a local statistical model, they are too small, too short-lived, and have incorrect relationships between each other. This can be improved by incorporating time memory and spatial dependence in the modeling. Our results imply that a local approach to a statistical representation of convection is not viable, and a statistical model must account for nonlocal influence in order to have large-scale convective coherence that more closely resembles the real world.
C1 [Tan, Jackson; Jakob, Christian] Monash Univ, ARC Ctr Excellence Climate Syst Sci, Melbourne, Vic 3004, Australia.
[Tan, Jackson; Jakob, Christian] Monash Univ, Sch Earth Atmosphere & Environm, Melbourne, Vic 3004, Australia.
[Lane, Todd P.] Univ Melbourne, ARC Ctr Excellence Climate Syst Sci, Melbourne, Vic, Australia.
[Lane, Todd P.] Univ Melbourne, Sch Earth Sci, Melbourne, Vic, Australia.
RP Tan, J (reprint author), NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
EM jackson.tan@nasa.gov
RI Lane, Todd/A-8804-2011; Jakob, Christian/A-1082-2010;
OI Lane, Todd/0000-0003-0171-6927; Jakob, Christian/0000-0002-5012-3207;
Tan, Jackson/0000-0001-7085-3074
FU Australian Research Council Centre of Excellence for Climate System
Science [CE110001028]; Monash University Postgraduate Publication Award
FX The authors thank Kais Hamza and Karsten Peters for discussions on the
study and three anonymous reviewers for their helpful comments. This
project is funded under the Australian Research Council Centre of
Excellence for Climate System Science (CE110001028). J. T. acknowledges
support from Monash University Postgraduate Publication Award. Data and
codes pertaining to this paper can be obtained by contacting the
corresponding author (jackson.tan@nasa.gov).
NR 56
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U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 16
PY 2015
VL 120
IS 3
BP 931
EP 944
DI 10.1002/2014JD022680
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC7KT
UT WOS:000350547000004
ER
PT J
AU Boisvert, LN
Wu, DL
Vihma, T
Susskind, J
AF Boisvert, L. N.
Wu, D. L.
Vihma, T.
Susskind, J.
TI Verification of air/surface humidity differences from AIRS and
ERA-Interim in support of turbulent flux estimation in the Arctic
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE moisture flux; AIRS; ERA-Interim; Arctic; sea ice
ID ATMOSPHERIC BOUNDARY-LAYER; SEA-SURFACE TEMPERATURE; PROFILE
RELATIONSHIPS; HEAT-BUDGET; ICE; MODELS; CLOUD; SHEBA; OCEAN;
AMPLIFICATION
AB Evaporation from the Arctic Ocean and its marginal seas is essential for air moisture, cloudiness, and precipitation, as well as for the associated feedbacks, which contribute to the Arctic amplification of climate warming. However, evaporation in the Arctic is still associated with large uncertainties. The Boisvert et al. (2013) moisture flux scheme (BMF13) is based on application of the Atmospheric Infrared Sounder (AIRS) data, which produces high-quality, global, daily atmospheric temperature and moisture profiles even in the presence of clouds. Comparing the results of BMF13 against the ERA-Interim reanalysis, we found differences up to 55Wm(-2) in the surface latent heat flux in the Beaufort-East Siberian Seas (BESS). We found out that the quality of the input data for the BMF13 and ERA-Interim flux schemes was the main cause for the differences. Differences in the input data sets cause moisture flux estimates to differ up to 1.6x10(-2)gm(-2)s(-1) (40Wm(-2) latent heat flux) in the BESS region, when both data sets were applied to the BMF13 scheme. Thus, the input data sets, AIRS version 6 and ERA-Interim reanalysis, were compared with a variety of in situ data. In skin temperature ERA-Interim had twice as large an error as AIRS version 6, but smaller errors in air specific humidity. The results suggested that AIRS data and the BMF13 scheme are a good option to estimate the moisture flux in the Arctic. However, the differences detected demonstrate a need for more in situ measurements of air temperature and humidity in the Arctic.
C1 [Boisvert, L. N.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Wu, D. L.; Susskind, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vihma, T.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
RP Boisvert, LN (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM linette.n.boisvert@nasa.gov
RI Wu, Dong/D-5375-2012
FU Earth System Science Interdisciplinary Center (ESSIC) [683]; NASA-ROSES
IDS [12-IDS12-0120]; Academy of Finland [259537, 283101]
FX We thank Timo Palo, Erko Jakobson, and Jaak Jaagus from the University
of Tartu, Estonia, for providing us with the Tara observations. The work
of Linette Boisvert was supported by the Earth System Science
Interdisciplinary Center (ESSIC) Task 683. Support for the work of Dong
Wu was provided by NASA-ROSES 2012 IDS proposal: 12-IDS12-0120. The work
of Timo Vihma was supported by the Academy of Finland (contracts 259537
and 283101). The moisture flux data are available from Linette Boisvert
(linette.n.boisvert@nasa.gov). The authors would also like to thank the
three anonymous reviewers for their helpful feedback and suggestions and
John Bliasdell for his discussions of the AIRS data.
NR 55
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U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 16
PY 2015
VL 120
IS 3
BP 945
EP 963
DI 10.1002/2014JD021666
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC7KT
UT WOS:000350547000005
ER
PT J
AU Boylan, P
Wang, JH
Cohn, SA
Fetzer, E
Maddy, ES
Wong, S
AF Boylan, Patrick
Wang, Junhong
Cohn, Stephen A.
Fetzer, Eric
Maddy, Eric S.
Wong, Sun
TI Validation of AIRS version 6 temperature profiles and surface-based
inversions over Antarctica using Concordiasi dropsonde data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE surface-based inversions; AIRS; antarctica; dropsonde; temperature
inversions; condordiasi
ID SOUTH-POLE; MASS-BALANCE; PRODUCTS; CLIMATE; ICE; GREENLAND; STRENGTH;
PLATEAU; SOUNDER; CLOUDS
AB During the 2010 Concordiasi field experiment, 635 dropsondes were released from the lower stratosphere providing in situ atmospheric profiles from the release height (similar to 60hPa) to the surface over Antarctica. They provide a unique data set of high vertical resolution temperature profiles over the entire Antarctic continent and surrounding ocean. This study uses temperature profiles and derived surface-based inversion (SBI) properties from the sonde data set to evaluate Atmospheric Infrared Sounder (AIRS) versions 5 (v5) and 6 (v6) temperature profiles. A total of 1486 matched pairs of profiles are available for analysis. The AIRS averaging kernel, representing the AIRS measurement sensitivity, is applied to the dropsonde profiles. The AIRS data are compared to kernel-averaged dropsonde profiles and found, on average, to have a small cold bias (similar to 0.5 degrees C) (for v6) in the troposphere. AIRS v6 is improved over v5 with both profile-averaged bias and root-mean-square errors reduced by over 25%. Compared to the kernel-averaged dropsonde profiles, AIRS v6 accurately detects the existence of SBIs in 79% of the profiles and agrees on the inversion depth 79% of the time. AIRS correctly identifies SBIs in 59% of cases when compared to the full-resolution sonde. AIRS systematically underestimates the SBI intensity. This is due to warmer reported AIRS surface air temperatures (T-a) than T-a measured with the dropsonde. Replacement of AIRS T-a with that measured by the dropsonde improves the agreement in both SBI detection and intensity. If AIRS T-a could be improved, AIRS has the potential to be a stand-alone SBI detection tool over Antarctica.
C1 [Boylan, Patrick; Cohn, Stephen A.] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA.
[Wang, Junhong] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
[Fetzer, Eric; Wong, Sun] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Maddy, Eric S.] Riverside Technol Inc, NOAA, NESDIS, JCSDA, College Pk, MD USA.
RP Boylan, P (reprint author), Natl Ctr Atmospher Res, Earth Observing Lab, POB 3000, Boulder, CO 80307 USA.
EM boylan@ucar.edu
RI Maddy, Eric/G-3683-2010
OI Maddy, Eric/0000-0003-1151-339X
FU NSF [ANT-0733007]; National Science Foundation
FX This project is supported by NSF project ANT-0733007. The National
Center for Atmospheric Research is sponsored by the National Science
Foundation. We would like to thank Minghui Diao, Jordan Powers, and
Andrew Gettelman for their insightful comments. The dropsonde data are
available at https://www.eol.ucar.edu/field_projects/concordiasi. The
AIRS data products are available at
http://disc.sci.gsfc.nasa.gov/AIRS/data-holdings/by-data-product-V6. Any
opinions, findings, and conclusions or recommendations expressed in this
publication are those of the authors and do not necessarily reflect the
views of the National Science Foundation.
NR 54
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U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 16
PY 2015
VL 120
IS 3
BP 992
EP 1007
DI 10.1002/2014JD022551
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC7KT
UT WOS:000350547000008
ER
PT J
AU Banda, N
Krol, M
van Noije, T
van Weele, M
Williams, JE
Le Sager, P
Niemeier, U
Thomason, L
Rockmann, T
AF Banda, Narcisa
Krol, Maarten
van Noije, Twan
van Weele, Michiel
Williams, Jason E.
Le Sager, Philippe
Niemeier, Ulrike
Thomason, Larry
Rockmann, Thomas
TI The effect of stratospheric sulfur from Mount Pinatubo on tropospheric
oxidizing capacity and methane
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE volcanic eruption; Pinatubo; OH; UV radiation; oxidizing capacity;
methane
ID LARGE VOLCANIC-ERUPTIONS; MODIFIED BAND APPROACH; CLIMATE MODEL;
MT-PINATUBO; NORTHERN-HEMISPHERE; ATMOSPHERIC METHANE; METHYL
CHLOROFORM; PHOTOLYSIS RATES; GROWTH-RATE; EL-CHICHON
AB The eruption of Mount Pinatubo in 1991 injected a large amount of SO2 into the stratosphere, which formed sulfate aerosols. Increased scattering and absorption of UV radiation by the enhanced stratospheric SO2 and aerosols decreased the amount of UV radiation reaching the troposphere, causing changes in tropospheric photochemistry. These changes affected the oxidizing capacity of the atmosphere and the removal rate of CH4 in the years following the eruption. We use the three-dimensional chemistry transport model TM5 coupled to the aerosol microphysics module M7 to simulate the evolution of SO2 and sulfate aerosols from the Pinatubo eruption. Their effect on tropospheric photolysis frequencies and concentrations of OH and CH4 is quantified for the first time. We find that UV attenuation by stratospheric sulfur decreased the photolysis frequencies of both ozone and NO2 by about 2% globally, decreasing global OH concentrations by a similar amount in the first 2 years after the eruption. SO2 absorption mainly affects OH primary production by ozone photolysis, while aerosol scattering also alters OH recycling. The effect of stratospheric sulfur on global OH and CH4 is dominated by the effect of aerosol extinction, while SO2 absorption contributes by 12.5% to the overall effect in the first year after the eruption. The reduction in OH concentrations causes an increase in the CH4 growth rate of 4 and 2 ppb/yr in the first and second years after the eruption, respectively, contributing 11 Tg to the 27 Tg observed CH4 burden change in late 1991 and early 1992.
C1 [Banda, Narcisa; Krol, Maarten; Rockmann, Thomas] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands.
[Banda, Narcisa; van Noije, Twan; van Weele, Michiel; Williams, Jason E.; Le Sager, Philippe] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Krol, Maarten] Univ Wageningen & Res Ctr, Meteorol & Air Qual, Wageningen, Netherlands.
[Krol, Maarten] Netherlands Inst Space Res SRON, Utrecht, Netherlands.
[Niemeier, Ulrike] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[Thomason, Larry] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Banda, N (reprint author), Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands.
EM n.l.banda@uu.nl
RI Rockmann, Thomas/F-4479-2015; Krol, Maarten/E-3414-2013;
OI Rockmann, Thomas/0000-0002-6688-8968; Thomason,
Larry/0000-0002-1902-0840
FU Netherlands Organisation for Scientific Research (NWO); EU FP7
Integrated Project PEGASOS
FX This work was supported by the Netherlands Organisation for Scientific
Research (NWO) and the EU FP7 Integrated Project PEGASOS. We thank
SURFsara (www.surfsara.nl) for the support in using the Dutch national
supercomputer Cartesius. We would like to thank the anonymous reviewers
for their helpful and constructive comments. AVHRR data used in this
study were obtained from NOAA's National Climatic Data Center
(http://www.ncdc.noaa.gov). Model output presented in this paper is
available upon request from the corresponding author.
NR 77
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U1 3
U2 28
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 FEB 16
PY 2015
VL 120
IS 3
BP 1202
EP 1220
DI 10.1002/2014JD022137
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC7KT
UT WOS:000350547000020
ER
PT J
AU Greenhouse, MA
Benson, SW
Englander, J
Falck, RD
Fixsen, DJ
Gardner, JP
Kruk, JW
Oleson, SR
Thronson, HA
AF Greenhouse, Matthew A.
Benson, Scott W.
Englander, Jacob
Falck, Robert D.
Fixsen, Dale J.
Gardner, Jonathan P.
Kruk, Jeffrey W.
Oleson, Steven R.
Thronson, Harley A.
TI Breakthrough capability for UVOIR space astronomy: Reaching the darkest
sky
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Solar electric propulsion; Zodiacal light; Space astronomy
ID COBE
AB We describe how availability of new solar electric propulsion (SEP) technology can substantially increase the science capability of space astronomy missions working within the near-UV to far-infrared (UVOIR) spectrum by making dark sky orbits accessible for the first time. We present a proof of concept case study in which SEP is used to enable a 700 kg Explorer-class observatory payload to reach an orbit beyond where the zodiacal dust limits observatory sensitivity. The resulting scientific performance advantage relative to a Sun-Earth L2 point orbit is presented and discussed. We find that making SEP available to astrophysics Explorers can enable this small payload program to rival the science performance of much larger long development-time systems. We also present flight dynamics analysis which illustrates that this concept can be extended beyond Explorers to substantially improve the sensitivity performance of heavier (7000 kg) flagship-class astrophysics payloads such as the UVOIR successor to the James Webb Space Telescope by using high power SEP that is being developed for the Asteroid Redirect Robotics Mission. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Greenhouse, Matthew A.; Englander, Jacob; Gardner, Jonathan P.; Kruk, Jeffrey W.; Thronson, Harley A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Benson, Scott W.; Falck, Robert D.; Oleson, Steven R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Fixsen, Dale J.] Univ Maryland, College Pk, MD 20742 USA.
RP Greenhouse, MA (reprint author), NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Mail Code 443-2, Greenbelt, MD 20771 USA.
EM matt.greenhouse@nasa.gov
FU NASA Goddard Space Flight Center; NASA Glenn Research Center; Glenn
COMPASS team
FX This work was supported by internal research and development funding of
the NASA Goddard Space Flight Center and the NASA Glenn Research Center.
We thank the Glenn COMPASS team for extensive engineering analysis and
support.
NR 16
TC 0
Z9 0
U1 2
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 15
PY 2015
VL 55
IS 4
BP 1222
EP 1233
DI 10.1016/j.asr.2014.11.007
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CB4AP
UT WOS:000349570900019
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI Einstein's Dice and Schrodinger's Cat: How Two Great Minds Battled
Quantum Randomness To Create a Unified Theory of Physics.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
NR 1
TC 0
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U1 1
U2 3
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD FEB 15
PY 2015
VL 140
IS 3
BP 125
EP 125
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA CB5EQ
UT WOS:000349650700248
ER
PT J
AU Blanchard, M
Dauphas, N
Hu, MY
Roskosz, M
Alp, EE
Golden, DC
Sio, CK
Tissot, FLH
Zhao, J
Gao, L
Morris, RV
Fornace, M
Floris, A
Lazzeri, M
Balan, E
AF Blanchard, M.
Dauphas, N.
Hu, M. Y.
Roskosz, M.
Alp, E. E.
Golden, D. C.
Sio, C. K.
Tissot, F. L. H.
Zhao, J.
Gao, L.
Morris, R. V.
Fornace, M.
Floris, A.
Lazzeri, M.
Balan, E.
TI Reduced partition function ratios of iron and oxygen in goethite
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID NUCLEAR RESONANT SCATTERING; ISOTOPE FRACTIONATION FACTORS;
DENSITY-OF-STATES; MOSSBAUER-SPECTROSCOPY; SYNCHROTRON-RADIATION;
CRYSTAL-STRUCTURE; AQUEOUS FE(II); EQUILIBRIUM; HEMATITE; WATER
AB First-principles calculations based on the density functional theory (DFT) with or without the addition of a Hubbard U correction, are performed on goethite in order to determine the iron and oxygen reduced partition function ratios (beta-factors). The calculated iron phonon density of states (pDOS), force constant and beta-factor are compared with reevaluated experimental beta-factors obtained from Nuclear Resonant Inelastic X-ray Scattering (NRIXS) measurements. The reappraisal of old experimental data is motivated by the erroneous previous interpretation of the low- and high-energy ends of the NRIXS spectrum of goethite and jarosite samples (Dauphas et al., 2012). Here the NRIXS data are analyzed using the SciPhon software that corrects for non-constant baseline. New NRIXS measurements also demonstrate the reproducibility of the results. Unlike for hematite and pyrite, a significant discrepancy remains between DFT, NRIXS and the existing Mossbauer-derived data. Calculations suggest a slight overestimation of the NRIXS signal possibly related to the baseline definition. The intrinsic features of the samples studied by NRIXS and Mossbauer spectroscopy may also contribute to the discrepancy (e. g., internal structural and/or chemical defects, microstructure, surface contribution). As for oxygen, DFT results indicate that goethite and hematite have similar beta-factors, which suggests almost no fractionation between the two minerals at equilibrium. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Blanchard, M.; Lazzeri, M.; Balan, E.] Univ Paris 06, Sorbonne Univ, Inst Mineral Phys Mat & Cosmochim, Museum Natl Hist Nat,UMR CNRS 7590,IRD UMR 206, F-75005 Paris, France.
[Dauphas, N.; Sio, C. K.; Tissot, F. L. H.; Fornace, M.] Univ Chicago, Dept Geophys Sci, Origins Lab, Chicago, IL 60637 USA.
[Dauphas, N.; Sio, C. K.; Tissot, F. L. H.; Fornace, M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hu, M. Y.; Alp, E. E.; Zhao, J.; Gao, L.] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA.
[Roskosz, M.] Univ Lille 1, Unite Mat & Transformat, CNRS UMR 8207, F-59655 Villeneuve Dascq, France.
[Golden, D. C.] Engn & Sci Contract Grp Hamilton Sundstrand, Houston, TX USA.
[Morris, R. V.] NASA, Johnson Space Ctr, Houston, TX USA.
[Floris, A.] Kings Coll London, Dept Phys, London WC2R 2LS, England.
RP Blanchard, M (reprint author), Univ Paris 06, Sorbonne Univ, Inst Mineral Phys Mat & Cosmochim, Museum Natl Hist Nat,UMR CNRS 7590,IRD UMR 206, 4 Pl Jussieu, F-75005 Paris, France.
EM marc.blanchard@impmc.upmc.fr
RI Blanchard, Marc/A-8698-2013; Floris, Andrea/L-5389-2013; BALAN,
Etienne/B-1149-2013; Floris, Andrea /D-7081-2013; Lazzeri,
Michele/N-7615-2016
OI Floris, Andrea/0000-0002-3160-6676; Floris, Andrea /0000-0002-3160-6676;
Lazzeri, Michele/0000-0002-6644-6617
FU GENCI-IDRIS [2014-i2014041519]; French National Research Agency (ANR,
project "CrIMin") [11-JS56-001]; French National Research Agency (ANR,
project "FrIHIDDA") [2011JS56 004 01]; NSF [EAR 1144429]; NASA
[NNX12AH60G]; U.S. DOE [DE-AC02-06CH11357]
FX L. Paulatto is acknowledged for his technical support to the
computational work. This work was performed using HPC resources from
GENCI-IDRIS (Grant 2014-i2014041519). This work has been supported by
the French National Research Agency (ANR, projects 11-JS56-001 "CrIMin"
and 2011JS56 004 01 "FrIHIDDA"), grants from NSF (EAR 1144429) and NASA
(NNX12AH60G). Use of the Advanced Photon Source, an Office of Science
User Facility operated for the U. S. Department of Energy (DOE) Office
of Science by Argonne National Laboratory, was supported by the U.S. DOE
under Contract No. DE-AC02-06CH11357.
NR 53
TC 6
Z9 6
U1 4
U2 38
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 FEB 15
PY 2015
VL 151
BP 19
EP 33
DI 10.1016/j.gca.2014.12.006
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AZ9DK
UT WOS:000348511600002
ER
PT J
AU Desai, AR
Xu, K
Tian, H
Weishampel, P
Thom, J
Baumann, D
Andrews, AE
Cook, BD
King, JY
Kolka, R
AF Desai, Ankur R.
Xu, Ke
Tian, Hanqin
Weishampel, Peter
Thom, Jonathan
Baumann, Dan
Andrews, Arlyn E.
Cook, Bruce D.
King, Jennifer Y.
Kolka, Randall
TI Landscape-level terrestrial methane flux observed from a very tall tower
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Methane; Eddy covariance; Regional flux; Land-atmosphere
ID CARBON-DIOXIDE FLUXES; PROCESS-BASED MODEL; EDDY-COVARIANCE; NATURAL
WETLANDS; CLIMATE-CHANGE; TUNDRA ECOSYSTEM; INTEGRATED MODEL;
UNITED-STATES; NORTH-AMERICA; UPPER MIDWEST
AB Simulating the magnitude and variability of terrestrial methane sources and sinks poses a challenge to ecosystem models because the biophysical and biogeochemical processes that lead to methane emissions from terrestrial and freshwater ecosystems are, by their nature, episodic and spatially disjunct. As a consequence, model predictions of regional methane emissions based on field campaigns from short eddy covariance towers or static chambers have large uncertainties, because measurements focused on a particular known source of methane emission will be biased compared to regional estimates with regards to magnitude, spatial scale, or frequency of these emissions. Given the relatively large importance of predicting future terrestrial methane fluxes for constraining future atmospheric methane growth rates, a clear need exists to reduce spatiotemporal uncertainties. In 2010, an Ameriflux tower (US-PFa) near Park Falls, WI, USA, was instrumented with closed-path methane flux measurements at 122 m above ground in a mixed wetland-upland landscape representative of the Great Lakes region. Two years of flux observations revealed an average annual methane (CH4) efflux of 785 +/- 75 mg C-CH4 m(-2) yr(-1), compared to a mean CO2 sink of -80g C-CO2 m(-2) yr(-1), a ratio of 1% in magnitude on a mole basis. Interannual variability in methane flux was 30% of the mean flux and driven by suppression of methane emissions during dry conditions in late summer 2012. Though relatively small, the magnitude of the methane source from the very tall tower measurements was mostly within the range previously measured using static chambers at nearby wetlands, but larger than a simple scaling of those fluxes to the tower footprint. Seasonal patterns in methane fluxes were similar to those simulated in the Dynamic Land Ecosystem Model (DLEM), but magnitude depends on model parameterization and input data, especially regarding wetland extent. The model was unable to simulate short-term (sub-weekly) variability. Temperature was found to be a stronger driver of regional CH4 flux than moisture availability or net ecosystem production at the daily to monthly scale. Taken together, these results emphasize the multi-timescale dependence of drivers of regional methane flux and the importance of long, continuous time series for their characterization. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Desai, Ankur R.; Xu, Ke; Thom, Jonathan] Univ Wisconsin, Ctr Climat Res, Madison, WI 53706 USA.
[Tian, Hanqin] Auburn Univ, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA.
[Weishampel, Peter] Natl Ecol Observ Network Inc, Great Lakes Domain, Land O Lakes, WI USA.
[Baumann, Dan] US Geol Survey, Wisconsin Water Sci Ctr, Rhinelander, WI USA.
[Andrews, Arlyn E.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[King, Jennifer Y.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Kolka, Randall] US Forest Serv, USDA, No Res Stn, Grand Rapids, MI USA.
RP Desai, AR (reprint author), Univ Wisconsin, Ctr Climat Res, Madison, WI 53706 USA.
EM desai@aos.wisc.edu
RI Andrews, Arlyn/K-3427-2012; Desai, Ankur/A-5899-2008; King, Jennifer
Y./I-5986-2015; Tian, Hanqin/A-6484-2012
OI Desai, Ankur/0000-0002-5226-6041; King, Jennifer Y./0000-0003-3433-5952;
Tian, Hanqin/0000-0002-1806-4091
FU National Science Foundation (NSF) biology directorate [DEB-0845166,
DBI-1062204]; NASA NACP Project [NNG05GD51G]; USDA Forest Service
Northern Global Change program; NOAA
FX This work was supported by National Science Foundation (NSF) biology
directorate grants DEB-0845166 and DBI-1062204. We also acknowledge the
contributions of R. Strand and J. Ayers at State of Wisconsin
Educational Communications Board, K. Davis at The Pennsylvania State
University, and P. Bolstad at the University of Minnesota. Static
chamber measurements were supported by NASA NACP Project # NNG05GD51G
and the USDA Forest Service Northern Global Change program. Jonathan
Kofler and Jonathan Williams were funded by NOAA to provide site and
CO2 and CH4 profile instrument support. This
project contributes to the North American Carbon Program. Any use of
trade, firm, or product names is for descriptive purposes only and does
not imply endorsement by the U.S. Government.
NR 114
TC 6
Z9 6
U1 6
U2 53
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD FEB 15
PY 2015
VL 201
BP 61
EP 75
DI 10.1016/j.agrformet.2014.10.017
PG 15
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA AY9IN
UT WOS:000347863900007
ER
PT J
AU Aydemir, U
Zevalkink, A
Bux, S
Snyder, GJ
AF Aydemir, U.
Zevalkink, A.
Bux, S.
Snyder, G. J.
TI High temperature transport properties of BaZn2Sn2
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE Stannides; Zintl phase; Tin-flux; Crystal structure; Electronic
transport; Thermal transport
ID THERMOELECTRIC-MATERIALS; INTERMETALLIC COMPOUNDS; CRYSTAL-STRUCTURE;
TERNARY PHASES; ZN-SN; EFFICIENCY; CHEMISTRY; METAL; TIN
AB BaZn2Sn2 (space group P4/nmm, a = 4.7459(5) angstrom, c = 11.330(2) angstrom, Z = 2) crystallizes in the CaBe2Ge2 structure type with a polyanionic framework comprising alternately stacked PbO-like {ZnSn4/4} and anti-PbO-like {SnZn4/4} layers along the c-axis. BaZn2Sn2 samples were obtained by either direct solid state reaction of the elements or from a Sn-flux method in very high yield with very small amount of b-Sn as the secondary phase. The samples were characterized by powder X-ray diffraction (PXRD) and scanning electron microscopy (SEM). The chemical compositions were determined to be off-stoichiometric with Zn/Sn ratio lower than 1.0 and Sn-2 atoms in the crystal structure were found to be either loosely bonded or not bonded which might lead to an incomplete charge balance. Electrical and thermal transport measurements have been performed in the temperature range 300-773 K. BaZn2Sn2 displays the electrical resistivity of a metal (or semimetal) along with very low Seebeck coefficients and relatively high thermal conductivity. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Aydemir, U.; Snyder, G. J.] CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA.
[Aydemir, U.] Koc Univ, Dept Chem, Istanbul, Turkey.
[Zevalkink, A.; Bux, S.] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA USA.
RP Aydemir, U (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM uaydemir@caltech.edu
RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015; Aydemir,
Umut/P-8424-2015
OI Snyder, G. Jeffrey/0000-0003-1414-8682; Aydemir,
Umut/0000-0003-1164-1973
FU Scientific and Technological Research Council of Turkey; NASA Science
Missions Directorate's Radioisotope Power Systems Technology Advancement
Program; National Aeronautics and Space Administration
FX U. Aydemir acknowledges the financial assistance of The Scientific and
Technological Research Council of Turkey. This research was partially
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration and was supported by the NASA Science Missions
Directorate's Radioisotope Power Systems Technology Advancement Program.
NR 40
TC 1
Z9 1
U1 1
U2 64
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD FEB 15
PY 2015
VL 622
BP 402
EP 407
DI 10.1016/j.jallcom.2014.10.090
PG 6
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA AU6ZE
UT WOS:000345749500063
ER
PT J
AU Bansal, NP
Goldsby, JC
Rogers, RB
Susner, MA
Sumption, MD
AF Bansal, Narottam P.
Goldsby, Jon C.
Rogers, Richard B.
Susner, Michael A.
Sumption, Michael D.
TI Chemical synthesis of superconducting MgB2 nanopowder
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE MgB2; Chemical synthesis; Nanopowder; Superconductor
ID DEGRADATION; REFINEMENT
AB Superconducting MgB2 nanopowder has been synthesized through chemical reaction between lithium borohydride and magnesium hydride at relatively low temperatures. From quantitative Rietveld analysis, the average crystallite size of MgB2 powder was evaluated to be 33 nm. The superconducting transition temperature of the MgB2 nanopowder was found to be 38.8-38.9 K from magnetization and DC susceptibility measurements. Powder morphology has been evaluated by scanning electron microscopy. Published by Elsevier B.V.
C1 [Bansal, Narottam P.; Goldsby, Jon C.; Rogers, Richard B.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Susner, Michael A.; Sumption, Michael D.] Ohio State Univ, Dept Mat Sci & Engn, Ctr Superconducting & Magnet Mat, Columbus, OH 43210 USA.
RP Bansal, NP (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM Narottam.P.Bansal@nasa.gov
RI Susner, Michael/G-3275-2015; Susner, Michael/B-1666-2013; Sumption,
Mike/N-5913-2016
OI Susner, Michael/0000-0002-1211-8749; Susner,
Michael/0000-0002-1211-8749; Sumption, Mike/0000-0002-4243-8380
FU NASA
FX Thanks are due to Dr Anita Garg for SEM and Jon Mackey for technical
assistance during powder processing. Funding for this research was
provided by NASA's Fixed Wing Project.
NR 15
TC 2
Z9 2
U1 4
U2 54
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD FEB 15
PY 2015
VL 622
BP 986
EP 988
DI 10.1016/j.jallcom.2014.11.040
PG 3
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA AU6ZE
UT WOS:000345749500152
ER
PT J
AU Verkhoglyadova, OP
Zank, GP
Li, G
AF Verkhoglyadova, Olga P.
Zank, Gary P.
Li, Gang
TI A theoretical perspective on particle acceleration by interplanetary
shocks and the Solar Energetic Particle problem
SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS
LA English
DT Review
DE SEP; Particle acceleration; CME; Interplanetary shocks
ID HYDROMAGNETIC WAVE EXCITATION; EJECTION-DRIVEN SHOCKS; CORONAL MASS
EJECTIONS; FOCUSED TRANSPORT APPROACH; INTERSTELLAR PICKUP IONS; PROTON
PEAK INTENSITIES; GRADUAL SEP EVENTS; COSMIC-RAYS; CHARGED-PARTICLES;
MAGNETIC-FIELD
AB Understanding the physics of Solar Energetic Particle (SEP) events is of importance to the general question of particle energization throughout the cosmos as well as playing a role in the technologically critical impact of space weather on society. The largest, and often most damaging, events are the so-called gradual SEP events, generally associated with shock waves driven by coronal mass ejections (CMEs). We review the current state of knowledge about particle acceleration at evolving interplanetary shocks with application to SEP events that occur in the inner heliosphere. Starting with a brief outline of recent theoretical progress in the field, we focus on current observational evidence that challenges conventional models of SEP events, including complex particle energy spectra, the blurring of the distinction between gradual and impulsive events, and the difference inherent in particle acceleration at quasi-parallel and quasi-perpendicular shocks. We also review the important problem of the seed particle population and its injection into particle acceleration at a shock.
We begin by discussing the properties and characteristics of non-relativistic interplanetary shocks, from their formation close to the Sun to subsequent evolution through the inner heliosphere. The association of gradual SEP events with shocks is discussed.
Several approaches to the energization of particles have been proposed, including shock drift acceleration, diffusive shock acceleration (DSA), acceleration by large-scale compression regions, acceleration by random velocity fluctuations (sometimes known as the "pump mechanism"), and others. We review these various mechanisms briefly and focus on the DSA mechanism. Much of our emphasis will be on our current understanding of the parallel and perpendicular diffusion coefficients for energetic particles and models of plasma turbulence in the vicinity of the shock. Because of its importance both to the DSA mechanism itself and to the particle composition of SEP events, we address in some detail the injection problem. Although steady-state models can improve our understanding of the diffusive shock acceleration mechanism, SEP events are inherently time-dependent. We therefore review the time-dependent theory of DSA in some detail, including estimating possible maximum particle energies and particle escape from the shock complex. We also discuss generalizations of the diffusive transport approach to modeling particle acceleration by considering a more general description based on the focused transport equation. The escape of accelerated particles from the shock requires that their subsequent transport in the interplanetary medium be modeled and the consequence of interplanetary transport can lead to the complex spectra and compositional profiles that are observed frequently. The different approaches to particle transport in the inner heliosphere are reviewed. The various numerical models that have been developed to solve the gradual SEP problem are reviewed. Explicit comparisons of modeling results with observations of large SEP events are discussed. A summary of current progress and the outlook on the SEP problem and remaining open questions conclude the review. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Verkhoglyadova, Olga P.; Zank, Gary P.; Li, Gang] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35889 USA.
[Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zank, Gary P.; Li, Gang] UAH, Dept Space Sci, Huntsville, AL 35899 USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NSF SHINE [AGS-0962658]; NASA [EPSCoR NNX09AP74A, NNX11AO64G, PO 13390]
FX This research was partially supported by NSF SHINE AGS-0962658 grant and
NASA grants EPSCoR NNX09AP74A, NNX11AO64G, the subaward PO 13390. The
authors would like to thank Dr. Jacobus leRoux for insightful
discussions.
NR 163
TC 4
Z9 4
U1 1
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0370-1573
EI 1873-6270
J9 PHYS REP
JI Phys. Rep.-Rev. Sec. Phys. Lett.
PD FEB 12
PY 2015
VL 557
BP 1
EP 23
DI 10.1016/j.physrep.2014.10.004
PG 23
WC Physics, Multidisciplinary
SC Physics
GA CB3BM
UT WOS:000349503100001
ER
PT J
AU Sarkhel, S
Mathews, JD
Raizada, S
Sekar, R
Chakrabarty, D
Guharay, A
Jee, G
Kim, JH
Kerr, RB
Ramkumar, G
Sridharan, S
Wu, Q
Mlynczak, MG
Russell, JM
AF Sarkhel, Sumanta
Mathews, John D.
Raizada, Shikha
Sekar, Ramanathan
Chakrabarty, Dibyendu
Guharay, Amitava
Jee, Geonhwa
Kim, Jeong-Han
Kerr, Robert B.
Ramkumar, Geetha
Sridharan, Sundararajan
Wu, Qian
Mlynczak, Martin G.
Russell, James M., III
TI A case study on occurrence of an unusual structure in the sodium layer
over Gadanki, India
SO EARTH PLANETS AND SPACE
LA English
DT Article
ID KELVIN-HELMHOLTZ BILLOWS; STRATIFIED COMPRESSIBLE FLOWS; SPORADIC-E;
LOWER THERMOSPHERE; LOW LATITUDES; GRAVITY-WAVE; KM ALTITUDE; NIGHTGLOW;
LIDAR; EVOLUTION
AB The height-time-concentration map of neutral sodium (Na) atoms measured by a Na lidar during the night of 18 to 19 March 2007 over Gadanki, India (13.5 degrees N, 79.2 degrees E) reveals an unusual structure in the Na layer for around 30 min in the altitude range of 92 to 98 km which is similar to the usual 'C' type structures observed at other locations. In order to understand the physical mechanism behind the generation of this unusual event, an investigation is carried out combining the data from multiple instruments that include the meteor wind radar over Thiruvananthapuram, India (8.5 degrees N, 77 degrees E) and the SABER instrument onboard the TIMED satellite. The temperature and wind profiles from the data set provided by these instruments allow us to infer the Richardson number which is found to be noticeably less than the canonical threshold of 0.25 above 92 km over Thiruvananthapuram suggesting the plausible generation of Kelvin-Helmholtz (KH) billows over southwestern part of the Indian subcontinent. Based on the average wind speed and direction over Thiruvananthapuram, it is proposed that the KH-billow structure was modified due to the background wind and was advected with it in nearly 'frozen-in' condition (without significant decay) in the northeastward direction reaching the Na lidar location (Gadanki). This case study, therefore, presents a scenario wherein the initially deformed KH-billow structure survived for a few hours (instead of a few minutes or tens of minutes as reported in earlier works) in an apparently 'frozen-in' condition under favorable background conditions. In this communication, we suggest a hypothesis where this deformed KH-billow structure plays crucial role in creating the abovementioned unusual structure observed in the Na layer over Gadanki.
C1 [Sarkhel, Sumanta; Mathews, John D.] Penn State Univ, Radar Space Sci Lab, Elect Engn East 323, University Pk, PA 16802 USA.
[Sarkhel, Sumanta; Raizada, Shikha; Kerr, Robert B.] SRI Int, Ctr Geospace Studies, Arecibo Observ, Space & Atmospher Sci, Arecibo, PR USA.
[Sarkhel, Sumanta; Jee, Geonhwa; Kim, Jeong-Han] Korea Polar Res Inst, Div Climate Change, Inchon 406840, South Korea.
[Sarkhel, Sumanta] Indian Inst Technol Roorkee, Dept Phys, Roorkee 247667, Uttar Pradesh, India.
[Sekar, Ramanathan; Chakrabarty, Dibyendu] Phys Res Lab, Space & Atmospher Sci Div, Ahmadabad 380009, Gujarat, India.
[Guharay, Amitava] Natl Inst Space Res, Sao Paulo, Brazil.
[Ramkumar, Geetha] Vikram Sarabhai Space Ctr, Space Phys Lab, Thiruvananthapuram, Kerala, India.
[Sridharan, Sundararajan] Natl Atmospher Res Lab, Gadanki, India.
[Wu, Qian] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
RP Sarkhel, S (reprint author), Penn State Univ, Radar Space Sci Lab, Elect Engn East 323, University Pk, PA 16802 USA.
EM sarkhel.fph@iitr.ac.in
RI Sarkhel, Sumanta/I-7525-2015;
OI Wu, Qian/0000-0002-7508-3803
FU National Science Foundation (NSF) [ATM 07-21613, AGS 1241407]; NSF
[AST-1100968]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo,
Brazil; Korea Polar Research Institute, South Korea [PE15010];
Department of Space, Government of India
FX J. D. Mathews' and part of S. Sarkhel's component of this effort was
supported under the National Science Foundation (NSF) grant ATM 07-21613
and AGS 1241407 to The Pennsylvania State University, USA. The Arecibo
Observatory is operated by SRI International under a cooperative
agreement with the NSF (AST-1100968), and in alliance with Ana G.
Mendez-Universidad Metropolitana, and the Universities Space Research
Association. A. Guharay acknowledges support of the Fundacao de Amparo a
Pesquisa do Estado de Sao Paulo, Brazil to this present research work.
G. Jee, J. Kim, and part of S. Sarkhel's effort is supported by grant
PE15010 in the Korea Polar Research Institute, South Korea. NCAR is
supported by the NSF. The SKiYMET radar installed at the Space Physics
Laboratory was sanctioned under the 10th 5-year plan of the Department
of Space, Government of India. The authors thank the director and the
supporting staff members of the National Atmospheric Research
Laboratory, Gadanki, India for their cooperation in making the
observational campaign successful. S. Sarkhel thanks V. Lakshmi
Narayanan and S. Gurubaran for useful discussion. This work is also
partially supported by the Department of Space, Government of India.
NR 54
TC 2
Z9 2
U1 2
U2 10
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD FEB 11
PY 2015
VL 67
AR 19
DI 10.1186/s40623-015-0183-5
PG 15
WC Geosciences, Multidisciplinary
SC Geology
GA CD9PA
UT WOS:000351429100001
ER
PT J
AU Marinucci, A
Matt, G
Bianchi, S
Lu, TN
Arevalo, P
Balokovic, M
Ballantyne, D
Bauer, FE
Boggs, SE
Christensen, FE
Craig, WW
Gandhi, P
Hailey, CJ
Harrison, F
Puccetti, S
Rivers, E
Walton, DJ
Stern, D
Zhang, W
AF Marinucci, A.
Matt, G.
Bianchi, S.
Lu, T. N.
Arevalo, P.
Balokovic, M.
Ballantyne, D.
Bauer, F. E.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Hailey, C. J.
Harrison, F.
Puccetti, S.
Rivers, E.
Walton, D. J.
Stern, D.
Zhang, W.
TI The Seyfert 2 galaxy NGC 2110: hard X-ray emission observed by NuSTAR
and variability of the iron K alpha line
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: NGC 2110; galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; XMM-NEWTON; SUZAKU
OBSERVATIONS; COMPTON-THICK; COLD MATTER; REFLECTION; AGN; SPECTRUM;
NGC-2110
AB We present NuSTAR observations of the bright Seyfert 2 galaxy NGC 2110 obtained in 2012, when the source was at the highest flux level ever observed, and in 2013, when the source was at a more typical flux level. We include archival observations from other X-ray satellites, namely XMM-Newton, Suzaku, BeppoSAX, Chandra and Swift. Simultaneous NuSTAR and Swift broad-band spectra (in the 3-80 keV range) indicate a cutoff energy E-c > 210 keV, with no detectable contribution from Compton reflection. NGC 2110 is one of the very few sources where no evidence for distant Compton-thick scattering is found and, by using temporal information collected over more than a decade, we investigate variations of the iron K alpha line on time-scales of years. The Fe K alpha line is likely the sum of two components: one constant (originating from distant Compton-thick material) and the other one variable and linearly correlated with the source flux (possibly arising from Compton-thin material much closer to the black hole).
C1 [Marinucci, A.; Matt, G.; Bianchi, S.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Lu, T. N.; Balokovic, M.; Harrison, F.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Ballantyne, D.; Bauer, F. E.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
[Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Marinucci, A (reprint author), Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
EM marinucci@fis.uniroma3.it
RI Bianchi, Stefano/B-4804-2010; Boggs, Steven/E-4170-2015; XRAY,
SUZAKU/A-1808-2009
OI Bianchi, Stefano/0000-0002-4622-4240; Boggs, Steven/0000-0001-9567-4224;
FU Italian Space Agency [ASI/INAF I/037/12/0-011/13]; European Union
[312789]; NASA [NNG08FD60C]; National Aeronautics and Space
Administration; International Fulbright Science and Technology Award
FX AM and GM acknowledge financial support from Italian Space Agency under
grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh
Framework Programme (FP7/2007-2013) under grant agreement n.312789. 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).; MB acknowledges support from the International
Fulbright Science and Technology Award.
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JI Mon. Not. Roy. Astron. Soc.
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SC Astronomy & Astrophysics
GA CC3TK
UT WOS:000350272700012
ER
PT J
AU Petroff, E
Bailes, M
Barr, ED
Barsdell, BR
Bhat, NDR
Bian, F
Burke-Spolaor, S
Caleb, M
Champion, D
Chandra, P
Da Costa, G
Delvaux, C
Flynn, C
Gehrels, N
Greiner, J
Jameson, A
Johnston, S
Kasliwal, MM
Keane, EF
Keller, S
Kocz, J
Kramer, M
Leloudas, G
Malesani, D
Mulchaey, JS
Ng, C
Ofek, EO
Perley, DA
Possenti, A
Schmidt, BP
Shen, Y
Stappers, B
Tisserand, P
van Straten, W
Wolf, C
AF Petroff, E.
Bailes, M.
Barr, E. D.
Barsdell, B. R.
Bhat, N. D. R.
Bian, F.
Burke-Spolaor, S.
Caleb, M.
Champion, D.
Chandra, P.
Da Costa, G.
Delvaux, C.
Flynn, C.
Gehrels, N.
Greiner, J.
Jameson, A.
Johnston, S.
Kasliwal, M. M.
Keane, E. F.
Keller, S.
Kocz, J.
Kramer, M.
Leloudas, G.
Malesani, D.
Mulchaey, J. S.
Ng, C.
Ofek, E. O.
Perley, D. A.
Possenti, A.
Schmidt, B. P.
Shen, Yue
Stappers, B.
Tisserand, P.
van Straten, W.
Wolf, C.
TI A real-time fast radio burst: polarization detection and multiwavelength
follow-up
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE polarization; radiation mechanisms: general; intergalactic medium; radio
continuum: general
ID GAMMA-RAY BURST; 25 APRIL 1998; CIRCULAR-POLARIZATION; UNUSUAL
SUPERNOVA; MAGNETIC-FIELD; PULSAR SURVEY; CRAB PULSAR; AD LEONIS;
EMISSION; DISCOVERY
AB Fast radio bursts (FRBs) are one of the most tantalizing mysteries of the radio sky; their progenitors and origins remain unknown and until now no rapid multiwavelength follow-up of an FRB has been possible. New instrumentation has decreased the time between observation and discovery from years to seconds, and enables polarimetry to be performed on FRBs for the first time. We have discovered an FRB (FRB 140514) in real-time on 2014 May 14 at 17:14:11.06 UTC at the Parkes radio telescope and triggered follow-up at other wavelengths within hours of the event. FRB 140514 was found with a dispersion measure (DM) of 562.7(6) cm(-3) pc, giving an upper limit on source redshift of z less than or similar to 0.5. FRB 140514 was found to be 21 +/- 7 per cent (3 sigma) circularly polarized on the leading edge with a 1 sigma upper limit on linear polarization <10 per cent. We conclude that this polarization is intrinsic to the FRB. If there was any intrinsic linear polarization, as might be expected from coherent emission, then it may have been depolarized by Faraday rotation caused by passing through strong magnetic fields and/or high-density environments. FRB 140514 was discovered during a campaign to re-observe known FRB fields, and lies close to a previous discovery, FRB 110220; based on the difference in DMs of these bursts and time-on-sky arguments, we attribute the proximity to sampling bias and conclude that they are distinct objects. Follow-up conducted by 12 telescopes observing from X-ray to radio wavelengths was unable to identify a variable multiwavelength counterpart, allowing us to rule out models in which FRBs originate from nearby (z < 0.3) supernovae and long duration gamma-ray bursts.
C1 [Petroff, E.; Bailes, M.; Barr, E. D.; Caleb, M.; Flynn, C.; Jameson, A.; Keane, E. F.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Petroff, E.; Johnston, S.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Barsdell, B. R.; Kocz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Bian, F.; Caleb, M.; Da Costa, G.; Keller, S.; Schmidt, B. P.; Tisserand, P.; Wolf, C.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Burke-Spolaor, S.; Perley, D. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Champion, D.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Chandra, P.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Delvaux, C.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kasliwal, M. M.; Mulchaey, J. S.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Kocz, J.; Shen, Yue] CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA.
[Kramer, M.; Stappers, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Leloudas, G.; Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr DARK, DK-2100 Copenhagen O, Denmark.
[Leloudas, G.; Ofek, E. O.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
[Shen, Yue] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Tisserand, P.] Univ Paris 06, Inst Astrophys Paris, Sorbonne Univ, F-75005 Paris, France.
[Tisserand, P.] CNRS, UMR 7095, Inst Astrophys, F-75014 Paris, France.
RP Petroff, E (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
EM epetroff@astro.swin.edu.au
OI Champion, David/0000-0003-1361-7723; Schmidt, Brian/0000-0001-6589-1287;
van Straten, Willem/0000-0003-2519-7375
FU Commonwealth of Australia; Australian Research Council Centre of
Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; ARC
[DP120101237]; Leibniz-Prize; DFG [HA 1850/28-1]; Danish National
Research council; Curtin Research Fellowship; EXTraS - European Union
[607452]; Hubble Fellowship; Carnegie-Princeton Fellowship; Instrument
Center for Danish Astrophysics (IDA); Willner Family Leadership
Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science;
Israel Science Foundation; Minerva; Weizmann-UK; I-CORE Program of the
Planning and Budgeting Committee; NASA by the Space Telescope Science
Institute [HST-HF-51296.01-A]; NASA [NAS 5-26555]; ARC via CAASTRO;
[LF0992131]
FX The Parkes radio telescope and the ATCA are part of the Australia
Telescope National Facility which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO. Parts
of this research were conducted by the Australian Research Council
Centre of Excellence for All-sky Astrophysics (CAASTRO), through project
number CE110001020. We thank the staff of the GMRT that made these
observations possible. GMRT is run by the National Centre for Radio
Astrophysics of the Tata Institute of Fundamental Research. Research
with the ANU SkyMapper telescope is supported in part through ARC
Discovery Grant DP120101237. We thank the Carnegie Supernova Project
team (PI M. Phillips) and intermediate Palomar Transient Factory team
(PI S. Kulkarni) for promptly taking follow-up data. Part of the funding
for GROND (both hardware as well as personnel) was generously granted
from the Leibniz-Prize to Professor G. Hasinger (DFG grand HA
1850/28-1). The Dark Cosmology Centre is supported by the Danish
National Research council. We thank A. Krauss for prompt observations
with the Effelsberg Radio Telescope. Partly based on observations made
with the NOT, 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.; We thank the
anonymous referee for valuable input which improved the clarity of this
paper. EP would like to thank M. Murphy, J. Cooke, and C. Vale for
useful discussion and valuable comments. NDRB is supported by a Curtin
Research Fellowship. CD acknowledges support through EXTraS, funded from
the European Union's Seventh Framework Programme for research,
technological development and demonstration under grant agreement no
607452. MMK acknowledges generous support from the Hubble Fellowship and
Carnegie-Princeton Fellowship. DM acknowledged the Instrument Center for
Danish Astrophysics (IDA) for support. EOO is incumbent of the Arye
Dissentshik career development chair and is grateful to support by
grants from the Willner Family Leadership Institute Ilan Gluzman
(Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation,
Minerva, Weizmann-UK and the I-CORE Program of the Planning and
Budgeting Committee and The Israel Science Foundation. Support for DAP
was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A
awarded by the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., for
NASA, under contract NAS 5-26555. BPS, CW, and PT acknowledge funding
from the ARC via CAASTRO and grand LF0992131.
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GA CC3TK
UT WOS:000350272700018
ER
PT J
AU Nikolov, N
Sing, DK
Burrows, AS
Fortney, JJ
Henry, GW
Pont, F
Ballester, GE
Aigrain, S
Wilson, PA
Huitson, CM
Gibson, NP
Desert, JM
des Etangs, AL
Showman, AP
Vidal-Madjar, A
Wakeford, HR
Zahnle, K
AF Nikolov, N.
Sing, D. K.
Burrows, A. S.
Fortney, J. J.
Henry, G. W.
Pont, F.
Ballester, G. E.
Aigrain, S.
Wilson, P. A.
Huitson, C. M.
Gibson, N. P.
Desert, J. -M.
des Etangs, A. Lecavelier
Showman, A. P.
Vidal-Madjar, A.
Wakeford, H. R.
Zahnle, K.
TI HST hot-Jupiter transmission spectral survey: haze in the atmosphere of
WASP-6b
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: observational; techniques: spectroscopic; planets and
satellites: atmospheres; stars: activity; planets and satellites:
individual: WASP-6b
ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; MASS DWARF STARS;
SECONDARY ECLIPSE PHOTOMETRY; GIANT PLANET ATMOSPHERES; INFRARED ARRAY
CAMERA; EXTRASOLAR PLANET; MU-M; EMISSION-SPECTRUM; BROWN DWARFS
AB We report Hubble Space Telescope optical to near-infrared transmission spectroscopy of the hot-Jupiter WASP-6b, measured with the Space Telescope Imaging Spectrograph and Spitzer's InfraRed Array Camera. The resulting spectrum covers the range 0.29-4.5 mu m. We find evidence for modest stellar activity of WASP-6 and take it into account in the transmission spectrum. The overall main characteristic of the spectrum is an increasing radius as a function of decreasing wavelength corresponding to a change of Delta(R-p/R-*) = 0.0071 from 0.33 to 4.5 mu m. The spectrum suggests an effective extinction cross-section with a power law of index consistent with Rayleigh scattering, with temperatures of 973 +/- 144K at the planetary terminator. We compare the transmission spectrum with hot-Jupiter atmospheric models including condensate-free and aerosol-dominated models incorporating Mie theory. While none of the clear-atmosphere models is found to be in good agreement with the data, we find that the complete spectrum can be described by models that include significant opacity from aerosols including Fe-poor Mg2SiO4, MgSiO3, KCl and Na2S dust condensates. WASP-6b is the second planet after HD 189733b which has equilibrium temperatures near similar to 1200K and shows prominent atmospheric scattering in the optical.
C1 [Nikolov, N.; Sing, D. K.; Pont, F.; Wilson, P. A.; Wakeford, H. R.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England.
[Burrows, A. S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Henry, G. W.] Tennessee State Univ, Nashville, TN 37209 USA.
[Ballester, G. E.; Showman, A. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Aigrain, S.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Wilson, P. A.; des Etangs, A. Lecavelier; Vidal-Madjar, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Huitson, C. M.; Desert, J. -M.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA.
[Gibson, N. P.] European So Observ, D-85748 Garching, Germany.
[Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Nikolov, N (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
EM nikolov.nkn@gmail.com
RI Nikolov, Nikolay/H-6183-2015;
OI Nikolov, Nikolay/0000-0002-6500-3574; Sing, David /0000-0001-6050-7645;
Wakeford, Hannah/0000-0003-4328-3867; Gibson, Neale/0000-0002-9308-2353
FU NASA; European Research Council under the European Union [336792]; STFC
[ST/J0016/1]; STFC; Space Telescope Science Institute [HST-GO-12473]
FX This work is based on observations with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute (STScI)
operated by AURA, Inc. This work is based in part on observations made
with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. The research leading to these results has received
funding from the European Research Council under the European Unions
Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 336792.
NN and DS acknowledge support from STFC consolidated grant ST/J0016/1.
PW acknowledges support from STFC grant. All US-based co-authors
acknowledge support from the Space Telescope Science Institute under
HST-GO-12473 grants to their respective institutions.
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PG 16
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SC Astronomy & Astrophysics
GA CC3TK
UT WOS:000350272700036
ER
PT J
AU Moor, A
Kospal, A
Abraham, P
Apai, D
Balog, Z
Grady, C
Henning, T
Juhasz, A
Kiss, C
Krivov, AV
Pawellek, N
Szabo, GM
AF Moor, A.
Kospal, A.
Abraham, P.
Apai, D.
Balog, Z.
Grady, C.
Henning, Th.
Juhasz, A.
Kiss, Cs.
Krivov, A. V.
Pawellek, N.
Szabo, Gy. M.
TI Stirring in massive, young debris discs from spatially resolved Herschel
images
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; stars: individual: HD 9672; stars: individual: HD
16743; stars: individual: HD 21997; stars: individual: HD 95086;
infrared: stars
ID A-TYPE STARS; GENEVA-COPENHAGEN SURVEY; SPITZER-SPACE-TELESCOPE; ICY
PLANET FORMATION; MAIN-SEQUENCE STARS; VEGA-TYPE STARS; SUN-LIKE STARS;
F-TYPE STARS; BETA-PICTORIS; HR 8799
AB A significant fraction of main-sequence stars are encircled by dusty debris discs, where the short-lived dust particles are replenished through collisions between planetesimals. Most destructive collisions occur when the orbits of smaller bodies are dynamically stirred up, either by the gravitational effect of locally formed Pluto-sized planetesimals (self-stirring scenario), or via secular perturbation caused by an inner giant planet (planetary stirring). The relative importance of these scenarios in debris systems is unknown. Here, we present new Herschel Space Observatory imagery of 11 discs selected from the most massive and extended known debris systems. All discs were found to be extended at far-infrared wavelengths, five of them being resolved for the first time. We evaluated the feasibility of the self-stirring scenario by comparing the measured disc sizes with the predictions of the model calculated for the ages of our targets. We concluded that the self-stirring explanation works for seven discs. However, in four cases, the predicted pace of outward propagation of the stirring front, assuming reasonable initial disc masses, was far too low to explain the radial extent of the cold dust. Therefore, for HD 9672, HD 16743, HD 21997, and HD 95086, another explanation is needed. We performed a similar analysis for beta Pic and HR 8799, reaching the same conclusion. We argue that planetary stirring is a promising possibility to explain the disc properties in these systems. In HR 8799 and HD 95086, we may already know the potential perturber, since their known outer giant planets could be responsible for the stirring process. Interestingly, the discs around HD 9672, HD 21997, and beta Pic are also unique in harbouring detectable amount of molecular CO gas. Our study demonstrates that among the largest and most massive debris discs self-stirring may not be the only active scenario, and potentially planetary stirring is responsible for destructive collisions and debris dust production in a number of systems.
C1 [Moor, A.; Kospal, A.; Abraham, P.; Kiss, Cs.; Szabo, Gy. M.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Kospal, A.] European Space Agcy, ESA ESTEC, SRE S, NL-2200 AG Noordwijk, Netherlands.
[Apai, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, D.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Balog, Z.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Grady, C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Juhasz, A.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Krivov, A. V.; Pawellek, N.] Univ Jena, Astrophys Inst, D-07745 Jena, Germany.
[Krivov, A. V.; Pawellek, N.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany.
[Szabo, Gy. M.] Gothard Astrophys Observ, ELTE, H-9704 Szombathely, Hungary.
RP Moor, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.
EM moor@konkoly.hu
FU Momentum grant of the MTA CSFK Lendulet Disk Research Group; ESA PECS
[4000110889/14/NL/NDe]; Hungarian Research Fund OTKA [K101393, K104607];
Bolyai Research Fellowship of the Hungarian Academy of Sciences;
National Aeronautics and Space Administration; National Science
Foundation
FX We are grateful to our referee for the useful comments. This work was
supported by the Momentum grant of the MTA CSFK Lendulet Disk Research
Group, the ESA PECS Contract No. 4000110889/14/NL/NDe as well as the
Hungarian Research Fund OTKA grants K101393 and K104607. AM and GyMSz
acknowledges support from the Bolyai Research Fellowship of the
Hungarian Academy of Sciences. This publication makes use of data
products from the Wide-field Infrared Survey Explorer, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. The publication also
makes use of data products from the Two Micron All Sky Survey, which is
a joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/California Institute of Technology,
funded by the National Aeronautics and Space Administration and the
National Science Foundation. Our research has made use of the VizieR
catalogue access tool, CDS, Strasbourg, France.
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JI Mon. Not. Roy. Astron. Soc.
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DI 10.1093/mnras/stu2442
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TK
UT WOS:000350272700047
ER
PT J
AU Fox, OD
Silverman, JM
Filippenko, AV
Mauerhan, J
Becker, J
Borish, HJ
Cenko, SB
Clubb, KI
Graham, M
Hsiao, E
Kelly, PL
Lee, WH
Marion, GH
Milisavljevic, D
Parrent, J
Shivvers, I
Skrutskie, M
Smith, N
Wilson, J
Zheng, WK
AF Fox, Ori D.
Silverman, Jeffrey M.
Filippenko, Alexei V.
Mauerhan, Jon
Becker, Juliette
Borish, H. Jacob
Cenko, S. Bradley
Clubb, Kelsey I.
Graham, Melissa
Hsiao, Eric
Kelly, Patrick L.
Lee, William H.
Marion, G. H.
Milisavljevic, Dan
Parrent, Jerod
Shivvers, Isaac
Skrutskie, Michael
Smith, Nathan
Wilson, John
Zheng, Weikang
TI On the nature of Type IIn/Ia-CSM supernovae: optical and near-infrared
spectra of SN 2012ca and SN 2013dn
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; supernovae: general; supernovae: individual:
SN2005ip; supernovae: individual: SN 2009dc; supernovae: individual: SN
2012ca; supernovae: individual: SN 2013dn
ID CORE-COLLAPSE SUPERNOVAE; IA SUPERNOVAE; CIRCUMSTELLAR MEDIUM; DUST
FORMATION; MASSIVE STAR; STRIPPED-ENVELOPE; I. OBSERVATIONS; II
SUPERNOVAE; SKY SURVEY; SPECTROSCOPY
AB A growing subset of Type Ia supernovae (SNe Ia) shows evidence via narrow emission lines for unexpected interaction with a dense circumstellar medium (SNe IIn/Ia-CSM). The precise nature of the progenitor, however, remains debated owing to spectral ambiguities arising from a strong contribution from the CSM interaction. Late-time spectra offer potential insight if the post-shock cold, dense shell becomes sufficiently thin and/or the ejecta begin to cross the reverse shock. To date, only a few high-quality spectra of this kind exist. Here we report on the late-time optical and infrared spectra of the SNe Ia-CSM 2012ca and 2013dn. These SNe Ia-CSM spectra exhibit low [Fe III]/[Fe II] ratios and strong [Ca II] at late epochs. Such characteristics are reminiscent of the super-Chandrasekhar-mass candidate SN 2009dc, for which these features suggested a low-ionization state due to high densities, although the broad Fe features admittedly show similarities to the blue 'quasi-continuum' observed in some core collapse SNe Ibn and IIn. Neither SN 2012ca nor any of the other SNe Ia-CSM in this paper show evidence for broad oxygen, carbon, or magnesium in their spectra. Similar to the interacting Type IIn SN 2005ip, a number of high-ionization lines are identified in SN 2012ca, including [S III], [Ar III], [Ar X], [Fe VIII], [Fe X], and possibly [Fe XI]. The total bolometric energy output does not exceed 10(51) erg, but does require a large kinetic-to-radiative conversion efficiency. All of these observations taken together suggest that SNe Ia-CSM are more consistent with a thermonuclear explosion than a core collapse event, although detailed radiative transfer models are certainly necessary to confirm these results.
C1 [Fox, Ori D.; Filippenko, Alexei V.; Mauerhan, Jon; Clubb, Kelsey I.; Graham, Melissa; Kelly, Patrick L.; Shivvers, Isaac; Zheng, Weikang] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Silverman, Jeffrey M.; Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Becker, Juliette] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Borish, H. Jacob; Skrutskie, Michael; Wilson, John] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Hsiao, Eric] Carnegie Inst Sci, Las Campanas Observ, Casilla 601, Chile.
[Hsiao, Eric] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Lee, William H.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Milisavljevic, Dan; Parrent, Jerod] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Fox, OD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM ofox@berkeley.edu
OI Shivvers, Isaac/0000-0003-3373-8047; Becker,
Juliette/0000-0002-7733-4522
FU NSF [PHYS-1066293, AST-1211916]; W. M. Keck Foundation; NASA
[NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT
[INFR-2009-01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT; NSF
Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771];
TABASGO Foundation; Richard and Rhoda Goldman Fund; Christopher R.
Redlich Fund
FX We thank the referee, Stefano Benetti, for useful comments that
strengthened this paper. Insightful discussions were shared with many at
the Aspen Center for Physics, including Ryan Foley, Ryan Chornock, and
Craig Wheeler. This work was supported in part by NSF Grant No.
PHYS-1066293 and the hospitality of the Aspen Center for Physics. Some
of the data presented herein were obtained at the W. M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA; the observatory was made possible by the generous financial
support of the W. M. Keck Foundation. We are grateful to the staffs of
the Lick and Keck Observatory for their assistance with the
observations, and thank the RATIR instrument team and the staff of the
Observatorio Astronomico Nacional on Sierra San Pedro Martir. RATIR is a
collaboration between the University of California, the Universidad
Nacional Autonoma de Mexxico, NASA Goddard Space Flight Center, and
Arizona State University, benefiting from the loan of an H2RG detector
from Teledyne Scientific and Imaging. RATIR, the automation of the
Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on
Sierra, San Pedro, Martir, and the operation of both is funded by the
partner institutions and through NASA grants NNX09AH71G, NNX09AT02G,
NNX10AI27G, and NNX12AE66G, CONACyT grant INFR-2009-01-122785, UNAM
PAPIIT grant IN113810, and a UC MEXUS-CONACyT grant. JMS is supported by
an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award
AST-1302771. AVF's supernova group at UC Berkeley received support
through NSF grant AST-1211916, the TABASGO Foundation, Gary and Cynthia
Bengier, the Richard and Rhoda Goldman Fund, and the Christopher R.
Redlich Fund.
NR 102
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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 FEB 11
PY 2015
VL 447
IS 1
BP 772
EP 785
DI 10.1093/mnras/stu2435
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TK
UT WOS:000350272700061
ER
PT J
AU Boyajian, T
von Braun, K
Feiden, GA
Huber, D
Basu, S
Demarque, P
Fischer, DA
Schaefer, G
Mann, AW
White, TR
Maestro, V
Brewer, J
Lamell, CB
Spada, F
Lopez-Morales, M
Ireland, M
Farrington, C
van Belle, GT
Kane, SR
Jones, J
ten Brummelaar, TA
Ciardi, DR
McAlister, HA
Ridgway, S
Goldfinger, PJ
Turner, NH
Sturmann, L
AF Boyajian, Tabetha
von Braun, Kaspar
Feiden, Gregory A.
Huber, Daniel
Basu, Sarbani
Demarque, Pierre
Fischer, Debra A.
Schaefer, Gail
Mann, Andrew W.
White, Timothy R.
Maestro, Vicente
Brewer, John
Lamell, C. Brooke
Spada, Federico
Lopez-Morales, Mercedes
Ireland, Michael
Farrington, Chris
van Belle, Gerard T.
Kane, Stephen R.
Jones, Jeremy
ten Brummelaar, Theo A.
Ciardi, David R.
McAlister, Harold A.
Ridgway, Stephen
Goldfinger, P. J.
Turner, Nils H.
Sturmann, Laszlo
TI Stellar diameters and temperatures - VI. High angular resolution
measurements of the transiting exoplanet host stars HD 189733 and HD
209458 and implications for models of cool dwarfs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: interferometric; stars: fundamental parameters; stars:
individual: HD 189733; stars: individual: HD 209458; stars: late-type;
infrared: stars
ID INFRARED FLUX METHOD; INTEGRAL-FIELD SPECTROGRAPH; BASE-LINE
INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; LOW-MASS STARS; CHARA ARRAY;
ASTROPHYSICAL PARAMETERS; FUNDAMENTAL PROPERTIES; EXTRASOLAR PLANETS;
MAIN-SEQUENCE
AB We present direct radii measurements of the well-known transiting exoplanet host stars HD 189733 and HD 209458 using the CHARA Array interferometer. We find the limb-darkened angular diameters to be theta(LD) = 0.3848 +/- 0.0055 and 0.2254 +/- 0.0072 mas for HD 189733 and HD 209458, respectively. HD 189733 and HD 209458 are currently the only two transiting exoplanet systems where detection of the respective planetary companion's orbital motion from high-resolution spectroscopy has revealed absolute masses for both star and planet. We use our new measurements together with the orbital information from radial velocity and photometric time series data, Hipparcos distances, and newly measured bolometric fluxes to determine the stellar effective temperatures (T-eff = 4875 +/- 43, 6092 +/- 103 K), stellar linear radii (R-* = 0.805 +/- 0.016, 1.203 +/- 0.061 R-circle dot), mean stellar densities (rho(*) = 1.62 +/- 0.11, 0.58 +/- 0.14 rho(circle dot)), planetary radii (R-p = 1.216 +/- 0.024, 1.451 +/- 0.074 R-Jup), and mean planetary densities (rho(p) = 0.605 +/- 0.029, 0.196 +/- 0.033 rho(Jup)) for HD 189733b and HD 209458b, respectively. The stellar parameters for HD 209458, an F9 dwarf, are consistent with indirect estimates derived from spectroscopic and evolutionary modelling. However, we find that models are unable to reproduce the observational results for the K2 dwarf, HD 189733. We show that, for stellar evolutionary models to match the observed stellar properties of HD 189733, adjustments lowering the solar-calibrated mixing-length parameter to alpha(MLT) = 1.34 need to be employed.
C1 [Boyajian, Tabetha; Basu, Sarbani; Demarque, Pierre; Fischer, Debra A.; Brewer, John; Lamell, C. Brooke] Yale Univ, New Haven, CT 06520 USA.
[von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[von Braun, Kaspar] Mirasol Inst, D-81679 Munich, Germany.
[von Braun, Kaspar; van Belle, Gerard T.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Feiden, Gregory A.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
[Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
[Schaefer, Gail; Farrington, Chris; ten Brummelaar, Theo A.; Goldfinger, P. J.; Turner, Nils H.; Sturmann, Laszlo] Mt Wilson Observ, CHARA Array, Mount Wilson, CA 91023 USA.
[Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[White, Timothy R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Maestro, Vicente] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Spada, Federico] Leibniz Inst f ur Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ireland, Michael] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Jones, Jeremy; McAlister, Harold A.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30303 USA.
[Jones, Jeremy; McAlister, Harold A.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Ridgway, Stephen] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Boyajian, T (reprint author), Yale Univ, New Haven, CT 06520 USA.
EM tabetha.boyajian@yale.edu
RI Feiden, Gregory/F-1505-2015;
OI Feiden, Gregory/0000-0002-2012-7215; Spada,
Federico/0000-0001-6948-4259; Brewer, John/0000-0002-9873-1471; Ciardi,
David/0000-0002-5741-3047
FU NASA [ADAP12-0172, 14-XRP14_2-0147, NNX14AB92G]; NSF [AST-1105930];
National Science Foundation through NSF [AST-0606958, AST-0908253];
Georgia State University through the College of Arts and Sciences; W. M.
Keck Foundation
FX TSB acknowledges support provided through NASA grants ADAP12-0172 and
14-XRP14_2-0147. DH acknowledges support by NASA Grant NNX14AB92G issued
through the Kepler Participating Scientist Program. SB acknowledges
partial support of NSF grant AST-1105930. Judit Sturmann keeps some
tight beams in place - hats off to you girl! The CHARA Array is funded
by the National Science Foundation through NSF grants AST-0606958 and
AST-0908253 and by Georgia State University through the College of Arts
and Sciences, as well as the W. M. Keck Foundation. This research made
use of the SIMBAD and VIZIER Astronomical Databases, operated at CDS,
Strasbourg, France (http://cdsweb.u-strasbg.fr/), and of NASA's
Astrophysics Data System, of the Jean-Marie Mariotti Center SearchCal
service (http://www.jmmc.fr/searchcal), co-developed by FIZEAU and
LAOG/IPAG.
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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 FEB 11
PY 2015
VL 447
IS 1
BP 846
EP 857
DI 10.1093/mnras/stu2502
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TK
UT WOS:000350272700066
ER
PT J
AU Zhang, C
Binienda, WK
Goldberg, RK
AF Zhang, Chao
Binienda, Wieslaw K.
Goldberg, Robert K.
TI Free-edge effect on the effective stiffness of single-layer triaxially
braided composite
SO COMPOSITES SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Textile composites; Elastic properties; Finite element analysis;
Statistics; Free-edge effect
AB Free-edge effect is known to play an important role in the failure of triaxially braided composites, especially under transverse tension loading conditions. However, there is little understanding available regarding the free-edge effect on the elastic property of the material. The emphasis of the present study is to examine the impact of the free-edge effect on the effective elastic response of a single-layer triaxially braided composite. Transverse tension straight-sided coupon specimens with various widths are tested and analyzed. The experimental results demonstrate an obvious increase in the tangent modulus and failure strength as the specimen width increases. The surface out-of-plane displacement contours present a continuous out-of-plane warping behavior distributed periodically along the free edges in an antisymmetric way. A meso-scale finite element model is utilized to study the coupon specimens; it is found to correlate well with the experimental data in predicting elastic properties and out-of-plane warping behavior. The results indicate that free-edge effect is an inherent factor of the antisymmetric braided architecture of bias fiber bundles. By conducting a dimensional analysis, the relationships between effective moduli and specimen width are quantified using Weibull equations; this method could potentially be used to predict the material properties of large structural components using small-scale test data. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Zhang, Chao; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Zhang, C (reprint author), Natl Renewable Energy Lab, Computat Sci Ctr, Golden, CO 80401 USA.
EM Chao.Zhang@nrel.gov
RI Zhang, Chao/H-3397-2013
NR 23
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U1 0
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0266-3538
EI 1879-1050
J9 COMPOS SCI TECHNOL
JI Compos. Sci. Technol.
PD FEB 11
PY 2015
VL 107
BP 145
EP 153
DI 10.1016/j.compscitech.2014.12.016
PG 9
WC Materials Science, Composites
SC Materials Science
GA CB4DV
UT WOS:000349579300019
ER
PT J
AU Archibald, RF
Kaspi, VM
Ng, CY
Scholz, P
Beardmore, AP
Gehrels, N
Kennea, JA
AF Archibald, R. F.
Kaspi, V. M.
Ng, C. -Y.
Scholz, P.
Beardmore, A. P.
Gehrels, N.
Kennea, J. A.
TI REPEATED, DELAYED TORQUE VARIATIONS FOLLOWING X-RAY FLUX ENHANCEMENTS IN
THE MAGNETAR 1E 1048.1-5937
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; pulsars: individual (1E 1048.1-5937); stars: neutron;
X-rays: stars
ID SOFT GAMMA-REPEATERS; NEUTRON-STARS; PULSAR 1E-1048.1-5937; SPIN-DOWN;
FREE PRECESSION; XTE J1810-197; OUTBURST; EMISSION; VARIABILITY; BURSTS
AB We report on two years of flux and spin evolution monitoring of 1E 1048.1-5937, a 6.5 s X-ray pulsar identified as a magnetar. Using Swift X-Ray Telescope data, we observed an X-ray outburst consisting of an increase in the persistent 1-10 keV flux by a factor of 6.3 +/- 0.2, beginning on 2011 December 31 (MJD 55926). Following a delay of similar to 100 days, the magnetar entered a period of large torque variability, with. reaching a factor of 4.55 +/- 0.05 times the nominal value, before decaying in an oscillatory manner over a timescale of months. We show by comparing to previous outbursts from the source that this pattern of behavior may repeat itself with a quasi-period of similar to 1800 days. We compare this phenomenology to periodic torque variations in radio pulsars, finding some similarities that suggest a magnetospheric origin for the behavior of 1E 1048.1-5937.
C1 [Archibald, R. F.; Kaspi, V. M.; Scholz, P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gehrels, N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
RP Archibald, RF (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
OI /0000-0002-5847-2612
FU Commonwealth of Australia for operation as a National Facility managed
by CSIRO; Walter C. Sumner Memorial Fellowship; NSERC Discovery Grant;
Accelerator Supplement, Centre de Recherche en Astrophysique du Quebec;
Canadian Institute for Advanced Study; Canada Research Chairs Program;
Lorne Trottier Chair in Astrophysics and Cosmology
FX We thank Jamie Stevens for carrying out the ATCA observations. The
Australia Telescope Compact Array is part of the Australia Telescope
National Facility which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO.9 R.F.A.
receives support from a Walter C. Sumner Memorial Fellowship. V.M.K.
receives support from an NSERC Discovery Grant and Accelerator
Supplement, Centre de Recherche en Astrophysique du Quebec, an R. Howard
Webster Foundation Fellowship from the Canadian Institute for Advanced
Study, the Canada Research Chairs Program and the Lorne Trottier Chair
in Astrophysics and Cosmology. We thank M. Lyutikov, D. Tsang, and K.
Gourgouliatos for useful discussions. We also thank an anonymous referee
for comments that improved the manuscript. We acknowledge the use of
public data from the Swift data archive. This research has made use of
data and software provided by the High Energy Astrophysics Science
Archive Research Center (HEASARC), which is a service of the
Astrophysics Science Division at NASA/GSFC and the High Energy
Astrophysics Division of the Smithsonian Astrophysical Observatory. The
scientific results reported in this article are based in part on
observations made by the Chandra X-ray Observatory. This research has
made use of CIAO software provided by the Chandra X-ray Center (CXC).
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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 FEB 10
PY 2015
VL 800
IS 1
AR 33
DI 10.1088/0004-637X/800/1/33
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900033
ER
PT J
AU Balokovic, M
Matt, G
Harrison, FA
Zoghbi, A
Ballantyne, DR
Boggs, SE
Christensen, FE
Craig, WW
Esmerian, CJ
Fabian, AC
Furst, F
Hailey, CJ
Marinucci, A
Parker, ML
Reynolds, CS
Stern, D
Walton, DJ
Zhang, WW
AF Balokovic, M.
Matt, G.
Harrison, F. A.
Zoghbi, A.
Ballantyne, D. R.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Esmerian, C. J.
Fabian, A. C.
Fuerst, F.
Hailey, C. J.
Marinucci, A.
Parker, M. L.
Reynolds, C. S.
Stern, D.
Walton, D. J.
Zhang, W. W.
TI CORONAL PROPERTIES OF THE SEYFERT 1.9 GALAXY MCG-05-23-016 DETERMINED
FROM HARD X-RAY SPECTROSCOPY WITH NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (MCG-5-23-016); galaxies: nuclei;
galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLES; BEPPOSAX OBSERVATIONS; COMPTON
REFLECTION; XMM-NEWTON; IC 4329A; MCG-5-23-16; EMISSION; SPECTRUM; LINE
AB Measurements of the high-energy cut-off in the coronal continuum of active galactic nuclei have long been elusive for all but a small number of the brightest examples. We present a direct measurement of the cut-off energy in the nuclear continuum of the nearby Seyfert 1.9 galaxy MCG-05-23-016 with unprecedented precision. The high sensitivity of NuSTAR up to 79 keV allows us to clearly disentangle the spectral curvature of the primary continuum from that of its reflection component. Using a simple phenomenological model for the hard X-ray spectrum, we constrain the cut-off energy to 116(-5)(+6) keV with 90% confidence. Testing for more complex models and nuisance parameters that could potentially influence the measurement, we find that the cut-off is detected robustly. We further use simple Comptonized plasma models to provide independent constraints for both the kinetic temperature of the electrons in the corona and its optical depth. At the 90% confidence level, we find kT(e) = 29 +/- 2 keV and tau(e) = 1.23 +/- 0.08 assuming a slab (disk-like) geometry, and kT(e) = 25 +/- 2 keV and tau(e) = 3.5 +/- 0.2 assuming a spherical geometry. Both geometries are found to fit the data equally well and their two principal physical parameters are correlated in both cases. With the optical depth in the tau(e) greater than or similar to 1 regime, the data are pushing the currently available theoretical models of the Comptonized plasma to the limits of their validity. Since the spectral features and variability arising from the inner accretion disk have been observed previously in MCG-05-23-016, the inferred high optical depth implies that a spherical or disk-like corona cannot be homogeneous.
C1 [Balokovic, M.; Harrison, F. A.; Esmerian, C. J.; Fuerst, F.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Matt, G.; Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Zoghbi, A.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Zoghbi, A.; Reynolds, C. S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA.
[Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fabian, A. C.; Parker, M. L.] Inst Astron, Cambridge CB3 0HA, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Balokovic, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015; Zoghbi, Abderahmen/A-8445-2017
OI Boggs, Steven/0000-0001-9567-4224; Zoghbi,
Abderahmen/0000-0002-0572-9613
FU International Fulbright Science and Technology Award; Italian Space
Agency [ASI/INAF I/037/12/0-011/13]; European Union Seventh Framework
Programme (FP7) [312789]; NASA [NNX14AF86G, NNG08FD60C]; National
Aeronautics and Space Administration
FX M.B. acknowledges support from the International Fulbright Science and
Technology Award. A.M. and G.M. acknowledge financial support from the
Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the
European Union Seventh Framework Programme (FP7/2007-2013) under grant
agreement No. 312789. C.S.R. thanks NASA for support under ADAP grant
NNX14AF86G. This work was supported under NASA Contract No. NNG08FD60C,
and made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR Operations, Software and Calibration
teams for support with the execution and analysis of these observations.
This research has made use of the NuSTAR Data Analysis Software
(NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC,
Italy) and the California Institute of Technology (USA). This research
has made use of NASA's Astrophysics Data System.
NR 44
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2015
VL 800
IS 1
AR 62
DI 10.1088/0004-637X/800/1/62
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900062
ER
PT J
AU Barclay, T
Endl, M
Huber, D
Foreman-Mackey, D
Cochran, WD
MacQueen, PJ
Rowe, JF
Quintana, EV
AF Barclay, Thomas
Endl, Michael
Huber, Daniel
Foreman-Mackey, Daniel
Cochran, William D.
MacQueen, Phillip J.
Rowe, Jason F.
Quintana, Elisa V.
TI RADIAL VELOCITY OBSERVATIONS AND LIGHT CURVE NOISE MODELING CONFIRM THAT
KEPLER-91b IS A GIANT PLANET ORBITING A GIANT STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; planetary systems; stars:
individual (Kepler-91, KIC 8219268, KOI-2133); techniques: photometric;
techniques: radial velocities
ID SYSTEMATIC-ERROR CORRECTION; HOBBY-EBERLY TELESCOPE; SOLAR-TYPE STARS;
51 PEGASI; COMPANION; ASTEROSEISMOLOGY; SPECTROGRAPH; ARCHITECTURE;
EXOPLANET; TIME
AB Kepler-91b is a rare example of a transiting hot Jupiter around a red giant star, providing the possibility to study the formation and composition of hot Jupiters under different conditions compared to main-sequence stars. However, the planetary nature of Kepler-91b, which was confirmed using phase-curve variations by Lillo-Box et al., was recently called into question based on a re-analysis of Kepler data. We have obtained ground-based radial velocity observations from the Hobby-Eberly Telescope and unambiguously confirm the planetary nature of Kepler-91b by simultaneously modeling the Kepler and radial velocity data. The star exhibits temporally correlated noise due to stellar granulation which we model as a Gaussian Process. We hypothesize that it is this noise component that led previous studies to suspect Kepler-91b to be a false positive. Our work confirms the conclusions presented by Lillo-Box et al. that Kepler-91b is a 0.73 +/- 0.13 M-Jup planet orbiting a red giant star.
C1 [Barclay, Thomas; Huber, Daniel; Rowe, Jason F.; Quintana, Elisa V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Endl, Michael; Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Huber, Daniel; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[Foreman-Mackey, Daniel] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
RP Barclay, T (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA.
FU MAST for non-HST data is provided by the NASA Office of Space Science
[NNX09AF08G]; National Science Foundation [DMS-1127914]; Applied
Mathematical Sciences Institute; NASA Senior Fellowship at the Ames
Research Center; Oak Ridge Associated Universities; NASA; NASA
[NNX14AB92G]
FX This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission Directorate.
Wewould like to express our gratitude to all those who have worked on
the Kepler pipeline over the many years of theKepler mission. Some
Kepler data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST) at the Space Telescope Science
Institute (STScI). STScI is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support
for MAST for non-HST data is provided by the NASA Office of Space
Science via grant NNX09AF08G and by other grants and contracts. Our MCMC
sampling was performed on the Pleiades supercomputer of the NASA
Advanced Supercomputing Division at NASA's Ames Research Center. We used
data obtained from The Hobby-Eberly Telescope (HET), a joint project of
the University of Texas at Austin, the Pennsylvania State University,
Stanford University, Ludwig-Maximilians-Universitat Munchen, and
Georg-August-Universitat Gottingen. The HET is named in honor of its
principal benefactors, William P. Hobby and Robert E. Eberly. We thank
the Statistical and Applied Mathematical Sciences Institute (SAMSI) for
hosting the Modern Statistical and Computational Methods for Analysis of
Kepler Data workshop where the idea for this work came about. The work
performed at SAMSI was partially supported by the National Science
Foundation under grant DMS-1127914 to the Statistical and Applied
Mathematical Sciences Institute. Any opinions, findings, and conclusions
or recommendations expressed in this material are those of the author(s)
and do not necessarily reflect the views of the National Science
Foundation. We thank Ruth Angus (University of Oxford) for valuable
discussions on noise sources in RV observations. We thank Jeffrey C.
Smith, Joe Catanzarite (both SETI Inst.), and David Kipping
(Harvard/CfA) for suggestions on how to improve the manuscript. E.V.
Quintana is supported by a NASA Senior Fellowship at the Ames Research
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. D. Huber acknowledges support by NASA under grant
NNX14AB92G issued through the Kepler Participating Scientist Program.
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SC Astronomy & Astrophysics
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UT WOS:000349236900046
ER
PT J
AU Boyer, ML
McQuinn, KBW
Barmby, P
Bonanos, AZ
Gehrz, RD
Gordon, KD
Groenewegen, MAT
Lagadec, E
Lennon, D
Marengo, M
McDonald, I
Meixner, M
Skillman, E
Sloan, GC
Sonneborn, G
van Loon, JT
Zijlstra, A
AF Boyer, Martha L.
McQuinn, Kristen B. W.
Barmby, Pauline
Bonanos, Alceste Z.
Gehrz, Robert D.
Gordon, Karl D.
Groenewegen, M. A. T.
Lagadec, Eric
Lennon, Daniel
Marengo, Massimo
McDonald, Iain
Meixner, Margaret
Skillman, Evan
Sloan, G. C.
Sonneborn, George
van Loon, Jacco Th.
Zijlstra, Albert
TI AN INFRARED CENSUS OF DUST IN NEARBY GALAXIES WITH SPITZER (DUSTiNGS).
II. DISCOVERY OF METAL-POOR DUSTY AGB STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: stellar content; infrared: stars; Local
Group; stars: AGB and post-AGB; stars: carbon
ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; LONG-PERIOD VARIABLES;
GRAVITATIONAL LENSING EXPERIMENT.; DWARF SPHEROIDAL GALAXY; LOCAL GROUP
GALAXIES; MASS-LOSS RETURN; YOUNG STELLAR OBJECTS; MU-M RANGE; EVOLVED
STARS
AB The DUSTiNGS survey (DUST in Nearby Galaxies with Spitzer) is a 3.6 and 4.5 mu m imaging survey of 50 nearby dwarf galaxies designed to identify dust-producing asymptotic giant branch (AGB) stars and massive stars. Using two epochs, spaced approximately six months apart, we identify a total of 526 dusty variable AGB stars (sometimes called "extreme" or x-AGB stars; [3.6]-[4.5] > 0.1 mag). Of these, 111 are in galaxies with [Fe/H] < -1.5 and 12 are in galaxies with [Fe/H] < -2.0, making them the most metal-poor dust-producing AGB stars known. We compare these identifications to those in the literature and find that most are newly discovered large-amplitude variables, with the exception of approximate to 30 stars in NGC 185 and NGC 147, 1 star in IC 1613, and 1 star in Phoenix. The chemical abundances of the x-AGB variables are unknown, but the low metallicities suggest that they are more likely to be carbon-rich than oxygen-rich and comparisons with existing optical and near-IR photometry confirm that 70 of the x-AGB variables are confirmed or likely carbon stars. We see an increase in the pulsation amplitude with increased dust production, supporting previous studies suggesting that dust production and pulsation are linked. We find no strong evidence linking dust production with metallicity, indicating that dust can form in very metal-poor environments.
C1 [Boyer, Martha L.; Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, Martha L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[McQuinn, Kristen B. W.; Gehrz, Robert D.; Skillman, Evan] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Bonanos, Alceste Z.] Natl Observ Athens, IAASARS, GR-15236 Penteli, Greece.
[Gordon, Karl D.; Meixner, Margaret] STScI, Baltimore, MD 21218 USA.
[Groenewegen, M. A. T.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Lagadec, Eric] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France.
[Lennon, Daniel] European Space Astron Ctr, ESA, E-28691 Madrid, Spain.
[Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[McDonald, Iain; Zijlstra, Albert] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[van Loon, Jacco Th.] Keele Univ, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
RP Boyer, ML (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM martha.boyer@nasa.gov
RI Bonanos, Alceste/K-5392-2013; Barmby, Pauline/I-7194-2016;
OI Bonanos, Alceste/0000-0003-2851-1905; Barmby,
Pauline/0000-0003-2767-0090; Lennon, Daniel/0000-0003-3063-4867
FU Spitzer [GO80063]; NASA Astrophysics Data Analysis Program
[N3-ADAP13-0058]; NASA Postdoctoral Program at the Goddard Space Flight
Center; NASA; United States Air Force; European Union (European Social
Fund); National Resources under the "ARISTEIA" action of the Operational
Programme "Education and Lifelong Learning" in Greece
FX We thank Patricia Whitelock & Michael Feast for discussions about
stellar variability that improved the paper and the referee for helpful
comments. This work is supported by Spitzer via grant GO80063 and by the
NASA Astrophysics Data Analysis Program grant number N3-ADAP13-0058. M.
L. B. is supported by the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by ORAU through a contract with NASA. R. D.
G. was supported by NASA and the United States Air Force. A.Z.B.
acknowledges funding by the European Union (European Social Fund) and
National Resources under the "ARISTEIA" action of the Operational
Programme "Education and Lifelong Learning" in Greece.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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ER
PT J
AU Gatuzz, E
Garcia, J
Kallman, TR
Mendoza, C
Gorczyca, TW
AF Gatuzz, E.
Garcia, J.
Kallman, T. R.
Mendoza, C.
Gorczyca, T. W.
TI ISMabs: A COMPREHENSIVE X-RAY ABSORPTION MODEL FOR THE INTERSTELLAR
MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
ID XMM-NEWTON OBSERVATION; K-SHELL PHOTOIONIZATION; CROSS-SECTIONS;
NEUTRON-STAR; LOW/HARD STATE; ATOMIC OXYGEN; SCORPIUS X-1; CYG X-2;
SPECTROSCOPY; BINARIES
AB We present an X-ray absorption model for the interstellar medium, to be referred to as ISMabs, that takes into account both neutral and ionized species of cosmically abundant elements, and includes the most accurate atomic data available. Using high-resolution spectra from eight X-ray binaries obtained with the Chandra High Energy Transmission Grating Spectrometer, we proceed to benchmark the atomic data in the model particularly in the neon K-edge region. Compared with previous photoabsorption models, which solely rely on neutral species, the inclusion of ions leads to improved spectral fits. Fit parameters comprise the column densities of abundant contributors that allow direct estimates of the ionization states. ISMabs is provided in the appropriate format to be implemented in widely used X-ray spectral fitting packages such as XSPEC, ISIS, and SHERPA.
C1 [Gatuzz, E.; Mendoza, C.] IVIC, Ctr Fis, Caracas 1020A, Venezuela.
[Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
RP Gatuzz, E (reprint author), IVIC, Ctr Fis, POB 20632, Caracas 1020A, Venezuela.
EM egatuzz@ivic.gob.ve; javier@head.cfa.harvard.edu;
timothy.r.kallman@nasa.gov; claudio@ivic.gob.ve;
thomas.gorczyca@wmich.edu
OI Mendoza, Claudio/0000-0002-2854-4806
FU Chandra Theory Program [15400673]
FX This work was supported by grant 15400673 of the Chandra Theory Program.
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ER
PT J
AU Guo, YC
Ferguson, HC
Bell, EF
Koo, DC
Conselice, CJ
Giavalisco, M
Kassin, S
Lu, Y
Lucas, R
Mandelker, N
McIntosh, DM
Primack, JR
Ravindranath, S
Barro, G
Ceverino, D
Dekel, A
Faber, SM
Fang, JJ
Koekemoer, AM
Noeske, K
Rafelski, M
Straughn, A
AF Guo, Yicheng
Ferguson, Henry C.
Bell, Eric F.
Koo, David C.
Conselice, Christopher J.
Giavalisco, Mauro
Kassin, Susan
Lu, Yu
Lucas, Ray
Mandelker, Nir
McIntosh, Daniel M.
Primack, Joel R.
Ravindranath, Swara
Barro, Guillermo
Ceverino, Daniel
Dekel, Avishai
Faber, Sandra M.
Fang, Jerome J.
Koekemoer, Anton M.
Noeske, Kai
Rafelski, Marc
Straughn, Amber
TI CLUMPY GALAXIES IN CANDELS. I. THE DEFINITION OF UV CLUMPS AND THE
FRACTION OF CLUMPY GALAXIES AT 0.5 < z < 3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: irregular; galaxies:
starburst; galaxies: star formation; galaxies: structure
ID STAR-FORMING GALAXIES; SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; ULTRA DEEP
FIELD; EXTRAGALACTIC LEGACY SURVEY; KILOPARSEC-SCALE CLUMPS; ACTIVE
GALACTIC NUCLEI; LESS-THAN 1.5; H II REGIONS; HIGH-REDSHIFT
AB Although giant clumps of stars are thought to be crucial to galaxy formation and evolution, the most basic demographics of clumps are still uncertain, mainly because the definition of clumps has not been thoroughly discussed. In this paper, we carry out a study of the basic demographics of clumps in star-forming galaxies at 0.5 < z < 3, using our proposed physical definition that UV-bright clumps are discrete star-forming regions that individually contribute more than 8% of the rest-frame UV light of their galaxies. Clumps defined this way are significantly brighter than the H II regions of nearby large spiral galaxies, either individually or blended, when physical spatial resolution and cosmological dimming are considered. Under this definition, we measure the fraction of star-forming galaxies that have at least one off-center clump (f(clumpy)) and the contributions of clumps to the rest-frame UV light and star formation rate (SFR) of star-forming galaxies in the CANDELS/GOODS-S and UDS fields, where our mass-complete sample consists of 3239 galaxies with axial ratio q > 0.5. The redshift evolution of f(clumpy) changes with the stellar mass (M-*) of the galaxies. Low-mass (log(M-*/M-circle dot) < 9.8) galaxies keep an almost constant f(clumpy) of similar to 60% from z similar to 3 to z similar to 0.5. Intermediate-mass and massive galaxies drop their f(clumpy) from 55% at z similar to 3 to 40% and 15%, respectively, at z similar to 0.5. We find that (1) the trend of disk stabilization predicted by violent disk instability matches the f(clumpy) trend of massive galaxies; (2) minor mergers are a viable explanation of the f(clumpy) trend of intermediate-mass galaxies at z < 1.5, given a realistic observability timescale; and (3) major mergers are unlikely responsible for the f(clumpy) trend in all masses at z < 1.5. The clump contribution to the rest-frame UV light of star-forming galaxies shows a broad peak around galaxies with log(M-*/M-circle dot) similar to 10.5 at all redshifts. The clump contribution in the intermediate-mass and massive galaxies is possibly linked to the molecular gas fraction of the galaxies. The clump contribution to the SFR of star-forming galaxies, generally around 4%-10%, also shows dependence on the galaxy M-*, but for a given galaxy M-*, its dependence on the redshift is mild.
C1 [Guo, Yicheng; Koo, David C.; Barro, Guillermo; Faber, Sandra M.; Fang, Jerome J.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ferguson, Henry C.; Kassin, Susan; Lucas, Ray; Ravindranath, Swara; Koekemoer, Anton M.; Noeske, Kai] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Lu, Yu] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA USA.
[Mandelker, Nir; Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel.
[McIntosh, Daniel M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Ceverino, Daniel] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Rafelski, Marc; Straughn, Amber] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Guo, YC (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM ycguo@ucolick.org
OI Kassin, Susan/0000-0002-3838-8093; Koekemoer, Anton/0000-0002-6610-2048;
Bell, Eric/0000-0002-5564-9873
FU NASA through a grant from the Space Telescope Science Institute
[HST-GO-12060, HST-GO-13309]; NASA [NAS5-26555]; NSF [AST 08-08133]
FX We thank the anonymous referee for constructive comments that improve
this article. Support for Program number HST-GO-12060 and HST-GO-13309
were 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 partial support from NSF grant AST 08-08133.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000349236900039
ER
PT J
AU Henderson, BL
Gudipati, MS
AF Henderson, Bryana L.
Gudipati, Murthy S.
TI DIRECT DETECTION OF COMPLEX ORGANIC PRODUCTS IN ULTRAVIOLET (Ly alpha)
AND ELECTRON-IRRADIATED ASTROPHYSICAL AND COMETARY ICE ANALOGS USING
TWO-STEP LASER ABLATION AND IONIZATION MASS SPECTROMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; evolution; ISM: molecules; methods:
laboratory: solid state; molecular processes; radiation mechanisms:
non-thermal; techniques: spectroscopic
ID MOLECULAR LINE SURVEY; STAR-FORMING REGIONS; RACEMIC AMINO-ACIDS; O1
HALE-BOPP; INTERSTELLAR ICE; METHYL FORMATE; COSMIC-RAY; ORION-KL;
EXTRATERRESTRIAL ICES; CLATHRATE STRUCTURES
AB As discovery of complex molecules and ions in our solar system and the interstellar medium has proliferated, several groups have turned to laboratory experiments in an effort to simulate and understand these chemical processes. So far only infrared (IR) and ultraviolet (UV) spectroscopy has been able to directly probe these reactions in ices in their native, low-temperature states. Here we report for the first time results using a complementary technique that harnesses two-step two-color laser ablation and ionization to measure mass spectra of energetically processed astrophysical and cometary ice analogs directly without warming the ices-a method for hands-off in situ ice analysis. Electron bombardment and UV irradiation of H2O, CH3OH, and NH3 ices at 5K and 70K led to complex irradiation products, including HCO, CH3CO, formamide, acetamide, methyl formate, and HCN. Many of these species, whose assignment was also strengthened by isotope labeling studies and correlate with IR-based spectroscopic studies of similar irradiated ices, are important ingredients for the building blocks of life. Some of them have been detected previously via astronomical observations in the interstellar medium and in cometary comae. Other species such as CH3CO (acetyl) are yet to be detected in astrophysical ices or interstellar medium. Our studies suggest that electron and UV photon processing of astrophysical ice analogs leads to extensive chemistry even in the coldest reaches of space, and lend support to the theory of comet-impact-induced delivery of complex organics to the inner solar system.
C1 [Henderson, Bryana L.; Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Gudipati, Murthy/F-7575-2011
FU JPL's DRDF; NASA Spitzer Science Center; NASA funding through Planetary
Atmospheres and Cassini Data Analysis Programs; NASA Postdoctoral
Program for a NPP fellowship
FX This research was enabled through partial funding from JPL's DRDF and
R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" at
JPL, NASA Spitzer Science Center, NASA funding through Planetary
Atmospheres and Cassini Data Analysis Programs. This research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. B. L. H. thanks NASA Postdoctoral Program for a NPP
fellowship. We thank Dr. Robert Wagner (Karlsruhe Institute of
Technology, Germany) for helping with the LabView software integration
of the experimental setup.
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SC Astronomy & Astrophysics
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UT WOS:000349236900066
ER
PT J
AU Kuhn, J
Mennesson, B
Liewer, K
Martin, S
Loya, F
Millan-gabet, R
Serabyn, E
AF Kuehn, J.
Mennesson, B.
Liewer, K.
Martin, S.
Loya, F.
Millan-gabet, R.
Serabyn, E.
TI EXPLORING INTERMEDIATE (5-40AU) SCALES AROUND AB AURIGAE WITH THE
PALOMAR FIBER NULLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: interferometers; protoplanetary disks-stars: individual
(AB Aurigae); stars: pre-main sequence; stars: variables: T Tauri,
Herbig Ae/Be; techniques: interferometric
ID NEAR-INFRARED EMISSION; HERBIG-AE/BE STARS; HALE TELESCOPE; DISK;
OBJECTS; IOTA; AU; INTERFEROMETER; OPTICS; DUST
AB We report on recent K-s-band interferometric observations of the young pre-main-sequence star AB Aurigae obtained with the Palomar Fiber Nuller (PFN). Reaching a contrast of a few 10(-4) inside a field of view extending from 35 to 275 mas (5-40 AU at AB Aur's distance), the PFN is able to explore angular scales that are intermediate between those accessed by coronagraphic imaging and long baseline interferometry. This intermediate region is of special interest given that many young stellar objects are believed to harbor extended halos at such angular scales. Using destructive interference (nulling) between two sub-apertures of the Palomar 200 inch telescope and rotating the telescope pupil, we measured a resolved circumstellar excess at all probed azimuth angles. The astrophysical null measured over the full rotation is fairly constant, with a mean value of 1.52%, and a slight additional azimuthal modulation of +/- 0.2%. The isotropic astrophysical null is indicative of circumstellar emission dominated by an azimuthally extended source, possibly a halo, or one or more rings of dust, accounting for several percent of the total K-s-band flux. The modest azimuthal variation may be explained by some skewness or anisotropy of the spatially extended source, e.g., an elliptical or spiral geometry, or clumping, but it could also be due to the presence of a point source located at a separation of similar to 120 mas (17 AU) with similar to 6 x 10(-3) of the stellar flux. We combine our results with previous Infrared Optical Telescope Array observations of AB Aur at H band, and demonstrate that a dust ring located at similar to 30 mas (4.3 AU) represents the best-fitting model to explain both sets of visibilities. We are also able to test a few previously hypothesized models of the incoherent component evident at longer interferometric baselines.
C1 [Kuehn, J.; Mennesson, B.; Liewer, K.; Martin, S.; Loya, F.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Millan-gabet, R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Kuhn, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jonas.kuehn@a3.epfl.ch
RI Kuhn, Jonas/H-2338-2011
OI Kuhn, Jonas/0000-0002-6344-4835
FU Swiss National Science Foundation [PA00 P2 136416]
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. The data presented
are based on observations obtained at the Hale Telescope, Palomar
Observatory, as part of a continuing collaboration between Caltech,
NASA/JPL, and Cornell University. We particularly thank the staff of the
Palomar Observatory for their assistance in mounting the PFN and in
conducting the observations at the Hale telescope. J.K. is supported by
a Swiss National Science Foundation Advanced Postdoc Mobility fellowship
(PA00 P2 136416). We also thank Rens Waters for the helpful discussions.
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UT WOS:000349236900055
ER
PT J
AU Liao, K
Treu, T
Marshall, P
Fassnacht, CD
Rumbaugh, N
Dobler, G
Aghamousa, A
Bonvin, V
Courbin, F
Hojjati, A
Jackson, N
Kashyap, V
Kumar, SR
Linder, E
Mandel, K
Meng, XL
Meylan, G
Moustakas, LA
Prabhu, TP
Romero-Wolf, A
Shafieloo, A
Siemiginowska, A
Stalin, CS
Tak, H
Tewes, M
van Dyk, D
AF Liao, Kai
Treu, Tommaso
Marshall, Phil
Fassnacht, Christopher D.
Rumbaugh, Nick
Dobler, Gregory
Aghamousa, Amir
Bonvin, Vivien
Courbin, Frederic
Hojjati, Alireza
Jackson, Neal
Kashyap, Vinay
Kumar, S. Rathna
Linder, Eric
Mandel, Kaisey
Meng, Xiao-Li
Meylan, Georges
Moustakas, Leonidas A.
Prabhu, Tushar P.
Romero-Wolf, Andrew
Shafieloo, Arman
Siemiginowska, Aneta
Stalin, Chelliah S.
Tak, Hyungsuk
Tewes, Malte
van Dyk, David
TI STRONG LENS TIME DELAY CHALLENGE. II. RESULTS OF TDC1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: strong; methods: data analysis
ID HUBBLE CONSTANT; COSMOLOGICAL PARAMETERS; EXPANSION HISTORY; DARK
ENERGY; QUASARS; VARIABILITY; COSMOGRAIL; DISTANCES; GALAXIES; UNIVERSE
AB We present the results of the first strong lens time delay challenge. The motivation, experimental design, and entry level challenge are described in a companion paper. This paper presents the main challenge, TDC1, which consisted of analyzing thousands of simulated light curves blindly. The observational properties of the light curves cover the range in quality obtained for current targeted efforts (e.g., COSMOGRAIL) and expected from future synoptic surveys (e.g., LSST), and include simulated systematic errors. Seven teams participated in TDC1, submitting results from 78 different method variants. After describing each method, we compute and analyze basic statisticsmeasuring accuracy (or bias) A, goodness of fit chi(2), precision P, and success rate f. For some methods we identify outliers as an important issue. Other methods show that outliers can be controlled via visual inspection or conservative quality control. Several methods are competitive, i.e., give vertical bar A vertical bar < 0.03, P < 0.03, and chi(2) < 1.5, with some of the methods already reaching sub-percent accuracy. The fraction of light curves yielding a time delay measurement is typically in the range f = 20%-40%. It depends strongly on the quality of the data: COSMOGRAIL-quality cadence and light curve lengths yield significantly higher f than does sparser sampling. Taking the results of TDC1 at face value, we estimate that LSST should provide around 400 robust time-delay measurements, each with P < 0.03 and vertical bar A vertical bar < 0.01, comparable to current lens modeling uncertainties. In terms of observing strategies, we find that A and f depend mostly on season length, while P depends mostly on cadence and campaign duration.
C1 [Liao, Kai] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China.
[Liao, Kai; Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Marshall, Phil] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA.
[Fassnacht, Christopher D.; Rumbaugh, Nick] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Dobler, Gregory] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Aghamousa, Amir; Shafieloo, Arman] Asia Pacific Ctr Theoret Phys, Pohang 790784, Gyeongbuk, South Korea.
[Bonvin, Vivien; Courbin, Frederic; Meylan, Georges] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland.
[Hojjati, Alireza] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hojjati, Alireza] Simon Fraser Univ, Dept Phys, Burnaby, BC V5A 1S6, Canada.
[Jackson, Neal] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Kashyap, Vinay; Mandel, Kaisey; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kumar, S. Rathna; Prabhu, Tushar P.; Stalin, Chelliah S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Linder, Eric] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Linder, Eric] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Linder, Eric] Korea Astron & Space Sci Inst, Taejon 305248, South Korea.
[Meng, Xiao-Li; Tak, Hyungsuk] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA.
[Moustakas, Leonidas A.; Romero-Wolf, Andrew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shafieloo, Arman] POSTECH, Dept Phys, Pohang 790784, Gyeongbuk, South Korea.
[Tewes, Malte] Argelander Inst Astron, D-53121 Bonn, Germany.
[van Dyk, David] Univ London Imperial Coll Sci Technol & Med, Dept Math, London SW7 2AZ, England.
[Liao, Kai; Treu, Tommaso] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Dobler, Gregory] NYU, Ctr Urban Sci Progress, Brooklyn, NY 11201 USA.
RP Liao, K (reprint author), Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China.
OI Prabhu, Tushar/0000-0003-0797-5057; Moustakas,
Leonidas/0000-0003-3030-2360
FU National Science Foundation collaborative grant "Collaborative Research:
Accurate cosmology with strong gravitational lens time delays"
[AST-1312329, AST-1450141]; Packard Foundation through a Packard
Research Fellowship; China Scholarship Council; U.S. Department of
Energy [DE-AC02-76SF00515]; Swiss National Science Foundation (SNSF);
DFG [Hi 1495/2-1]; Korea Ministry of Education, Science and Technology,
Gyeongsangbuk-Do; Pohang City for Independent Junior Research Groups at
the Asia Pacific Center for Theoretical Physics; National Research
Foundation of Korea [NRF-2013R1A1A2013795]; DOE [DE-SC-0007867,
DE-AC02-05CH11231]; NSERC grant; NSF [AST-1211196]
FX We acknowledge the LSST Dark Energy Science Collaboration for hosting
several meetings of the "Evil" Team, and the private code repository
used in this work. We thank the referee for constructive criticism which
helped improved this paper. T.T., C.D.F., and K.L. acknowledge support
from the National Science Foundation collaborative grant "Collaborative
Research: Accurate cosmology with strong gravitational lens time delays"
(AST-1312329 and AST-1450141). T.T. gratefully acknowledges support by
the Packard Foundation through a Packard Research Fellowship. K.L. is
supported by China Scholarship Council. The work of P.J.M. was supported
by the U.S. Department of Energy under contract number
DE-AC02-76SF00515. V.B. and F.C. are supported by the Swiss National
Science Foundation (SNSF). M.T. acknowledges support by the DFG grant Hi
1495/2-1. A.A and A.S. wish to acknowledge support from the Korea
Ministry of Education, Science and Technology, Gyeongsangbuk-Do and
Pohang City for Independent Junior Research Groups at the Asia Pacific
Center for Theoretical Physics. A.S. would like to acknowledge the
support of the National Research Foundation of Korea
(NRF-2013R1A1A2013795). E.L. is supported by DOE grant DE-SC-0007867 and
contract No. DE-AC02-05CH11231. A.H. is supported by an NSERC grant and
thanks the Institute for the Early Universe, Korea, for computational
resources. A.A., A.S., A.H., and E.L. thank IBS Korea for hospitality.
The work of L.A.M. and A.R.W. was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. K.M. is supported at
Harvard by NSF grant AST-1211196.
NR 46
TC 20
Z9 20
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2015
VL 800
IS 1
AR 11
DI 10.1088/0004-637X/800/1/11
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900011
ER
PT J
AU Matsuura, M
Dwek, E
Barlow, MJ
Babler, B
Baes, M
Meixner, M
Cernicharo, J
Clayton, GC
Dunne, L
Fransson, C
Fritz, J
Gear, W
Gomez, HL
Groenewegen, MAT
Indebetouw, R
Ivison, RJ
Jerkstrand, A
Lebouteiller, V
Lim, TL
Lundqvist, P
Pearson, CP
Roman-Duval, J
Royer, P
Staveley-Smith, L
Swinyard, BM
van Hoof, PAM
van Loon, JT
Verstappen, J
Wesson, R
Zanardo, G
Blommaert, JADL
Decin, L
Reach, WT
Sonneborn, G
Van de Steene, GC
Yates, JA
AF Matsuura, M.
Dwek, E.
Barlow, M. J.
Babler, B.
Baes, M.
Meixner, M.
Cernicharo, Jose
Clayton, Geoff C.
Dunne, L.
Fransson, C.
Fritz, Jacopo
Gear, Walter
Gomez, H. L.
Groenewegen, M. A. T.
Indebetouw, R.
Ivison, R. J.
Jerkstrand, A.
Lebouteiller, V.
Lim, T. L.
Lundqvist, P.
Pearson, C. P.
Roman-Duval, J.
Royer, P.
Staveley-Smith, Lister
Swinyard, B. M.
van Hoof, P. A. M.
van Loon, J. Th.
Verstappen, Joris
Wesson, Roger
Zanardo, Giovanna
Blommaert, Joris A. D. L.
Decin, Leen
Reach, W. T.
Sonneborn, George
Van de Steene, Griet C.
Yates, Jeremy A.
TI A STUBBORNLY LARGE MASS OF COLD DUST IN THE EJECTA OF SUPERNOVA 1987A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; infrared: stars; ISM: supernova
remnants; submillimeter: ISM; submillimeter: stars; supernovae:
individual (Supernova 1987A)
ID CORE-COLLAPSE SUPERNOVAE; LARGE-MAGELLANIC-CLOUD; SN 1987A; INTERSTELLAR
DUST; CRAB-NEBULA; EARLY UNIVERSE; HIGH-REDSHIFT; P SUPERNOVAE;
LIGHT-CURVE; STAR MASS
AB We present new Herschel photometric and spectroscopic observations of Supernova 1987A, carried out in 2012. Our dedicated photometric measurements provide new 70 mu m data and improved imaging quality at 100 and 160 mu m compared to previous observations in 2010. Our Herschel spectra show only weak CO line emission, and provide an upper limit for the 63 mu m [O-I] line flux, eliminating the possibility that line contaminations distort the previously estimated dustmass. The far-infrared spectral energy distribution (SED) is well fitted by thermal emission from cold dust. The newly measured 70 mu m flux constrains the dust temperature, limiting it to nearly a single temperature. The far-infrared emission can be fitted by 0.5 +/- 0.1M(circle dot) of amorphous carbon, about a factor of two larger than the current nucleosynthetic mass prediction for carbon. The observation of SiO molecules at early and late phases suggests that silicates may also have formed and we could fit the SED with a combination of 0.3M(circle dot) of amorphous carbon and 0.5M(circle dot) of silicates, totalling 0.8M(circle dot) of dust. Our analysis thus supports the presence of a large dust reservoir in the ejecta of SN 1987A. The inferred dust mass suggests that supernovae can be an important source of dust in the interstellar medium, from local to high-redshift galaxies.
C1 [Matsuura, M.; Barlow, M. J.; Swinyard, B. M.; Yates, Jeremy A.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Dwek, E.; Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab Code 665, Greenbelt, MD 20771 USA.
[Babler, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Baes, M.; Fritz, Jacopo; Verstappen, Joris] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Meixner, M.; Roman-Duval, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Cernicharo, Jose] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28850 Madrid, Spain.
[Clayton, Geoff C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Dunne, L.; Ivison, R. J.] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Fransson, C.; Lundqvist, P.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Gear, Walter; Gomez, H. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Groenewegen, M. A. T.; van Hoof, P. A. M.; Van de Steene, Griet C.] Koninklijke Sterrenwacht Belgie, B-1180 Brussels, Belgium.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ivison, R. J.] European So Observ, D-85748 Garching, Germany.
[Jerkstrand, A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Lebouteiller, V.] CEA Saclay, AIM, F-91191 Gif Sur Yvette, France.
[Lim, T. L.; Pearson, C. P.; Swinyard, B. M.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Royer, P.; Blommaert, Joris A. D. L.; Decin, Leen] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Staveley-Smith, Lister; Zanardo, Giovanna] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
[van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Verstappen, Joris] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands.
[Wesson, Roger] European So Observ, Santiago 19001, Chile.
[Blommaert, Joris A. D. L.] Vrije Univ Brussel, Dept Phys & Astrophys, Astron & Astrophys Res Grp, B-1050 Brussels, Belgium.
[Reach, W. T.] Univ Space Res Assoc, NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
RP Matsuura, M (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM mikako@star.ucl.ac.uk
RI Barlow, Michael/A-5638-2009; Jerkstrand, Anders/K-9648-2015; Ivison,
R./G-4450-2011; Staveley-Smith, Lister/A-1683-2011;
OI Barlow, Michael/0000-0002-3875-1171; Jerkstrand,
Anders/0000-0001-8005-4030; Ivison, R./0000-0001-5118-1313;
Staveley-Smith, Lister/0000-0002-8057-0294; Fransson,
Claes/0000-0001-8532-3594; Lebouteiller, Vianney/0000-0002-7716-6223;
Reach, William/0000-0001-8362-4094; Cernicharo, Jose/0000-0002-3518-2524
FU UK STFC [ST/J001511/1]; European Research Council; Belgian Science
Policy Office through the ESA PRODEX program
FX M.M. acknowledges support from the UK STFC (ST/J001511/1). R.J.I. and L.
Dunne acknowledge support from the European Research Council in the form
of Advanced Grant COSMICISM. P.v.H. acknowledges support from the
Belgian Science Policy Office through the ESA PRODEX program.
NR 67
TC 34
Z9 34
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2015
VL 800
IS 1
AR 50
DI 10.1088/0004-637X/800/1/50
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900050
ER
PT J
AU Montez, R
Kastner, JH
Balick, B
Behar, E
Blackman, E
Bujarrabal, V
Chu, YH
Corradi, RLM
De Marco, O
Frank, A
Freeman, M
Frew, DJ
Guerrero, MA
Jones, D
Lopez, JA
Miszalski, B
Nordhaus, J
Parker, QA
Sahai, R
Sandin, C
Schonberner, D
Soker, N
Sokoloski, JL
Steffen, M
Toala, JA
Ueta, T
Villaver, E
Zijlstra, A
AF Montez, R., Jr.
Kastner, J. H.
Balick, B.
Behar, E.
Blackman, E.
Bujarrabal, V.
Chu, Y. -H.
Corradi, R. L. M.
De Marco, O.
Frank, A.
Freeman, M.
Frew, D. J.
Guerrero, M. A.
Jones, D.
Lopez, J. A.
Miszalski, B.
Nordhaus, J.
Parker, Q. A.
Sahai, R.
Sandin, C.
Schonberner, D.
Soker, N.
Sokoloski, J. L.
Steffen, M.
Toala, J. A.
Ueta, T.
Villaver, E.
Zijlstra, A.
TI THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION
FROM THE CENTRAL STARS OF PLANETARY NEBULAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary nebulae: general
ID BINARY CENTRAL STAR; MAGNETIC WHITE-DWARFS; GIANT BRANCH STARS; OLD
PLANETARIES; HELIX-NEBULA; SKY SURVEY; MASS-LOSS; O STARS; EVOLUTION;
STELLAR
AB We present X-ray spectral analysis of 20 point-like X-ray sources detected in Chandra Planetary Nebula Survey observations of 59 planetary nebulae (PNe) in the solar neighborhood. Most of these 20 detections are associated with luminous central stars within relatively young, compact nebulae. The vast majority of these point-like X-ray-emitting sources at PN cores display relatively "hard" (>= 0.5 keV) X-ray emission components that are unlikely to be due to photospheric emission from the hot central stars (CSPN). Instead, we demonstrate that these sources are well modeled by optically thin thermal plasmas. From the plasma properties, we identify two classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray luminosities, L-X, that appear uncorrelated with the CSPN bolometric luminosity, L-bol and (2) lower-temperature plasmas with L-X/L-bol similar to 10(-7). We suggest these two classes correspond to the physical processes of magnetically active binary companions and self-shocking stellar winds, respectively. In many cases this conclusion is supported by corroborative multiwavelength evidence for the wind and binary properties of the PN central stars. By thus honing in on the origins of X-ray emission from PN central stars, we enhance the ability of CSPN X-ray sources to constrain models of PN shaping that invoke wind interactions and binarity.
C1 [Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37212 USA.
[Kastner, J. H.; Freeman, M.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Kastner, J. H.; Freeman, M.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
[Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Behar, E.; Soker, N.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Blackman, E.; Frank, A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Blackman, E.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA.
[Bujarrabal, V.] Observ Astron Nacl, Alcala De Henares, Spain.
[Chu, Y. -H.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan.
[Corradi, R. L. M.; Jones, D.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[De Marco, O.; Frew, D. J.; Parker, Q. A.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[De Marco, O.; Frew, D. J.; Parker, Q. A.] Macquarie Univ, Macquarie Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia.
[Guerrero, M. A.; Toala, J. A.] CSIC, IAA, E-18008 Granada, Spain.
[Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico.
[Miszalski, B.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Miszalski, B.] Southern African Large Telescope Fdn, ZA-7935 Observatory, South Africa.
[Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA.
[Nordhaus, J.] Rochester Inst Technol, Natl Tech Inst Deaf, Rochester, NY 14623 USA.
[Parker, Q. A.] Australian Astron Observ, Epping, NSW 2121, Australia.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sandin, C.; Schonberner, D.; Steffen, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Ueta, T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Zijlstra, A.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
RP Montez, R (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37212 USA.
RI Jones, David/G-8109-2014
OI Guerrero, Martin/0000-0002-7759-106X; Frew, David/0000-0002-3108-5284;
Balick, Bruce/0000-0002-3139-3201; Jones, David/0000-0003-3947-5946
FU Chandra X-ray Observatory Center [GO1-12025A, GO3-14019A, GO3-14019B];
NASA [NAS8-03060]; IBM-Einstein Fellowship at IAS; Simons Foundation
Fellowship; Spanish MICINN [AYA 2011-29754-C03-02]; FEDER funds
FX This research was supported via award numbers GO1-12025A and GO3-14019A
to Rochester Institute of Technology and GO3-14019B to Vanderbilt
University issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of NASA under contract NAS8-03060 (RIT). R.S.'s contribution to the
research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA, and supported via an award issued by the Chandra X-Ray Observatory
Center. This research has made use of data obtained from the Chandra
Data Archive and the Chandra Source Catalog, and software provided by
the Chandra X-ray Center (CXC) in the application packages CIAO. This
research has made use of data and/or software provided by the High
Energy Astrophysics Science Archive Research Center (HEASARC), which is
a service of the Astrophysics Science Division at NASA/GSFC and the High
Energy Astrophysics Division of the Smithsonian Astrophysical
Observatory. E.B. acknowledges support from an IBM-Einstein Fellowship
at IAS, and a Simons Foundation Fellowship. J.A.T. and M.A.G. are
supported by the Spanish MICINN grant AYA 2011-29754-C03-02 co-funded
with FEDER funds.
NR 75
TC 3
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2015
VL 800
IS 1
AR 8
DI 10.1088/0004-637X/800/1/8
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900008
ER
PT J
AU Schimoia, JS
Storchi-Bergmann, T
Grupe, D
Eracleous, M
Peterson, BM
Baldwin, JA
Nemmen, RS
Winge, C
AF Schimoia, Jaderson S.
Storchi-Bergmann, Thaisa
Grupe, Dirk
Eracleous, Michael
Peterson, Bradley M.
Baldwin, Jack A.
Nemmen, Rodrigo S.
Winge, Claudia
TI SHORT-TIMESCALE MONITORING OF THE X-RAY, UV, AND BROAD DOUBLE-PEAK
EMISSION LINE OF THE NUCLEUS OF NGC 1097
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: individual (NGC 1097); galaxies:
nuclei; galaxies: Seyfert; line: profiles
ID ACTIVE GALACTIC NUCLEI; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; TERM
PROFILE VARIABILITY; GALAXY 3C 390.3; ACCRETION DISK; BLACK-HOLE; BALMER
LINES; REGION SIZES; ARP 102B; NGC-1097
AB Recent studies have suggested that the short-timescale (less than or similar to 7 days) variability of the broad (similar to 10,000 km s(-1)) double-peaked H alpha profile of the LINER nucleus of NGC 1097 could be driven by a variable X-ray emission from a central radiatively inefficient accretion flow. To test this scenario, we have monitored the NGC 1097 nucleus in X-ray and UV continuum with Swift and the H alpha flux and profile in the optical spectrum using SOAR and Gemini-South from 2012 August to 2013 February. During the monitoring campaign, the H alpha flux remained at a very low level-three times lower than the maximum flux observed in previous campaigns and showing only limited (similar to 20%) variability. The X-ray variations were small, only similar to 13% throughout the campaign, while the UV did not show significant variations. We concluded that the timescale of the H alpha profile variation is close to the sampling interval of the optical observations, which results in only a marginal correlation between the X-ray and H alpha fluxes. We have caught the active galaxy nucleus in NGC 1097 in a very low activity state, in which the ionizing source was very weak and capable of ionizing just the innermost part of the gas in the disk. Nonetheless, the data presented here still support the picture in which the gas that emits the broad double-peaked Balmer lines is illuminated/ionized by a source of high-energy photons which is located interior to the inner radius of the line-emitting part of the disk.
C1 [Schimoia, Jaderson S.; Storchi-Bergmann, Thaisa] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil.
[Storchi-Bergmann, Thaisa; Peterson, Bradley M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Storchi-Bergmann, Thaisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Grupe, Dirk] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA.
[Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Eracleous, Michael] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Peterson, Bradley M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Baldwin, Jack A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48864 USA.
[Nemmen, Rodrigo S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508090 Sao Paulo, Brazil.
[Winge, Claudia] Gemini South Observ, La Serena, Chile.
[Grupe, Dirk] Swift Miss Operat Ctr, State Coll, PA 16801 USA.
[Eracleous, Michael] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Eracleous, Michael] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nemmen, Rodrigo S.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
RP Schimoia, JS (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, Campus Vale, Porto Alegre, RS, Brazil.
EM silva.schimoia@ufrgs.br
RI Nemmen, Rodrigo/O-6841-2014;
OI Grupe, Dirk/0000-0002-9961-3661
FU CNPq; National Council for Scientific and Technological
Development-Brazil; NASA Swift program [NAS5-00136]; NSF [AST-1008882];
NSF; National Science Foundation (United States); National Research
Council (Canada); CONICYT (Chile); Australian Research Council
(Australia); Ministerio da Ciencia, Tecnologia e Inovacao (Brazil);
Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina)
FX J.S.S. acknowledges CNPq, the National Council for Scientific and
Technological Development-Brazil, for support and The Ohio State
University for their hospitality. At Penn State, D.G. and M.E.
acknowledge support from the NASA Swift program through contract
NAS5-00136. Additionally, M.E. acknowledges the warm hospitality of the
Center for Relativistic Astrophysics at Georgia Tech and the Department
of Astronomy at the University of Washington. B.M.P. is grateful for
support by the NSF through grant AST-1008882 to The Ohio State
University.; This research has made use of the XRT Data Analysis
Software (XRTDAS) developed under the responsibility of the ASI Science
Data Center (ASDC), Italy. This research has made use of data obtained
through the High Energy Astrophysics Science Archive Research Center
Online Service, provided by the NASA/Goddard Space Flight Center. This
research is based on observations obtained at the Southern Astrophysical
Research (SOAR) telescope, which is a joint project of the Ministerio da
Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do
Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the
University of North Carolina at Chapel Hill (UNC), and Michigan State
University (MSU). This research is also based on observations obtained
at the Gemini Observatory, which is operated by the Association of
Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina).
NR 45
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2015
VL 800
IS 1
AR 63
DI 10.1088/0004-637X/800/1/63
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900063
ER
PT J
AU Vanderburg, A
Montet, BT
Johnson, JA
Buchhave, LA
Zeng, L
Pepe, F
Cameron, AC
Latham, DW
Molinari, E
Udry, S
Lovis, C
Matthews, JM
Cameron, C
Law, N
Bowler, BP
Angus, R
Baranec, C
Bieryla, A
Boschin, W
Charbonneau, D
Cosentino, R
Dumusque, X
Figueira, P
Guenther, DB
Harutyunyan, A
Hellier, C
Kuschnig, R
Lopez-Morales, M
Mayor, M
Micela, G
Moffat, AFJ
Pedani, M
Phillip, DF
Piotto, G
Pollacco, D
Queloz, D
Rice, K
Riddle, R
Rowe, JF
Rucinski, SM
Sasselov, D
Segransan, D
Sozzetti, A
Szentgyorgyi, A
Watson, C
Weiss, WW
AF Vanderburg, Andrew
Montet, Benjamin T.
Johnson, John Asher
Buchhave, Lars A.
Zeng, Li
Pepe, Francesco
Cameron, Andrew Collier
Latham, David W.
Molinari, Emilio
Udry, Stephane
Lovis, Christophe
Matthews, Jaymie M.
Cameron, Chris
Law, Nicholas
Bowler, Brendan P.
Angus, Ruth
Baranec, Christoph
Bieryla, Allyson
Boschin, Walter
Charbonneau, David
Cosentino, Rosario
Dumusque, Xavier
Figueira, Pedro
Guenther, David B.
Harutyunyan, Avet
Hellier, Coel
Kuschnig, Rainer
Lopez-Morales, Mercedes
Mayor, Michel
Micela, Giusi
Moffat, Anthony F. J.
Pedani, Marco
Phillip, David F.
Piotto, Giampaolo
Pollacco, Don
Queloz, Didier
Rice, Ken
Riddle, Reed
Rowe, Jason F.
Rucinski, Slavek M.
Sasselov, Dimitar
Segransan, Damien
Sozzetti, Alessandro
Szentgyorgyi, Andrew
Watson, Chris
Weiss, Werner W.
TI CHARACTERIZING K2 PLANET DISCOVERIES: A SUPER-EARTH TRANSITING THE
BRIGHT K DWARF HIP 116454
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: detection; techniques: photometric
ID LASER ADAPTIVE OPTICS; NEPTUNE-MASS PLANET; SKY SURVEY; PROPER-MOTION;
SHORT-PERIOD; HD 97658B; EXOPLANET; KEPLER; STARS; MISSION
AB We report the first planet discovery from the two-wheeled Kepler (K2) mission: HIP 116454 b. The host star HIP 116454 is a bright (V = 10.1, K = 8.0) K1 dwarf with high proper motion and a parallax-based distance of 55.2 +/- 5.4 pc. Based on high-resolution optical spectroscopy, we find that the host star is metal-poor with [Fe/H]= -0.16 +/- 0.08 and has a radius R-star = 0.716 +/- 0.024 R-circle dot and mass M-star = 0.775 +/- 0.027M(circle dot). The star was observed by the Kepler spacecraft during its Two-Wheeled Concept Engineering Test in 2014 February. During the 9 days of observations, K2 observed a single transit event. Using a new K2 photometric analysis technique, we are able to correct small telescope drifts and recover the observed transit at high confidence, corresponding to a planetary radius of R-p = 2.53 +/- 0.18 R-circle plus. Radial velocity observations with the HARPS-N spectrograph reveal a 11.82 +/- 1.33 M-circle plus planet in a 9.1 day orbit, consistent with the transit depth, duration, and ephemeris. Follow-up photometric measurements from the MOST satellite confirm the transit observed in the K2 photometry and provide a refined ephemeris, making HIP 116454 b amenable for future follow-up observations of this latest addition to the growing population of transiting super-Earths around nearby, bright stars.
C1 [Vanderburg, Andrew; Montet, Benjamin T.; Johnson, John Asher; Buchhave, Lars A.; Zeng, Li; Latham, David W.; Angus, Ruth; Bieryla, Allyson; Charbonneau, David; Dumusque, Xavier; Lopez-Morales, Mercedes; Phillip, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Montet, Benjamin T.; Bowler, Brendan P.; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA.
[Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Mayor, Michel; Segransan, Damien] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Molinari, Emilio; Boschin, Walter; Cosentino, Rosario; Harutyunyan, Avet; Pedani, Marco; Piotto, Giampaolo] INAF Fdn Galileo Galilei, E-38712 Brena Baja, Spain.
[Molinari, Emilio; Piotto, Giampaolo] INAF IASF Milano, I-20133 Milan, Italy.
[Matthews, Jaymie M.] Univ British Columbia, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Sydney, NS B1P 6L2, Canada.
[Law, Nicholas] Univ N Carolina, Chapel Hill, NC 27599 USA.
[Angus, Ruth] Univ Oxford, Oxford, England.
[Baranec, Christoph] Univ Hawaii Manoa, Hilo, HI 96720 USA.
[Figueira, Pedro] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal.
[Guenther, David B.] St Marys Univ, Halifax, NS B3H 3C3, Canada.
[Hellier, Coel] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Micela, Giusi] INAF Osservatorio Astron Palermo, I-90124 Palermo, Italy.
[Moffat, Anthony F. J.] Univ Montreal, Montreal, PQ H3C 3J7, Canada.
[Moffat, Anthony F. J.] Obs Mont Megant, Notre Dame Des Bois, PQ J0B 2E0, Canada.
[Pollacco, Don] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Rice, Ken] Univ Edinburgh, Inst Astron, Royal Observ, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rucinski, Slavek M.] Univ Toronto, Toronto, ON M5S 3H4, Canada.
[Sozzetti, Alessandro] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy.
[Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM avanderburg@cfa.harvard.edu
RI Rice, Ken/H-5084-2011; Figueira, Pedro/J-4916-2013;
OI Rice, Ken/0000-0002-6379-9185; Figueira, Pedro/0000-0001-8504-283X;
Sozzetti, Alessandro/0000-0002-7504-365X; Montet,
Benjamin/0000-0001-7516-8308; Zeng, Li/0000-0003-1957-6635; Molinari,
Emilio/0000-0002-1742-7735; Cameron, Andrew/0000-0002-8863-7828;
Buchhave, Lars A./0000-0003-1605-5666
FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA
Science Mission directorate; National Aeronautics and Space
Administration under the Exoplanet Exploration Program; National Science
Foundation Graduate Research Fellowship [DGE 1144152, DGE 1144469];
David and Lucile Packard Foundation; Alfred P. Sloan Foundation;
Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT
[IF/01037/2013]; POPH/FSE (EC) by FEDER through the program "Programa
Operacional de Factores de Competitividade-COMPETE; Austrian Science
Fund [FWF P22691-N16]; European Union Seventh Framework Programme (FP7)
[313014 (ETAEARTH)]; John Templeton Foundation; Prodex program of the
Swiss Space Office (SSO); Harvard University Origin of Life Initiative
(HUOLI); Scottish Universities Physics Alliance (SUPA); University of
Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National
Astrophysical Institute (INAF); University of St. Andrews; Queens
University Belfast; University of Edinburgh; California Institute of
Technology; Inter-University Centre for Astronomy and Astrophysics;
National Science Foundation [AST-0906060, AST-0960343, AST-1207891];
Mount Cuba Astronomical Foundation; W.M. Keck Foundation; UK's Science
and Technology Facilities Council (STFC); U.S. Government [NAG W-2166];
National Geographic Society; National Science Foundation; Sloan
Foundation; Samuel Oschin Foundation; Eastman Kodak Corporation; 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/NotreDame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX Some of the data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX13AC07G and by other
grants and contracts. This paper includes data collected by the Kepler
mission. Funding for the Kepler mission is provided by the NASA Science
Mission directorate.; This research has made use of NASA's Astrophysics
Data System; the SIMBAD database and VizieR catalog access tool,
operated at CDS, Strasbourg, France; the Exoplanet Orbit Database and
the Exoplanet Data Explorer at http://www.exoplanets.org; PyAstronomy,
the repository and documentation for which can be found at
https://github.com/sczesla/PyAstronomy; and the NASA Exoplanet Archive,
which is operated by the California Institute of Technology, under
contract with the National Aeronautics and Space Administration under
the Exoplanet Exploration Program.; A.V. and B.T.M. are supported by the
National Science Foundation Graduate Research Fellowship, grants No. DGE
1144152 and DGE 1144469, respectively. J.A.J. is supported by generous
grants from the David and Lucile Packard and Alfred P. Sloan
Foundations. C.B. acknowledges support from the Alfred P. Sloan
Foundation. P.F. acknowledges support by Fundacao para a Ciencia e a
Tecnologia (FCT) through Investigador FCT contracts of reference
IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program
"Programa Operacional de Factores de Competitividade-COMPETE." W.W.W.
was supported by the Austrian Science Fund (FWF P22691-N16). The
research leading to these results has received funding from the European
Union Seventh Framework Programme (FP7/2007-2013) under grant Agreement
No. 313014 (ETAEARTH). This publication was made possible through the
support of a grant from the John Templeton Foundation. The opinions
expressed in this publication are those of the authors and do not
necessarily reflect the views of the John Templeton Foundation.; This
work is based on observations made with the Italian Telescopio Nazionale
Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo
Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias. The HARPS-N project was funded by the Prodex program of the
Swiss Space Office (SSO), the Harvard University Origin of Life
Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA),
the University of Geneva, the Smithsonian Astrophysical Observatory
(SAO), and the Italian National Astrophysical Institute (INAF),
University of St. Andrews, Queens University Belfast, and University of
Edinburgh.; The Robo-AO system is supported by collaborating partner
institutions, the California Institute of Technology and the
Inter-University Centre for Astronomy and Astrophysics, and by the
National Science Foundation under grant Nos. AST-0906060, AST-0960343,
and AST-1207891, by the Mount Cuba Astronomical Foundation, by a gift
from Samuel Oschin.; Some of the data presented herein were obtained at
the W.M. Keck Observatory, which is operated as a scientific partnership
among the California Institute of Technology, the University of
California, and the National Aeronautics and Space Administration. The
observatory was made possible by the generous financial support of the
W.M. Keck Foundation. The authors wish to recognize and acknowledge the
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.; WASP-South is hosted by the SAAO and SuperWASP by the Isaac
Newton Group and the Instituto de Astrofisica deCanarias; we gratefully
acknowledge their ongoing support and assistance. Funding for WASP comes
from consortium universities and from the UK's Science and Technology
Facilities Council (STFC).; The Digitized Sky Surveys were produced at
the Space Telescope Science Institute under U.S. Government grant NAG
W-2166. The images of these surveys are based on photographic data
obtained using the Oschin Schmidt Telescope on Palomar Mountain and the
U.K. Schmidt Telescope. The plates were processed into the present
compressed digital form with the permission of these institutions.; The
National Geographic Society-Palomar Observatory Sky Atlas (POSS-I) was
made by the California Institute of Technology with grants from the
National Geographic Society. The Second Palomar Observatory Sky Survey
(POSS-II) was made by the California Institute of Technology with funds
from the National Science Foundation, the National Geographic Society,
the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman
Kodak Corporation. The Oschin Schmidt Telescope is operated by the
California Institute of Technology and Palomar Observatory.; Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
participating institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. The SDSS-III web site is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the participating institutions of the SDSS-III
Collaboration, including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, Carnegie Mellon
University, University of Florida, the French Participation Group, the
German Participation Group, Harvard University, the Instituto de
Astrofisica de Canarias, the Michigan State/NotreDame/JINA Participation
Group, Johns Hopkins University, Lawrence Berkeley National Laboratory,
Max Planck Institute for Astrophysics, Max Planck Institute for
Extraterrestrial Physics, New Mexico State University, New York
University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University.
NR 73
TC 31
Z9 31
U1 2
U2 32
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 FEB 10
PY 2015
VL 800
IS 1
AR 59
DI 10.1088/0004-637X/800/1/59
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA9IQ
UT WOS:000349236900059
ER
PT J
AU Cordiner, MA
Palmer, MY
Nixon, CA
Irwin, PGJ
Teanby, NA
Charnley, SB
Mumma, MJ
Kisiel, Z
Serigano, J
Kuan, YJ
Chuang, YL
Wang, KS
AF Cordiner, M. A.
Palmer, M. Y.
Nixon, C. A.
Irwin, P. G. J.
Teanby, N. A.
Charnley, S. B.
Mumma, M. J.
Kisiel, Z.
Serigano, J.
Kuan, Y. -J.
Chuang, Y. -L.
Wang, K. -S.
TI ETHYL CYANIDE ON TITAN: SPECTROSCOPIC DETECTION AND MAPPING USING ALMA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: individual (Titan); techniques: interferometric;
planets and satellites: atmospheres; techniques: imaging spectroscopy
ID UPPER-ATMOSPHERE; MICROWAVE-SPECTRA; CHEMISTRY; NITRILES; HC3N;
PHOTOCHEMISTRY; PROPIONITRILE; DISTRIBUTIONS; STRATOSPHERE; SIMULATION
AB We report the first spectroscopic detection of ethyl cyanide (C2H5CN) in Titan's atmosphere, obtained using spectrally and spatially resolved observations of multiple emission lines with the Atacama Large Millimeter/submillimeter Array (ALMA). The presence of C2H5CN in Titan's ionosphere was previously inferred from Cassini ion mass spectrometry measurements of C2H5CNH+. Here we report the detection of 27 rotational lines from C2H5CN (in 19 separate emission features detected at >3 sigma confidence) in the frequency range 222-241 GHz. Simultaneous detections of multiple emission lines from HC3N, CH3CN, and CH3CCH were also obtained. In contrast to HC3N, CH3CN, and CH3CCH, which peak in Titan's northern (spring) hemisphere, the emission from C2H5CN is found to be concentrated in the southern (autumn) hemisphere, suggesting a distinctly different chemistry for this species, consistent with a relatively short chemical lifetime for C2H5CN. Radiative transfer models show that C2H5CN is most concentrated at altitudes greater than or similar to 200 km, suggesting production predominantly in the stratosphere and above. Vertical column densities are found to be in the range (1-5) x 10(14) cm(-2).
C1 [Cordiner, M. A.; Palmer, M. Y.; Nixon, C. A.; Charnley, S. B.; Mumma, M. J.; Serigano, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cordiner, M. A.; Serigano, J.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Palmer, M. Y.] St Olaf Coll, Dept Chem, Northfield, MN 55057 USA.
[Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Kisiel, Z.] Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland.
[Kuan, Y. -J.; Chuang, Y. -L.] Natl Taiwan Normal Univ, Taipei 116, Taiwan.
[Kuan, Y. -J.; Wang, K. -S.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM martin.cordiner@nasa.gov
RI Nixon, Conor/A-8531-2009; Kisiel, Zbigniew/K-8798-2016;
OI Nixon, Conor/0000-0001-9540-9121; Kisiel, Zbigniew/0000-0002-2570-3154;
Palmer, Maureen/0000-0001-9132-5588; Irwin, Patrick/0000-0002-6772-384X
FU NASA's Planetary Atmospheres and Planetary Astronomy programs; Goddard
Center for Astrobiology; Leverhulme Trust; UK Science and Technology
Facilities Council
FX This research was supported by NASA's Planetary Atmospheres and
Planetary Astronomy programs, The Goddard Center for Astrobiology, The
Leverhulme Trust, and the UK Science and Technology Facilities Council.
It makes use of ALMA data set ADS/JAO.ALMA#2011.0.00319.S. ALMA is a
partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc.
NR 32
TC 8
Z9 8
U1 2
U2 25
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 FEB 10
PY 2015
VL 800
IS 1
AR L14
DI 10.1088/2041-8205/800/1/L14
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB0KY
UT WOS:000349316000014
ER
PT J
AU Roy, J
Ray, PS
Bhattacharyya, B
Stappers, B
Chengalur, JN
Deneva, J
Camilo, F
Johnson, TJ
Wolff, M
Hessels, JWT
Bassa, CG
Keane, EF
Ferrara, EC
Harding, AK
Wood, KS
AF Roy, Jayanta
Ray, Paul S.
Bhattacharyya, Bhaswati
Stappers, Ben
Chengalur, Jayaram N.
Deneva, Julia
Camilo, Fernando
Johnson, Tyrel J.
Wolff, Michael
Hessels, Jason W. T.
Bassa, Cees G.
Keane, Evan F.
Ferrara, Elizabeth C.
Harding, Alice K.
Wood, Kent S.
TI DISCOVERY OF PSR J1227-4853: A TRANSITION FROM A LOW-MASS X-RAY BINARY
TO A REDBACK MILLISECOND PULSAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; binaries: eclipsing; pulsars: individual
(PSR J1227-4853); X-rays: binaries
ID J1023+0038; STATE; ROTATION; LINK
AB XSS J12270-4859 is an X-ray binary associated with the Fermi Large Area Telescope gamma-ray source 1FGL J1227.9-4852. In 2012 December, this source underwent a transition where the X-ray and optical luminosity dropped and the spectral signatures of an accretion disk disappeared. We report the discovery of a 1.69 millisecond pulsar (MSP), PSR J1227-4853, at a dispersion measure of 43.4 pc cm(-3) associated with this source, using the Giant Metrewave Radio Telescope (GMRT) at 607MHz. This demonstrates that, post-transition, the system hosts an active radio MSP. This is the third system after PSR J1023+0038 and PSR J1824-2452I showing evidence of state switching between radio MSP and low-mass X-ray binary states. We report timing observations of PSR J1227-4853 with the GMRT and Parkes, which give a precise determination of the rotational and orbital parameters of the system. The companion mass measurement of 0.17-0.46M(circle dot) suggests that this is a redback system. PSR J1227-4853 is eclipsed for about 40% of its orbit at 607 MHz with additional short-duration eclipses at all orbital phases. We also find that the pulsar is very energetic, with a spin-down luminosity of similar to 10(35) erg s(-1). We report simultaneous imaging and timing observations with the GMRT, which suggests that eclipses are caused by absorption rather than dispersion smearing or scattering.
C1 [Roy, Jayanta; Bhattacharyya, Bhaswati; Stappers, Ben] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Roy, Jayanta; Chengalur, Jayaram N.] Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Ray, Paul S.; Wolff, Michael; Wood, Kent S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Deneva, Julia] Naval Res Lab, NRC Res Associate, Washington, DC 20375 USA.
[Camilo, Fernando] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Wolff, Michael] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Johnson, Tyrel J.] Naval Res Lab, Washington, DC 20375 USA.
[Hessels, Jason W. T.; Bassa, Cees G.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Hessels, Jason W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Keane, Evan F.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Ferrara, Elizabeth C.; Harding, Alice K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Roy, J (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
OI Ray, Paul/0000-0002-5297-5278
FU Commonwealth of Australia; Chief of Naval Research (CNR); Marie Curie
grant (FP7) of the EU; NWO Vidi fellowship; ERC Starting Grant "DRAGNET"
[337062]
FX The GMRT is run by the National Centre for Radio Astrophysics of the
Tata Institute of Fundamental Research, India. We acknowledge support of
GMRT telescope operators for observations. We thank Andrew Lyne for
discussion on the GMRT timing model. The Parkes radio telescope is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. We acknowledge the help of John Reynolds in
understanding the time offset at GMRT while combining with Parkes data.
This work at NRL was supported by the Chief of Naval Research (CNR).
B.B. acknowledges the support of Marie Curie grant (FP7) of the EU.
J.W.T.H. acknowledges funding from an NWO Vidi fellowship and ERC
Starting Grant "DRAGNET" (337062).
NR 31
TC 25
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2015
VL 800
IS 1
AR L12
DI 10.1088/2041-8205/800/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB0KY
UT WOS:000349316000012
ER
PT J
AU Safron, EJ
Fischer, WJ
Megeath, ST
Furlan, E
Stutz, AM
Stanke, T
Billot, N
Rebull, LM
Tobin, JJ
Ali, B
Allen, LE
Booker, J
Watson, DM
Wilson, TL
AF Safron, Emily J.
Fischer, William J.
Megeath, S. Thomas
Furlan, Elise
Stutz, Amelia M.
Stanke, Thomas
Billot, Nicolas
Rebull, Luisa M.
Tobin, John J.
Ali, Babar
Allen, Lori E.
Booker, Joseph
Watson, Dan M.
Wilson, T. L.
TI HOPS 383: AN OUTBURSTING CLASS 0 PROTOSTAR IN ORION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: formation; stars:
protostars
ID YOUNG STELLAR OBJECTS; SPECTROSCOPIC SURVEY; EMBEDDED PROTOSTARS; DISK
FRAGMENTATION; NEBULA CLUSTER; MCNEILS NEBULA; STAR-FORMATION; BROWN
DWARFS; VARIABILITY; ACCRETION
AB We report the dramatic mid-infrared brightening between 2004 and 2006 of Herschel Orion Protostar Survey (HOPS) 383, a deeply embedded protostar adjacent to NGC 1977 in Orion. By 2008, the source became a factor of 35 brighter at 24 mu m with a brightness increase also apparent at 4.5 mu m. The outburst is also detected in the submillimeter by comparing APEX/SABOCA to SCUBA data, and a scattered-light nebula appeared in NEWFIRM K-s imaging. The post-outburst spectral energy distribution indicates a Class 0 source with a dense envelope and a luminosity between 6 and 14 L-circle dot Post-outburst time-series mid-and far-infrared photometry show no long-term fading and variability at the 18% level between 2009 and 2012. HOPS 383 is the first outbursting Class 0 object discovered, pointing to the importance of episodic accretion at early stages in the star formation process. Its dramatic rise and lack of fading over a 6 year period hint that it may be similar to FU Ori outbursts, although the luminosity appears to be significantly smaller than the canonical luminosities of such objects.
C1 [Safron, Emily J.; Megeath, S. Thomas; Booker, Joseph] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Observ, Toledo, OH 43606 USA.
[Fischer, William J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Furlan, Elise; Rebull, Luisa M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Stutz, Amelia M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Stanke, Thomas] European So Observ, Garching, Germany.
[Billot, Nicolas] Inst Radio Astron Milimetr, Granada, Spain.
[Tobin, John J.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Ali, Babar] Space Sci Inst, Boulder, CO USA.
[Allen, Lori E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Wilson, T. L.] Naval Res Lab, Washington, DC 20375 USA.
RP Safron, EJ (reprint author), Univ Toledo, Dept Phys & Astron, Ritter Astrophys Observ, 2801 W Bancroft St, Toledo, OH 43606 USA.
EM wjfischer@gmail.com
OI Fischer, William J/0000-0002-3747-2496; Rebull,
Luisa/0000-0001-6381-515X; Stutz, Amelia/0000-0003-2300-8200; Furlan,
Elise/0000-0001-9800-6248
FU National Aeronautics and Space Administration (NASA) through Jet
Propulsion Laboratory, California Institute of Technology (JPL/Caltech);
NASA; NASA Postdoctoral Program at Goddard Space Flight Center; Deutsche
Forschungsgemeinschaft priority program 1573 ("Physics of the
Interstellar Medium")
FX Support for this work was provided by the National Aeronautics and Space
Administration (NASA) through awards issued by the Jet Propulsion
Laboratory, California Institute of Technology (JPL/Caltech). We include
data from Herschel, a European Space Agency space observatory with
science instruments provided by European-led consortia and with
important participation from NASA. We use data from the Spitzer Space
Telescope and the Infrared Processing and Analysis Center Infrared
Science Archive, which are operated by JPL/Caltech under a contract with
NASA. We also include data from APEX, a collaboration between the
Max-PlanckI-nstitut fur Radioastronomie, the European Southern
Observatory, and the Onsala Space Observatory. This paper makes use of
data products from WISE, which is a joint project of the University of
California, Los Angeles, and JPL/Caltech, funded by NASA. This paper
uses observations taken at Kitt Peak National Observatory, National
Optical Astronomy Observatory, which is operated by the Association of
Universities for Research in Astronomy under cooperative agreement with
the National Science Foundation. The work of W.F. was supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. The work of A.S. was supported by the Deutsche
Forschungsgemeinschaft priority program 1573 ("Physics of the
Interstellar Medium").
NR 46
TC 18
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2015
VL 800
IS 1
AR L5
DI 10.1088/2041-8205/800/1/L5
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB0KY
UT WOS:000349316000005
ER
PT J
AU Shenoy, R
Smith, M
Park, M
AF Shenoy, Rajiv
Smith, Marilyn
Park, Michael
TI An efficient and robust localization scheme on massively distributed
systems
SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN ENGINEERING
LA English
DT Article
DE parallelized; localization; search; neighbor walk; advancing front;
hierarchy; adaptive grid; overset grid
ID UNSTRUCTURED GRIDS; INTERPOLATION; CONSERVATION; SIMULATIONS; ALGORITHMS
AB A parallel localization scheme is presented to enable solution transfers between unstructured grids. The scheme relies on neighbor walks to reduce the number of candidate elements that are visited to find the enclosing element. An advancing front method efficiently allows a subset of nodes to efficiently sweep through the grid, progressively reducing search spaces. The algorithm is parallelized permitting solution transfers over arbitrary grid decompositions. A hierarchical localization process helps prevent the neighbor walk algorithm from failing when encountering the boundaries of a concave domain by localizing the boundaries before the interior of the domain is localized. Random selections of the next step interrupt cyclic loops that may occur during a neighbor walk. The complexity of the search algorithm is verified over parallel decompositions and is effectively independent of the number of partitions. Copyright (c) 2014 John Wiley & Sons, Ltd.
C1 [Shenoy, Rajiv; Smith, Marilyn] Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Park, Michael] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
RP Shenoy, R (reprint author), Georgia Inst Technol, Guggenheim Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA.
EM rajivrshenoy@gmail.com
FU Office of Naval Research (ONR) [N0001409-1-1019]
FX The Office of Naval Research (ONR) provided financial support for this
research through ONR Grant N0001409-1-1019 with technical monitor, Judah
Milgram. The DoD High Performance Computing Modernization Program
provided access to the Navy and Army Engineer Research and Development
Center DoD Supercomputing Resource Centers for computational time used
for the simulations. Additional computational support was provided by
NASA Langley Research Center's facilities. These facilities enabled
successful and timely completion of all simulations and are gratefully
acknowledged, along with the Navy S/AAA Odessa Murray. The authors would
also like to thank Dan Prosser of Georgia Tech for his efforts in
conducting timing simulations. The views and conclusions contained in
this document are the authors' own and should not be interpreted as
representing the official policies, either expressed or implied, of the
U.S. Government.
NR 18
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0029-5981
EI 1097-0207
J9 INT J NUMER METH ENG
JI Int. J. Numer. Methods Eng.
PD FEB 10
PY 2015
VL 101
IS 6
BP 470
EP 488
DI 10.1002/nme.4812
PG 19
WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary
Applications
SC Engineering; Mathematics
GA AY7HD
UT WOS:000347730800003
ER
PT J
AU Stecker, FW
Scully, ST
Liberati, S
Mattingly, D
AF Stecker, Floyd W.
Scully, Sean T.
Liberati, Stefano
Mattingly, David
TI Searching for traces of Planck-scale physics with high energy neutrinos
SO PHYSICAL REVIEW D
LA English
DT Article
ID LORENTZ INVARIANCE; GAMMA-RAYS; RADIATION; FIELDS; TESTS
AB High-energy cosmic neutrino observations provide a sensitive test of Lorentz invariance violation (LIV), which may be a consequence of quantum gravity theories. We consider a class of nonrenormalizable, Lorentz invariance violating operators that arise in an effective field theory (EFT) description of Lorentz invariance violation in the neutrino sector inspired by Planck-scale physics and quantum gravity models. We assume a conservative generic scenario for the redshift distribution of extragalactic neutrino sources and employ Monte Carlo techniques to describe superluminal neutrino propagation, treating kinematically allowed energy losses of superluminal neutrinos caused by both vacuum pair emission (VPE) and neutrino splitting. We consider EFTs with both nonrenormalizable CPT -odd and nonrenormalizable CPT -even operator dominance. We then compare the spectra derived using our Monte Carlo calculations in both cases with the spectrum observed by IceCube in order to determine the implications of our results regarding Planck-scale physics. We find that if the dropoff in the neutrino flux above similar to 2 PeV is caused by Planck-scale physics, rather than by a limiting energy in the source emission, a potentially significant pileup effect would be produced just below the dropoff energy in the case of CPT -even operator dominance. However, such a clear dropoff effect would not be observed if the CPT -odd, CPT -violating term dominates.
C1 [Stecker, Floyd W.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stecker, Floyd W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Scully, Sean T.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
[Liberati, Stefano] SISSA Int Sch Adv Studies, I-34136 Trieste, Italy.
[Liberati, Stefano] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy.
[Mattingly, David] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
RP Stecker, FW (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Liberati, Stefano/0000-0002-7632-7443
FU John Templeton Foundation
FX We thank Andrew Cohen and Alan Kostelecky for helpful comments. S. L.
acknowledges support of a grant from the John Templeton Foundation.
NR 36
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U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD FEB 9
PY 2015
VL 91
IS 4
AR 045009
DI 10.1103/PhysRevD.91.045009
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CC3HU
UT WOS:000350238400005
ER
PT J
AU Borgentun, C
Frez, C
Briggs, RM
Fradet, M
Forouhar, S
AF Borgentun, Carl
Frez, Clifford
Briggs, Ryan M.
Fradet, Mathieu
Forouhar, Siamak
TI Single-mode high-power interband cascade lasers for mid-infrared
absorption spectroscopy
SO OPTICS EXPRESS
LA English
DT Article
ID 2.3 MU-M; ROOM-TEMPERATURE
AB For high-sensitivity absorption spectroscopy, single-mode light sources capable of emitting high optical output power in the 3 to 5 mu m wavelength range are vital. Here, we report on interband cascade lasers that emit 20 mW of optical power in a single spectral mode at room temperature and up to 40 mW at 0 degrees C using second-order laterally coupled Bragg gratings for distributed feedback. The lasers employ a double-ridge design with a narrow 3-mu m-wide top ridge to confine the optical mode and a 9-mu m-wide ridge for current confinement. The lasers were developed for an integrated cavity output spectroscopy instrument for stratospheric detection of hydrogen chloride at a wavelength of 3.3746 mu m and emit at the target wavelength with more than 34 mW of single-mode power. (C) 2015 Optical Society of America
C1 [Borgentun, Carl; Frez, Clifford; Briggs, Ryan M.; Fradet, Mathieu; Forouhar, Siamak] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Forouhar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM siamak.forouhar@jpl.nasa.gov
FU NASA's Advanced Component Technology program through the Jet Propulsion
Laboratory, California Institute of Technology, under NASA
FX The work was supported by NASA's Advanced Component Technology program
through the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. The reported lasers were
fabricated on epitaxial wafers designed and grown by the group of Dr.
Jerry Meyer at the Naval Research Laboratory.
NR 13
TC 1
Z9 1
U1 1
U2 10
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD FEB 9
PY 2015
VL 23
IS 3
BP 2446
EP 2450
DI 10.1364/OE.23.002446
PG 5
WC Optics
SC Optics
GA CB5SV
UT WOS:000349688800070
PM 25836112
ER
PT J
AU Chen, JR
Numata, K
Wu, ST
AF Chen, Jeffrey R.
Numata, Kenji
Wu, Stewart T.
TI Impact of broadened laser line-shape on retrievals of atmospheric
species from lidar sounding absorption spectra
SO OPTICS EXPRESS
LA English
DT Article
ID CO2 COLUMN ABSORPTION; AIRBORNE MEASUREMENTS; ERROR REDUCTION;
CARBON-DIOXIDE; PRECISION; NM
AB We examine the impact of broadened laser line-shape on retrievals of atmospheric species from lidar-sounding absorption spectra. The laser is assumed to be deterministically modulated into a stable, nearly top-hat frequency comb to suppress the stimulated Brillouin scattering, allowing over 10-fold pulse energy increase without adding measurement noise. Our model remains accurate by incorporating the laser line-shape factor into the effective optical depth. Retrieval errors arising from measurement noise and model bias are analyzed parametrically and numerically to provide deeper insight. The stable laser line-shape broadening minimally degrades the column-averaged retrieval, but can significantly degrade the multiple-layer retrievals. (C) 2015 Optical Society of America
C1 [Chen, Jeffrey R.; Numata, Kenji; Wu, Stewart T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Chen, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jeffrey.r.chen@nasa.gov
FU NASA Goddard Internal Research and Development program
FX The authors gratefully acknowledge Drs. J. Mao, X. Sun, J. Abshire, H.
Riris and other members of the Goddard CO2 sounder team for
their help. They are also indebted to Dr. A. Amediek of DLR for sharing
surface reflectance measurement data. This work was supported by the
NASA Goddard Internal Research and Development program.
NR 21
TC 0
Z9 0
U1 2
U2 7
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 FEB 9
PY 2015
VL 23
IS 3
BP 2660
EP 2675
DI 10.1364/OE.23.002660
PG 16
WC Optics
SC Optics
GA CB5SV
UT WOS:000349688800087
PM 25836129
ER
PT J
AU Veitch, J
Raymond, V
Farr, B
Farr, W
Graff, P
Vitale, S
Aylott, B
Blackburn, K
Christensen, N
Coughlin, M
Del Pozzo, W
Feroz, F
Gair, J
Haster, CJ
Kalogera, V
Littenberg, T
Mandel, I
O'Shaughnessy, R
Pitkin, M
Rodriguez, C
Rover, C
Sidery, T
Smith, R
Van Der Sluys, M
Vecchio, A
Vousden, W
Wade, L
AF Veitch, J.
Raymond, V.
Farr, B.
Farr, W.
Graff, P.
Vitale, S.
Aylott, B.
Blackburn, K.
Christensen, N.
Coughlin, M.
Del Pozzo, W.
Feroz, F.
Gair, J.
Haster, C. -J.
Kalogera, V.
Littenberg, T.
Mandel, I.
O'Shaughnessy, R.
Pitkin, M.
Rodriguez, C.
Roever, C.
Sidery, T.
Smith, R.
Van Der Sluys, M.
Vecchio, A.
Vousden, W.
Wade, L.
TI Parameter estimation for compact binaries with ground-based
gravitational-wave observations using the LALInference software library
SO PHYSICAL REVIEW D
LA English
DT Article
ID CHAIN MONTE-CARLO; BAYESIAN-INFERENCE; RADIATION; EFFICIENT; LIKELIHOOD;
ALGORITHMS; ASTRONOMY; COSMOLOGY; NETWORK; SIGNALS
AB The Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors will begin operation in the coming years, with compact binary coalescence events a likely source for the first detections. The gravitational waveforms emitted directly encode information about the sources, including the masses and spins of the compact objects. Recovering the physical parameters of the sources from the GW observations is a key analysis task. This work describes the LALInference software library for Bayesian parameter estimation of compact binary signals, which builds on several previous methods to provide a well-tested toolkit which has already been used for several studies. We show that our implementation is able to correctly recover the parameters of compact binary signals from simulated data from the advanced GW detectors. We demonstrate this with a detailed comparison on three compact binary systems: a binary neutron star, a neutron star-black hole binary and a binary black hole, where we show a cross comparison of results obtained using three independent sampling algorithms. These systems were analyzed with nonspinning, aligned spin and generic spin configurations respectively, showing that consistent results can be obtained even with the full 15-dimensional parameter space of the generic spin configurations. We also demonstrate statistically that the Bayesian credible intervals we recover correspond to frequentist confidence intervals under correct prior assumptions by analyzing a set of 100 signals drawn from the prior. We discuss the computational cost of these algorithms, and describe the general and problem-specific sampling techniques we have used to improve the efficiency of sampling the compact binary coalescence parameter space.
C1 [Veitch, J.; Farr, W.; Aylott, B.; Del Pozzo, W.; Haster, C. -J.; Mandel, I.; Sidery, T.; Vecchio, A.; Vousden, W.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Veitch, J.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Raymond, V.; Blackburn, K.; Smith, R.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Farr, B.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Farr, B.; Kalogera, V.; Littenberg, T.; Rodriguez, C.] CIERA, Evanston, IL 60208 USA.
[Farr, B.; Kalogera, V.; Littenberg, T.; Rodriguez, C.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Graff, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vitale, S.] MIT, Cambridge, MA 02138 USA.
[Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Coughlin, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Feroz, F.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Gair, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[O'Shaughnessy, R.; Wade, L.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[O'Shaughnessy, R.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Pitkin, M.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Roever, C.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany.
[Roever, C.] Univ Med Ctr Gottingen, Dept Med Stat, D-37073 Gottingen, Germany.
[Van Der Sluys, M.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
RP Veitch, J (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM john.veitch@ligo.org
RI Vecchio, Alberto/F-8310-2015;
OI Vecchio, Alberto/0000-0002-6254-1617; Rover,
Christian/0000-0002-6911-698X; O'Shaughnessy,
Richard/0000-0001-5832-8517; Farr, Ben/0000-0002-2916-9200; Del Pozzo,
Walter/0000-0003-3978-2030; Vitale, Salvatore/0000-0003-2700-0767;
Mandel, Ilya/0000-0002-6134-8946; Pitkin, Matthew/0000-0003-4548-526X
FU NEMO computing cluster at the Center for Gravitation and Cosmology at
UWM under NSF [PHY-0923409, PHY-0600953]; Atlas computing cluster at the
Albert Einstein Institute, Hannover; LIGO computing clusters at Caltech,
Livingston and Hanford; ARCCA cluster at Cardiff University; Netherlands
Organization for Scientific Research (NWO); U.K. Science and Technology
Facilities Council (STFC [ST/K005014/1]; California Institute of
Technology (Caltech); National Science Foundation (NSF) Graduate
Research Fellowship Program, under NSF [DGE 1144152]; Royal Society;
National Science Foundation and the LIGO Laboratory; National Science
Foundation [PHY-0757058, PHY-1204371, PHY-0970074, PHY-1307429];
Leverhulme and Newton Trusts; NSF LIGO [PHY-1307020]; UWM Research
Growth Initiative; STFC [ST/L000946/1]
FX The authors gratefully acknowledge the support of the LIGO-Virgo
Collaboration in the development of the LALInference toolkit, including
internal review of the codes and results. We thank Neil Cornish and
Thomas Dent for useful feedback on the manuscript. The results presented
here were produced using the computing facilities of the LIGO DataGrid
and XSEDE, including the following: the NEMO computing cluster at the
Center for Gravitation and Cosmology at UWM under NSF Grants No.
PHY-0923409 and No. PHY-0600953; the Atlas computing cluster at the
Albert Einstein Institute, Hannover; the LIGO computing clusters at
Caltech, Livingston and Hanford; and the ARCCA cluster at Cardiff
University. Figures 7-9 were produced with the help of triangle.py [89].
J. V. was supported by the research program of the Foundation for
Fundamental Research on Matter (FOM), which is partially supported by
the Netherlands Organization for Scientific Research (NWO), and by the
U.K. Science and Technology Facilities Council (STFC) Grant No.
ST/K005014/1. V. R. was supported by a Richard Chase Tolman fellowship
at the California Institute of Technology (Caltech). P. G. was supported
by an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. M. C. was supported by the National Science
Foundation (NSF) Graduate Research Fellowship Program, under NSF Grant
No. DGE 1144152. J. G.'s work was supported by the Royal Society. S. V.
acknowledges the support of the National Science Foundation and the LIGO
Laboratory. LIGO was constructed by the California Institute of
Technology and Massachusetts Institute of Technology with funding from
the National Science Foundation and operates under Grant No.
PHY-0757058. N. C.'s work was supported by NSF Grant No. PHY-1204371. F.
F. is supported by a research fellowship from Leverhulme and Newton
Trusts. T. L., V. K. and C. R. acknowledge the support of the NSF LIGO
Grant No. PHY-1307020. R. O'S. acknowledges the support of NSF Grants
No. PHY-0970074 and No. PHY-1307429, and the UWM Research Growth
Initiative. M. P. is funded by the STFC under Grant No. ST/L000946/1.
NR 85
TC 84
Z9 83
U1 1
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD FEB 6
PY 2015
VL 91
IS 4
AR 042003
DI 10.1103/PhysRevD.91.042003
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CB2DX
UT WOS:000349438000001
ER
PT J
AU Elele, EO
Shen, YY
Pettit, DR
Khusid, B
AF Elele, Ezinwa O.
Shen, Yueyang
Pettit, Donald R.
Khusid, Boris
TI Detection of a Dynamic Cone-Shaped Meniscus on the Surface of Fluids in
Electric Fields
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID WATER DROPS; DEFORMATION; SINGULARITY; DISCHARGES; PINCHOFF; COLLAPSE;
METAL; JETS
AB A cone-shaped meniscus of electrified fluids, often called a Taylor cone, is observed in rain drops and lightning and employed in various physical instruments and experimental techniques, but the way it evolves from a rounded shape to a cone is a long-standing puzzle. Earth's gravity and microgravity measurements on the meniscus whose height is just shy of droplet ejection reveal that field-driven cusp evolution exhibits a universal self-similarity insensitive to the forcing field and scaled by the fluid surface tension and density. Our work paves the way for dynamic control of field-driven phenomena in fluids.
C1 [Elele, Ezinwa O.; Shen, Yueyang; Khusid, Boris] New Jersey Inst Technol, Newark, NJ 07102 USA.
[Pettit, Donald R.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Elele, EO (reprint author), New Jersey Inst Technol, Newark, NJ 07102 USA.
FU National Aeronautics and Space Administration [NNX09AK06G, NNX13AQ53G]
FX We are thankful to Andreas Acrivos, Osman A. Basaran, and Paul H. Steen
for stimulating discussions and comments on the interpretation of
experimental data. Research funded by National Aeronautics and Space
Administration Grants No. NNX09AK06G and No. NNX13AQ53G.
NR 32
TC 2
Z9 2
U1 4
U2 22
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 FEB 5
PY 2015
VL 114
IS 5
AR 054501
DI 10.1103/PhysRevLett.114.054501
PG 5
WC Physics, Multidisciplinary
SC Physics
GA CE8CZ
UT WOS:000352070100006
PM 25699447
ER
PT J
AU Graham, MJ
Djorgovski, SG
Stern, D
Glikman, E
Drake, AJ
Mahabal, AA
Donalek, C
Larson, S
Christensen, E
AF Graham, Matthew J.
Djorgovski, S. G.
Stern, Daniel
Glikman, Eilat
Drake, Andrew J.
Mahabal, Ashish A.
Donalek, Ciro
Larson, Steve
Christensen, Eric
TI A possible close supermassive black-hole binary in a quasar with optical
periodicity
SO NATURE
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SURVEY SPECTROSCOPIC SAMPLE;
PHOTOMETRIC STANDARD STARS; TIME TRANSIENT SURVEY; ACCRETION DISK; JET
PRECESSION; VARIABILITY; PARSEC; MASS
AB Quasars have long been known to be variable sources at all wavelengths. Their optical variability is stochastic and can be due to a variety of physical mechanisms; it is also well-described statistically in terms of a damped random walk model(1). The recent availability of large collections of astronomical timeseries of flux measurements (light curves(2-5)) offers new data sets for a systematic exploration of quasar variability. Here we report the detection of a strong, smooth periodic signal in the optical variability of the quasar PG 1302-102 with a mean observed period of 1,884 +/- 88 days. It was identified in a search for periodic variability in a data set of light curves for 247,000 known, spectroscopically confirmed quasars with a temporal baseline of about 9 years. Although the interpretation of this phenomenon is still uncertain, the most plausible mechanisms involve a binary system of two supermassive black holes with a subparsec separation. Such systems are an expected consequence of galaxy mergers and can provide important constraints on models of galaxy formation and evolution.
C1 [Graham, Matthew J.; Djorgovski, S. G.; Drake, Andrew J.; Mahabal, Ashish A.; Donalek, Ciro] CALTECH, Pasadena, CA 91125 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Larson, Steve; Christensen, Eric] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA.
RP Graham, MJ (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM mjg@caltech.edu
FU NSF [AST-0909182, IIS-1118031, AST-1313422]; W.M. Keck Foundation; NASA
FX This work was supported in part by NSF grants AST-0909182, IIS-1118031
and AST-1313422. We thank J. S. Stuart, MIT Lincoln Laboratory, for
assistance with the LINEAR data. We also thank the staff of the Keck and
Palomar Observatories for their help with observations, and the CRTS
team. Some of the data presented here were obtained at the W.M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California and
NASA. The observatory was made possible by the financial support of the
W.M. Keck Foundation. The work of D.S. was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 53
TC 47
Z9 47
U1 0
U2 6
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD FEB 5
PY 2015
VL 518
IS 7537
BP 74
EP +
DI 10.1038/nature14143
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CA7LE
UT WOS:000349098000033
PM 25561176
ER
PT J
AU Zhong, T
Zhou, HC
Horansky, RD
Lee, C
Verma, VB
Lita, AE
Restelli, A
Bienfang, JC
Mirin, RP
Gerrits, T
Nam, SW
Marsili, F
Shaw, MD
Zhang, ZS
Wang, LG
Englund, D
Wornell, GW
Shapiro, JH
Wong, FNC
AF Zhong, Tian
Zhou, Hongchao
Horansky, Robert D.
Lee, Catherine
Verma, Varun B.
Lita, Adriana E.
Restelli, Alessandro
Bienfang, Joshua C.
Mirin, Richard P.
Gerrits, Thomas
Nam, Sae Woo
Marsili, Francesco
Shaw, Matthew D.
Zhang, Zheshen
Wang, Ligong
Englund, Dirk
Wornell, Gregory W.
Shapiro, Jeffrey H.
Wong, Franco N. C.
TI Photon-efficient quantum key distribution using time-energy entanglement
with high-dimensional encoding
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
DE quantum cryptography; quantum communications; quantum entanglement
ID COMMUNICATION; STATES
AB Conventional quantumkey distribution (QKD) typically uses binary encoding based on photon polarization or time-bin degrees of freedomand achieves a key capacity of atmost one bit per photon. Under photon-starved conditions the rate of detection events ismuch lower than the photon generation rate, because of losses in long distance propagation and the relatively long recovery times of available singlephoton detectors. Multi-bit encoding in the photon arrival times can be beneficial in such photonstarved situations. Recent security proofs indicate high-dimensional encoding in the photon arrival times is robust and can be implemented to yield high secure throughput. In this work we demonstrate entanglement-basedQKDwith high-dimensional encodingwhose security against collectiveGaussian attacks is provided by a high-visibility Franson interferometer. We achieve unprecedented key capacity and throughput for an entanglement-basedQKDsystembecause of four principal factors: Franson interferometry that does not degrade with loss; error correction coding that can tolerate high error rates; optimized time-energy entanglement generation; and highly efficientWSi superconducting nanowire single-photon detectors. The secure key capacity yields asmuch as 8.7 bits per coincidence. When optimized for throughput we observe a secure key rate of 2.7 Mbit s(-1) after 20 kmfiber transmissionwith a key capacity of 6.9 bits per photon coincidence. Our results demonstrate a viable approach to high-rate QKDusing practical photonic entanglement and single-photon detection technologies.
C1 [Zhong, Tian; Zhou, Hongchao; Lee, Catherine; Zhang, Zheshen; Wang, Ligong; Englund, Dirk; Wornell, Gregory W.; Shapiro, Jeffrey H.; Wong, Franco N. C.] MIT, Elect Res Lab, Cambridge, MA 02139 USA.
[Horansky, Robert D.; Verma, Varun B.; Lita, Adriana E.; Mirin, Richard P.; Gerrits, Thomas; Nam, Sae Woo] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Restelli, Alessandro; Bienfang, Joshua C.] Univ Maryland, Joint Quantum Inst, Gaithersburg, MD 20899 USA.
[Restelli, Alessandro; Bienfang, Joshua C.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
[Marsili, Francesco; Shaw, Matthew D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zhong, T (reprint author), MIT, Elect Res Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM tzhong@mit.edu
RI Restelli, Alessandro/A-4897-2009;
OI Restelli, Alessandro/0000-0002-1289-3171; Mirin,
Richard/0000-0002-4472-4655
FU DARPA InPho program under Army Research Office [W911NF-10-1-0416];
National Aeronautics and Space Administration
FX The authors acknowledge technical discussions with Yuval Kochman. This
work was supported in part by the DARPA InPho program under Army
Research Office Grant No. W911NF-10-1-0416. Part of this work was
carried out at the Jet Propulsion Laboratory, under contract with the
National Aeronautics and Space Administration.
NR 32
TC 16
Z9 16
U1 1
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD FEB 4
PY 2015
VL 17
AR 022002
DI 10.1088/1367-2630/17/2/022002
PG 10
WC Physics, Multidisciplinary
SC Physics
GA CF9EC
UT WOS:000352864700001
ER
PT J
AU Petropoulos, GP
Kalivas, DP
Georgopoulou, IA
Srivastava, PK
AF Petropoulos, George P.
Kalivas, Dionissios P.
Georgopoulou, Iro A.
Srivastava, Prashant K.
TI Urban vegetation cover extraction from hyperspectral imagery and
geographic information system spatial analysis techniques: case of
Athens, Greece
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE Earth observation; geographical information systems; Hyperion; support
vector machines; spectral angle mapper; Athens; Greece
ID SUPPORT VECTOR MACHINES; LANDSAT TM IMAGERY; OBJECT-BASED
CLASSIFICATION; BURNT AREA DELINEATION; SPECTRAL ANGLE MAPPER; ECOSYSTEM
SERVICES; NEURAL-NETWORK; AIR-POLLUTION; SHADE TREES; ENERGY USE
AB The present study aimed at evaluating the performance of two different pixel-based classifiers [spectral angle mapper (SAM) and support vector machines (SVMs)] in discriminating different land-cover classes in a typical urban setting, focusing particularly on urban vegetation cover by utilizing hyperspectral (EO-1 Hyperion) data. As a case study, the city of Athens, Greece, was used. Validation of urban vegetation predictions was based on the error matrix statistics. Additionally, the final urban vegetation cover maps were compared at a municipality level against reference urban vegetation cover estimates derived from the digitization of very high-resolution imagery. To ensure consistency and comparability of the results, the same training and validation points dataset were used to compare the different classifiers. The results showed that SVMs outperformed SAM in terms of both classification and urban vegetation cover mapping with an overall accuracy of 86.53% and Kappa coefficient 0.823, whereas for SAM classification, the accuracy statistics obtained were 75.13% and 0.673, respectively. Our results confirmed the ability of both techniques, when combined with Hyperion imagery, to extract urban vegetation cover for the case of a densely populated city with complex urban features, such as Athens. Our findings offer significant information at the local scale as regards to the presence of open green spaces in the urban environment of Athens. Such information is vital for successful infrastructure development, urban landscape planning, and improvement of urban environment. More widely, this study also contributes significantly toward an objective assessment of Hyperion in detecting and mapping urban vegetation cover. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales.
[Petropoulos, George P.; Kalivas, Dionissios P.; Georgopoulou, Iro A.] Agr Univ Athens, Dept Nat Resources Management & Agr Engn, Athens 11855, Greece.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Petropoulos, GP (reprint author), Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales.
EM george.petropoulos@aber.ac.uk
RI Petropoulos, George/F-2384-2013;
OI Petropoulos, George/0000-0003-1442-1423; Kalivas,
Dionissios/0000-0001-7031-4863
NR 54
TC 2
Z9 2
U1 4
U2 25
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD FEB 4
PY 2015
VL 9
AR 096088
DI 10.1117/1.JRS.9.096088
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CC6MW
UT WOS:000350480200001
ER
PT J
AU Weck, PJ
Schaffner, DA
Brown, MR
Wicks, RT
AF Weck, P. J.
Schaffner, D. A.
Brown, M. R.
Wicks, R. T.
TI Permutation entropy and statistical complexity analysis of turbulence in
laboratory plasmas and the solar wind
SO PHYSICAL REVIEW E
LA English
DT Article
ID TIME-SERIES; FLUCTUATIONS; SPECTRA
AB The Bandt-Pompe permutation entropy and the Jensen-Shannon statistical complexity are used to analyze fluctuating time series of three different turbulent plasmas: the magnetohydrodynamic (MHD) turbulence in the plasma wind tunnel of the Swarthmore Spheromak Experiment (SSX), drift-wave turbulence of ion saturation current fluctuations in the edge of the Large Plasma Device (LAPD), and fully developed turbulent magnetic fluctuations of the solar wind taken from the Wind spacecraft. The entropy and complexity values are presented as coordinates on the CH plane for comparison among the different plasma environments and other fluctuation models. The solar wind is found to have the highest permutation entropy and lowest statistical complexity of the three data sets analyzed. Both laboratory data sets have larger values of statistical complexity, suggesting that these systems have fewer degrees of freedom in their fluctuations, with SSX magnetic fluctuations having slightly less complexity than the LAPD edge I-sat. The CH plane coordinates are compared to the shape and distribution of a spectral decomposition of the wave forms. These results suggest that fully developed turbulence (solar wind) occupies the lower-right region of the CH plane, and that other plasma systems considered to be turbulent have less permutation entropy and more statistical complexity. This paper presents use of this statistical analysis tool on solar wind plasma, as well as on an MHD turbulent experimental plasma.
C1 [Weck, P. J.; Schaffner, D. A.; Brown, M. R.] Swarthmore Coll, Swarthmore, PA 19081 USA.
[Wicks, R. T.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Weck, PJ (reprint author), Swarthmore Coll, Swarthmore, PA 19081 USA.
RI Wicks, Robert/A-1180-2009
OI Wicks, Robert/0000-0002-0622-5302
FU DOE (USA) through the Office of Fusion Energy Sciences (OFES); NSF (USA)
through the Center for Magnetic Self-Organization (CMSO)
FX The authors gratefully acknowledge useful discussions with J. Maggs, G.
Morales, W. Gekelman, B. Friedman, T. Carter, and D. Guice. This work
was supported by the DOE (USA) through the Office of Fusion Energy
Sciences (OFES) and by the NSF (USA) through the Center for Magnetic
Self-Organization (CMSO).
NR 40
TC 8
Z9 8
U1 2
U2 19
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
EI 1550-2376
J9 PHYS REV E
JI Phys. Rev. E
PD FEB 4
PY 2015
VL 91
IS 2
AR 023101
DI 10.1103/PhysRevE.91.023101
PG 7
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA CA9MT
UT WOS:000349249000004
PM 25768612
ER
PT J
AU Nguyen, TB
Crounse, JD
Teng, AP
Clair, JMS
Paulot, F
Wolfe, GM
Wennberg, PO
AF Nguyen, Tran B.
Crounse, John D.
Teng, Alex P.
Clair, Jason M. St.
Paulot, Fabien
Wolfe, Glenn M.
Wennberg, Paul O.
TI Rapid deposition of oxidized biogenic compounds to a temperate forest
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE biosphere-atmosphere exchange; isoprene; dry deposition; OVOCs; fluxes
ID SECONDARY ORGANIC AEROSOL; GASEOUS DRY DEPOSITION; HYDROGEN-PEROXIDE;
ISOPRENE EPOXYDIOLS; REACTIVE UPTAKE; DECIDUOUS FOREST; EDDY COVARIANCE;
ATMOSPHERIC DEPOSITION; NITROGEN DEPOSITION; FLUX MEASUREMENTS
AB We report fluxes and dry deposition velocities for 16 atmospheric compounds above a southeastern United States forest, including: hydrogen peroxide (H2O2), nitric acid (HNO3), hydrogen cyanide (HCN), hydroxymethyl hydroperoxide, peroxyacetic acid, organic hydroxy nitrates, and other multifunctional species derived from the oxidation of isoprene and monoterpenes. The data suggest that dry deposition is the dominant daytime sink for small, saturated oxygenates. Greater than 6 wt %C emitted as isoprene by the forest was returned by dry deposition of its oxidized products. Peroxides account for a large fraction of the oxidant flux, possibly eclipsing ozone in more pristine regions. The measured organic nitrates comprise a sizable portion (15%) of the oxidized nitrogen input into the canopy, with HNO3 making up the balance. We observe that water-soluble compounds (e.g., strong acids and hydroperoxides) deposit with low surface resistance whereas compounds with moderate solubility (e.g., organic nitrates and hydroxycarbonyls) or poor solubility (e.g., HCN) exhibited reduced uptake at the surface of plants. To first order, the relative deposition velocities of water-soluble compounds are constrained by their molecular diffusivity. From resistance modeling, we infer a substantial emission flux of formic acid at the canopy level (similar to 1 nmol m(-2).s(-1)). GEOS-Chem, a widely used atmospheric chemical transport model, currently under-estimates dry deposition for most molecules studied in this work. Reconciling GEOS-Chem deposition velocities with observations resulted in up to a 45% decrease in the simulated surface concentration of trace gases.
C1 [Nguyen, Tran B.; Crounse, John D.; Teng, Alex P.; Clair, Jason M. St.; Wennberg, Paul O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Paulot, Fabien] Natl Ocean & Atmospher Adm, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Paulot, Fabien] Princeton Univ, Princeton, NJ 08544 USA.
[Wolfe, Glenn M.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
RP Wennberg, PO (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM tbn@caltech.edu; wennberg@caltech.edu
RI Wolfe, Glenn/D-5289-2011; Chem, GEOS/C-5595-2014; Crounse,
John/C-3700-2014;
OI Crounse, John/0000-0001-5443-729X; Teng, Alexander/0000-0002-6434-0501
FU National Science Foundation (NSF) [AGS-1240604, AGS-1331360]; Earth
Observing Laboratory at the National Center for Atmospheric Research;
Atmospheric Research and Analysis; Electric Power Research Institute
FX We thank the organizers and committee members of the SOAS campaign: A.
G. Carlton, A. H. Goldstein, J. L. Jimenez, R. W. Pinder, J. de Gouw, B.
J. Turpin, and A. B. Guenther. We acknowledge C. J. Groff at Purdue
University for his help with leaf area index measurements and tree
surveys. We thank D. J. Jacob and the Atmospheric Chemistry Modeling
Group at Harvard University for making GEOS-Chem available for this
work. Meteorological data used in the GEOS-Chem simulations were
provided by the Global Modeling and Assimilation Office at NASA Goddard
Space Flight Center. We acknowledge funding from the National Science
Foundation (NSF) under Grant AGS-1240604 and NSF Postdoctoral Research
Fellowship program Award AGS-1331360. Financial and logistical support
for SOAS was provided by the NSF, the Earth Observing Laboratory at the
National Center for Atmospheric Research (operated by NSF), the
personnel at Atmospheric Research and Analysis, and the Electric Power
Research Institute.
NR 94
TC 31
Z9 32
U1 15
U2 95
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 FEB 3
PY 2015
VL 112
IS 5
BP E392
EP E401
DI 10.1073/pnas.1418702112
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CA7HF
UT WOS:000349087700005
PM 25605913
ER
PT J
AU Spak, KS
Agnes, GS
Inman, DJ
AF Spak, Kaitlin S.
Agnes, Gregory S.
Inman, Daniel J.
TI Modeling vibration response and damping of cables and cabled structures
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID DISTRIBUTED-PARAMETER-SYSTEMS; VALIDATION
AB In an effort to model the vibration response of cabled structures, the distributed transfer function method is developed to model cables and a simple cabled structure. The model includes shear effects, tension, and hysteretic damping for modeling of helical stranded cables, and includes a method for modeling cable attachment points using both linear and rotational damping and stiffness. The damped cable model shows agreement with experimental data for four types of stranded cables, and the damped cabled beam model shows agreement with experimental data for the cables attached to a beam structure, as well as improvement over the distributed mass method for cabled structure modeling. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Spak, Kaitlin S.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24060 USA.
[Agnes, Gregory S.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
[Inman, Daniel J.] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Spak, KS (reprint author), Exponent, 149 Commonwealth Ave, Menlo Pk, CA 94025 USA.
EM kspak@vt.edu
FU NASA Space Technology Research Fellowship; San Gabriel Valley AIAA
Chapter and Virginia Space Grant Consortium; AFOSR [FA9550-10-1-0427];
National Aeronautics and Space Administration
FX The first author thanks the NASA Space Technology Research Fellowship
program for generous support and the San Gabriel Valley AIAA Chapter and
Virginia Space Grant Consortium for additional funding. Cables for
testing were provided at cost by Southern California Braiding, Co, The
third author gratefully acknowledges the support of AFOSR Grant number
FA9550-10-1-0427 monitored by Dr. David Stargel. This research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 15
TC 2
Z9 2
U1 2
U2 21
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD FEB 3
PY 2015
VL 336
BP 240
EP 256
DI 10.1016/j.jsv.2014.10.009
PG 17
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA AU2FR
UT WOS:000345432300016
ER
PT J
AU Stoica, A
AF Stoica, Adrian
TI Foreword and Editorial
SO INTERNATIONAL JOURNAL OF SECURITY AND ITS APPLICATIONS
LA English
DT Editorial Material
C1 NASA, Jet Prop Lab, Pasadena, CA USA.
RP Stoica, A (reprint author), NASA, Jet Prop Lab, Pasadena, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SCIENCE & ENGINEERING RESEARCH SUPPORT SOC
PI DAEJON
PA RM 402, MAN-JE BLDG, 449-8 OJUNG-DONG, DAEDOEK-GU, DAEJON, 00000, SOUTH
KOREA
SN 1738-9976
J9 INT J SECUR APPL
JI Int. J. Secur. Appl.
PD FEB
PY 2015
VL 9
IS 2
BP V
EP VIII
PG 4
WC Computer Science, Information Systems
SC Computer Science
GA CR5HZ
UT WOS:000361373100001
ER
PT J
AU Cowings, P
Toscano, W
Kanis, D
Saicheur, T
Ravikumar, A
Gebreyesus, F
AF Cowings, Patricia
Toscano, William
Kanis, Dionisios
Saicheur, Theparat
Ravikumar, Anusha
Gebreyesus, Fiyore
TI Fluid Loading Effects on Temporal Profiles of Cardiovascular Responses
to Head-Down Tilt
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE orthostatic intolerance; autonomic responses; simulated microgravity
ID ORTHOSTATIC INTOLERANCE; SPACE-FLIGHT; HYPOTENSION; VARIABLES
AB BACKGROUND: Susceptibility of healthy astronauts to orthostatic hypotension and presyncope is exacerbated upon return from spaceflight. Up to 64% of astronauts experience postflight orthostatic intolerance. A promising countermeasure for postflight orthostatic intolerance is fluid loading by giving crew salt tablets and water prior to re-entry. The primary goal of the current study was to determine the optimal time window prior to re-entry when individual crewpersons would initiate fluid loading.
METHODS: There were 16 subjects who were given two 6-h exposures, with and without fluid loading (conditions), to head-down tilt (HDT) to simulate the effects of microgravity. Pre- and post-HDT stand tests of orthostatic tolerance were given. Physiological measurements recorded included heart rate, blood pressure, peripheral blood volume, total peripheral resistance, and impedance cardiography. Echocardiography measures of stroke volume and cardiac output were also recorded.
RESULTS: Data were analyzed with three-way repeated measures ANOVA (gender 3 condition 3 time). Only the condition 3 time interaction was significant for mean arterial pressure. Post hoc multiple comparison tests revealed significant increases in mean arterial pressure occurred between hours 1 and 3 of HDT after fluid loading (10 mmHg higher than no fluid).
DISCUSSION: These findings indicate that the optimal time for crew to begin fluid loading is within 1 to 3 h prior to re-entry. Nonsignificant trends of multiple cardiovascular responses showed similar time profiles. The large amount of individual variability suggests that fluid loading alone may be an inadequate countermeasure for all crewmembers. Further research is needed on possible adjunct methods of tailoring countermeasures for individuals.
C1 [Cowings, Patricia; Toscano, William; Kanis, Dionisios; Saicheur, Theparat; Ravikumar, Anusha; Gebreyesus, Fiyore] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
RP Cowings, P (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA.
EM patricia.s.cowings@nasa.gov
FU National Aeronautics and Space Administration, Human Research Program
(HRP), Human Health Countermeasures element (HHC)
FX This work was supported by the National Aeronautics and Space
Administration, Human Research Program (HRP), Human Health
Countermeasures element (HHC), as directed research.
NR 14
TC 1
Z9 1
U1 1
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD FEB
PY 2015
VL 86
IS 2
BP 88
EP 96
DI 10.3357/AMHP.4065.2015
PG 9
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CM0AG
UT WOS:000357340000004
PM 25946732
ER
PT J
AU Poulter, B
Cadule, P
Cheiney, A
Ciais, P
Hodson, E
Peylin, P
Plummer, S
Spessa, A
Saatchi, S
Yue, C
Zimmermann, NE
AF Poulter, Benjamin
Cadule, Patricia
Cheiney, Audrey
Ciais, Philippe
Hodson, Elke
Peylin, Philippe
Plummer, Stephen
Spessa, Allan
Saatchi, Sassan
Yue, Chao
Zimmermann, Niklaus E.
TI Sensitivity of global terrestrial carbon cycle dynamics to variability
in satellite-observed burned area
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; VEGETATION MODEL; CLIMATE-CHANGE; FIRE
EMISSIONS; EARTH SYSTEM; FOREST; ECOSYSTEMS; GROWTH; PRODUCTS; SAVANNA
AB Fire plays an important role in terrestrial ecosystems by regulating biogeochemistry, biogeography, and energy budgets, yet despite the importance of fire as an integral ecosystem process, significant advances remain to improve its prognostic representation in carbon cycle models. To recommend and to help prioritize model improvements, this study investigates the sensitivity of a coupled global biogeography and biogeochemistry model, LPJ, to observed burned area measured by three independent satellite-derived products, GFED v3.1, L3JRC, and GlobCarbon. Model variables are compared with benchmarks that include pantropical aboveground biomass, global tree cover, and CO2 and CO trace gas concentrations. Depending on prescribed burned area product, global aboveground carbon stocks varied by 300 Pg C, and woody cover ranged from 50 to 73 Mkm(2). Tree cover and biomass were both reduced linearly with increasing burned area, i.e., at regional scales, a 10% reduction in tree cover per 1000 km(2), and 0.04-to-0.40 Mg C reduction per 1000 km(2). In boreal regions, satellite burned area improved simulated tree cover and biomass distributions, but in savanna regions, model-data correlations decreased. Global net biome production was relatively insensitive to burned area, and the long-term land carbon sink was robust, similar to 2.5 Pg C yr(-1), suggesting that feedbacks from ecosystem respiration compensated for reductions in fuel consumption via fire. CO2 transport provided further evidence that heterotrophic respiration compensated any emission reductions in the absence of fire, with minor differences in modeled CO2 fluxes among burned area products. CO was a more sensitive indicator for evaluating fire emissions, with MODIS-GFED burned area producing CO concentrations largely in agreement with independent observations in high latitudes. This study illustrates how ensembles of burned area data sets can be used to diagnose model structures and parameters for further improvement and also highlights the importance in considering uncertainties and variability in observed burned area data products for model applications.
C1 [Poulter, Benjamin] Montana State Univ, Inst Ecosyst, Bozeman, MT 59717 USA.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Poulter, Benjamin; Cadule, Patricia; Cheiney, Audrey; Ciais, Philippe; Peylin, Philippe; Yue, Chao] LSCE CEA CNRS UVSQ, Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Hodson, Elke; Zimmermann, Niklaus E.] Swiss Fed Res Inst WSL, Dynam Macroecol, Birmensdorf, Switzerland.
[Plummer, Stephen] European Space Agcy, ESA Climate Off, Harwell, Berks, England.
[Spessa, Allan] Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Poulter, B (reprint author), Montana State Univ, Inst Ecosyst, Bozeman, MT 59717 USA.
EM benjamin.poulter@montana.edu
RI Zimmermann, Niklaus/A-4276-2008; Vuichard, Nicolas/A-6629-2011;
OI Zimmermann, Niklaus/0000-0003-3099-9604; Poulter,
Benjamin/0000-0002-9493-8600
FU FP7 Marie Curie Incoming International Fellowship [220546]; fire_cci
project - European Space Agency
FX B. P. acknowledges funding from an FP7 Marie Curie Incoming
International Fellowship (grant 220546). This study was partly supported
by the fire_cci project (http://www.esa-fire-cci.org/), funded by the
European Space Agency. The climate, land cover, and burned area data
sets used in this study are available at
http://badc.nerc.ac.uk/data/cru/, http://poulterlab.com/datasets/ and
http://www.globalfiredata.org/. We appreciate the constructive feedback
from three anonymous reviewers that greatly improved the discussion on
integrating burned area data within process-based models.
NR 88
TC 6
Z9 6
U1 3
U2 24
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD FEB
PY 2015
VL 29
IS 2
BP 207
EP 222
DI 10.1002/2013GB004655
PG 16
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA CH9UF
UT WOS:000354381200007
ER
PT J
AU Wang, W
Shu, CW
Yee, HC
Kotov, DV
Sjogreen, B
AF Wang, Wei
Shu, Chi-Wang
Yee, H. C.
Kotov, Dmitry V.
Sjoegreen, Bjoern
TI High Order Finite Difference Methods with Subcell Resolution for Stiff
Multispecies Discontinuity Capturing
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE Stiff reaction term; shock capturing; detonation; WENO; ENO subcell
resolution; multispecies; multireactions
ID HYPERBOLIC CONSERVATION-LAWS; RANDOM PROJECTION METHOD; REACTING
SHOCK-WAVES; SOURCE TERMS; EFFICIENT IMPLEMENTATION; NUMERICAL
STRUCTURE; EULER EQUATIONS; ENO SCHEMES; PROPAGATION; DETONATIONS
AB In this paper, we extend the high order finite-difference method with subcell resolution (SR) in [34] for two-species stiff one-reaction models to multispecies and multireaction inviscid chemical reactive flows, which are significantly more difficult because of the multiple scales generated by different reactions. For reaction problems, when the reaction time scale is very small, the reaction zone scale is also small and the governing equations become very stiff. Wrong propagation speed of discontinuity may occur due to the underresolved numerical solution in both space and time. The present SR method for reactive Euler system is a fractional step method. In the convection step, any high order shock-capturing method can be used. In the reaction step, an ODE solver is applied but with certain computed flow variables in the shock region modified by the Harten subcell resolution idea. Several numerical examples of multispecies and multireaction reactive flows are performed in both one and two dimensions. Studies demonstrate that the SR method can capture the correct propagation speed of discontinuities in very coarse meshes.
C1 [Wang, Wei] Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA.
[Shu, Chi-Wang] Brown Univ, Div Appl Math, Providence, RI 02912 USA.
[Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kotov, Dmitry V.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Sjoegreen, Bjoern] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
RP Wang, W (reprint author), Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA.
EM weiwang1@fiu.edu; shu@dam.brown.edu; helen.m.yee@nasa.gov;
dmitry.v.kotov@nasa.gov; sjogreen2@llnl.gov
FU NASA [NNX12AJ62A]; NSF [DMS-1112700]; DOE/SciDAC SAP grant
[DE-AI02-06ER25796]
FX The research of W. Wang is supported by NASA grant NNX12AJ62A. The
research of C.-W. Shu is supported by NASA grant NNX12AJ62A and NSF
grant DMS-1112700. The research of H. C. Yee and D. V. Kotov is
supported by DOE/SciDAC SAP grant DE-AI02-06ER25796.
NR 34
TC 2
Z9 2
U1 0
U2 1
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
EI 1991-7120
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD FEB
PY 2015
VL 17
IS 2
BP 317
EP 336
DI 10.4208/cicp.250214.130814a
PG 20
WC Physics, Mathematical
SC Physics
GA CH0EY
UT WOS:000353693400001
ER
PT J
AU Peterson, DA
Hyer, EJ
Campbell, JR
Fromm, MD
Hair, JW
Butler, CF
Fenn, MA
AF Peterson, David A.
Hyer, Edward J.
Campbell, James R.
Fromm, Michchael D.
Hair, Johnathan W.
Butler, Carolyn F.
Fenn, Marta A.
TI THE 2013 RIM FIRE Implications for Predicting Extreme Fire Spread,
Pyroconvection, and Smoke Emissions
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID PIXEL-BASED CALCULATION; AMERICAN BOREAL FOREST; RADIATIVE POWER; MODIS
OBSERVATIONS; UNITED-STATES; INITIAL ASSESSMENT; MODEL SIMULATIONS;
RELEASED MOISTURE; PYRO-CONVECTION; WILDLAND FIRES
C1 [Peterson, David A.] CNR, Washington, DC 20418 USA.
[Peterson, David A.; Hyer, Edward J.; Campbell, James R.] Naval Res Lab, Monterey, CA USA.
[Fromm, Michchael D.] Naval Res Lab, Washington, DC 20375 USA.
[Hair, Johnathan W.; Butler, Carolyn F.; Fenn, Marta A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Butler, Carolyn F.; Fenn, Marta A.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Peterson, DA (reprint author), CNR, Naval Res Lab, 7 Grace Hopper Ave, Monterey, CA 93943 USA.
EM david.peterson.ctr@nrlmry.navy.mil
RI Campbell, James/C-4884-2012; Hyer, Edward/E-7734-2011; peterson,
david/L-2350-2016
OI Campbell, James/0000-0003-0251-4550; Hyer, Edward/0000-0001-8636-2026;
FU Naval Research Laboratory; NASA SEAC4RS program under NASA [NNH12AT27i];
NASA [NNG13HH10I]; Micro Pulse Lidar Network; SEAC4RS Science Team
FX We thank Ralph Kahn (NASA Goddard), Jeffrey Reid (Naval Research
Laboratory), Bob Yokelson (University of Montana), and the National
Weather Service in Monterey, California, for their helpful advice. We
are all grateful to Shelly Crook at the Stanislaus National Forest
Service, as well as Mark Schug, Brad Quayle, and many other USFS
employees for providing the NIROPS fire perimeter data used in this
study. We also acknowledge contributions from the NASA
SEAC4RS Science Team, especially the DIAL/HSRL lidar group,
project scientist Brian Toon, and project managers Hal Maring and
Kenneth Jucks. This research was performed while David Peterson held a
National Research Council Research Associateship Award at the Naval
Research Laboratory. Edward Hyer's contributions were supported by the
NASA SEAC4RS program under NASA Award NNH12AT27i. James
Campbell acknowledges the support of NASA Interagency Agreement
NNG13HH10I, on behalf of the Micro Pulse Lidar Network and
SEAC4RS Science Team.
NR 87
TC 16
Z9 16
U1 4
U2 27
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 FEB
PY 2015
VL 96
IS 2
BP 229
EP 247
DI 10.1175/BAMS-D-14-00060.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CG5DA
UT WOS:000353310100006
ER
PT J
AU Yong, B
Liu, D
Gourley, JJ
Tian, YD
Huffman, GJ
Ren, LL
Hong, Y
AF Yong, Bin
Liu, Die
Gourley, Jonathan J.
Tian, Yudong
Huffman, George J.
Ren, Liliang
Hong, Yang
TI GLOBAL VIEW OF REAL-TIME TRMM MULTISATELLITE PRECIPITATION ANALYSIS
Implications for Its Successor Global Precipitation Measurement Mission
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID HYDROLOGIC PREDICTION; RAINFALL PRODUCTS; UNITED-STATES; ANALYSIS TMPA;
SATELLITE; BASINS; DATASETS; CYCLE
C1 [Yong, Bin; Liu, Die; Ren, Liliang] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing 210098, Jiangsu, Peoples R China.
[Gourley, Jonathan J.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
[Hong, Yang] Univ Oklahoma, Adv Radar Res Ctr, Natl Weather Ctr, Norman, OK 73019 USA.
[Hong, Yang] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
RP Yong, B (reprint author), Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, 1 Xikang Rd, Nanjing 210098, Jiangsu, Peoples R China.
EM yongbin_hhu@126.com
RI Gourley, Jonathan/C-7929-2016; Huffman, George/F-4494-2014; Measurement,
Global/C-4698-2015; Hong, Yang/D-5132-2009; Yong, Bin/C-2257-2014
OI Gourley, Jonathan/0000-0001-7363-3755; Huffman,
George/0000-0003-3858-8308; Hong, Yang/0000-0001-8720-242X; Yong,
Bin/0000-0003-1466-2091
FU National Science Foundation of China [51379056]
FX This work was financially supported by National Science Foundation of
China (51379056). The TMPA data used in this study were provided by the
NASA Goddard Space Flight Center's Mesoscale Atmospheric Processes
Laboratory and PPS, which develop and compute the TMPA as a contribution
to TRMM. The authors thank three anonymous reviewers, who helped to
improve the earlier version of this paper.
NR 42
TC 32
Z9 33
U1 4
U2 31
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD FEB
PY 2015
VL 96
IS 2
BP 283
EP 296
DI 10.1175/BAMS-D-14-00017.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CG5DA
UT WOS:000353310100009
ER
PT J
AU Watkins, JA
Ehlmann, BL
Yin, A
AF Watkins, Jessica A.
Ehlmann, Bethany L.
Yin, An
TI Long-runout landslides and the long-lasting effects of early water
activity on Mars
SO GEOLOGY
LA English
DT Article
ID VALLES-MARINERIS; MARTIAN LANDSLIDES; HISTORY; ZONE
AB Long-runout subaerial landslides (>50 km) are rare on Earth but are common features shaping Mars' Valles Marineris troughs. In this study, we investigated the highly debated emplacement mechanisms of these Martian landslides by combining spectral and satellite-image analyses. Our results suggest that hydrated silicates played a decisive role in facilitating landslide transport by lubricating the basal sliding zone. This new understanding implies that clay minerals, generated as a result of water-rock interactions in the Noachian and Hesperian (4.1-3.3 Ga), exert a long-lasting influence on geomorphic processes that shape the surface of the planet.
C1 [Watkins, Jessica A.; Yin, An] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Watkins, Jessica A.; Yin, An] Univ Calif Los Angeles, Inst Planets & Exoplanets iPLEX, Los Angeles, CA 90095 USA.
[Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Watkins, JA (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
EM jwatkins11@ucla.edu; ehlmann@caltech.edu; yin@ess.ucla.edu
FU National Science Foundation [DGE-1144087]
FX This project is supported by National Science Foundation Graduate
Research Fellowship DGE-1144087 to Watkins. This paper benefited from
critical reviews by A. Lucas, C. Okubo, editor J. Spotila, and anonymous
reviewers.
NR 30
TC 4
Z9 4
U1 3
U2 9
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 FEB
PY 2015
VL 43
IS 2
BP 107
EP 110
DI 10.1130/G36215.1
PG 4
WC Geology
SC Geology
GA CE8ME
UT WOS:000352095800003
ER
PT J
AU Huang, GQ
Zhou, K
Trawny, N
Roumeliotis, SI
AF Huang, Guoquan
Zhou, Ke
Trawny, Nikolas
Roumeliotis, Stergios I.
TI A Bank of Maximum A Posteriori (MAP) Estimators for Target Tracking
SO IEEE TRANSACTIONS ON ROBOTICS
LA English
DT Article
DE Algebraic geometry; analytical solution; maximum a posteriori (MAP)
estimator; nonlinear estimation; system of polynomial equations; target
tracking
ID BEARINGS-ONLY TRACKING; PARTICLE FILTERS; KALMAN FILTER; LOCALIZATION;
OBSERVABILITY
AB Nonlinear estimation problems, such as range-only and bearing-only target tracking, are often addressed using linearized estimators, e. g., the extended Kalman filter (EKF). These estimators generally suffer from linearization errors as well as the inability to track multimodal probability density functions. In this paper, we propose a bank of batch maximum a posteriori (MAP) estimators as a general estimation framework that provides relinearization of the entire state trajectory, multihypothesis tracking, and an efficient hypothesis generation scheme. Each estimator in the bank is initialized using a locally optimal state estimate for the current time step. Every time a new measurement becomes available, we relax the original batch-MAP problem and solve it incrementally. More specifically, we convert the relaxed one-step-ahead cost function into polynomial or rational form and compute all the local minima analytically. These local minima generate highly probable hypotheses for the target's trajectory and hence greatly improve the quality of the overall MAP estimate. Additionally, pruning of least probable hypotheses and marginalization of old states are employed to control the computational cost. Monte Carlo simulation and real-world experimental results show that the proposed approach significantly outperforms the standard EKF, the batch-MAP estimator, and the particle filter.
C1 [Huang, Guoquan] Univ Delaware, Dept Mech Engn, Newark, DE 19716 USA.
[Zhou, Ke] Starkey Hearing Technol, Eden Prairie, MN 55344 USA.
[Trawny, Nikolas] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Roumeliotis, Stergios I.] Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA.
RP Huang, GQ (reprint author), Univ Delaware, Dept Mech Engn, Newark, DE 19716 USA.
EM ghuang@udel.edu; ke_zhou@starkey.com; nikolas.trawny@jpl.nasa.gov;
stergios@cs.umn.edu
FU University of Delaware College of Engineering; University of Minnesota
through the Digital Technology Center; AFOSR [FA9550-10-1-0567]
FX This work was supported by University of Delaware College of
Engineering, University of Minnesota through the Digital Technology
Center, and the AFOSR (FA9550-10-1-0567).
NR 50
TC 0
Z9 1
U1 2
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1552-3098
EI 1941-0468
J9 IEEE T ROBOT
JI IEEE Trans. Robot.
PD FEB
PY 2015
VL 31
IS 1
BP 85
EP 103
DI 10.1109/TRO.2014.2378432
PG 19
WC Robotics
SC Robotics
GA CE7YN
UT WOS:000352057900008
ER
PT J
AU Halkides, DJ
Waliser, DE
Lee, T
Menemenlis, D
Guan, B
AF Halkides, D. J.
Waliser, Duane E.
Lee, Tong
Menemenlis, Dimitris
Guan, Bin
TI Quantifying the processes controlling intraseasonal mixed-layer
temperature variability in the tropical Indian Ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; SEA-SURFACE TEMPERATURE; MOIST THERMODYNAMIC
STRUCTURE; HEAT-BALANCE; EQUATORIAL PACIFIC; CIRCULATION MODEL;
DYNAMICS; WIND; PREDICTION; WAVES
AB Spatial and temporal variation of processes that determine ocean mixed-layer (ML) temperature (MLT) variability on the timescale of the Madden-Julian Oscillation (MJO) in the Tropical Indian Ocean (TIO) are examined in a heat-conserving ocean state estimate for years 1993-2011. We introduce a new metric for representing spatial variability of the relative importance of processes. In general, horizontal advection is most important at the Equator. Subsurface processes and surface heat flux are more important away from the Equator, with surface heat flux being the more dominant factor. Analyses at key sites are discussed in the context of local dynamics and literature. At 0 degrees, 80.5 degrees E, for MLT events > 2 standard deviations, ocean dynamics account for more than two thirds of the net tendency during cooling and warming phases. Zonal advection alone accounts for similar to 40% of the net tendency. Moderate events (1-2 standard deviations) show more differences between events, and some are dominated by surface heat flux. At 8 degrees S, 67 degrees E in the Seychelles-Chagos Thermocline Ridge (SCTR) area, surface heat flux accounts for similar to 70% of the tendency during strong cooling and warming phases; subsurface processes linked to ML depth (MLD) deepening (shoaling) during cooling (warming) account for similar to 30%. MLT is more sensitive to subsurface processes in the SCTR, due to the thin MLD, thin barrier layer and raised thermocline. Results for 8 degrees S, 67 degrees E support assertions by Vialard et al. (2008) not previously confirmed due to measurement error that prevented budget closure and the small number of events studied. The roles of MLD, barrier layer thickness, and thermocline depth on different timescales are examined.
C1 [Halkides, D. J.; Waliser, Duane E.; Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn JIERESSE, Los Angeles, CA 90095 USA.
[Halkides, D. J.; Waliser, Duane E.; Lee, Tong; Menemenlis, Dimitris; Guan, Bin] CALTECH, Jet Prop Lab, Div Earth Sci, Pasadena, CA USA.
RP Halkides, DJ (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn JIERESSE, Los Angeles, CA 90095 USA.
EM halkides@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
FU National Aeronautics and Space Administration (NASA); NASA Physical
Oceanography grants; National Oceanographic Partnership Program (NOPP);
NASA Earth Science Physical Oceanography Program; NASA MEaSUREs DISCOVER
Project
FX (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 (NASA). NASA Physical Oceanography
grants are acknowledged. Data used in this study include ocean state
estimation and forcing fields from the Estimating the Circulation and
Climate of the Ocean (ECCO) project (http://www.ecco-group.org);
Microwave OI SST data produced by Remote Sensing Systems and sponsored
by National Oceanographic Partnership Program (NOPP), the NASA Earth
Science Physical Oceanography Program, and the NASA MEaSUREs DISCOVER
Project (www.remss.com); temperature and salinity climatologies from the
2013 World Ocean Atlas (WOA) (http://www.nodc.noaa.gov/OC5/woa13);
surface heat fluxes from the Woods Hole Oceanographic Institute's
Objectively Analyzed Air-Sea Flux (OAFlux) with International Satellite
Cloud Climatology Project (ISCCP) data
(http://oaflux.whoi.edu/heatflux.html); surface wind speeds derived from
QuickSCAT satellite scatterometer data processed at IFREMER
(http://cersat.ifremer.fr/data/products/cal-val/
NR 73
TC 5
Z9 5
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD FEB
PY 2015
VL 120
IS 2
BP 692
EP 715
DI 10.1002/2014JC010139
PG 24
WC Oceanography
SC Oceanography
GA CE9HM
UT WOS:000352154800007
ER
PT J
AU Song, YT
Lee, T
Moon, JH
Qu, TD
Yueh, S
AF Song, Y. Tony
Lee, Tong
Moon, Jae-Hong
Qu, Tangdong
Yueh, Simon
TI Modeling skin-layer salinity with an extended surface-salinity layer
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID OCEAN SALINITY; AQUARIUS; ARGO; VARIABILITY; VALIDATION; SMOS; SYSTEM;
IMPACT; ERROR; RAIN
AB Due to near-surface salinity stratification, it is problematic to compare satellite-measured surface salinity within the first few centimeters (skin-layer) of the ocean with Argo-measured top-level salinity at about 5 m or with ocean models that do not resolve the skin layer. Although an instrument can be designed to measure the surface salinity, a global scale measurement is currently not available. A regional model can be configured to have a vertical grid in centimeters but it would be computationally prohibited on a global scale due to time step constraints. Here we propose an extended surface-salinity layer (ESSL) within a global ocean circulation model to diagnose skin SSS without increasing the computational cost, while allowing comparable solutions with both satellite and Argo salinity at the respective depths. Using a quarter-degree global ocean model, we show that the ESSL improves near-surface salinity significantly in comparisons with the Aquarius SSS and Argo salinity at 5 and 10 m, respectively. Comparing with data-assimilated HYCOM results reveal that the ESSL provides much stronger seasonal variability of SSS, similar to the Aquarius observations. We also demonstrate that the ESSL solution can be used to constrain the global mean SSS in Aquarius SSS retrieval.
C1 [Song, Y. Tony; Lee, Tong; Yueh, Simon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Moon, Jae-Hong] Jeju Natl Univ, Dept Earth & Marine Sci, Jeju, South Korea.
[Qu, Tangdong] Univ Hawaii, Int Pacific Res Ctr, SOEST, Honolulu, HI 96822 USA.
RP Song, YT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Tony.Song@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA's Aquarius
Science team
FX The research described here was conducted at the Jet Propulsion
Laboratory, California Institute of Technology, under contracts with the
National Aeronautics and Space Administration (NASA). The University of
Hawaii component of the research is supported under NASA's Aquarius
Science team. Assistance from Wendy Tang and Akiko Hayashi in reading
data sets and valuable comments from Gary Lagerloef is greatly
appreciated. Data used in this study are available at
http://podaac.jpl.nasa.gov/aquarius. SOEST contribution 9254, and IPRC
contribution IPRC-1097.
NR 39
TC 3
Z9 3
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD FEB
PY 2015
VL 120
IS 2
BP 1079
EP 1095
DI 10.1002/2014JC010346
PG 17
WC Oceanography
SC Oceanography
GA CE9HM
UT WOS:000352154800030
ER
PT J
AU Whitcraft, AK
Becker-Reshef, I
Killough, BD
Justice, CO
AF Whitcraft, Alyssa K.
Becker-Reshef, Inbal
Killough, Brian D.
Justice, Christopher O.
TI Meeting Earth Observation Requirements for Global Agricultural
Monitoring: An Evaluation of the Revisit Capabilities of Current and
Planned Moderate Resolution Optical Earth Observing Missions
SO REMOTE SENSING
LA English
DT Article
ID CONTERMINOUS UNITED-STATES; LAND-SURFACE TEMPERATURE; TERM ACQUISITION
PLAN; COVER DATA; MODIS DATA; SAR; REFLECTANCE; COMPLETION; ARCHIVE;
SCIENCE
AB Agriculture is a highly dynamic process in space and time, with many applications requiring data with both a relatively high temporal resolution (at least every 8 days) and fine-to-moderate (FTM < 100 m) spatial resolution. The relatively infrequent revisit of FTM optical satellite observatories coupled with the impacts of cloud occultation have translated into a barrier for the derivation of agricultural information at the regional-to-global scale. Drawing upon the Group on Earth Observations Global Agricultural Monitoring (GEOGLAM) Initiative's general satellite Earth observation (EO) requirements for monitoring of major production areas, Whitcraft et al. (this issue) have described where, when, and how frequently satellite data acquisitions are required throughout the agricultural growing season at 0.05 degrees, globally. The majority of areas and times of year require multiple revisits to probabilistically yield a view at least 70%, 80%, 90%, or 95% clear within eight days, something that no present single FTM optical observatory is capable of delivering. As such, there is a great potential to meet these moderate spatial resolution optical data requirements through a multi-space agency/multi-mission constellation approach. This research models the combined revisit capabilities of seven hypothetical constellations made from five satellite sensors-Landsat 7 Enhanced Thematic Mapper (Landsat 7 ETM+), Landsat 8 Operational Land Imager and Thermal Infrared Sensor (Landsat 8 OLI/TIRS), Resourcesat-2 Advanced Wide Field Sensor (Resourcesat-2 AWiFS), Sentinel-2A Multi-Spectral Instrument (MSI), and Sentinel-2B MSI-and compares these capabilities with the revisit frequency requirements for a reasonably cloud-free clear view within eight days throughout the agricultural growing season. Supplementing Landsat 7 and 8 with missions from different space agencies leads to an improved capacity to meet requirements, with Resourcesat-2 providing the largest incremental improvement in requirements met. The best performing constellation can meet 71%-91% of the requirements for a view at least 70% clear, and 45%-68% of requirements for a view at least 95% clear, varying by month. Still, gaps exist in persistently cloudy regions/periods, highlighting the need for data coordination and for consideration of active EO for agricultural monitoring. This research highlights opportunities, but not actual acquisition rates or data availability/access; systematic acquisitions over actively cropped agricultural areas as well as a policy which guarantees continuous access to high quality, interoperable data are essential in the effort to meet EO requirements for agricultural monitoring.
C1 [Whitcraft, Alyssa K.; Becker-Reshef, Inbal; Justice, Christopher O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Killough, Brian D.] Natl Aeronaut & Space Adm, Langley Res Ctr, Comm Earth Observat Satellites Syst Engn Off, Hampton, VA 23681 USA.
RP Whitcraft, AK (reprint author), Univ Maryland, Dept Geog Sci, 4321 Hartwick Rd Suite 410, College Pk, MD 20742 USA.
EM alyssakw@umd.edu; ireshef@umd.edu; brian.d.killough@nasa.gov;
cjustice@umd.edu
FU NASA Earth and Space Science Fellowship [NNX11AL56H]; NASA Applied
Sciences [NNX1AQ79G]
FX The authors would like to acknowledge Paul Kessler and Shaun Deacon in
the CEOS Systems Engineering office for their assistance with the COVE
simulation. We thank the CEOS Ad Hoc Team for GEOGLAM for their
contributions in the development of the EO data requirements table. We
thank Eric Vermote (NASA-GSFC), Samuel Goward (UMD) and Jeffrey Masek
(NASA-GSFC) for their feedback and guidance. Finally, the authors would
like to acknowledge the NASA Earth and Space Science Fellowship
(NNX11AL56H) and NASA Applied Sciences (NNX1AQ79G) for their support of
this work.
NR 61
TC 8
Z9 8
U1 0
U2 17
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2015
VL 7
IS 2
BP 1482
EP 1503
DI 10.3390/rs70201482
PG 22
WC Remote Sensing
SC Remote Sensing
GA CF2TQ
UT WOS:000352400900016
ER
PT J
AU Gastellu-Etchegorry, JP
Yin, TG
Lauret, N
Cajgfinger, T
Gregoire, T
Grau, E
Feret, JB
Lopes, M
Guilleux, J
Dedieu, G
Malenovsky, Z
Cook, BD
Morton, D
Rubio, J
Durrieu, S
Cazanave, G
Martin, E
Ristorcelli, T
AF Gastellu-Etchegorry, Jean-Philippe
Yin, Tiangang
Lauret, Nicolas
Cajgfinger, Thomas
Gregoire, Tristan
Grau, Eloi
Feret, Jean-Baptiste
Lopes, Mailys
Guilleux, Jordan
Dedieu, Gerard
Malenovsky, Zbynek
Cook, Bruce Douglas
Morton, Douglas
Rubio, Jeremy
Durrieu, Sylvie
Cazanave, Gregory
Martin, Emmanuel
Ristorcelli, Thomas
TI Discrete Anisotropic Radiative Transfer (DART 5) for Modeling Airborne
and Satellite Spectroradiometer and LIDAR Acquisitions of Natural and
Urban Landscapes
SO REMOTE SENSING
LA English
DT Article
ID BIDIRECTIONAL REFLECTANCE MODEL; PULSED-LASER SYSTEMS; TERRESTRIAL
ENVIRONMENTS; LIGHT-SCATTERING; CANOPY; FOREST; RESOLUTION; IMAGES;
SURFACE; RETRIEVAL
AB Satellite and airborne optical sensors are increasingly used by scientists, and policy makers, and managers for studying and managing forests, agriculture crops, and urban areas. Their data acquired with given instrumental specifications (spectral resolution, viewing direction, sensor field-of-view, etc.) and for a specific experimental configuration (surface and atmosphere conditions, sun direction, etc.) are commonly translated into qualitative and quantitative Earth surface parameters. However, atmosphere properties and Earth surface 3D architecture often confound their interpretation. Radiative transfer models capable of simulating the Earth and atmosphere complexity are, therefore, ideal tools for linking remotely sensed data to the surface parameters. Still, many existing models are oversimplifying the Earth-atmosphere system interactions and their parameterization of sensor specifications is often neglected or poorly considered. The Discrete Anisotropic Radiative Transfer (DART) model is one of the most comprehensive physically based 3D models simulating the Earth-atmosphere radiation interaction from visible to thermal infrared wavelengths. It has been developed since 1992. It models optical signals at the entrance of imaging radiometers and laser scanners on board of satellites and airplanes, as well as the 3D radiative budget, of urban and natural landscapes for any experimental configuration and instrumental specification. It is freely distributed for research and teaching activities. This paper presents DART physical bases and its latest functionality for simulating imaging spectroscopy of natural and urban landscapes with atmosphere, including the perspective projection of airborne acquisitions and LIght Detection And Ranging (LIDAR) waveform and photon counting signals.
C1 [Gastellu-Etchegorry, Jean-Philippe; Yin, Tiangang; Lauret, Nicolas; Cajgfinger, Thomas; Gregoire, Tristan; Grau, Eloi; Feret, Jean-Baptiste; Lopes, Mailys; Guilleux, Jordan; Dedieu, Gerard] Univ Toulouse, CNRS, Ctr Etud Spatiales BIOsphere CESBIO UPS, CNES,IRD, F-31401 Toulouse 9, France.
[Malenovsky, Zbynek] Univ Wollongong, Inst Conservat Biol, Sch Biol Sci, Wollongong, NSW 2522, Australia.
[Malenovsky, Zbynek] Univ Tasmania, Sch Land & Food, Hobart, Tas 7001, Australia.
[Cook, Bruce Douglas; Morton, Douglas; Rubio, Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Durrieu, Sylvie] AgroParisTech ENGREF, TETIS Irstea, Cirad, F-34196 Montpellier 05, France.
[Cazanave, Gregory; Martin, Emmanuel; Ristorcelli, Thomas] Magellium, F-31520 Ramonville St Agne, France.
RP Gastellu-Etchegorry, JP (reprint author), Univ Toulouse, CNRS, Ctr Etud Spatiales BIOsphere CESBIO UPS, CNES,IRD, F-31401 Toulouse 9, France.
EM jean-philippe.gastellu-etchegorry@cesbio.cnes.fr;
tiangang.yin.85@gmail.com; nicolas.lauret@cesbio.cnes.fr;
cajgfingert@cesbio.cnes.fr; gregoiret@cesbio.cnes.fr;
eloi.grau@gmail.com; jb.feret@gmail.com; mailys.lopes@gmail.com;
guilleuxj@cesbio.cnes.fr; gerard.dedieu@cesbio.cnes.fr;
zbynek.malenovsky@gmail.com; bruce.cook@nasa.gov;
douglas.morton@nasa.gov; rubio.jeremy@gmail.com;
sylvie.durrieu@teledetection.fr; gregory.cazanave@magellium.fr;
emmanuel.martin@magellium.fr; thomas.ristorcelli@magellium.fr
RI Malenovsky, Zbynek/A-7819-2011; Morton, Douglas/D-5044-2012;
OI Malenovsky, Zbynek/0000-0002-1271-8103; Lopes,
Mailys/0000-0002-3804-7950; Grau, Eloi/0000-0001-5757-7239
FU ANR; Centre National d'Etudes Spatiales (CNES); ARC [DP140101488]
FX This work was supported by the ANR in the frame of the FOLI3D project
and by the Centre National d'Etudes Spatiales (CNES) in the frame of the
TOSCA projects "Stem-Leaf" and "Geostationary satellite". Part of the
work was conducted in the frame of the NASA project "DART-LIDAR".
Contribution of J.-B. Feret was supported by a CNES post-doctoral
research grant and contribution of Z. Malenovsky was supported by the
ARC Discovery project DP140101488 "AirLIFT". The authors are grateful
for the Toulouse city geo-database provided by Toulouse town hall and
thankful to all scientists who contributed to DART development since its
first steps in 1992.
NR 69
TC 19
Z9 20
U1 6
U2 30
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2015
VL 7
IS 2
BP 1667
EP 1701
DI 10.3390/rs70201667
PG 35
WC Remote Sensing
SC Remote Sensing
GA CF2TQ
UT WOS:000352400900024
ER
PT J
AU Singh, SK
Srivastava, PK
Singh, D
Han, DW
Gautam, SK
Pandey, AC
AF Singh, Sudhir Kumar
Srivastava, Prashant K.
Singh, Dharmveer
Han, Dawei
Gautam, Sandeep Kumar
Pandey, A. C.
TI Modeling groundwater quality over a humid subtropical region using
numerical indices, earth observation datasets, and X-ray diffraction
technique: a case study of Allahabad district, India
SO ENVIRONMENTAL GEOCHEMISTRY AND HEALTH
LA English
DT Article
DE Water quality index; XRD; Synthetic pollution index; Ganga basin; Remote
sensing and GIS; Multivariate analysis
ID MULTIVARIATE STATISTICAL TECHNIQUES; SURFACE-WATER QUALITY; GOMTI RIVER
INDIA; BRAGGS LAW; LAND-USE; POLLUTION; GIS; IMPACT; CHEMISTRY; CHINA
AB Water is undoubtedly the vital commodity for all living creatures and required for well-being of the human society. The present work is based on the surveys and chemical analyses performed on the collected groundwater samples in a part of the Ganga basin in order to understand the sources and evolution of the water quality in the region. The two standard indices such as water quality index and synthetic pollution index for the classification of water in the region are computed. The soil and sediment analysis are carried out with the help of X-ray diffractometer (XRD) for the identification of possible source of ions in water from rock and soil weathering. The dominant minerals which include quartz, muscovite, plagioclase, and orthoclase are reported in the area. The study further utilizes the multivariate statistical techniques for handling large and complex datasets in order to get better information about the groundwater quality. The following statistical methods such as cluster analysis (CA), factor analysis (FA), and principal component analysis (PCA) are applied to handle the large datasets and to understand the latent structure of the data. Through FA/PCAs, we have identified a total of 3 factors in pre-monsoon and 4 factors in post-monsoon season, which are responsible for the whole data structure. These factors explain 77.62 and 82.39 % of the total variance of the pre- and post-monsoon datasets. On the other hand, CA depicted the regions that have similar pollutants origin. The average value of synthetic pollution index of groundwater during pre-monsoon is 9.27, while during post-monsoon, it has been recorded as 8.74. On the other hand, the average values of water quality index of groundwater during pre-monsoon and post-monsoon seasons are found as 217.59 and 233.02, respectively. The study indicates that there occurs an extensive urbanization with gradual vast development of various small-and large-scale industries, which is responsible for degradation in water quality. The overall analysis reveals that the agricultural runoff, waste disposal, leaching, and irrigation with waste-water are the main causes of groundwater pollution followed by some degree of pollution from geogenic sources such as rock and soil weathering, confirmed through XRD analysis.
C1 [Singh, Sudhir Kumar; Pandey, A. C.] Univ Allahabad, Nehru Sci Ctr, K Banerjee Ctr Atmospher & Ocean Studies, IIDS, Allahabad 211002, Uttar Pradesh, India.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Srivastava, Prashant K.; Han, Dawei] Univ Bristol, Dept Civil Engn, Bristol, Avon, England.
[Singh, Dharmveer] Univ Allahabad, Dept Chem, Allahabad 211002, Uttar Pradesh, India.
[Gautam, Sandeep Kumar] Jawaharlal Nehru Univ, Sch Environm Sci, New Delhi 110067, India.
RP Srivastava, PK (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Code 617,Room G208,Bldg 33, Greenbelt, MD 20771 USA.
EM prashant.k.srivastava@nasa.gov
OI Gautam, Sandeep K/0000-0002-3914-9887
FU School of Environmental Sciences, Jawaharlal Nehru University;
University Grant Commission, New Delhi [42-74/2013(SR)]
FX Authors are grateful to School of Environmental Sciences, Jawaharlal
Nehru University and University Grant Commission, New Delhi, Grant No.
(F. No. 42-74/2013(SR) for their technical and financial support,
respectively. The views expressed here are those of the authors solely
and do not constitute a statement of policy, decision, or position on
behalf of NASA or the authors' affiliated institutions.
NR 51
TC 7
Z9 7
U1 1
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0269-4042
EI 1573-2983
J9 ENVIRON GEOCHEM HLTH
JI Environ. Geochem. Health
PD FEB
PY 2015
VL 37
IS 1
BP 157
EP 180
DI 10.1007/s10653-014-9638-z
PG 24
WC Engineering, Environmental; Environmental Sciences; Public,
Environmental & Occupational Health; Water Resources
SC Engineering; Environmental Sciences & Ecology; Public, Environmental &
Occupational Health; Water Resources
GA CE3TK
UT WOS:000351751600012
PM 25086613
ER
PT J
AU Wenny, BN
Helder, D
Hong, J
Leigh, L
Thome, KJ
Reuter, D
AF Wenny, Brian N.
Helder, Dennis
Hong, Jungseok
Leigh, Larry
Thome, Kurtis J.
Reuter, Dennis
TI Pre- and Post-Launch Spatial Quality of the Landsat 8 Thermal Infrared
Sensor
SO REMOTE SENSING
LA English
DT Article
AB The Thermal Infrared Sensor (TIRS) for the Landsat 8 platform was designed and built at NASA Goddard Space Flight Center (GSFC). TIRS data will extend the data record for thermal observations from the heritage Landsat sensors, dating back to the launch of Landsat 4 in 1982. The two-band (10.9 and 12.0 mu m) pushbroom sensor with a 185 km-wide swath uses a staggered arrangement of quantum well infrared photodetector (QWIPs) arrays. The required spatial resolution is 100 m for TIRS, with the assessment of crop moisture and water resources being science drivers for that resolution. The evaluation of spatial resolution typically relies on a straight knife-edge technique to determine the spatial edge response of a detector system, and such an approach was implemented for TIRS. Flexibility in the ground calibration equipment used for TIRS thermal-vacuum chamber testing also made possible an alternate strategy that implemented a circular target moved in precise sub-pixel increments across the detectors to derive the edge response. On-orbit, coastline targets were developed to evaluate the spatial response performance. Multiple targets were identified that produced similar results to one another. Even though there may be a slight bias in the point spread function (PSF)/modulation transfer function (MTF) estimates towards poorer performance using this approach, it does have the ability to track relative changes for monitoring long-term instrument status. The results for both pre- and post-launch response analysis show general good agreement and consistency with edge slope along-track values of 0.53 and 0.58 pre- and post-launch and across-track values 0f 0.59 and 0.55 pre- and post-launch.
C1 [Wenny, Brian N.] Sigma Space Corp, Lanham, MD 20706 USA.
[Helder, Dennis; Hong, Jungseok; Leigh, Larry] S Dakota State Univ, Coll Engn, Off Engn Res, Brookings, SD 57007 USA.
[Thome, Kurtis J.; Reuter, Dennis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wenny, BN (reprint author), Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA.
EM brian.n.wenny@nasa.gov; dennis.helder@sdstate.edu;
jungseok.hong@sdstate.edu; larry.leigh@sdstate.edu;
kurtis.thome@nasa.gov; dennis.c.reuter@nasa.gov
RI Thome, Kurtis/D-7251-2012
NR 19
TC 4
Z9 4
U1 2
U2 9
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2015
VL 7
IS 2
BP 1962
EP 1980
DI 10.3390/rs70201962
PG 19
WC Remote Sensing
SC Remote Sensing
GA CF1BK
UT WOS:000352278400001
ER
PT J
AU Jackson, BV
Odstrcil, D
Yu, HS
Hick, PP
Buffington, A
Mejia-Ambriz, JC
Kim, J
Hong, S
Kim, Y
Han, J
Tokumaru, M
AF Jackson, B. V.
Odstrcil, D.
Yu, H. -S.
Hick, P. P.
Buffington, A.
Mejia-Ambriz, J. C.
Kim, J.
Hong, S.
Kim, Y.
Han, J.
Tokumaru, M.
TI The UCSD kinematic IPS solar wind boundary and its use in the ENLIL 3-D
MHD prediction model
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID REMOTE-SENSING OBSERVATIONS; INTERPLANETARY SCINTILLATION OBSERVATIONS;
TIME-DEPENDENT TOMOGRAPHY; ADVANCED COMPOSITION EXPLORER; CORONAL MASS
EJECTIONS; HELIOSPHERIC TOMOGRAPHY; RECONSTRUCTION; DISTURBANCES; CME;
STREAMS
AB The University of California, San Diego interplanetary scintillation (IPS) time-dependent kinematic 3-D reconstruction technique has been used and expanded upon for over a decade to provide predictions of heliospheric solar wind parameters. These parameters include global reconstructions of velocity, density, and (through potential field modeling and extrapolation upward from the solar surface) radial and tangential interplanetary magnetic fields. Time-dependent results can be extracted at any solar distance within the reconstructed volume and are now being exploited as inner boundary values to drive the ENLIL 3-D MHD model in near real time. The advantage of this coupled system is that it uses the more complete physics of 3-D MHD modeling to provide an automatic prediction of coronal mass ejections and solar wind stream structures several days prior to their arrival at Earth without employing coronagraph observations. Here we explore, with several examples, the current differences between the IPS real-time kinematic analyses and those from the ENLIL 3-D MHD modeling using IPS-derived real-time boundaries. Future possibilities for this system include incorporating many different worldwide IPS stations as input to the remote sensing analysis using ENLIL as a kernel in the iterative 3-D reconstructions.
C1 [Jackson, B. V.; Yu, H. -S.; Hick, P. P.; Buffington, A.; Mejia-Ambriz, J. C.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Odstrcil, D.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mejia-Ambriz, J. C.] Univ Nacl Autonoma Mexico, Unidad Michoacan, Inst Geofis, SCiESMEX, Morelia, Michoacan, Mexico.
[Kim, J.; Hong, S.; Kim, Y.; Han, J.] Natl Radio Res Agcy, Korean Space Weather Ctr, Jeju Si, South Korea.
[Tokumaru, M.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
RP Jackson, BV (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
EM bvjackson@ucsd.edu
FU AFOSR [FA9550-11-1-0324]; NSF [AGS-1053766, AGS-1358399]; UC MEXUS
CONACyT program while at UCSD; NASA/NSF LWS Partnership for
Collaborative Space Weather Modeling program Collaborative Space Weather
[11-LWSCSW11-0034]
FX The KSWC initiated and have supported this project from its onset with
partial funding to B.V. Jackson and D. Odstrcil. In addition, B.V.
Jackson, H.-S. Yu., and A. Buffington have been partially funded by
AFOSR contract FA9550-11-1-0324 and NSF contracts AGS-1053766 and
AGS-1358399 to the University of California, San Diego. J. Mejia-Ambriz
thanks and acknowledges his support from the UC MEXUS CONACyT program
while at UCSD. D. Odstrcil also acknowledges support from the NASA/NSF
LWS Partnership for Collaborative Space Weather Modeling program
Collaborative Space Weather 11-LWSCSW11-0034 project for this effort.
The SWIFT IPS observations were carried out under the solar wind program
of the Solar-Terrestrial Environment Laboratory (STELab) of Nagoya
University. The STELab near-real-time IPS observations used in these
analyses are available online at . We are grateful for the SOHO LASCO
team and especially K. Schenk for providing alerts (e-mail: email
xmlns:xlink="http://www.w3.org/1999/xlink"
xlink:href="Soho-halo-alert@grace.nascom.nasa.gov">Soho-halo-alert@grace
.nascom.nasa.gov) and for making available the LASCO C2 and C3
observations at used in these analyses. We thank the ACE spacecraft
group for making their data available in real time for use at UCSD
through the Space Weather Prediction Center, NOAA, Boulder, and for
Figure rid="#swe20202-fig-0004" at and to the Wind spacecraft group for
making their data available for Figures rid="#swe20202-fig-0006" and
rid="#swe20202-fig-0007" at . A special thanks is warranted for the
SOHO/CELIAS data made available to UCSD in near real time by the Proton
Monitor group at the University of Maryland, College Park, USA at
ftp://space.umd.edu/pm/houraverages.txt.
NR 63
TC 7
Z9 7
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD FEB
PY 2015
VL 13
IS 2
BP 104
EP 115
DI 10.1002/2014SW001130
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CE0ZP
UT WOS:000351541000003
ER
PT J
AU Liu, TT
Bish, DL
Socki, RA
Harvey, RP
Tonui, E
AF Liu, Tingting
Bish, David L.
Socki, Richard A.
Harvey, Ralph P.
Tonui, Eric
TI Mineralogy and formation of evaporite deposits from the Lewis Cliff ice
tongue, Antarctica
SO ANTARCTIC SCIENCE
LA English
DT Article
DE borate; carbonate; mirabilite; nahcolite; qilianshanite; sulfate
ID MCMURDO DRY VALLEYS; NORTHERN GREAT-PLAINS; VICTORIA LAND; GEOCHEMISTRY;
ORIGIN; LAKES; SULFATE; CANADA; BRINES; SALTS
AB The mineralogy of evaporites from the Lewis Cliff ice tongue (LCIT), Antarctica, and their mineral stabilities and transformation behaviours under different temperature and relative humidity (RH) conditions have been evaluated to elucidate formation mechanism(s). A variety of sodium (Na)-rich evaporite minerals were documented using RH-controlled powder X-ray diffraction (XRD) methods including Na-sulfates (mirabilite and thenardite), Na-carbonate/bicarbonates (nahcolite, occasional trona and natron) and Na-borates (qilianshanite and borax). Mirabilite begins to dehydrate to thenardite, and natron to trona and natrite when exposed to room temperature, even when maintained at RH values similar to those measured at the LCIT (50-70%). The boron-mineral qilianshanite was discovered for the first time in Antarctica within the evaporite mounds. The mirabilite-rich mounds are deduced to have formed via a freezing/sublimation process that occurred in glacial or subglacial bodies of water supplied by glacial tills containing microbially oxidized sulfate ions. The needle-like nahcolite crystals growing on the exteriors of the mounds suggest a dissolution/precipitation process involving atmospheric CO2 and water. The co-existence of nahcolite and boron-bearing minerals indicates the presence of a Na+-, HCO3--and boron-bearing alkaline brine, which produces qilianshanite as a secondary mineral by reaction of nahcolite and borax in atmospheric CO2 and H2O.
C1 [Liu, Tingting; Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Socki, Richard A.] NASA, Johnson Space Ctr, Jacobs JETS, UTAS, Houston, TX 77058 USA.
[Harvey, Ralph P.] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA.
[Tonui, Eric] BP Amer, Upstream Res & Technol, Houston, TX 77079 USA.
RP Liu, TT (reprint author), Ohio State Univ, Sch Earth Sci, 125 South Oval Mall, Columbus, OH 43210 USA.
EM liu.2189@osu.edu
FU NSF; Indiana University
FX Sample collection was supported by an NSF grant to R. Harvey, and
further mineralogical analysis was supported by the Haydn Murray fund at
Indiana University. Authors acknowledge the valuable comments and
insights provided by two anonymous reviewers, which further improved the
quality of the work. Authors declare no competing interests from this
work.
NR 40
TC 2
Z9 2
U1 3
U2 9
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0954-1020
EI 1365-2079
J9 ANTARCT SCI
JI Antarct. Sci.
PD FEB
PY 2015
VL 27
IS 1
BP 73
EP 84
DI 10.1017/S0954102014000406
PG 12
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA CD7TI
UT WOS:000351294900010
ER
PT J
AU Wu, L
Boyd, JL
Daniels, V
Wang, ZW
Chow, DSL
Putcha, L
AF Wu, Lei
Boyd, Jason L.
Daniels, Vernie
Wang, Zuwei
Chow, Diana S-L.
Putcha, Lakshmi
TI Dose Escalation Pharmacokinetics of Intranasal Scopolamine Gel
Formulation
SO JOURNAL OF CLINICAL PHARMACOLOGY
LA English
DT Article
DE scopolamine; intranasal; pharmacokinetics; dose escalation
ID MOTION SICKNESS; TRANSDERMAL SCOPOLAMINE; HEALTHY-VOLUNTEERS;
DRUG-DELIVERY; NASAL SPRAY; PHARMACODYNAMICS; PREVENTION;
BIOAVAILABILITY; MISSIONS; EFFICACY
AB Astronauts experience Space Motion Sickness requiring treatment with an anti-motion sickness medication, scopolamine during space missions. Bioavailability after oral administration of scopolamine is low and variable, and absorption form transdermal patch is slow and prolonged. Intranasal administration achieves faster absorption and higher bioavailability of drugs that are subject to extrahepatic, first pass metabolism after oral dosing. We examined pharmacokinetics of 0.1, 0.2, and 0.4 mg doses of the Investigational New Drug formulation of intranasal scopolamine gel (INSCOP) in 12 healthy subjects using a randomized, double-blind cross-over study design. Subjects received one squirt of 0.1 g of gel containing either 0.1 mg or 0.2 mg/0.1 mL scopolamine or placebo in each nostril. Serial blood samples and total urine voids were collected after dosing and drug concentrations were determined using a modified LC-MS-MS method. Results indicate dose-linear pharmacokinetics of scopolamine with linear increases in C-max and AUC within the dose range tested. Plasma drug concentrations were significantly lower in females than in males after administration of 0.4 dose. All three doses were well tolerated with no unexpected or serious adverse side effects reported. These results suggest that intranasal scopolamine gel formulation (INSCOP) offers a fast, reliable, and safe alternative for the treatment of motion sickness.
C1 [Wu, Lei; Chow, Diana S-L.] Univ Houston, Coll Pharm, Houston, TX 77030 USA.
[Boyd, Jason L.] Univ Space Res Assoc, Houston, TX USA.
[Daniels, Vernie; Wang, Zuwei] Wyle Labs, Houston, TX USA.
[Putcha, Lakshmi] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Putcha, L (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,MC SK3, Houston, TX 77058 USA.
EM lakshmi.putcha-1@nasa.gov
FU National Space Biomedical Research Institute
FX This work was supported by a grant from the National Space Biomedical
Research Institute. The authors acknowledge the clinical services
provided and thank the staff of MDS Pharma Services, Lincoln, NE, and
Matthew Hayat, PhD, for assistance with SAS.
NR 34
TC 1
Z9 1
U1 4
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0091-2700
EI 1552-4604
J9 J CLIN PHARMACOL
JI J. Clin. Pharmacol.
PD FEB
PY 2015
VL 55
IS 2
BP 195
EP 203
DI 10.1002/jcph.391
PG 9
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA CD7WG
UT WOS:000351305200010
PM 25187210
ER
PT J
AU Corbett, JE
Tfaily, MM
Burdige, DJ
Glaser, PH
Chanton, JP
AF Corbett, J. Elizabeth
Tfaily, Malak M.
Burdige, David J.
Glaser, Paul H.
Chanton, Jeffrey P.
TI The relative importance of methanogenesis in the decomposition of
organic matter in northern peatlands
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE peatlands; permafrost; CO2 production; CH4 loss; bog; fen
ID ANAEROBIC CARBON MINERALIZATION; LAKE AGASSIZ PEATLAND; LOST RIVER
PEATLAND; METHANE PRODUCTION; STABLE CARBON; PORE-WATER; BOG; MINNESOTA;
WETLANDS; RESPIRATION
AB Using an isotope-mass balance approach and assuming the equimolar production of CO2 and CH4 from methanogenesis (e.g., anaerobic decomposition of cellulose), we calculate that the proportion of total CO2 production from methanogenesis varies from 37 to 83% across a variety of northern peatlands. In a relative sense, methanogenesis was a more important pathway for decomposition in bogs (8013% of CO2 production) than in fens (645.7% of CO2 production), but because fens contain more labile substrates they may support higher CH4 production overall. The concentration of CO2 produced from methanogenesis (CO2-meth) can be considered equivalent to CH4 concentration before loss due to ebullition, plant-mediated transport, or diffusion. Bogs produced slightly less CO2-meth than fens (2.91.3 and 3.71.4mmol/L, respectively). Comparing the quantity of CH4 present to CO2-meth, fens lost slightly more CH4 than bogs (89 +/- 2.8% and 82 +/- 5.3%, respectively) likely due to the presence of vascular plant roots. In collapsed permafrost wetlands, bog moats produced half the amount of CO2-meth (0.8 +/- 0.2mmol/L) relative to midbogs (1.6 +/- 0.6mmol/L) and methanogenesis was less important (42 +/- 6.6% of total CO2 production relative to 55 +/- 8.1%). We hypothesize that the lower methane production potential in collapsed permafrost wetlands occurs because recently thawed organic substrates are being first exposed to the initial phases of anaerobic decomposition following collapse and flooding. Bog moats lost a comparable amount of CH4 as midbogs (63 +/- 7.0% and 64 +/- 9.3%).
C1 [Corbett, J. Elizabeth; Tfaily, Malak M.; Chanton, Jeffrey P.] Florida State Univ, Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Corbett, J. Elizabeth] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Tfaily, Malak M.] Florida State Univ, Dept Chem & Biochem, Tallahassee, FL 32306 USA.
[Tfaily, Malak M.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Burdige, David J.] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA.
[Glaser, Paul H.] Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN USA.
RP Corbett, JE (reprint author), Florida State Univ, Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
EM jecorbet@gmail.com
OI TFAILY, MALAK/0000-0002-3036-2833
FU National Science Foundation [EAR-0628349, DEB 0841158]; Oak Ridge
Associated Universities; NASA
FX This research was supported by the National Science Foundation,
EAR-0628349 and DEB 0841158. This research was supported by an
appointment to the NASA Postdoctoral Program at the Goddard Institute
for Space Studies administered by Oak Ridge Associated Universities
through a contract with NASA. The authors thank Claire Langford and
Tyler Mauney for their help with the laboratory work. Data presented in
this paper can be obtained by sending a written request to the
corresponding author.
NR 65
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Z9 8
U1 7
U2 43
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 FEB
PY 2015
VL 120
IS 2
BP 280
EP 293
DI 10.1002/2014JG002797
PG 14
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA CD9FI
UT WOS:000351402800007
ER
PT J
AU Neveu, M
Desch, SJ
Castillo-Rogez, JC
AF Neveu, Marc
Desch, Steven J.
Castillo-Rogez, Julie C.
TI Core cracking and hydrothermal circulation can profoundly affect Ceres'
geophysical evolution
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Ceres; fracturing; core; hydrothermal circulation; water-rock
interaction; thermal evolution
ID KUIPER-BELT OBJECTS; CHONDRITE PARENT BODIES; TRANS-NEPTUNIAN OBJECTS;
ADAPTIVE OPTICS IMAGES; DWARF-PLANET CERES; EQUATION-OF-STATE;
CARBONACEOUS CHONDRITE; FRACTURE-TOUGHNESS; THERMAL EVOLUTION;
POROUS-MEDIUM
AB Observations and models of Ceres suggest that its evolution was shaped by interactions between liquid water and silicate rock. Hydrothermal processes in a heated core require both fractured rock and liquid. Using a new core cracking model coupled to a thermal evolution code, we find volumes of fractured rock always large enough for significant interaction to occur. Therefore, liquid persistence is key. It is favored by antifreezes such as ammonia, by silicate dehydration which releases liquid, and by hydrothermal circulation itself, which enhances heat transport into the hydrosphere. The effect of heating from silicate hydration seems minor. Hydrothermal circulation can profoundly affect Ceres' evolution: it prevents core dehydration via temperature resets, core cooling events lasting approximate to 50 Myr during which Ceres' interior temperature profile becomes very shallow and its hydrosphere is largely liquid. Whether Ceres has experienced such extensive hydrothermalism may be determined through examination of its present-day structure. A large, fully hydrated core (radius 420 km) would suggest that extensive hydrothermal circulation prevented core dehydration. A small, dry core (radius 350 km) suggests early dehydration from short-lived radionuclides, with shallow hydrothermalism at best. Intermediate structures with a partially dehydrated core seem ambiguous, compatible both with late partial dehydration without hydrothermal circulation, and with early dehydration with extensive hydrothermal circulation. Thus, gravity measurements by the Dawn orbiter, whose arrival at Ceres is imminent, could help discriminate between scenarios for Ceres' evolution.
C1 [Neveu, Marc; Desch, Steven J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA.
[Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Neveu, M (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA.
EM mneveu@asu.edu
OI Neveu, Marc/0000-0002-6220-2869
FU NASA Astrobiology Institute at Arizona State University; NASA Outer
Planets Research and Earth and Space Science Fellowship programs
FX We thank Everett Shock for discussions on cracking phenomena that helped
improve this paper. Comments from two referees and the Associate Editor
greatly helped improve this manuscript. This study was funded by the
NASA Astrobiology Institute team at Arizona State University and by the
NASA Outer Planets Research and Earth and Space Science Fellowship
programs. Part of this work has been carried out at the Keck Institute
for Space Studies and at the Jet Propulsion Laboratory, California
Institute of Technology. The code used in this study is freely available
at https://github.com/MarcNeveu/IcyDwarf.
NR 153
TC 7
Z9 7
U1 3
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB
PY 2015
VL 120
IS 2
BP 123
EP 154
DI 10.1002/2014JE004714
PG 32
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CD8RK
UT WOS:000351363300001
ER
PT J
AU Jordan, AP
Stubbs, TJ
Wilson, JK
Schwadron, NA
Spence, HE
AF Jordan, A. P.
Stubbs, T. J.
Wilson, J. K.
Schwadron, N. A.
Spence, H. E.
TI Dielectric breakdown weathering of the Moon's polar regolith
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; space weathering; solar energetic particles; regolith; permanently
shadowed region; dielectric breakdown
ID PROTON FLUENCE MODEL; ELECTRICAL INSULATION CHARACTERISTICS; ENERGETIC
PARTICLE EVENTS; LUNAR SOIL; SOLAR; ENVIRONMENT; REGIONS; FLARES; PULSES
AB Galactic cosmic rays and solar energetic particles (SEPs) can charge the Moon's subsurface, a process expected to be particularly important in the polar regions. Experiments have shown that sufficient fluences (i.e., time-integrated fluxes) of energetic charged particles can cause dielectric breakdown, in which the electric field rapidly vaporizes small, filamentary channels within a dielectric. Lunar regolith has both the characteristics and, in some polar locations, the environment needed to make breakdown likely. We combine the Jet Propulsion Laboratory proton fluence model with temperature measurements from the Lunar Reconnaissance Orbiter's (LRO's) Diviner instrument and related temperature modeling to estimate how often breakdown occurs in the polar regions. We find that all gardened regolith within permanently shadowed regions (PSRs) has likely experienced up to 2x10(6) SEP events capable of causing breakdown, while the warmest polar regions have experienced about 2 orders of magnitude fewer events. We also use measurements from the Cosmic Ray Telescope for the Effects of Radiation on LRO to show that at least two breakdown-inducing events may have occurred since LRO arrived at the Moon in 2009. Finally, we discuss how such breakdown weathering may increase the percentage of fine and monomineralic grains within PSRs; explain the presence of so-called fairy castle regolith structures; and contribute to other low-albedo features detected by LRO's Lyman Alpha Mapping Project, possibly establishing a correlation between these features and the average temperatures within craters that are only partly in permanent shadow.
C1 [Jordan, A. P.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Jordan, A. P.; Stubbs, T. J.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
[Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Jordan, AP (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
EM a.p.jordan@unh.edu
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
FU NASA [NNG11PA03C, NNX10AB17A, NNX14AG13A]
FX This work was supported by NASA grants NNG11PA03C, NNX10AB17A, and
NNX14AG13A. The authors wish to thank Alex Boyd for helpful discussions.
The authors also thank the ACE/EPAM team and its Principal Investigator
Robert Gold of JHU/APL for the providing the ACE data via CDAWeb at
http://cdaweb.gsfc.nasa.gov/. The LRO/Diviner Level 4 Polar Resource
Products and LRO/CRaTER Level 2 data are available at the NASA Planetary
Data System at http://pds.nasa.gov. The authors also thank the two
reviewers for their helpful comments and suggestions.
NR 61
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U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB
PY 2015
VL 120
IS 2
BP 210
EP 225
DI 10.1002/2014JE004710
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CD8RK
UT WOS:000351363300005
ER
PT J
AU Bougher, SW
Pawlowski, D
Bell, JM
Nelli, S
McDunn, T
Murphy, JR
Chizek, M
Ridley, A
AF Bougher, S. W.
Pawlowski, D.
Bell, J. M.
Nelli, S.
McDunn, T.
Murphy, J. R.
Chizek, M.
Ridley, A.
TI Mars Global Ionosphere-Thermosphere Model: Solar cycle, seasonal, and
diurnal variations of the Mars upper atmosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; upper atmosphere; general circulation model; aeronomy
ID ULTRAVIOLET SPECTROMETER EXPERIMENT; NUMERICAL WEATHER PREDICTION;
GENERAL-CIRCULATION MODELS; ELECTRON-DENSITY PROFILES; MARTIAN
UPPER-ATMOSPHERE; ACCELEROMETER DATA; AEROBRAKING OPERATIONS;
INTERANNUAL VARIABILITY; SURVEYOR ACCELEROMETER; MIDDLE-ATMOSPHERE
AB A new Mars Global Ionosphere-Thermosphere Model (M-GITM) is presented that combines the terrestrial GITM framework with Mars fundamental physical parameters, ion-neutral chemistry, and key radiative processes in order to capture the basic observed features of the thermal, compositional, and dynamical structure of the Mars atmosphere from the ground to the exosphere (0-250 km). Lower, middle, and upper atmosphere processes are included, based in part upon formulations used in previous lower and upper atmosphere Mars GCMs. This enables the M-GITM code to be run for various seasonal, solar cycle, and dust conditions. M-GITM validation studies have focused upon simulations for a range of solar and seasonal conditions. Key upper atmosphere measurements are selected for comparison to corresponding M-GITM neutral temperatures and neutral-ion densities. In addition, simulated lower atmosphere temperatures are compared with observations in order to provide a first-order confirmation of a realistic lower atmosphere. M-GITM captures solar cycle and seasonal trends in the upper atmosphere that are consistent with observations, yielding significant periodic changes in the temperature structure, the species density distributions, and the large-scale global wind system. For instance, mid afternoon temperatures near approximate to 200 km are predicted to vary from approximate to 210 to 350 K (equinox) and approximate to 190 to 390 k (aphelion to perihelion) over the solar cycle. These simulations will serve as a benchmark against which to compare episodic variations (e.g., due to solar flares and dust storms) in future M-GITM studies. Additionally, M-GITM will be used to support MAVEN mission activities (2014-2016).
C1 [Bougher, S. W.; Ridley, A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Pawlowski, D.] Eastern Michigan Univ, Dept Phys, Ypsilanti, MI 48197 USA.
[Bell, J. M.] Natl Inst Aerosp, Hampton, VA USA.
[Nelli, S.] ITS, Harris, Las Cruces, NM USA.
[McDunn, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Murphy, J. R.; Chizek, M.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
RP Bougher, SW (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM bougher@umich.edu
RI Bougher, Stephen/C-1913-2013; Ridley, Aaron/F-3943-2011
OI Bougher, Stephen/0000-0002-4178-2729; Ridley, Aaron/0000-0001-6933-8534
FU National Science Foundation (NSF) [ATM-0535811]; NASA [NNX10AO17G]
FX Funding support for this work was provided in part by the National
Science Foundation (NSF) through grant ATM-0535811 to the University of
Michigan. In addition, the Mars Data Analysis Program (MDAP) also
supported a portion of this research through NASA grant NNX10AO17G.
Finally, the authors wish to acknowledge extensive use of NAS
supercomputer facilities in the production of the M-GITM simulations
presented in this paper. All Mars data sets used to validate the M-GITM
model can be accessed via the NASA PDS or the ESA PSA. All outputs
required to create the M-GITM figures and tables in this paper can be
accessed via data cubes to be supplied by the corresponding author upon
request. Contact email: bougher@umich.edu.
NR 130
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U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB
PY 2015
VL 120
IS 2
BP 311
EP 342
DI 10.1002/2014JE004715
PG 32
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CD8RK
UT WOS:000351363300010
ER
PT J
AU Nose, M
Oimatsu, S
Keika, K
Kletzing, CA
Kurth, WS
De Pascuale, S
Smith, CW
MacDowall, RJ
Nakano, S
Reeves, GD
Spence, HE
Larsen, BA
AF Nose, M.
Oimatsu, S.
Keika, K.
Kletzing, C. A.
Kurth, W. S.
De Pascuale, S.
Smith, C. W.
MacDowall, R. J.
Nakano, S.
Reeves, G. D.
Spence, H. E.
Larsen, B. A.
TI Formation of the oxygen torus in the inner magnetosphere: Van Allen
Probes observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE inner magnetosphere; oxygen torus; magnetic storm; plasmasphere; ring
current; ULF waves
ID ION COMPOSITION MEASUREMENTS; EQUATORIAL MAGNETOSPHERE; OUTER
PLASMASPHERE; PLASMAPAUSE; IONOSPHERE; MODEL; DENSITY; ENERGY; PHASE;
SHEET
AB We study the formation process of an oxygen torus during the 12-15 November 2012 magnetic storm, using the magnetic field and plasma wave data obtained by Van Allen Probes. We estimate the local plasma mass density ((L)) and the local electron number density (n(eL)) from the resonant frequencies of standing Alfven waves and the upper hybrid resonance band. The average ion mass (M) can be calculated by M approximate to (L)/n(eL) under the assumption of quasi-neutrality of plasma. During the storm recovery phase, both Probe A and Probe B observe the oxygen torus at L = 3.0-4.0 and L = 3.7-4.5, respectively, on the morning side. The oxygen torus has M = 4.5-8 amu and extends around the plasmapause that is identified at L approximate to 3.2-3.9. We find that during the initial phase, M is 4-7 amu throughout the plasma trough and remains at approximate to 1 amu in the plasmasphere, implying that ionospheric O+ ions are supplied into the inner magnetosphere already in the initial phase of the magnetic storm. Numerical calculation under a decrease of the convection electric field reveals that some of thermal O+ ions distributed throughout the plasma trough are trapped within the expanded plasmasphere, whereas some of them drift around the plasmapause on the dawnside. This creates the oxygen torus spreading near the plasmapause, which is consistent with the Van Allen Probes observations. We conclude that the oxygen torus identified in this study favors the formation scenario of supplying O+ in the inner magnetosphere during the initial phase and subsequent drift during the recovery phase.
C1 [Nose, M.] Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Kyoto, Japan.
[Oimatsu, S.] Kyoto Univ, Grad Sch Sci, Dept Geophys, Kyoto, Japan.
[Keika, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Kletzing, C. A.; Kurth, W. S.; De Pascuale, S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Smith, C. W.; Spence, H. E.] Univ New Hampshire, Inst Earth Oceans & Space, Durham, NH 03824 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Nakano, S.] Res Org Informat & Syst, Inst Stat Math, Tokyo, Japan.
[Reeves, G. D.; Larsen, B. A.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
RP Nose, M (reprint author), Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Kyoto, Japan.
EM nose@kugi.kyoto-u.ac.jp
RI Nose, Masahito/B-1900-2015; Reeves, Geoffrey/E-8101-2011;
OI Kletzing, Craig/0000-0002-4136-3348; Kurth, William/0000-0002-5471-6202;
Nose, Masahito/0000-0002-2789-3588; Reeves,
Geoffrey/0000-0002-7985-8098; Nakano, Shin'ya/0000-0003-0772-4610; De
Pascuale, Sebastian/0000-0001-7142-0246
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT)
[25287127]; 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]
FX The AL and Dst indices were provided by the World Data Center for
Geomagnetism, Kyoto, and are available at http://wdc.kugi.kyoto-u.ac.jp.
The Kp index was provided by H. J. Linthe at the Helmholtz Centre
Potsdam, GFZ German Research Centre for Geosciences and is available at
http://www.gfz-potsdam.de/kp-index. The Wp index can be downloaded from
http://s-cubed.info. The EMFISIS data are available at
http://emfisis.physics.uiowa.edu. The ECT-HOPE data are available at
http://www.rbsp-ect.lanl.gov. The electron number density at a local
probe position can be obtained on request from W. S. Kurth
(william-kurth@uiowa.edu). Geomagnetic field by the Tsyganenko 1989c
model was calculated with GEOPACK routines developed by N. A. Tsyganenko
and coded by H. Korth. We are thankful to K. Takahashi, and Y. Obana for
their helpful comments. This study was supported by the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), grant-in-aid
for Scientific Research (B) (grant 25287127). The work at Iowa was
supported 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. Part of the work by one of
coauthors (KK) has been done at the ERG-Science Center operated by
ISAS/JAXA and STEL/Nagoya University.
NR 38
TC 7
Z9 7
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB
PY 2015
VL 120
IS 2
BP 1182
EP 1196
DI 10.1002/2014JA020593
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD8QL
UT WOS:000351360800025
ER
PT J
AU Li, X
Selesnick, RS
Baker, DN
Jaynes, AN
Kanekal, SG
Schiller, Q
Blum, L
Fennell, J
Blake, JB
AF Li, X.
Selesnick, R. S.
Baker, D. N.
Jaynes, A. N.
Kanekal, S. G.
Schiller, Q.
Blum, L.
Fennell, J.
Blake, J. B.
TI Upper limit on the inner radiation belt MeV electron intensity
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE inner radiation belt; Van Allen Probes; CubeSat; MeV electron; CSSWE;
Earth's magnetosphere
ID 24 MARCH 1991; SLOT REGION; ULTRARELATIVISTIC ELECTRONS; RELATIVISTIC
ELECTRONS; DISTRIBUTIONS; SIMULATION; PROTONS; MISSION; STORM; SSC
AB No instruments in the inner radiation belt are immune from the unforgiving penetration of the highly energetic protons (tens of MeV to GeV). The inner belt proton flux level, however, is relatively stable; thus, for any given instrument, the proton contamination often leads to a certain background noise. Measurements from the Relativistic Electron and Proton Telescope integrated little experiment on board Colorado Student Space Weather Experiment CubeSat, in a low Earth orbit, clearly demonstrate that there exist sub-MeV electrons in the inner belt because their flux level is orders of magnitude higher than the background, while higher-energy electron (>1.6 MeV) measurements cannot be distinguished from the background. Detailed analysis of high-quality measurements from the Relativistic Electron and Proton Telescope on board Van Allen Probes, in a geo-transfer-like orbit, provides, for the first time, quantified upper limits on MeV electron fluxes in various energy ranges in the inner belt. These upper limits are rather different from flux levels in the AE8 and AE9 models, which were developed based on older data sources. For 1.7, 2.5, and 3.3 MeV electrons, the upper limits are about 1 order of magnitude lower than predicted model fluxes. The implication of this difference is profound in that unless there are extreme solar wind conditions, which have not happened yet since the launch of Van Allen Probes, significant enhancements of MeV electrons do not occur in the inner belt even though such enhancements are commonly seen in the outer belt.
C1 [Li, X.; Baker, D. N.; Jaynes, A. N.; Schiller, Q.; Blum, L.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Li, X.; Schiller, Q.; Blum, L.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Selesnick, R. S.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fennell, J.; Blake, J. B.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90245 USA.
RP Li, X (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM lix@lasp.colorado.edu
OI Blum, Lauren/0000-0002-4797-5476
FU NASA [NNH14AX18I]; Air Force Research Laboratory under the Heliophysics
Guest Investigators Program, at University of Colorado; RBSP-ECT through
JHU/APL under NASA [967399, NAS5-01072]; NSF [AGSW 0940277]; Air Force
Research Laboratory [FA9453-14-M-0256]
FX We thank Bob Johnston for help with the AE9 V1.2 model. This work was
supported in part by NASA agreement NNH14AX18I with the Air Force
Research Laboratory under the Heliophysics Guest Investigators Program,
at University of Colorado by RBSP-ECT funding through JHU/APL contract
967399 under prime NASA contract NAS5-01072, NSF (CubeSat program) grant
AGSW 0940277, and a subcontract (FA9453-14-M-0256) from the Air Force
Research Laboratory. Van Allen Probes REPT and ephemeris data are
available from the ECT Science Operations and Data Center,
http://www.rbsp-ect.lanl.gov; CSSWE/REPTile and ephemeris data are
available from NASA/CDAWeb database,
http://cdaweb.gsfc.nasa.gov/istp$_$public/.
NR 39
TC 24
Z9 24
U1 3
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB
PY 2015
VL 120
IS 2
BP 1215
EP 1228
DI 10.1002/2014JA020777
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD8QL
UT WOS:000351360800027
ER
PT J
AU Hartwig, J
Styborski, J
AF Hartwig, Jason
Styborski, Jeremy
TI Flow Visualization and Stream Temperature Measurement of Liquid Hydrogen
Line Chill Down Experiments
SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME
LA English
DT News Item
C1 [Hartwig, Jason] NASA, Glenn Res Ctr, Prop & Propellants, Cleveland, OH 44135 USA.
[Styborski, Jeremy] Pratt & Whitney, Hot Sect Engn, Turbine Durabil, E Hartford, CT 06118 USA.
RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, Prop & Propellants, Cleveland, OH 44135 USA.
EM Jason.W.Hartwig@nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 2
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 FEB
PY 2015
VL 137
IS 2
AR 020904
PG 2
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA CD7UH
UT WOS:000351298800005
ER
PT J
AU Liu, YQ
Peters-Lidard, CD
Kumar, SV
Arsenault, KR
Mocko, DM
AF Liu, Yuqiong
Peters-Lidard, Christa D.
Kumar, Sujay V.
Arsenault, Kristi R.
Mocko, David M.
TI Blending satellite-based snow depth products with in situ observations
for streamflow predictions in the Upper Colorado River Basin
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE passive microwave; snow estimation; streamflow prediction; MODIS;
AMSR-E; terrian aspect
ID LAND-SURFACE MODEL; CONTINENTAL UNITED-STATES; RIO-GRANDE HEADWATERS;
RAIN-ON-SNOW; WATER EQUIVALENT; COVERED AREA; TEMPORAL VARIABILITY;
SUBGRID VARIABILITY; PASSIVE MICROWAVE; DATA ASSIMILATION
AB In snowmelt-driven river systems, it is critical to enable reliable predictions of the spatiotemporal variability in seasonal snowpack to support local and regional water management. Previous studies have shown that assimilating satellite-station blended snow depth data sets can lead to improved snow predictions, which however do not always translate into improved streamflow predictions, especially in complex mountain regions. In this study, we explore how an existing optimal interpolation-based blending strategy can be enhanced to reduce biases in satellite snow depth products for improving streamflow predictions. Two major new considerations are explored, including: (1) incorporating terrain aspect and (2) incorporating areal snow coverage information. The methodology is applied to the bias reduction of the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) snow depth estimates, which are then assimilated into the Noah land surface model via the ensemble Kalman Filtering (EnKF) for streamflow predictions in the Upper Colorado River Basin. Our results indicate that using only observations from low-elevation stations such as the Global Historical Climatology Network (GHCN) in the bias correction can lead to underestimation in streamflow, while using observations from high-elevation stations (e.g., the Snow Telemetry (SNOTEL) network) along with terrain aspect is critically important for achieving reliable streamflow predictions. Additionally incorporating areal snow coverage information from the Moderate Resolution Imaging Spectroradiometer (MODIS) can slightly improve the streamflow results further.
C1 [Liu, Yuqiong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Liu, Yuqiong; Peters-Lidard, Christa D.; Kumar, Sujay V.; Arsenault, Kristi R.; Mocko, David M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Kumar, Sujay V.; Arsenault, Kristi R.; Mocko, David M.] Sci Applicat Int Corp, Greenbelt, MD USA.
[Mocko, David M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Liu, YQ (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Yuqiong.Liu@nasa.gov
RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NASA; NOAA; Air Force Weather Agency (AFWA)
FX Major funding for this study was provided by NASA as part of NASA's
contribution to the National Climate Assessment program. Additional
funding comes from NOAA and the Air Force Weather Agency (AFWA).
Computing was provided by the NASA Center for Climate Simulation. The
NLDAS-2 forcing data set is archived and distributed by the Goddard
Earth Sciences (GES) Data and Information Services Center (DISC). We
thank the USDA Natural Resources Conservation Service for access to the
SNOTEL data (http://www.wcc.nrcs.usda.gov/snow), the National Climate
Data Center for access to the GHCN data
(ftp://ftp.ncdc.noaa.gov/pub/data/ghcn/daily), and the National Snow and
Ice Data Center for access to the AMSR-E snow depth data
(http://nsidc.org/data/amsre), the MODIS snow cover data
(http://nsidc.org/data/mod10c1), and the CMC snow depth data
(http://nsidc.org/data/nsidc-0447). The U.S. Bureau of Reclamation is
thanked for providing natural streamflow data for the Upper Colorado
River Basin
(http://www.usbr.gov/lc/region/g4000/NaturalFlow/supportNF.html). The
comments from three anonymous reviewers helped to greatly improve an
earlier version of this manuscript.
NR 75
TC 6
Z9 7
U1 2
U2 23
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 FEB
PY 2015
VL 51
IS 2
BP 1182
EP 1202
DI 10.1002/2014WR016606
PG 21
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA CD9ET
UT WOS:000351401200023
ER
PT J
AU Connaughton, V
Briggs, MS
Goldstein, A
Meegan, CA
Paciesas, WS
Preece, RD
Wilson-Hodge, CA
Gibby, MH
Greiner, J
Gruber, D
Jenke, P
Kippen, RM
Pelassa, V
Xiong, S
Yu, HF
Bhat, PN
Burgess, JM
Byrne, D
Fitzpatrick, G
Foley, S
Giles, MM
Guiriec, S
Van der Horst, AJ
Von Kienlin, A
McBreen, S
McGlynn, S
Tierney, D
Zhang, BB
AF Connaughton, V.
Briggs, M. S.
Goldstein, A.
Meegan, C. A.
Paciesas, W. S.
Preece, R. D.
Wilson-Hodge, C. A.
Gibby, M. H.
Greiner, J.
Gruber, D.
Jenke, P.
Kippen, R. M.
Pelassa, V.
Xiong, S.
Yu, H. -F.
Bhat, P. N.
Burgess, J. M.
Byrne, D.
Fitzpatrick, G.
Foley, S.
Giles, M. M.
Guiriec, S.
Van der Horst, A. J.
Von Kienlin, A.
McBreen, S.
McGlynn, S.
Tierney, D.
Zhang, B. -B.
TI LOCALIZATION OF GAMMA-RAY BURSTS USING THE FERMI GAMMA-RAY BURST MONITOR
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE gamma-ray burst: general; techniques: miscellaneous
ID 1ST 2 YEARS; SPECTRAL CATALOG; GRB 090902B; LOCATIONS
AB The Fermi Gamma-ray Burst Monitor (GBM) has detected over 1400 gamma-ray bursts (GRBs) since it began science operations in 2008 July. We use a subset of over 300 GRBs localized by instruments such as Swift, the Fermi Large Area Telescope, INTEGRAL, and MAXI, or through triangulations from the InterPlanetary Network, to analyze the accuracy of GBM GRB localizations. We find that the reported statistical uncertainties on GBM localizations, which can be as small as 1 degrees, underestimate the distance of the GBM positions to the true GRB locations and we attribute this to systematic uncertainties. The distribution of systematic uncertainties is well represented (68% confidence level) by a 3.degrees 7 Gaussian with a non-Gaussian tail that contains about 10% of GBM-detected GRBs and extends to approximately 14 degrees. A more complex model suggests that there is a dependence of the systematic uncertainty on the position of the GRB in spacecraft coordinates, with GRBs in the quadrants on the Y axis better localized than those on the X axis.
C1 [Connaughton, V.; Briggs, M. S.; Meegan, C. A.; Jenke, P.; Pelassa, V.; Xiong, S.; Bhat, P. N.; Burgess, J. M.; Zhang, B. -B.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Connaughton, V.; Briggs, M. S.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Goldstein, A.; Wilson-Hodge, C. A.] NASA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Paciesas, W. S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Preece, R. D.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
[Gibby, M. H.; Giles, M. M.] Jacobs Technol Inc, Huntsville, AL USA.
[Greiner, J.; Yu, H. -F.; Von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gruber, D.] Planetarium Sudtirol, I-39053 Karneid, Italy.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Yu, H. -F.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany.
[Byrne, D.; Fitzpatrick, G.; Foley, S.; McBreen, S.; McGlynn, S.; Tierney, D.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Guiriec, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Van der Horst, A. J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands.
RP Connaughton, V (reprint author), Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35899 USA.
EM valerie@nasa.gov
RI Zhang, Binbin/C-9035-2013;
OI Zhang, Binbin/0000-0003-2002-116X; Burgess, James/0000-0003-3345-9515
FU NASA; Bundesministerium fur Bildung und Forschung (BMBF) via the
Deutsches Zentrum fur Luft und Raumfahrt (DLR) [50 QV 0301];
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR [50
OG 1101]; DFG cluster of excellence "Origin and Structure of the
Universe"; Irish Research Council for Science, Engineering, and
Technology; Marie Curie Actions under FP7; Irish Research Council;
Science Foundation Ireland [09-RFP-AST-2400]
FX We thank an anonymous referee for very useful contributions to this
paper. The GBM project is supported by NASA. Support for the German
contribution to GBM was provided by the Bundesministerium fur Bildung
und Forschung (BMBF) via the Deutsches Zentrum fur Luft und Raumfahrt
(DLR) under contract number 50 QV 0301. A.v.K. was supported by the
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR
grant 50 OG 1101. H.F.Y. acknowledges support by the DFG cluster of
excellence "Origin and Structure of the Universe." A.G. and S.G. are
funded through the NASA Post-doctoral Fellowship Program. S.F.
acknowledges the support of the Irish Research Council for Science,
Engineering, and Technology, co-funded by Marie Curie Actions under FP7.
G.F. acknowledges the support of the Irish Research Council. D.T.
acknowledges support from Science Foundation Ireland under grant number
09-RFP-AST-2400.
NR 33
TC 12
Z9 12
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2015
VL 216
IS 2
AR 32
DI 10.1088/0067-0049/216/2/32
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD2ID
UT WOS:000350899000011
ER
PT J
AU Kennedy, GM
Wyatt, MC
Bailey, V
Bryden, G
Danchi, WC
Defrere, D
Haniff, C
Hinz, PM
Lebreton, J
Mennesson, B
Millan-Gabet, R
Morales, F
Panic, O
Rieke, GH
Roberge, A
Serabyn, E
Shannon, A
Skemer, AJ
Stapelfeldt, KR
Su, KYL
Weinberger, AJ
AF Kennedy, Grant M.
Wyatt, Mark C.
Bailey, Vanessa
Bryden, Geoffrey
Danchi, William C.
Defrere, Denis
Haniff, Chris
Hinz, Philip M.
Lebreton, Jeremy
Mennesson, Bertrand
Millan-Gabet, Rafael
Morales, Farisa
Panic, Olja
Rieke, George H.
Roberge, Aki
Serabyn, Eugene
Shannon, Andrew
Skemer, Andrew J.
Stapelfeldt, Karl R.
Su, Katherine Y. L.
Weinberger, Alycia J.
TI EXO-ZODI MODELING FOR THE LARGE BINOCULAR TELESCOPE INTERFEROMETER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; instrumentation: interferometers; zodiacal dust
ID MAIN-SEQUENCE STARS; SPITZER-SPACE-TELESCOPE; PLANETARY SYSTEM; DEBRIS
DISKS; LUMINOSITY FUNCTION; HABITABLE ZONES; DUST; ALIGNMENT; MISSION;
ORIGIN
AB Habitable zone dust levels are a key unknown that must be understood to ensure the success of future space missions to image Earth analogs around nearby stars. Current detection limits are several orders of magnitude above the level of the solar system's zodiacal cloud, so characterization of the brightness distribution of exo-zodi down to much fainter levels is needed. To this end, the Large Binocular Telescope Interferometer (LBTI) will detect thermal emission from habitable zone exo-zodi a few times brighter than solar system levels. Here we present a modeling framework for interpreting LBTI observations, which yields dust levels from detections and upper limits that are then converted into predictions and upper limits for the scattered light surface brightness. We apply this model to the HOSTS survey sample of nearby stars; assuming a null depth uncertainty of 10(-4) the LBTI will be sensitive to dust a few times above the solar system level around Sun-like stars, and to even lower dust levels for more massive stars.
C1 [Kennedy, Grant M.; Wyatt, Mark C.; Panic, Olja; Shannon, Andrew] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Bailey, Vanessa; Defrere, Denis; Hinz, Philip M.; Rieke, George H.; Skemer, Andrew J.; Su, Katherine Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bryden, Geoffrey; Mennesson, Bertrand; Morales, Farisa; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Danchi, William C.; Roberge, Aki; Stapelfeldt, Karl R.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Haniff, Chris] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Lebreton, Jeremy] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Lebreton, Jeremy; Millan-Gabet, Rafael] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Kennedy, GM (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RI Roberge, Aki/D-2782-2012
OI Skemer, Andrew/0000-0001-6098-3924; Su, Kate/0000-0002-3532-5580;
Kennedy, Grant/0000-0001-6831-7547; Bailey, Vanessa/0000-0002-5407-2806;
Roberge, Aki/0000-0002-2989-3725
FU National Aeronautics and Space Administration as part of its Exoplanet
Exploration Program; European Union through ERC [279973]; NASA
FX The Large Binocular Telescope Interferometer is funded by the National
Aeronautics and Space Administration as part of its Exoplanet
Exploration Program. This work was supported by the European Union
through ERC grant No. 279973 (G.M.K., O.P., A.B.S., and M.C.W.). We
thank the reviewer for valuable comments. Part of this work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, and at the NASA Exoplanet Science Center (NExScI), under
contract with NASA.
NR 35
TC 9
Z9 9
U1 2
U2 5
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 FEB
PY 2015
VL 216
IS 2
AR 23
DI 10.1088/0067-0049/216/2/23
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD2ID
UT WOS:000350899000002
ER
PT J
AU Weinberger, AJ
Bryden, G
Kennedy, GM
Roberge, A
Defrere, D
Hinz, PM
Millan-Gabet, R
Rieke, G
Bailey, VP
Danchi, WC
Haniff, C
Mennesson, B
Serabyn, E
Skemer, AJ
Stapelfeldt, KR
Wyatt, MC
AF Weinberger, Alycia J.
Bryden, Geoff
Kennedy, Grant M.
Roberge, Aki
Defrere, Denis
Hinz, Philip M.
Millan-Gabet, Rafael
Rieke, George
Bailey, Vanessa P.
Danchi, William C.
Haniff, Chris
Mennesson, Bertrand
Serabyn, Eugene
Skemer, Andrew J.
Stapelfeldt, Karl R.
Wyatt, Mark C.
TI TARGET SELECTION FOR THE LBTI EXOZODI KEY SCIENCE PROGRAM
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; surveys; techniques: interferometric
ID MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; SUN-LIKE STARS; DEBRIS DISKS;
LUMINOSITY FUNCTION; YOUNG STARS; SEARCH; NEARBY; PLANETS; DUST
AB The Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS) on the Large Binocular Telescope Interferometer will survey nearby stars for faint emission arising from similar to 300K dust (exozodiacal dust), and aims to determine the exozodiacal dust luminosity function. HOSTS results will enable planning for future space telescopes aimed at direct spectroscopy of habitable zone terrestrial planets, as well as greater understanding of the evolution of exozodiacal disks and planetary systems. We lay out here the considerations that lead to the final HOSTS target list. Our target selection strategy maximizes the ability of the survey to constrain the exozodi luminosity function by selecting a combination of stars selected for suitability as targets of future missions and as sensitive exozodi probes. With a survey of approximately 50 stars, we show that HOSTS can enable an understanding of the statistical distribution of warm dust around various types of stars and is robust to the effects of varying levels of survey sensitivity induced by weather conditions.
C1 [Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Bryden, Geoff; Mennesson, Bertrand; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kennedy, Grant M.; Wyatt, Mark C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Roberge, Aki; Danchi, William C.; Stapelfeldt, Karl R.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Defrere, Denis; Hinz, Philip M.; Rieke, George; Bailey, Vanessa P.; Skemer, Andrew J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Millan-Gabet, Rafael] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Haniff, Chris] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
RP Weinberger, AJ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM weinberger@dtm.ciw.edu
RI Roberge, Aki/D-2782-2012;
OI Roberge, Aki/0000-0002-2989-3725; Skemer, Andrew/0000-0001-6098-3924;
Weinberger, Alycia/0000-0001-6654-7859; Kennedy,
Grant/0000-0001-6831-7547; Bailey, Vanessa/0000-0002-5407-2806; Defrere,
Denis/0000-0003-3499-2506
FU National Aeronautics and Space Administration as part of its Exoplanet
Exploration Program; European Union through ERC [279973]
FX The Large Binocular Telescope Interferometer is funded by the National
Aeronautics and Space Administration as part of its Exoplanet
Exploration Program. This work of G.M.K. and M.C.W. was supported by the
European Union through ERC grant No. 279973. This research has made use
of the SIMBAD database and the VizieR catalog access tool, CDS,
Strasbourg, France and the Washington Double Star Catalog maintained at
the U.S. Naval Observatory.
NR 51
TC 7
Z9 7
U1 2
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2015
VL 216
IS 2
AR 24
DI 10.1088/0067-0049/216/2/24
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD2ID
UT WOS:000350899000003
ER
PT J
AU Cantrell, JH
Adler, L
Yost, WT
AF Cantrell, John H.
Adler, Laszlo
Yost, William T.
TI Subharmonic generation, chaos, and subharmonic resurrection in an
acoustically driven fluid-filled cavity
SO CHAOS
LA English
DT Article
ID HELMHOLTZ-DUFFING OSCILLATOR; ULTRASONIC WAVE SYSTEM; FINITE-AMPLITUDE
WAVES; PARAMETRIC PHENOMENA; SELF-MODULATION; SPECTROSCOPY; LAYER;
DIFFRACTION; INTERFACES; HARMONICS
AB Traveling wave solutions of the nonlinear acoustic wave equation are obtained for the fundamental and second harmonic resonances of a fluid-filled cavity. The solutions lead to the development of a non-autonomous toy model for cavity oscillations. Application of the Melnikov method to the model equation predicts homoclinic bifurcation of the Smale horseshoe type leading to a cascade of period doublings with increasing drive displacement amplitude culminating in chaos. The threshold value of the drive displacement amplitude at tangency is obtained in terms of the acoustic drive frequency and fluid attenuation coefficient. The model prediction of subharmonic generation leading to chaos is validated from acousto-optic diffraction measurements in a water-filled cavity using a 5MHz acoustic drive frequency and from the measured frequency spectrum in the bifurcation cascade regime. The calculated resonant threshold amplitude of 0.2 nm for tangency is consistent with values estimated for the experimental set-up. Experimental evidence for the appearance of a stable subharmonic beyond chaos is reported. (C) 2015 AIP Publishing LLC.
C1 [Cantrell, John H.; Yost, William T.] NASA, Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA.
[Adler, Laszlo] Ohio State Univ, Adler Consultants Inc, Columbus, OH 43210 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov
FU Advanced Composites Program Vehicle Systems Safety Technologies (VSST)
Program; Fixed Wing Program; Materials Genome Project at NASA Langley
Research Center, Hampton, Virginia, USA
FX This work was supported by the Advanced Composites Program Vehicle
Systems Safety Technologies (VSST) Program, the Fixed Wing Program, and
the Materials Genome Project at NASA Langley Research Center, Hampton,
Virginia, USA.
NR 39
TC 1
Z9 1
U1 1
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1054-1500
EI 1089-7682
J9 CHAOS
JI Chaos
PD FEB
PY 2015
VL 25
IS 2
AR 023115
DI 10.1063/1.4913521
PG 9
WC Mathematics, Applied; Physics, Mathematical
SC Mathematics; Physics
GA CC7KU
UT WOS:000350547100015
PM 25725651
ER
PT J
AU Puma, MJ
Bose, S
Chon, SY
Cook, BI
AF Puma, Michael J.
Bose, Satyajit
Chon, So Young
Cook, Benjamin I.
TI Assessing the evolving fragility of the global food system
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE global food system; complex networks; trade restrictions; extremes;
famine; staple foods; grain trade
ID CLIMATE-CHANGE; AGRICULTURAL TRADE; COMMODITY PRICES; LAST MILLENNIUM;
NUCLEAR-WAR; SOUTH-ASIA; SECURITY; IMPACTS; VOLATILITY; INSULATION
AB The world food crisis in 2008 highlighted the susceptibility of the global food system to price shocks. Here we use annual staple food production and trade data from 1992-2009 to analyse the changing properties of the global food system. Over the 18 year study period, we show that the global food system is relatively homogeneous (85% of countries have low or marginal food self-sufficiency) and increases in complexity, with the number of global wheat and rice trade connections doubling and trade flows increasing by 42 and 90%, respectively. The increased connectivity and flows within these global trade networks suggest that the global food system is vulnerable to systemic disruptions, especially considering the tendency for exporting countries to switch to non-exporting states during times of food scarcity in the global markets. To test this hypothesis, we superimpose continental-scale disruptions on the wheat and rice trade networks. We find greater absolute reductions in global wheat and rice exports along with larger losses in network connectivity as the networks evolve due to disruptions in European wheat and Asian rice production. Importantly, our findings indicate that least developed countries suffer greater import losses in more connected networks through their increased dependence on imports for staple foods (due to these large-scale disturbances): mean (median) wheat losses as percentages of staple food supply are 8.9% (3.8%) for 1992-1996, increasing to 11% (5.7%) for 2005-2009. Over the same intervals, rice losses increase from 8.2% (2.2%) to 14% (5.2%). Our work indicates that policy efforts should focus on balancing the efficiency of international trade (and its associated specialization) with increased resilience of domestic production and global demand diversity.
C1 [Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
[Bose, Satyajit] Columbia Univ, Earth Inst, New York, NY USA.
[Chon, So Young] Korea Volunteer Org Int, Seoul, South Korea.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Puma, MJ (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10027 USA.
EM mjp38@columbia.edu; sgb2@columbia.edu; kvo.sychon@gmail.com;
benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012;
OI Puma, Michael/0000-0002-4255-8454
FU Climate Center of LDEO; GISS; NASA [NNX08AJ75A]
FX MJ Puma and S Bose recognise the Climate Center of LDEO and GISS for
partial support of this research. MJ Puma gratefully acknowledges
partial support from the Interdisciplinary Global Change Research under
NASA cooperative agreement NNX08AJ75A supported by the NASA Climate and
Earth Observing Program. The authors also thank S Pati for his
assistance in the early stages of this research as well as I
Rodriguez-Iturbe and C Dalin for their helpful comments and suggestions.
MJ Puma thanks L Muchnik, who created the 'Complex Networks Package for
MatLab' (Version 1.6, 2013) (http://levmuchnik.net/
Content/Networks/ComplexNetworksPackage.html), which was highly valuable
for debugging early versions of the codes used in the analyses. MJ Puma
also thanks B Ferrarini of the Asian Development Bank for his generous
assistance with Cytoscape. Lastly, four anonymous reviewers provided
valuable comments that improved the quality of this manuscript.
NR 70
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U1 7
U2 43
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 FEB
PY 2015
VL 10
IS 2
AR 024007
DI 10.1088/1748-9326/10/2/024007
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CC7UI
UT WOS:000350573500009
ER
PT J
AU Dunn, MH
Tinetti, AF
Nark, DM
AF Dunn, Mark H.
Tinetti, Ana F.
Nark, Douglas M.
TI Open rotor noise prediction using the time domain formulations of
Farassat
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
ID QUADRUPOLE NOISE; PROPELLER NOISE; ROBUST METHOD; EFFICIENT
AB During his career at the NASA Langley Research Center (LaRC), Feridoun (Feri) Farassat (1944-2011) made significant contributions to the understanding of open rotor (OR) noise generating mechanisms and to the development of OR aeroacoustic prediction technology. His time domain solutions of the Ffowcs Williams and Hawkings equation for surfaces in arbitrary motion are valid over all flight speeds ranging from subsonic through transonic to supersonic, and have led to the creation of several open rotor noise prediction programs. Two of these solutions, known as Formulation 1A and Formulation 3, are described here and have been implemented in the open rotor noise prediction codes ASSPIN (Advanced Subsonic and Supersonic Propeller Induced Noise) and ASSPIN2. Validation studies comparing noise predictions made with these codes to measured noise data are presented for a full-scale, single-rotation propfan at cruise conditions and for sub-scale, contra-rotating rotors at take-off conditions. In his later years, Farassat collaborated with the authors on the development of level 1 (non-CFD) blade aerodynamics codes for providing low-cost, time domain, blade surface pressure data for ASSPIN2 input. Use of the level 1 aerodynamics codes and their interaction with ASSPIN2 are demonstrated with noise radiation studies for a model SR7 open rotor at take-off and cruise conditions.
C1 [Nark, Douglas M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM mhd314@aol.com
FU NASA LaRC
FX Most of the research presented here was sponsored by NASA LaRC through
various programs and contracts. The authors express their gratitude for
the privilege of working with and learning from Feri. He was teacher,
mentor, colleague, and friend. The authors also thank Dr. David D. Boyd
of NASA LaRC for providing the OVERFLOW2 predictions and for his
assistance with the analysis of the CFD results. Also, the authors thank
Dr. Kenneth Brentner for organizing this special edition and providing
valuable comments and suggestions for this paper.
NR 35
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U1 3
U2 5
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 1475-472X
J9 INT J AEROACOUST
JI Int. J. Aeroacoust.
PD FEB-APR
PY 2015
VL 14
IS 1-2
BP 51
EP 86
DI 10.1260/1475-472X.14.1-2.51
PG 36
WC Acoustics; Engineering, Aerospace; Mechanics
SC Acoustics; Engineering; Mechanics
GA CD0BT
UT WOS:000350735900005
ER
PT J
AU Miller, SAE
AF Miller, Steven A. E.
TI The scaling of broadband shock-associated noise with increasing
temperature
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
ID COMPUTATIONAL FLUID-DYNAMICS; SUPERSONIC JETS; PREDICTION; TURBULENCE;
AEROACOUSTICS; MODEL
AB A physical explanation for the saturation of broadband shock-associated noise (BBSAN) intensity with increasing jet stagnation temperature has eluded investigators. An explanation is proposed for this phenomenon with the use of an acoustic analogy. To isolate the relevant physics, the scaling of BBSAN peak intensity level at the sideline observer location is examined. The equivalent source within the framework of an acoustic analogy for BBSAN is based on local field quantities at shock wave - shear layer interactions. Propagation of sound through the jet shear layer is predicted with an adjoint vector Green's function solver of the linearized Euler equations. The combination of the equivalent source and adjoint vector Green's function allows for correct predictions of the saturation of BBSAN with increasing stagnation pressure and stagnation temperature. The sources and vector Green's function have arguments involving the steady Reynolds-Averaged Navier-Stokes solution of the jet. It is proposed that saturation of BBSAN with increasing jet temperature occurs due to a balance between the amplification of the sound propagation through the shear layer and the source term scaling.
C1 NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA.
RP Miller, SAE (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA.
EM s.miller@nasa.gov
FU National Aeronautics and Space Administration Fundamental Aeronautics
Program High Speed Project
FX The author benefited greatly from discussions with Boeing/A. D. Welliver
Professor Philip J. Morris of The Pennsylvania State University. The
availability of experimental data from Professor Dennis K. McLaughlin of
The Pennsylvania State University, Dr. James Bridges of NASA Glenn
Research Center at Lewis Field, and Dr. Viswanathan of the Boeing
Company made this work possible. The author is grateful for continuous
support from The National Aeronautics and Space Administration
Fundamental Aeronautics Program High Speed Project.
NR 35
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U1 1
U2 1
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 1475-472X
J9 INT J AEROACOUST
JI Int. J. Aeroacoust.
PD FEB-APR
PY 2015
VL 14
IS 1-2
BP 305
EP 325
DI 10.1260/1475-472X.14.1-2.305
PG 21
WC Acoustics; Engineering, Aerospace; Mechanics
SC Acoustics; Engineering; Mechanics
GA CD0BT
UT WOS:000350735900015
ER
PT J
AU Hardin, JC
AF Hardin, Jay C.
TI Some elegant derivations employing generalized functions
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
AB This note presents three derivations utilizing generalized function theory. These derivations are much more straightforward than are those employing conventional techniques which illustrate the power of generalized function theory.
C1 NASA Langley Res Ctr, Bath, NC 27808 USA.
RP Hardin, JC (reprint author), NASA Langley Res Ctr, Bath, NC 27808 USA.
EM jchardin@sprintmail.com
NR 4
TC 0
Z9 0
U1 0
U2 0
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 1475-472X
J9 INT J AEROACOUST
JI Int. J. Aeroacoust.
PD FEB-APR
PY 2015
VL 14
IS 1-2
BP 353
EP 358
DI 10.1260/1475-472X.14.1-2.353
PG 6
WC Acoustics; Engineering, Aerospace; Mechanics
SC Acoustics; Engineering; Mechanics
GA CD0BT
UT WOS:000350735900017
ER
PT J
AU Asseng, S
Ewert, F
Martre, P
Rotter, RP
Lobell, DB
Cammarano, D
Kimball, BA
Ottman, MJ
Wall, GW
White, JW
Reynolds, MP
Alderman, PD
Prasad, PVV
Aggarwal, PK
Anothai, J
Basso, B
Biernath, C
Challinor, AJ
De Sanctis, G
Doltra, J
Fereres, E
Garcia-Vile, M
Gayler, S
Hoogenboom, G
Hunt, LA
Izaurralde, RC
Jabloun, M
Jones, CD
Kersebaum, KC
Koehler, AK
Muller, C
Kumar, SN
Nendel, C
O'Leary, G
Olesen, JE
Palosuo, T
Priesack, E
Rezaei, EE
Ruane, AC
Semenov, MA
Shcherbak, I
Stockle, C
Stratonovitch, P
Streck, T
Supit, I
Tao, F
Thorburn, PJ
Waha, K
Wang, E
Wallach, D
Wolf, I
Zhao, Z
Zhu, Y
AF Asseng, S.
Ewert, F.
Martre, P.
Roetter, R. P.
Lobell, D. B.
Cammarano, D.
Kimball, B. A.
Ottman, M. J.
Wall, G. W.
White, J. W.
Reynolds, M. P.
Alderman, P. D.
Prasad, P. V. V.
Aggarwal, P. K.
Anothai, J.
Basso, B.
Biernath, C.
Challinor, A. J.
De Sanctis, G.
Doltra, J.
Fereres, E.
Garcia-Vile, M.
Gayler, S.
Hoogenboom, G.
Hunt, L. A.
Izaurralde, R. C.
Jabloun, M.
Jones, C. D.
Kersebaum, K. C.
Koehler, A-K.
Mueller, C.
Kumar, S. Naresh
Nendel, C.
O'Leary, G.
Olesen, J. E.
Palosuo, T.
Priesack, E.
Rezaei, E. Eyshi
Ruane, A. C.
Semenov, M. A.
Shcherbak, I.
Stoeckle, C.
Stratonovitch, P.
Streck, T.
Supit, I.
Tao, F.
Thorburn, P. J.
Waha, K.
Wang, E.
Wallach, D.
Wolf, I.
Zhao, Z.
Zhu, Y.
TI Rising temperatures reduce global wheat production
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID CLIMATE-CHANGE; SPRING WHEAT; DRYLAND WHEAT; YIELD; GROWTH; DROUGHT;
HEAT; CO2; AGRICULTURE; ADAPTATION
AB Crop models are essential tools for assessing the threat of climate change to local and global food production(1). Present models used to predict wheat grain yield are highly uncertain when simulating how crops respond to temperature(2). Here we systematically tested 30 different wheat crop models of the Agricultural Model Intercomparison and Improvement Project against field experiments in which growing season mean temperatures ranged from 15 degrees C to 32 degrees C, including experiments with artificial heating. Many models simulated yields well, but were less accurate at higher temperatures. The model ensemble median was consistently more accurate in simulating the crop temperature response than any single model, regardless of the input information used. Extrapolating the model ensemble temperature response indicates that warming is already slowing yield gains at a majority of wheat-growing locations. Global wheat production is estimated to fall by 6% for each degrees C of further temperature increase and become more variable over space and time.
C1 [Asseng, S.; Cammarano, D.] Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA.
[Ewert, F.; Rezaei, E. Eyshi] Univ Bonn, Inst Crop Sci & Resource Conservat INRES, D-53115 Bonn, Germany.
[Martre, P.; Kimball, B. A.] INRA, UMR Genet Divers & Ecophysiol Cereales GDEC 1095, F-63100 Clermont Ferrand, France.
[Martre, P.] Univ Blaise Pascal, GDEC UMR1095, F-63170 Aubiere, France.
[Roetter, R. P.; Palosuo, T.; Tao, F.] MTT Agr Res Finland, Plant Prod Res, FI-50100 Mikkeli, Finland.
[Lobell, D. B.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA.
[Lobell, D. B.] Stanford Univ, Ctr Food Secur & Environm, Stanford, CA 94305 USA.
[Kimball, B. A.; Wall, G. W.; White, J. W.] ARS, USDA, US Arid Land Agr Res Ctr, Maricopa, AZ 85138 USA.
[Ottman, M. J.] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA.
[Reynolds, M. P.; Alderman, P. D.] CIMMYT Int Adpo, Mexico City 06600, DF, Mexico.
[Prasad, P. V. V.] Kansas State Univ, Dept Agron, Manhattan, KS 66506 USA.
[Aggarwal, P. K.] Int Water Management Inst, CGIAR Res Program Climate Change Agr & Food Secur, New Delhi 110012, India.
[Anothai, J.; Hoogenboom, G.] Washington State Univ, Biol Syst Engn, Prosser, WA 99350 USA.
[Basso, B.; Shcherbak, I.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48823 USA.
[Basso, B.; Shcherbak, I.] Michigan State Univ, WK Kellogg Biol Stn, E Lansing, MI 48823 USA.
[Biernath, C.; Priesack, E.] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Soil Ecol, D-85764 Neuherberg, Germany.
[Challinor, A. J.; Koehler, A-K.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Challinor, A. J.] CIAT, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia.
[De Sanctis, G.] INRA, AgroClim US1116, F-84914 Avignon, France.
[Doltra, J.] Cantabrian Agr Res & Training Ctr CIFA, Muriedas 39600, Spain.
[Fereres, E.; Garcia-Vile, M.] IAS CSIC, Cordoba 14080, Spain.
[Fereres, E.; Garcia-Vile, M.] Univ Cordoba, E-14080 Cordoba, Spain.
[Gayler, S.] Univ Tubingen, WESS Water & Earth Syst Sci Competence Cluster, D-72074 Tubingen, Germany.
[Hunt, L. A.] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada.
[Izaurralde, R. C.; Jones, C. D.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Izaurralde, R. C.] Texas A&M Univ, Texas A&M AgriLife Res & Extens Ctr, Temple, TX 76502 USA.
[Jabloun, M.; Olesen, J. E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark.
[Kersebaum, K. C.; Nendel, C.] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany.
[Mueller, C.; Waha, K.] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Kumar, S. Naresh] IARI PUSA, Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India.
[O'Leary, G.] Dept Environm & Primary Ind, Landscape & Water Sci, Horsham, Vic 3400, Australia.
[Ruane, A. C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Semenov, M. A.; Stratonovitch, P.] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England.
[Stoeckle, C.] Washington State Univ, Biol Syst Engn, Pullman, WA 99164 USA.
[Streck, T.] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany.
[Supit, I.; Wolf, I.] Wageningen Univ, Plant Prod Syst & Earth Syst Sci, NL-6700 AA Wageningen, Netherlands.
[Tao, F.] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China.
[Thorburn, P. J.] CSIRO Agr Flagship, Dutton Pk, Qld 4102, Australia.
[Wang, E.; Zhao, Z.] CSIRO Agr Flagship, Black Mt, ACT 2601, Australia.
[Wallach, D.] INRA, UMR Agrosyst & Dev Terr AGIR 1248, F-31326 Castanet Tolosan, France.
[Zhao, Z.] China Agr Univ, Dept Agron & Biotechnol, Beijing 100193, Peoples R China.
[Zhu, Y.] Nanjing Agr Univ, Coll Agr, Nanjing 210095, Jiangsu, Peoples R China.
RP Asseng, S (reprint author), Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA.
EM sasseng@ufl.edu
RI Palosuo, Taru/B-9593-2012; Doltra, Jordi/C-2106-2015; Thorburn,
Peter/A-6884-2011; Challinor, Andrew/C-4992-2008; Wang,
Enli/K-7478-2012; Priesack, Eckart/M-7341-2014; Martre,
Pierre/G-5399-2013; Zhao, Zhigan/E-8963-2015; Mueller,
Christoph/E-4812-2016; Olesen, Jorgen/C-2905-2016; De Sanctis,
Giacomo/F-3498-2017; Garcia-Vila, Margarita/N-6805-2015
OI Wallach, Daniel/0000-0003-3500-8179; Kersebaum, Kurt
Christian/0000-0002-3679-8427; Priesack, Eckart/0000-0002-5088-9528;
Jabloun, Mohamed/0000-0003-1199-1316; Stratonovitch,
Pierre/0000-0002-5806-2066; Reynolds, Matthew Paul/0000-0002-4291-4316;
Cammarano, Davide/0000-0003-0918-550X; Eyshi Rezaei,
Ehsan/0000-0003-2603-8034; Palosuo, Taru/0000-0003-4322-3450; Challinor,
Andrew/0000-0002-8551-6617; Wang, Enli/0000-0002-6653-5791; Martre,
Pierre/0000-0002-7419-6558; Zhao, Zhigan/0000-0003-1533-7215; Mueller,
Christoph/0000-0002-9491-3550; Olesen, Jorgen/0000-0002-6639-1273; De
Sanctis, Giacomo/0000-0002-3527-8091; Garcia-Vila,
Margarita/0000-0001-5737-4669
FU International Food Policy Research Institute (IFPRI); USDA National
Institute for Food and Agriculture [32011-68002-30191]; KULUNDA
[01LL0905L]; FACCE MACSUR project through the German FederalMinistry of
Education and Research (BMBF) [031A103B, 2812ERA115]; German Science
Foundation [EW119/5-1]; FACCEMACSUR project by the Danish Strategic
Research Council; FACCE MACSUR project through the German Federal
Ministry of Food and Agriculture (BMEL); FACCE MACSUR project funded
through the Finnish Ministry of Agriculture and Forestry; National
Natural Science Foundation of China [41071030]; Helmholtz project
'REKLIM-Regional Climate Change: Causes and Effects' Topic 9: 'Climate
Change and Air Quality'; CGIAR Research Program on Climate Change,
Agriculture, and Food Security (CCAFS); Australian Grains Research and
Development Corporation; Department of Environment and Primary
Industries Victoria, Australia; Texas AgriLife Research, Texas AM
University; CSIRO; Chinese Academy of Sciences (CAS)
FX We thank the Agricultural Model Intercomparison and Improvement Project
and its leaders C. Rosenzweig from NASA Goddard Institute for Space
Studies and Columbia University (USA), J. Jones from University of
Florida (USA), J. Hatfield from United States Department of Agriculture
(USA) and J. Antle from Oregon State University (USA) for support. We
also thank M. Lopez from CIMMYT (Turkey), M. Usman Bashir from
University of Agriculture, Faisalabad (Pakistan), S. Soufizadeh from
Shahid Beheshti University (Iran), and J. Lorgeou and J-C. Deswarte from
ARVALIS-Institut du Vegetal (France) for assistance with selecting key
locations and quantifying regional crop cultivars, anthesis and maturity
dates and R. Raymundo for assistance with GIS. S. A. and D. C. received
financial support from the International Food Policy Research Institute
(IFPRI). C. S. was funded through USDA National Institute for Food and
Agriculture award 32011-68002-30191. C. M. received financial support
from the KULUNDA project (01LL0905L) and the FACCE MACSUR project
(031A103B) funded through the German FederalMinistry of Education and
Research (BMBF). F.E. received support from the FACCE MACSUR project
(031A103B) funded through the German Federal Ministry of Education and
Research (2812ERA115) and E.E.R. was funded through the German Science
Foundation (project EW119/5-1). M. J. and J.E.O. were funded through the
FACCEMACSUR project by the Danish Strategic Research Council. K.C.K. and
C.N. were funded by the FACCE MACSUR project through the German Federal
Ministry of Food and Agriculture (BMEL). F.T., T.P. and R.P.R. received
financial support from FACCE MACSUR project funded through the Finnish
Ministry of Agriculture and Forestry (MMM); F.T. was also funded through
National Natural Science Foundation of China (No. 41071030). C.B. was
funded through the Helmholtz project 'REKLIM-Regional Climate Change:
Causes and Effects' Topic 9: 'Climate Change and Air Quality'. M.P.R.
and P.D.A. received funding from the CGIAR Research Program on Climate
Change, Agriculture, and Food Security (CCAFS). G.O'L. was funded
through the Australian Grains Research and Development Corporation and
the Department of Environment and Primary Industries Victoria,
Australia. R.C.I. was funded by Texas AgriLife Research, Texas A&M
University. E.W. and Z.Z. were funded by CSIRO and the Chinese Academy
of Sciences (CAS) through the research project 'Advancing crop yield
while reducing the use of water and nitrogen' and by the CSIRO-MoE PhD
Research Program.
NR 29
TC 104
Z9 105
U1 66
U2 256
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 FEB
PY 2015
VL 5
IS 2
BP 143
EP 147
DI 10.1038/NCLIMATE2470
PG 5
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CC4MO
UT WOS:000350327700025
ER
PT J
AU Wong, HW
Peck, J
Bonomi, RE
Assif, J
Panerai, F
Reinisch, G
Lachaud, J
Mansour, NN
AF Wong, Hsi-Wu
Peck, Jay
Bonomi, Robin E.
Assif, James
Panerai, Francesco
Reinisch, Guillaume
Lachaud, Jean
Mansour, Nagi N.
TI Quantitative determination of species production from
phenol-formaldehyde resin pyrolysis
SO POLYMER DEGRADATION AND STABILITY
LA English
DT Article
DE Phenol-formaldehyde resin; Pyrolysis; Reaction kinetics; Species
production; Gas chromatography
ID CHROMATOGRAPHY-MASS-SPECTROMETRY; THERMAL-DEGRADATION; GAS
CHROMATOGRAPHY; CARBON/PHENOLIC COMPOSITE; CARBONIZATION
AB Batch pyrolysis of a commercial resole type phenol-formaldehyde resin was performed using a step-wise heating procedure in a temperature increment of 50 K from 320 to 1290 K. A resin sample of 50 mg was loaded in a reactor assembly specifically designed and built for this study. Mass loss was measured after each 50 K step and the production of pyrolysis products was quantified using gas chromatography techniques. The overall mass loss from the samples reached 39.2% after the entire procedure. Three major product families were identified: 1) water is the most dominant product at a pyrolysis temperature below 800 K; 2) phenol derivatives (aromatic alcohols) have significant yields at a pyrolysis temperature between 500 and 850 K; 3) permanent gases such as hydrogen, methane, carbon monoxide, and carbon dioxide have the highest yields at a temperature above 800 K. Minor products observed include aromatics, which are formed between 700 and 850 K, and C-2 to C-4 light hydrocarbons, which are only formed above 800 K and peak at 1000 K. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Wong, Hsi-Wu] Univ Massachusetts Lowell, Dept Chem Engn, Lowell, MA 01854 USA.
[Peck, Jay; Bonomi, Robin E.; Assif, James] Aerodyne Res Inc, Ctr Aerothermodynam, Billerica, MA 01821 USA.
[Panerai, Francesco] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Reinisch, Guillaume] Univ Texas Austin, Ctr Predict Engn & Computat Sci, Austin, TX 78712 USA.
[Lachaud, Jean] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Moffett Field, CA 94035 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Wong, HW (reprint author), Univ Massachusetts Lowell, Dept Chem Engn, Lowell, MA 01854 USA.
EM HsiWu_Wong@uml.edu
OI Assif, James/0000-0001-8906-5334; Lachaud, Jean/0000-0001-7397-1025
FU NASA's Fundamental Aeronautic Program Hypersonics NRA grant
[NNX12AG47A]; Space Technology Research Grants Program; von Karman
Institute (VKI) for Fluid Dynamics
FX This research was originally funded by NASA's Fundamental Aeronautic
Program Hypersonics NRA grant NNX12AG47A. It is currently supported by
the Space Technology Research Grants Program under the same grant
number. The authors would like to thank B. Helber, G. Glabeke, T. Magin,
J.-B. Gouriet and O. Chazot at the von Karman Institute (VKI) for Fluid
Dynamics for their support and collaboration with the TGA measurements.
NR 26
TC 3
Z9 3
U1 4
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0141-3910
EI 1873-2321
J9 POLYM DEGRAD STABIL
JI Polym. Degrad. Stabil.
PD FEB
PY 2015
VL 112
BP 122
EP 131
DI 10.1016/j.polymdegradstab.2014.12.020
PG 10
WC Polymer Science
SC Polymer Science
GA CC1IA
UT WOS:000350093200015
ER
PT J
AU Prokop, N
Greer, L
Krasowski, M
Flatico, J
Spina, D
AF Prokop, N.
Greer, L.
Krasowski, M.
Flatico, J.
Spina, D.
TI A miniature microcontroller curve tracing circuit for space flight
testing transistors
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID TECHNOLOGY
AB This paper describes a novel miniature microcontroller based curve tracing circuit, which was designed to monitor the environmental effects on Silicon Carbide Junction Field Effect Transistor (SiC JFET) device performance, while exposed to the low earth orbit environment onboard the International Space Station (ISS) as a resident experiment on the 7th Materials on the International Space Station Experiment (MISSE7). Specifically, the microcontroller circuit was designed to operate autonomously and was flown on the external structure of the ISS for over a year. This curve tracing circuit is capable of measuring current vs. voltage (I-V) characteristics of transistors and diodes. The circuit is current limited for low current devices and is specifically designed to test high temperature, high drain-to-source resistance SiC JFETs. The results of each I-V data set are transmitted serially to an external telemetered communication interface. This paper discusses the circuit architecture, its design, and presents example results.
C1 [Prokop, N.; Greer, L.; Krasowski, M.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Flatico, J.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
[Spina, D.] NASA, Glenn Res Ctr, Jacobs Technol, Cleveland, OH 44135 USA.
RP Prokop, N (reprint author), NASA, John H Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
FU NASA Aeronautics Research Mission Directorate in the Fundamental
Aeronautics Program under the Subsonic Fixed Wing Distributed Engine
Control Project
FX This work was funded by the NASA Aeronautics Research Mission
Directorate in the Fundamental Aeronautics Program under the Subsonic
Fixed Wing Distributed Engine Control Project. The authors would like to
thank Philip Neudeck of the NASA Glenn Research Center who provided the
SiC JFETs, Liang-Yu Chen of the Ohio Aerospace Institute who packaged
the SiC JFETs, and George Baaklini of the NASA Glenn Research Center for
advice and support. The authors are also grateful to Phillip Jenkins of
the Naval Research Laboratory for providing the opportunity to fly this
circuit on MISSE7, as well as the telemetry data, and his review of this
work.
NR 13
TC 0
Z9 0
U1 2
U2 5
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 FEB
PY 2015
VL 86
IS 2
AR 024707
DI 10.1063/1.4908163
PG 8
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA CC7MT
UT WOS:000350552700054
PM 25725870
ER
PT J
AU Chao, BF
Kuang, WJ
AF Chao, Benjamin Fong
Kuang, Weijia
TI Preface to the Special Issue on "Geomagnetic Research for Taiwan:
Present and Future"
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Editorial Material
ID CHI-CHI EARTHQUAKE
C1 [Kuang, Weijia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Chao, Benjamin Fong] Acad Sinica, Inst Earth Sci, Taipei 115, Taiwan.
RP Chao, BF (reprint author), Acad Sinica, Inst Earth Sci, Taipei 115, Taiwan.
EM bfchao@earth.sinica.edu.tw; weijia.kuang@gmail.com
RI Chao, Benjamin Fong/N-6156-2013
NR 8
TC 0
Z9 0
U1 0
U2 1
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD FEB
PY 2015
VL 26
IS 1
SI SI
BP I
EP II
DI 10.3319/TAO.2014.10.29.01(GRT)
PG 2
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA CC5HN
UT WOS:000350389800001
ER
PT J
AU Le, G
Slavin, JA
Pfaff, RF
AF Le, Guan
Slavin, James A.
Pfaff, Robert F.
TI Challenges in Measuring External Currents Driven by the Solar
Wind-Magnetosphere Interaction
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article; Proceedings Paper
CT Academic Workshop on Earth Sciences
CY NOV 18-20, 2012
CL Acad Sinica, Taipei, TAIWAN
HO Acad Sinica
DE Geomagnetism; Solar wind-magnetosphere interaction; Ionospheric
currents; Magnetospheric currents
ID FIELD-ALIGNED CURRENTS; TIME RING CURRENT; MAGNETIC-FIELD;
ELECTRIC-FIELDS; GEOMAGNETIC-FIELD; TAIL CURRENT; CLUSTER; DST;
ALTITUDE; SATELLITE
AB In studying the Earth's geomagnetism it has always been a challenge to separate the external currents originating from the ionosphere and magnetosphere. While the internal magnetic field changes very slowly in time scales of years and more, the ionospheric and magnetospheric current systems driven by the solar wind-magnetosphere interaction are very dynamic. They are intimately controlled by the ionospheric electrodynamics and ionosphere-magnetosphere coupling. Single spacecraft observations are not able to separate their spatial and temporal variations, and thus to accurately describe their configurations. To characterize and understand the external currents, satellite observations require both good spatial and temporal resolutions. This paper reviews our observations of the external currents from two recent Low Earth Orbit (LEO) satellite missions: Space Technology 5 (ST-5), NASA's first three-satellite constellation mission in LEO polar orbit and Communications/Navigation Outage Forecasting System (C/NOFS), an equatorial satellite developed by the US Air Force Research Laboratory. We present recommendations for future geomagnetism missions based on these observations.
C1 [Le, Guan; Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Greenbelt, MD 20771 USA.
[Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Le, G (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Greenbelt, MD 20771 USA.
EM Guan.Le@nasa.gov
RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012
OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X
NR 46
TC 0
Z9 0
U1 0
U2 5
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
EI 2311-7680
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD FEB
PY 2015
VL 26
IS 1
SI SI
BP 11
EP 25
DI 10.3319/TAO.2014.08.19.02(GRT)
PG 15
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA CC5HN
UT WOS:000350389800003
ER
PT J
AU Tyler, R
AF Tyler, Robert
TI Electromagnetic Coupling of Ocean Flow with the Earth System
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article; Proceedings Paper
CT Academic Workshop on Earth Sciences
CY NOV 18-20, 2012
CL Acad Sinica, Taipei, TAIWAN
HO Acad Sinica
DE Electrodynamics; Induction; Ocean flow; Electromagnetic coupling
ID ANTARCTIC CIRCUMPOLAR CURRENT; MAGNETIC-FIELDS; INTERMEDIATE WATER;
STRING FUNCTION; OUTER-CORE; SEA; INDUCTION; VARIABILITY; CIRCULATION;
ROTATION
AB The ocean is electromagnetically coupled with the Earth System. This results in momentum transfer, as well as a participation by the ocean in the Earth's observable electric and magnetic fields. The coupling is typically quite weak and quantitative analyses indicate that many of these connections may be discounted when considering the transfer of momentum. But because of systematic effects there are also cases where an immediate discount is not justified and electromagnetic transfer of ocean momentum should remain within the realm of consideration. For practical considerations, even if the coupling is weak these effects are phenomenologically important because the electric and magnetic fields associated with this coupling offer an observational means for inferring the ocean flow. While in situ measurements of the electric field have long been used to measure ocean transport, new opportunities for remote sensing ocean flow through ground and space magnetic observatories are now being considered. In this article a brief update of the status of these observational methods is given. Extending beyond these established elements of the ocean's electromagnetic involvement, an attempt is made to provide a quantitative discussion of lesser considered elements of the ocean's electromagnetic coupling with the mantle and fluid core.
C1 [Tyler, Robert] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tyler, Robert] NASAs, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA.
RP Tyler, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM robert.h.tyler@nasa.gov
FU NASA Earth Surface and Interior Program (via geomagnetic infrastructure
fund)
FX This research is supported by NASA Earth Surface and Interior Program
(via geomagnetic infrastructure fund).
NR 72
TC 0
Z9 0
U1 2
U2 6
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
EI 2311-7680
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD FEB
PY 2015
VL 26
IS 1
SI SI
BP 41
EP 52
DI 10.3319/TAO.2014.08.19.04(GRT)
PG 12
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA CC5HN
UT WOS:000350389800005
ER
PT J
AU Sun, ZB
Kuang, WJ
AF Sun, Zhibin
Kuang, Weijia
TI An Ensemble Algorithm Based Component for Geomagnetic Data Assimilation
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article; Proceedings Paper
CT Academic Workshop on Earth Sciences
CY NOV 18-20, 2012
CL Acad Sinica, Taipei, TAIWAN
HO Acad Sinica
DE Geomagnetic data assimilation; Ensemble algorithm; Geodynamo
ID SECULAR VARIATION; MHD SYSTEM; FIELD; MODEL
AB Geomagnetic data assimilation is one of the most recent developments in geomagnetic studies. It combines geodynamo model outputs and surface geomagnetic observations to provide more accurate estimates of the core dynamic state and provide accurate geomagnetic secular variation forecasting. To facilitate geomagnetic data assimilation studies, we develop a stand-alone data assimilation component for the geomagnetic community This component is used to calculate the forecast error covariance matrices and the gain matrix from a given geodynamo solution, which can then be used for sequential geomagnetic data assimilation. This component is very flexible and can be executed independently. It can also be easily integrated with arbitrary dynamo models.
C1 [Sun, Zhibin] Colorado State Univ, USDA, UV B Monitoring & Res Program, Ft Collins, CO 80523 USA.
[Kuang, Weijia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Sun, ZB (reprint author), Colorado State Univ, USDA, UV B Monitoring & Res Program, Ft Collins, CO 80523 USA.
EM sunzhib1@gmail.com
RI Kuang, Weijia/K-5141-2012
OI Kuang, Weijia/0000-0001-7786-6425
FU NASA Earth Surface and Interior Program; NSF CSEDI program [EAR0757880];
NASA NAS
FX We thank Dr. Andrew Tangborn for his suggestions and comments on
assimilation algorithms, and Dr. Weiyuan Jiang for computing support.
This work is supported by NASA Earth Surface and Interior Program, and
by NSF CSEDI program under the grant EAR0757880. Part of the numerical
simulation is supported by NASA NAS.
NR 24
TC 0
Z9 0
U1 0
U2 2
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
EI 2311-7680
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD FEB
PY 2015
VL 26
IS 1
SI SI
BP 53
EP 61
DI 10.3319/TAO.2014.08.19.05(GRT)
PG 9
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA CC5HN
UT WOS:000350389800006
ER
PT J
AU Mehta, U
Bowles, J
Melton, J
Huynh, L
Hagseth, P
AF Mehta, U.
Bowles, J.
Melton, J.
Huynh, L.
Hagseth, P.
TI Water injection pre-compressor cooling assist space access
SO AERONAUTICAL JOURNAL
LA English
DT Article
AB Advances in space activity are linked to reductions in launch cost. Air-breathing propulsion-assisted flight systems offer the potential for revolutionary change of the space operations paradigm. Horizontal launch of a space-access system provides mission flexibility, responsiveness, and affordability. One way to reduce launch cost is to increase the Mach number at which a launch vehicle is staged from a carrier aircraft. Without exceeding the engine and airframe design limits, the pre-compressor cooling technology allows an operational aircraft to operate at Mach numbers and altitudes beyond its basic operational limits This is an essential, near-term technology for reducing launch cost to place small-weight payloads in low Earth orbit. The advantage of this technology is assessed with a modified McDonnell Douglas QF-4C aircraft. Payloads are unachievable or marginal with an unmodified QF-4C. However, payloads weighing around 150 pounds are plausible with this aircraft when incorporating the water injection pre-compressor cooling (WIPCC) technology.
C1 [Mehta, U.; Bowles, J.; Melton, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huynh, L.] Sci & Technol Corp, Moffett Field, CA USA.
[Hagseth, P.] Lockheed Martin Co, Ft Worth, TX USA.
RP Mehta, U (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM unmeel.b.mehta@nasa.gov
NR 42
TC 0
Z9 0
U1 3
U2 3
PU ROYAL AERONAUTICAL SOC
PI LONDON
PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND
SN 0001-9240
J9 AERONAUT J
JI Aeronaut. J.
PD FEB
PY 2015
VL 119
IS 1212
BP 145
EP 171
PG 27
WC Engineering, Aerospace
SC Engineering
GA CC8JY
UT WOS:000350615700002
ER
PT J
AU Zhang, FF
Xu, HF
Shelobolina, ES
Konishi, H
Converse, B
Shen, ZZ
Roden, EE
AF Zhang, Fangfu
Xu, Huifang
Shelobolina, Evgenya S.
Konishi, Hiromi
Converse, Brandon
Shen, Zhizhang
Roden, Eric E.
TI The catalytic effect of bound extracellular polymeric substances
excreted by anaerobic microorganisms on Ca-Mg carbonate precipitation:
Implications for the "dolomite problem"
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Disordered dolomite; dolomite problem; sulfate-reducing bacteria;
fermenting bacteria; non-metabolizing biomass; bound EPS
ID SULFATE-REDUCING BACTERIA; SEDIMENTARY DOLOMITE; CALCIUM-CARBONATE;
GEN-NOV; DISORDERED DOLOMITE; EXOPOLYMERIC SUBSTANCES; MICROBIAL
MEDIATION; FRENCH-POLYNESIA; SOUTH-AUSTRALIA; COORONG REGION
AB Because of its rare occurrence in modern sediments, as well as the difficulty in synthesizing it under low-temperature conditions in the laboratory, the origin of sedimentary dolomite has remained a long-standing enigma, often referred to as the "dolomite problem." Recently, anaerobic microorganisms, such as sulfate-reducing bacteria and methanogens, have been recognized for mediating dolomite precipitation. However, the exact role of microorganisms in dolomite crystallization is still under debate and the possible involvement of anaerobic fermenting bacteria has not been studied. In this study, we characterized the effect of purified non-metabolizing biomass and bound extracellular polymeric substances (EPS) of a natural consortium of anaerobic microorganisms dominated by fermenting bacteria and sulfate-reducing bacteria on Ca-Mg carbonate precipitation. This natural consortium was enriched from sediments of Deep Springs Lake, California, where dolomite is still precipitating. Our data show that disordered dolomite, a precursor of some sedimentary stoichiometric ordered dolomite, can be precipitated in calcite-seeded Ca-Mg carbonate solutions containing purified non-metabolizing consortium biomass. Bound EPS extracted from the consortium culture were shown to be the active component that triggered the crystallization of disordered dolomite. Further experiments show that purified non-metabolizing biomass from pure cultures of both anaerobic fermenting and sulfate-reducing bacteria closely related to those organisms present in the consortium could also catalyze the precipitation of disordered dolomite. This study contributes to the understanding of the "dolomite problem" by revealing (1) the catalytic effect of bound EPS on Ca-Mg carbonate crystallization and (2) the possible involvement of anaerobic fermenting bacteria in sedimentary dolomite formation, which has not been reported previously.
C1 [Zhang, Fangfu; Xu, Huifang; Shelobolina, Evgenya S.; Konishi, Hiromi; Converse, Brandon; Shen, Zhizhang; Roden, Eric E.] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Zhang, FF (reprint author), Rice Univ, Brine Chem Consortium, Dept Civil & Environm Engn, Houston, TX 77005 USA.
EM hfxu@geology.wisc.edu
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S.
Department of Energy [DE-SC0001929]; Graduate Summer Research Grant from
ExxonMobil Exploration Company; Department of Geoscience, University of
Wisconsin-Madison
FX This work was made possible by financial support from NASA Astrobiology
Institute (N07-5489), NSF (EAR-095800), and U.S. Department of Energy
(DE-SC0001929) to H.X.; by a Graduate Summer Research Grant from
ExxonMobil Exploration Company and Department of Geoscience, University
of Wisconsin-Madison to F.Z. and Z.S.
NR 89
TC 5
Z9 6
U1 4
U2 36
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 FEB-MAR
PY 2015
VL 100
IS 2-3
BP 483
EP 494
DI 10.2138/am-2015-4999
PG 12
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CC1JI
UT WOS:000350096600015
ER
PT J
AU Xu, HF
AF Xu, Huifang
TI Direct observation of Ca-Na ordering and structure polarity in Ca-rich
intermediate plagioclase feldspar with incommensurate modulated
structure
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Intermediate plagioclase; aberration-corrected STEM; modulated
structure; Z-contrast imaging; incommensurate modulation; ordering;
e-plagioclase; bytownite
ID CALCIC PLAGIOCLASE; CRYSTAL-STRUCTURES; SOLID-SOLUTION; LABRADORITE;
ANORTHITE; SUPERSTRUCTURE; DECOMPOSITION; DIFFRACTION; MICROSCOPY;
RESOLUTION
AB Ca-Na ordering and structural polarity of subcells in an intermediate plagioclase with modulated structure have been observed using Z-contrast imaging with an aberration-corrected scanning transmission electron microscope. Neighboring lamellar domains with I1 symmetry are related by inversion twin operation, instead of anti-phase domain boundaries (or APBs) as in all previously reported structure models. The boundaries between lamellar domains have I (1) over bar symmetry instead of C (1) over bar symmetry. Modulated plagioclase has unique Ca-Na and Al-Si ordering structure that is different from those in end-member structures of anorthite and low albite. The modulated structures of intermediate plagioclase are not metastable structures formed during phase transition, but instead thermodynamically stable structures at low temperature due to Ca-Na ordering within the subcells with I1 symmetry.
C1 [Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
[Xu, Huifang] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA.
RP Xu, HF (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, 1215 W Dayton St, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NSF [EAR-095800, EAR-0810150, DMR-0619368]; NASA Astrobiology Institute
[N07-5489]
FX I dedicate this paper to David R. Veblen on the occasion of his 67th
birthday. This work is supported by NSF (EAR-095800, EAR-0810150, and
DMR-0619368, MRI) and NASA Astrobiology Institute (N07-5489). The author
thanks Hiromi Konishi for helping with image acquisition, Alex Kivit for
optimizing the microscope, and Zhizhang Shen and Nick Levitt for
insightful discussions and suggestions. The author also thanks Michael
Carpenter and an anonymous reviewer for their comments.
NR 33
TC 2
Z9 2
U1 1
U2 13
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 FEB-MAR
PY 2015
VL 100
IS 2-3
BP 510
EP 515
DI 10.2138/am-2015-5022
PG 6
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CC1JI
UT WOS:000350096600017
ER
PT J
AU Stevenson, A
Burkhardt, J
Cockell, CS
Cray, JA
Dijksterhuis, J
Fox-Powell, M
Kee, TP
Kminek, G
McGenity, TJ
Timmis, KN
Timson, DJ
Voytek, MA
Westall, F
Yakimov, MM
Hallsworth, JE
AF Stevenson, Andrew
Burkhardt, Juergen
Cockell, Charles S.
Cray, Jonathan A.
Dijksterhuis, Jan
Fox-Powell, Mark
Kee, Terence P.
Kminek, Gerhard
McGenity, Terry J.
Timmis, Kenneth N.
Timson, David J.
Voytek, Mary A.
Westall, Frances
Yakimov, Michail M.
Hallsworth, John E.
TI Multiplication of microbes below 0.690 water activity: implications for
terrestrial and extraterrestrial life
SO ENVIRONMENTAL MICROBIOLOGY
LA English
DT Review
ID DON-JUAN POND; BARBERTON GREENSTONE-BELT; SALTERN CRYSTALLIZER PONDS;
BIOLOGICAL ICE NUCLEATORS; PHASE ESCHERICHIA-COLI; UPPER MARTIAN
SURFACE; SOUTH-AFRICA; DEAD-SEA; EXTREME ENVIRONMENTS;
METABOLIC-ACTIVITY
AB Since a key requirement of known life forms is available water (water activity; a(w)), recent searches for signatures of past life in terrestrial and extraterrestrial environments have targeted places known to have contained significant quantities of biologically available water. However, early life on Earth inhabited high-salt environments, suggesting an ability to withstand low water-activity. The lower limit of water activity that enables cell division appears to be approximate to 0.605 which, until now, was only known to be exhibited by a single eukaryote, the sugar-tolerant, fungal xerophile Xeromyces bisporus. The first forms of life on Earth were, though, prokaryotic. Recent evidence now indicates that some halophilic Archaea and Bacteria have water-activity limits more or less equal to those of X.bisporus. We discuss water activity in relation to the limits of Earth's present-day biosphere; the possibility of microbial multiplication by utilizing water from thin, aqueous films or non-liquid sources; whether prokaryotes were the first organisms able to multiply close to the 0.605-a(w) limit; and whether extraterrestrial aqueous milieux of 0.605a(w) can resemble fertile microbial habitats found on Earth.
C1 [Stevenson, Andrew; Cray, Jonathan A.; Timson, David J.; Hallsworth, John E.] Queens Univ Belfast, Inst Global Food Secur, Sch Biol Sci, MBC, Belfast BT9 7BL, Antrim, North Ireland.
[Burkhardt, Juergen] Univ Bonn, Plant Nutr Grp, Inst Crop Sci & Resource Conservat, D-53115 Bonn, Germany.
[Cockell, Charles S.; Fox-Powell, Mark] Univ Edinburgh, UK Ctr Astrobiol, Sch Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland.
[Dijksterhuis, Jan] CBS Fungal Biodivers Ctr, NL-CT3584 Utrecht, Netherlands.
[Kee, Terence P.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Kminek, Gerhard] ESA ESTEC, NL-2200 Noordwijk, Netherlands.
[McGenity, Terry J.] Univ Essex, Sch Biol Sci, Colchester CO4 3SQ, Essex, England.
[Timmis, Kenneth N.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Microbiol, D-38106 Braunschweig, Germany.
[Voytek, Mary A.] NASA Headquaters, Washington, DC 20546 USA.
[Westall, Frances] CNRS, Ctr Biophys Mol, Ctr Rech Mat Haute Temperature, F-45071 Orleans 2, France.
[Yakimov, Michail M.] CNR, Ist Ambiente Marino Costiero, I-98122 Messina, Italy.
RP Hallsworth, JE (reprint author), Queens Univ Belfast, Inst Global Food Secur, Sch Biol Sci, MBC, Belfast BT9 7BL, Antrim, North Ireland.
EM j.hallsworth@qub.ac.uk
RI Hallsworth, John/K-7876-2013; Burkhardt, Juergen/B-6310-2012;
OI Burkhardt, Juergen/0000-0001-6539-1143; Yakimov,
Michail/0000-0003-1418-363X; McGenity, Terence/0000-0002-1497-8822;
Timson, David/0000-0002-0985-8818
FU Department of Agriculture and Rural Development (Northern Ireland);
Research and Enterprise Directorate of Queen's University Belfast
FX We are grateful to Dave W. Beaty (Jet Propulsion Laboratory, California
Institute of Technology, USA), Kathleen C. Benison (West Virginia
University, USA), Ben Clark (Space Science Institute, USA), Don A. Cowan
(University of Pretoria, South Africa), Roy M. Daniel (University of
Waikato, New Zealand), Michael J. Danson (University of Bath, UK), Peter
N. Golyshin (Bangor University, Wales), Jesse P. Harrison (UK Centre for
Astrobiology, The University of Edinburgh, UK), Ailsa D. Hocking (CSIRO
Division of Food and Nutritional Sciences, Australia), Barbara J. Javor
(Southwest Fisheries Science Center, USA), Tom L. Kieft (New Mexico
Tech., USA), Chris R. Omelon (University of Texas at Austin, USA),
Aharon Oren (The Hebrew University of Jerusalem, Israel), R. John Parkes
(Cardiff University, Wales), John D. Rummel (East Carolina University,
USA) and Andrew Steele (Carnegie Institution of Washington, USA) for
fruitful discussions. Invaluable technical and logistical assistance was
provided by Kalpa J. Hallsworth and Sarah D. Pandey (Bangor, UK) and
Knut Wichterich (University of Bonn, Germany). Funding was received from
the Department of Agriculture and Rural Development (Northern Ireland)
and the Research and Enterprise Directorate of Queen's University
Belfast.
NR 226
TC 34
Z9 34
U1 12
U2 76
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1462-2912
EI 1462-2920
J9 ENVIRON MICROBIOL
JI Environ. Microbiol.
PD FEB
PY 2015
VL 17
IS 2
BP 257
EP 277
DI 10.1111/1462-2920.12598
PG 21
WC Microbiology
SC Microbiology
GA CC7KM
UT WOS:000350546200002
PM 25142751
ER
PT J
AU Okojie, RS
Lukco, D
Nguyen, V
Savrun, E
AF Okojie, Robert S.
Lukco, Dorothy
Vu Nguyen
Savrun, Ender
TI 4H-SiC Piezoresistive Pressure Sensors at 800 degrees C With Observed
Sensitivity Recovery
SO IEEE ELECTRON DEVICE LETTERS
LA English
DT Article
DE 4H-SiC; piezoresistor; high temperature; pressure sensor
AB Uncooled MEMS-based 4H-SiC Wheatstone bridge configured piezoresistive pressure sensors were demonstrated from 23 degrees C to 800 degrees C. The full-scale output (FSO) voltage exhibited gradual decrease with increasing temperature from 23 degrees C to 400 degrees C, then swung upward as temperature increased further to where the values measured at 800 degrees C were nearly equal to or higher than the room temperature values. This newly observed FSO behavior in 4H-SiC contrasts sharply with the FSO behavior of silicon piezoresistive sensors that decrease continuously with increasing temperature. The increase in the sensor output sensitivity at 800 degrees C implies higher signal to noise ratio and improved fidelity, thereby offering promise of further insertion into >600 degrees C environments without the need for cooling and complex signal conditioning.
C1 [Okojie, Robert S.] NASA, Cleveland, OH 44135 USA.
[Lukco, Dorothy] Vantage Partners LLC, Brookpark, OH 44142 USA.
[Vu Nguyen; Savrun, Ender] Sienna Technol Inc, Woodinville, WA 98072 USA.
RP Okojie, RS (reprint author), NASA, Cleveland, OH 44135 USA.
EM robert.s.okojie@nasa.gov
FU National Aeronautics and Space Administration through the
Transformational Tools and Technologies Project within the Fundamental
Aeronautics Program
FX This work was supported by the National Aeronautics and Space
Administration through the Transformational Tools and Technologies
Project within the Fundamental Aeronautics Program. The review of this
letter was arranged by Editor A. Flewitt.
NR 11
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0741-3106
EI 1558-0563
J9 IEEE ELECTR DEVICE L
JI IEEE Electron Device Lett.
PD FEB
PY 2015
VL 36
IS 2
BP 174
EP 176
DI 10.1109/LED.2014.2379262
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA CC4PA
UT WOS:000350334100030
ER
PT J
AU Evans, NR
Szabo, R
Derekas, A
Szabados, L
Cameron, C
Matthews, JM
Sasselov, D
Kuschnig, R
Rowe, JF
Guenther, DB
Moffat, AFJ
Rucinski, SM
Weiss, WW
AF Evans, N. R.
Szabo, R.
Derekas, A.
Szabados, L.
Cameron, C.
Matthews, J. M.
Sasselov, D.
Kuschnig, R.
Rowe, J. F.
Guenther, D. B.
Moffat, A. F. J.
Rucinski, S. M.
Weiss, W. W.
TI Observations of Cepheids with the MOST satellite: contrast between
pulsation modes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; stars: individual: RT Aur; stars: individual:
SZ Tau; stars: variables: Cepheids
ID LOW-AMPLITUDE CEPHEIDS; RR LYRAE STARS; CLASSICAL CEPHEIDS;
RADIAL-VELOCITIES; PHOTOMETRIC DATA; VARIABLE-STARS; PERIOD CHANGES;
RT-AURIGAE; POLARIS; SPACE
AB The quantity and quality of satellite photometric data strings is revealing details in Cepheid variation at very low levels. Specifically, we observed a Cepheid pulsating in the fundamental mode and one pulsating in the first overtone with the Canadian MOST (Microvariability and Oscillations of Stars) satellite. The 3.7-d period fundamental mode pulsator (RT Aur) has a light curve that repeats precisely, and can be modelled by a Fourier series very accurately. The overtone pulsator (SZ Tau, 3.1 d period) on the other hand shows light-curve variation from cycle to cycle which we characterize by the variations in the Fourier parameters. We present arguments that we are seeing instability in the pulsation cycle of the overtone pulsator, and that this is also a characteristic of the O - C curves of overtone pulsators. On the other hand, deviations from cycle to cycle as a function of pulsation phase follow a similar pattern in both stars, increasing after minimum radius. In summary, pulsation in the overtone pulsator is less stable than that of the fundamental mode pulsator at both long and short time-scales.
C1 [Evans, N. R.; Sasselov, D.] Harvard Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Szabo, R.; Derekas, A.; Szabados, L.] Konkoly Observ Budapest, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary.
[Derekas, A.] ELTE Gothard Astrophys Observ, H-9074 Szombathely, Hungary.
[Cameron, C.] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada.
[Matthews, J. M.; Kuschnig, R.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Evans, NR (reprint author), Harvard Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA.
EM nevans@cfa.harvard.edu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Szabo, Robert/0000-0002-3258-1909
FU 'Lendulet-Young Researchers' Program of the Hungarian Academy of
Sciences; Hungarian OTKA [K83790]; European Community [269194, 312844];
ESA PECS [4000110889/14/NL/NDe]; Janos Bolyai Research Scholarship of
the Hungarian Academy of Sciences; ES-TEC [4000106398/12/NL/KML];
Chandra X-ray Center NASA [NAS8-03060]; NSERC (Canada); AFJM; Austrian
Science Fonds [FWF P22691-N16]
FX We are happy to thank Joseph E. Postma for his unpublished photometric
data. We also thank Zoltan Kollath for enlightening discussions.
Comments from an anonymous referee have improved the text, particularly
in Section 4. This project has been supported by the 'Lendulet-2009
Young Researchers' Program of the Hungarian Academy of Sciences, and the
Hungarian OTKA grant K83790. The research leading to these results has
received funding from the European Community's Seventh Framework
Programme (FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK)
and no. 312844 (SPACEINN). Funding has also been received from the ESA
PECS Contract No. 4000110889/14/NL/NDe. RS and AD were supported by the
Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences.
RS thanks the hospitality of CfA during a visit. Financial support for
LS was provided from the ES-TEC Contract No. 4000106398/12/NL/KML.
Support for this work was also provided from the Chandra X-ray Center
NASA Contract NAS8-03060 (for NRE). JMM, DBG, AFJM and SMR are grateful
for financial aid from NSERC (Canada) and AFJM also to FRQNT (Quebec).
WWW was supported by the Austrian Science Fonds (FWF P22691-N16) This
research has made use of the SIMBAD data base, operated at CDS,
Strasbourg, France.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2015
VL 446
IS 4
BP 4008
EP 4018
DI 10.1093/mnras/stu2371
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TH
UT WOS:000350272400059
ER
PT J
AU Bates, SD
Thornton, D
Bailes, M
Barr, E
Bassa, CG
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Champion, DJ
Flynn, CML
Jameson, A
Johnston, S
Keith, MJ
Kramer, M
Levin, L
Lyne, A
Milia, S
Ng, C
Petroff, E
Possenti, A
Stappers, BW
van Straten, W
Tiburzi, C
AF Bates, S. D.
Thornton, D.
Bailes, M.
Barr, E.
Bassa, C. G.
Bhat, N. D. R.
Burgay, M.
Burke-Spolaor, S.
Champion, D. J.
Flynn, C. M. L.
Jameson, A.
Johnston, S.
Keith, M. J.
Kramer, M.
Levin, L.
Lyne, A.
Milia, S.
Ng, C.
Petroff, E.
Possenti, A.
Stappers, B. W.
van Straten, W.
Tiburzi, C.
TI The High Time Resolution Universe survey - XI. Discovery of five
recycled pulsars and the optical detectability of survey white dwarf
companions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; stars: neutron; pulsars: general
ID BINARY MILLISECOND PULSAR; DOUBLE NEUTRON-STARS; X-RAY BINARIES; RADIO
PULSARS; PSR J1012+5307; GENERAL-RELATIVITY; COOLING AGE; SYSTEM;
TELESCOPE; EVOLUTION
AB We present the discovery of a further five recycled pulsar systems in the mid-Galactic latitude portion of the High Time Resolution Universe survey. The pulsars have rotational periods ranging from 2 to 66 ms, and four are in binary systems with orbital periods between 10.8 h and 9 d. Three of these binary systems are particularly interesting; PSR J1227-6208 has a pulse period of 34.5 ms and the highest mass function of all pulsars with near-circular orbits. The circular orbit suggests that the companion is not another neutron star, so future timing experiments may reveal one of the heaviest white dwarfs ever found (>1.3 M-circle dot). Timing observations of PSR J1431-4715 indicate that it is eclipsed by its companion which has a mass indicating it belongs to the redback class of eclipsing millisecond pulsars. PSR J1653-2054 has a companion with a minimum mass of only 0.08M(circle dot), placing it among the class of pulsars with low-mass companions. Unlike the majority of such systems, however, no evidence of eclipses is seen at 1.4 GHz.
C1 [Bates, S. D.; Thornton, D.; Keith, M. J.; Kramer, M.; Lyne, A.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Bates, S. D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Thornton, D.; Johnston, S.; Petroff, E.; Tiburzi, C.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Bailes, M.; Bhat, N. D. R.; Flynn, C. M. L.; Jameson, A.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Bailes, M.; Barr, E.; Bhat, N. D. R.; Flynn, C. M. L.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astron CAASTRO, Hawthorn, Vic 3122, Australia.
[Barr, E.; Champion, D. J.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bassa, C. G.] ASTRON, NL-7900 AA Dwingeloo, Netherlands.
[Bhat, N. D. R.] Curtin Univ, Iternat Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Burgay, M.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, Italy.
[Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91106 USA.
[Burke-Spolaor, S.] CALTECH, Pasadena, CA 91125 USA.
[Levin, L.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Milia, S.; Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
RP Bates, SD (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
EM sam.d.bates@gmail.com
OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344
FU Commonwealth of Australia
FX The Parkes Observatory is part of the Australia Telescope which is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. We thank the reviewer, Dipankar Bhattacharya,
for suggestions which helped improve the manuscript.
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JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2015
VL 446
IS 4
BP 4019
EP 4028
DI 10.1093/mnras/stu2350
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TH
UT WOS:000350272400060
ER
PT J
AU van der Horst, AJ
Levan, AJ
Pooley, GG
Wiersema, K
Kruhler, T
Perley, DA
Starling, RLC
Curran, PA
Tanvir, NR
Wijers, RAMJ
Strom, RG
Kouveliotou, C
Hartoog, OE
Xu, D
Fynbo, JPU
Jakobsson, P
AF van der Horst, A. J.
Levan, A. J.
Pooley, G. G.
Wiersema, K.
Kruhler, T.
Perley, D. A.
Starling, R. L. C.
Curran, P. A.
Tanvir, N. R.
Wijers, R. A. M. J.
Strom, R. G.
Kouveliotou, C.
Hartoog, O. E.
Xu, D.
Fynbo, J. P. U.
Jakobsson, P.
TI Detailed afterglow modelling and host galaxy properties of the dark GRB
111215A
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: individual: GRB 111215A
ID GAMMA-RAY-BURST; CORE-COLLAPSE SUPERNOVAE; SPITZER-SPACE-TELESCOPE;
OPTICAL AFTERGLOW; EXTINCTION CURVES; STAR-FORMATION; MILKY-WAY; DUST;
POPULATION; RESOLUTION
AB Gamma-ray burst (GRB) 111215A was bright at X-ray and radio frequencies, but not detected in the optical or near-infrared (nIR) down to deep limits. We have observed the GRB afterglow with the Westerbork Synthesis Radio Telescope and Arcminute Microkelvin Imager at radio frequencies, with the William Herschel Telescope and Nordic Optical Telescope in the nIR/optical, and with the Chandra X-ray Observatory. We have combined our data with the Swift X-Ray Telescope monitoring, and radio and millimetre observations from the literature to perform broad-band modelling, and determined the macro-and microphysical parameters of the GRB blast wave. By combining the broad-band modelling results with our nIR upper limits we have put constraints on the extinction in the host galaxy. This is consistent with the optical extinction we have derived from the excess X-ray absorption, and higher than in other dark bursts for which similar modelling work has been performed. We also present deep imaging of the host galaxy with the Keck I telescope, Spitzer Space Telescope, and Hubble Space Telescope (HST), which resulted in a well-constrained photometric redshift, giving credence to the tentative spectroscopic redshift we obtained with the Keck II telescope, and estimates for the stellar mass and star formation rate of the host. Finally, our high-resolution HST images of the host galaxy show that the GRB afterglow position is offset from the brightest regions of the host galaxy, in contrast to studies of optically bright GRBs.
C1 [van der Horst, A. J.; Wijers, R. A. M. J.; Hartoog, O. E.] Univ Amsterdam, Anton Pannekoek Inst, NL-1098 XH Amsterdam, Netherlands.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Pooley, G. G.] Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England.
[Wiersema, K.; Starling, R. L. C.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Kruhler, T.; Xu, D.; Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Kruhler, T.] European So Observ, Santiago 19, Chile.
[Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Curran, P. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Strom, R. G.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA.
[Xu, D.] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
RP van der Horst, AJ (reprint author), Univ Amsterdam, Anton Pannekoek Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
EM a.j.vanderhorst@uva.nl
RI Jakobsson, Pall/L-9950-2015;
OI Jakobsson, Pall/0000-0002-9404-5650; Wijers, Ralph/0000-0002-3101-1808
FU European Research Council [247295]; Science and Technology Facilities
Council (STFC); NASA through Hubble Fellowship [HSTHF-51296.01-A]; Space
Telescope Science Institute; NASA [NAS 5-26555]; Royal Society;
Australian Research Council [DP120102393]; Netherlands Foundation for
Scientific Research; University of Cambridge; STFC; W. M. Keck
Foundation
FX We would like to thank Alexander Kann for useful discussions, and Alex
Filippenko, Shri Kulkarni, Josh Bloom, Brad Cenko, and Jeff Silverman
for enabling or performing the Keck telescope observations presented in
this paper. AJvdH and RAMJW acknowledge support from the European
Research Council via Advanced Investigator Grant no. 247295. KW
acknowledges support from the Science and Technology Facilities Council
(STFC). Support for DAP was provided by NASA through Hubble Fellowship
grant HSTHF-51296.01-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555. RLCS is supported
by a Royal Society Fellowship. PAC acknowledges support from Australian
Research Council grant DP120102393. The Westerbork Synthesis Radio
Telescope is operated by Netherlands Institute for Radio Astronomy
(ASTRON) with support from the Netherlands Foundation for Scientific
Research. The Arcminute Microkelvin Imager arrays are supported by the
University of Cambridge and the STFC. The William Herschel Telescope and
Nordic Optical Telescope are operated on the island of La Palma by the
Isaac Newton Group and Nordic Optical Telescope Scientific Association,
respectively, in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias. Some of the data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California, and the National Aeronautics and Space
Administration (NASA); the Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. This work is based in
part on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA; Spitzer observations were
undertaken as part of large program 90062. Some observations were made
with the NASA/ESA Hubble Space Telescope, obtained at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555; HST observations were undertaken as part of program 12378. The
scientific results reported in this paper are based in part on
observations made by the Chandra X-ray Observatory, under ObsID 14052.
This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester.
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SC Astronomy & Astrophysics
GA CC3TH
UT WOS:000350272400067
ER
PT J
AU Mao, MY
Owen, F
Duffin, R
Keel, B
Lacy, M
Momjian, E
Morrison, G
Mroczkowski, T
Neff, S
Norris, RP
Schmitt, H
Toy, V
Veilleux, S
AF Mao, Minnie Y.
Owen, Frazer
Duffin, Ryan
Keel, Bill
Lacy, Mark
Momjian, Emmanuel
Morrison, Glenn
Mroczkowski, Tony
Neff, Susan
Norris, Ray P.
Schmitt, Henrique
Toy, Vicki
Veilleux, Sylvain
TI J1649+2635: a grand-design spiral with a large double-lobed radio source
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: general; galaxies: jets; galaxies: spiral;
radio continuum: galaxies
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; SUPERMASSIVE
BLACK-HOLES; DIGITAL-SKY-SURVEY; ELLIPTIC GALAXIES; STAR-FORMATION;
X-RAY; SEYFERT-GALAXIES; DYNAMICAL PROPERTIES; LUMINOSITY FUNCTIONS
AB We report the discovery of a grand-design spiral galaxy associated with a double-lobed radio source. J1649+2635 (z = 0.0545) is a red spiral galaxy with a prominent bulge that it is associated with a L-1.4GHz similar to 10(24) W Hz(-1) double-lobed radio source that spans almost 100 kpc. J1649+2635 has a black hole mass of M-BH similar to 3-7 x 10(8) M-circle dot and SFR similar to 0.26-2.6 M-circle dot yr(-1). The galaxy hosts an similar to 96 kpc diffuse optical halo, which is unprecedented for spiral galaxies. We find that J1649+2635 resides in an overdense environment with a mass of M-dyn = 7.7(-4.3)(+7.9) x 10(13) M-circle dot, likely a galaxy group below the detection threshold of the ROSAT All-Sky Survey. We suggest one possible scenario for the association of double-lobed radio emission from J1649+2635 is that the source may be similar to a Seyfert galaxy, located in a denser-than-normal environment. The study of spiral galaxies that host large-scale radio emission is important because although rare in the local Universe, these sources may be more common at high redshifts.
C1 [Mao, Minnie Y.; Owen, Frazer; Duffin, Ryan; Momjian, Emmanuel] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Duffin, Ryan] Univ Virginia, Charlottesville, VA 22904 USA.
[Keel, Bill] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Lacy, Mark] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Morrison, Glenn] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA.
[Morrison, Glenn] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Mroczkowski, Tony; Schmitt, Henrique] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Neff, Susan] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA.
[Norris, Ray P.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Toy, Vicki; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
RP Mao, MY (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
EM mmao@nrao.edu
RI Norris, Ray/A-1316-2008;
OI Norris, Ray/0000-0002-4597-1906; Mroczkowski, Tony/0000-0003-3816-5372
FU NSF [AST-1005313]; National Research Council Research Associateship
Award at the Naval Research Laboratory
FX The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. RD was a summer student at the National Radio
Astronomy Observatory. The portion of this research for which TM is
responsible was performed while he held a National Research Council
Research Associateship Award at the Naval Research Laboratory. These
results made use of the DCT at Lowell Observatory. Lowell is a private,
non-profit institution dedicated to astrophysical research and public
appreciation of astronomy and operates the DCT in partnership with
Boston University, the University of Maryland, the University of Toledo
and Northern Arizona University. The NSF funded the construction of the
LMI under grant AST-1005313.
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PD FEB
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IS 4
BP 4176
EP 4185
DI 10.1093/mnras/stu2302
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TH
UT WOS:000350272400073
ER
PT J
AU Amador, ES
Cable, ML
Chaudry, N
Cullen, T
Gentry, D
Jacobsen, MB
Murukesan, G
Schwieterman, EW
Stevens, AH
Stockton, A
Yin, C
Cullen, DC
Geppert, W
AF Amador, Elena S.
Cable, Morgan L.
Chaudry, Nosheen
Cullen, Thomas
Gentry, Diana
Jacobsen, Malene B.
Murukesan, Gayathri
Schwieterman, Edward W.
Stevens, Adam H.
Stockton, Amanda
Yin, Chang
Cullen, David C.
Geppert, Wolf
TI Synchronous in-field application of life-detection techniques in
planetary analog missions
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Astrobiology; Life detection; Mars; Analog; Mission simulation
ID TERRESTRIAL ANALOGS; MARS; ICELAND; ENVIRONMENTS; HABITABILITY;
ERUPTION; VOLCANO; GLASS; ICE
AB Field expeditions that simulate the operations of robotic planetary exploration missions at analog sites on Earth can help establish best practices and are therefore a positive contribution to the planetary exploration community. There are many sites in Iceland that possess heritage as planetary exploration analog locations and whose environmental extremes make them suitable for simulating scientific sampling and robotic operations.
We conducted a planetary exploration analog mission at two recent lava fields in Iceland, Fimmvorouhals (2010) and Eldfell (1973), using a specially developed field laboratory. We tested the utility of in-field site sampling down selection and tiered analysis operational capabilities with three life detection and characterization techniques: fluorescence microscopy (FM), adenine-triphosphate (ATP) bioluminescence assay, and quantitative polymerase chain reaction (qPCR) assay. The study made use of multiple cycles of sample collection at multiple distance scales and field laboratory analysis using the synchronous fife-detection techniques to heuristically develop the continuing sampling and analysis strategy during the expedition.
Here we report the operational lessons learned and provide brief summaries of scientific data. The full scientific data report will follow separately. We found that rapid in-field analysis to determine subsequent sampling decisions is operationally feasible, and that the chosen life detection and characterization techniques are suitable for a terrestrial life-detection field mission.
In-field analysis enables the rapid obtainment of scientific data and thus facilitates the collection of the most scientifically relevant samples within a single field expedition, without the need for sample relocation to external laboratories. The operational lessons learned in this study could be applied to future terrestrial field expeditions employing other analytical techniques and to future robotic planetary exploration missions. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Amador, Elena S.; Schwieterman, Edward W.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Cable, Morgan L.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chaudry, Nosheen; Cullen, Thomas; Cullen, David C.] Cranfield Univ, Sch Engn, Cranfield MK43 0AL, Beds, England.
[Gentry, Diana] Stanford Univ, Stanford, CA 94305 USA.
[Stockton, Amanda] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[Murukesan, Gayathri] Univ Turku, Dept Biochem Biochem, Turun 20014, Finland.
[Stevens, Adam H.] Open Univ, Dept Phys Sci, Milton Keynes MK15 0BT, Bucks, England.
[Yin, Chang; Geppert, Wolf] Royal Inst Technol, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden.
[Yin, Chang; Geppert, Wolf] Stockholm Univ, Astrobiol Ctr, SE-10691 Stockholm, Sweden.
RP Stevens, AH (reprint author), Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK15 0BT, Bucks, England.
EM adam.stevens@open.ac.uk
OI Stevens, Adam/0000-0001-8335-4143; Schwieterman,
Edward/0000-0002-2949-2163
NR 24
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U2 12
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 FEB
PY 2015
VL 106
BP 1
EP 10
DI 10.1016/j.pss.2014.11.006
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC7AD
UT WOS:000350519200001
ER
PT J
AU Giri, C
Goesmann, F
Steele, A
Gautier, T
Steininger, H
Kruger, H
Meierhenrich, UJ
AF Giri, Chaitanya
Goesmann, Fred
Steele, Andrew
Gautier, Thomas
Steininger, Harald
Krueger, Harald
Meierhenrich, Uwe J.
TI Competence evaluation of COSAC flight spare model mass spectrometer: In
preparation of arrival of Philae lander on comet
67P/Churyumov-Gerasimenko
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Churyumov-Gerasimenko; Rosetta; Philae; COSAC; Comets; Mass spectrometry
ID MISSION ROSETTA; HALLEY; GAS; CHIRALITY
AB The Cometary Sampling and Composition (COSAC) experiment onboard the Philae lander is a combined Gas Chromatograph-Mass Spectrometer targeted to determine the organic composition of the nucleus of comet 67P/Churyumov-Gerasimenko. The COSAC flight-model mass spectrometer (FM-MS) was scheduled to sample volatile organic species from 67P's coma prior to Philae's detachment from the Rosetta orbiter in November 2014. It was again scheduled to sample subsequent to Philae's touchdown but prior to drilling operations, thereby retrieving measurements of volatiles from the surface of an unperturbed nucleus. This article evaluates the competence of COSAC mass spectrometers in identifying volatile organic species in both cometary and laboratory-simulated environments. The evaluation was conducted on an operationally optimized COSAC flight spare model mass spectrometer (FS-MS) maintained in ultra-high vacuum. The FS-MS obtained analytical measurements by "sniffing" several organic molecule mixtures of diverse chemical functional groups and molecules with broader molecular masses introduced into the vacuum vessel housing the instrument. The results demonstrate that COSAC produces mass fragmentation patterns of organic species similar to those in calibration standard mass spectra; it is able to identify various organic species within mixtures present at low concentrations (100 ppm); and it can identify fragmentation patterns of non-introduced unknown species and those with high molecular masses within organic mixtures. These observations successfully substantiate the potential of the FM-MS to make qualitative measurements of organic species both in the rarefied environment of the coma and in the relatively enriched nucleus surface. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Giri, Chaitanya; Goesmann, Fred; Gautier, Thomas; Steininger, Harald; Krueger, Harald] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Gautier, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Giri, Chaitanya; Meierhenrich, Uwe J.] Univ Nice Sophia Antipolis, CNRS, UMR 7272, Inst Chim Nice, F-06108 Nice, France.
RP Giri, C (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
EM giri@mps.mpg.de
RI Meierhenrich, Uwe/A-1643-2008
OI Meierhenrich, Uwe/0000-0001-6422-3930
FU Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50QP1302]; Centre
national d'etudes spatiales (CNES); International Max Planck Research
School at the MPS
FX We gratefully acknowledge Dr. Helmut Rosenbauer, who headed the design
and construction of COSAC onboard the Philae Lander of Rosetta
spacecraft until the year 2004 and Henning Fischer for his technical
assistance during the experiments. The work on COSAC is funded by
Deutsches Zentrum fur Luft- und Raumfahrt (DLR) under contract number
50QP1302. It is also supported by Centre national d'etudes spatiales
(CNES). The PhD of CG was funded by the International Max Planck
Research School at the MPS.
NR 27
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2015
VL 106
BP 132
EP 141
DI 10.1016/j.pss.2014.12.017
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC7AD
UT WOS:000350519200011
ER
PT J
AU McKinna, LIW
AF McKinna, Lachlan I. W.
TI Three decades of ocean-color remote-sensing Trichodesmium spp. in the
World's oceans: A review
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID DIAZOTROPHIC CYANOBACTERIA TRICHODESMIUM; CHLOROPHYLL-A CONCENTRATION;
IMAGING SPECTRORADIOMETER MODIS; INHERENT OPTICAL-PROPERTIES;
GULF-OF-MEXICO; COASTAL WATERS; ATMOSPHERIC CORRECTION; BIOOPTICAL
PROPERTIES; SEAWIFS IMAGERY; ARABIAN SEA
AB Ocean-color sensors have provided the necessary platform for synoptic-scale detection and monitoring of the nitrogen-fixing marine cyanobacterium Trichodesmium spp. Such information is invaluable to global biogeochemical studies which require accurate estimates of atmospherically-fixed nitrogen. This article reviews literature from the past three decades and discusses the development of Trichodesmium-specific remote-sensing methods and how these have been revised with improved knowledge of bio-optical properties and remote-sensing technologies. Overall, the majority of Trichodesmium-specific detection methods have been non-quantitative and developed primarily for mapping the occurrence of dense surface aggregations of the cyanobacteria. The ability to positively discriminate and quantify low background concentrations of Trichodesmium (e.g. <3200 trichomes L-1) dispersed within the water column still remains an intractable problem. Furthermore, the spectral and spatial resolutions of existing ocean-color sensors are presently a limiting factor for quantitative Trichodesmium remote sensing. It is noted that planned next-generation sensors with higher spectral resolutions, in both low earth and geostationary orbits, are likely to enhance efforts to remotely-sense global Trichodesmium abundance. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [McKinna, Lachlan I. W.] James Cook Univ, Sch Engn & Phys Sci, Australian Inst Marine Sci, Townsville, Qld 4811, Australia.
[McKinna, Lachlan I. W.] James Cook Univ, Sch Engn & Phys Sci, Townsville, Qld 4781, Australia.
[McKinna, Lachlan I. W.] NASA, Goddard Space Flight Ctr, Ocean Ecol Lab, Greenbelt, MD 20771 USA.
RP McKinna, LIW (reprint author), NASA, Goddard Space Flight Ctr, Ocean Ecol Lab, Code 616, Greenbelt, MD 20771 USA.
EM lachlan.i.mckinna@nasa.gov
FU Australian Postgraduate Award; NASA
FX This research was funded in-part by an Australian Postgraduate Award
administered by James Cook University and a NASA Postdoctoral Program
Fellowship administered by Oak Ridge Associated Universities. All
ocean-color imagery presented within this article were produced using
SeaDAS 7.1 software from data freely available through the NASA Ocean
Color website (http://oceancolor.gsfc.nasa.gov/). Sincere thanks go to
Prof. Peter Ridd (James Cook University) and Dr. Jeremy Werdell (NASA
GSFC) for their kind editorial support. I also wish to recognize the
efforts of Dr. Toby Westberry, Prof. Ajit Subramaniam and two anonymous
reviewers for their attention to detail and insightful comments. The
space agencies who have launched ocean-color missions and made the data
available to the research community are also duly acknowledged. Finally,
I must recognize the pioneering efforts of ocean-color scientists whose
research has contributed greatly to our understanding of Trichodesmium
in the World's oceans.
NR 129
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD FEB
PY 2015
VL 131
BP 177
EP 199
DI 10.1016/j.pocean.2014.12.013
PG 23
WC Oceanography
SC Oceanography
GA CC7IH
UT WOS:000350540400013
ER
PT J
AU Anthonioz, F
Menard, F
Pinte, C
Le Bouquin, JB
Benisty, M
Thi, WF
Absil, O
Duchene, G
Augereau, JC
Berger, JP
Casassus, S
Duvert, G
Lazareff, B
Malbet, F
Millan-Gabet, R
Schreiber, MR
Traub, W
Zins, G
AF Anthonioz, F.
Menard, F.
Pinte, C.
Le Bouquin, J. -B.
Benisty, M.
Thi, W. -F.
Absil, O.
Duchene, G.
Augereau, J. -C.
Berger, J. -P.
Casassus, S.
Duvert, G.
Lazareff, B.
Malbet, F.
Millan-Gabet, R.
Schreiber, M. R.
Traub, W.
Zins, G.
TI The VLTI/PIONIER near- infrared interferometric survey of southern T
Tauri stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: interferometric; protoplanetary disks; binaries: general;
stars: variables: T Tauri,Herbig Ae/Be
ID HERBIG AE/BE STARS; YOUNG STARS; KECK INTERFEROMETER; STELLAR
POPULATION; CHAMELEON-I; INNER DISKS; GQ LUP; EMISSION; ASSOCIATIONS;
TRANSITION
AB Context. The properties of the inner disks of bright Herbig AeBe stars have been studied with near-infrared (NIR) interferometry and high resolution spectroscopy. The continuum (dust) and a few molecular gas species have been studied close to the central star; however, sensitivity problems limit direct information about the inner disks of the fainter T Tauri stars.
Aims. Our aim is to measure some of the properties (inner radius, brightness profile, shape) of the inner regions of circumstellar disk surrounding southern T Tauri stars. Methods. We performed a survey with the VLTI/PIONIER recombiner instrument at H-band of 21 T Tauri stars. The baselines used ranged from 11 m to 129 m, corresponding to a maximum resolution of similar to 3 mas (similar to 0.45 au at 150 pc).
Results. Thirteen disks are resolved well and the visibility curves are fullysampled as a function of baseline in the range 45-130 m for these 13 objects. A simple qualitative examination of visibility profiles allows us to identify a rapid drop-off in the visibilities at short baselines(< 10 MA) in 8 resolved disks. This is indicative of a significant contribution from an extended (R > 3 au, at 150 pc) contribution of light from the disk. We demonstrate that this component is compatible with scattered light, providing strong support to an earlier prediction. The amplitude of the drop-off and the amount of dust thermal emission changes from source to source suggesting that each disk is different. A by-product of the survey is the identification of a new milli-arcsec separation binary: WW Cha. Spectroscopic and interferometric data of AK Sco have also been fitted with a binary + disk model.
Conclusions. The visibility data are reproduced well when thermal emission and scattering from dust are fully considered. The inner radii measured are consistent with the expected dust sublimation radii. The modelling of AK Sco suggests a likely coplanarity between the disk and the binary's orbital plane.
C1 [Anthonioz, F.; Pinte, C.; Le Bouquin, J. -B.; Benisty, M.; Thi, W. -F.; Duchene, G.; Augereau, J. -C.; Duvert, G.; Lazareff, B.; Malbet, F.; Zins, G.] Univ Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
[Menard, F.] UMI FCA, UMI 3386, CNRS INSU France, Santiago 1058, Chile.
[Menard, F.] Univ Chile, Santiago 1058, Chile.
[Berger, J. -P.] European So Observ, D-85748 Garching, Germany.
[Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Millan-Gabet, R.; Traub, W.] CALTECH, Pasadena, CA 91125 USA.
[Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile.
[Schreiber, M. R.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
RP Anthonioz, F (reprint author), Univ Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
EM anthonioz.fabien@gmail.com
RI Casassus, Simon/I-8609-2016
FU Universite Joseph Fourier (UJF, Grenoble); Institut de Planetologie et
d'Astrophysique de Grenoble; "Agence Nationale pour la Recherche";
Institut National des Science de l'Univers (INSU); Smithsonian/NASA
Astrophysics Data System (ADS) and of the Centre de Donnees
astronomiques de Strasbourg (CDS); European Commission's 7th framework
programme (EC FP7) [284405, PERG06-GA-2009-256513]; Agence Nationale
pour la Recherche (ANR) of France [ANR-2010-JCJC-0504-01]; Millennium
Science Initiative, Chilean Ministry of Economy: Nucleus [Millennium
Science Initiative, Chilean Ministry of Economy: Nucleus P10-022-F]
FX PIONIER is funded by the Universite Joseph Fourier (UJF, Grenoble)
through its Poles TUNES and SMING, the Institut de Planetologie et
d'Astrophysique de Grenoble, the "Agence Nationale pour la Recherche"
with the programme ANR EXOZODI, and the Institut National des Science de
l'Univers (INSU) via the "Programme National de Physique Stellaire" and
"Programme National de Planetologie". The authors want to warmly thank
all the people involved in the VLTI project. This work is based on
observations made with the ESO telescopes. It made use of the
Smithsonian/NASA Astrophysics Data System (ADS) and of the Centre de
Donnees astronomiques de Strasbourg (CDS). All calculations and graphics
were performed with the open source software Yorick. We acknowledge
funding from the European Commission's 7th framework programme (EC FP7)
under grant agreement No. 284405 (DIANA) and contract
PERG06-GA-2009-256513 and also from Agence Nationale pour la Recherche
(ANR) of France under contract ANR-2010-JCJC-0504-01. FM., S.C. and M.S.
acknowledge support from Millennium Science Initiative, Chilean Ministry
of Economy: Nucleus P10-022-F This research has made use of the Simbad
database operated at the CDS, Strasbourg, France, and the Jean-Marie
Mariotti Center ASPRO and LITpro services co-developed by CRAL, IPAG,
and FIZEAU. We thank the anonymous referee for her/his suggestions for
improvement.
NR 59
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A41
DI 10.1051/0004-6361/201424520
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000041
ER
PT J
AU Cataldi, G
Brandeker, A
Olofsson, G
Chen, CH
Dent, WRF
Kamp, I
Roberge, A
Vandenbussche, B
AF Cataldi, G.
Brandeker, A.
Olofsson, G.
Chen, C. H.
Dent, W. R. F.
Kamp, I.
Roberge, A.
Vandenbussche, B.
TI Constraints on the gas content of the Fomalhaut debris belt Can gas-dust
interactions explain the belt's morphology?
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; planetary systems; stars: individual: Fomalhaut;
methods: observational; hydrodynamics; infrared: general
ID BETA-PICTORIS; PLANETARY SYSTEM; NEARBY STARS; ARRAY CAMERA; DISK;
IMAGES; ORBIT; RINGS; VEGA
AB Context. The 440 Myr old main-sequence A-star Fomalhaut is surrounded by an eccentric debris belt with sharp edges. This sort of a morphology is usually attributed to planetary perturbations, but the orbit of the only planetary candidate detected so far, Fomalhaut b, is too eccentric to efficiently shape the belt. Alternative models that could account for the morphology without invoking a planet are stellar encounters and gas-dust interactions.
Aims. We aim to test the possibility of gas-dust interactions as the origin of the observed morphology by putting upper limits on the total gas content of the Fomalhaut belt.
Methods. We derive upper limits on the CII 158 mu m and 01 63 pint emission by using non detections from the Photocletector Array Camera and Spectrometer (PACS) onboard the Herschel Space Observatory. Line fluxes are converted into total gas mass using the non-local thermodynamic equilibrium (non-LTE) code RADEX. We consider two different cases for the elemental abundances of the gas: solar abundances and abundances similar to those observed for the gas in the beta Pictoris debris disc.
Results. The gas mass is shown to be below the millimetre dust mass by a factor of at least similar to 3 (for solar abundances) respectively similar to 300 (for beta Pic-like abundances).
Conclusions. The lack of gas co-spatial with the dust implies that gas-dust interactions cannot efficiently shape the Fomalhaut debris belt. The morphology is therefore more likely due to a yet unseen planet (Fomalhaut c) or stellar encounters.
C1 [Cataldi, G.; Brandeker, A.; Olofsson, G.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Cataldi, G.; Brandeker, A.; Olofsson, G.] Stockholm Univ, Astrobiol Ctr, S-10691 Stockholm, Sweden.
[Chen, C. H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Dent, W. R. F.] ALMA SCO, Santiago, Chile.
[Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Roberge, A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Vandenbussche, B.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium.
RP Cataldi, G (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
EM gianni.cataldi@astro.su.se
RI Roberge, Aki/D-2782-2012
OI Roberge, Aki/0000-0002-2989-3725
FU Herschel Science Centre Helpdesk; BMVIT (Austria); ESA-PRODEX (Belgium);
CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain)
FX We would like to thank the referee, Jane Greaves, for useful and
constructive comments that helped to clarify this manuscript. We also
thank Elena Puga from the Herschel Science Centre Helpdesk for support
with the Herschel beam products. This research has made use of the
SIMBAD database (operated at CDS, Strasbourg, France), the MIST Atomic
Spectra Database, the NORAD-Atomic-Data database and NASA's Astrophysics
Data System. PACS has been developed by a consortium of institutes led
by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC
(Belgium); CEA, LAM (France); MPIA (Germany); INAF-FSI/OAA/OAP/OAT,
LENS, SISSA (Italy); IAC (Spain). This development has been supported by
the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES
(France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR L1
DI 10.1051/000476361/201425322
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000149
ER
PT J
AU Lyra, W
Turner, NJ
McNally, CP
AF Lyra, W.
Turner, N. J.
McNally, C. P.
TI Rossby wave instability does not require sharp resistivity gradients
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; planets and satellites: formation;
instabilities; magnetohydrodynamics (MHD); turbulence; methods:
numerical
ID DIFFERENTIALLY ROTATING-DISKS; THIN ACCRETION DISKS; PROTOPLANETARY
DISKS; MAGNETOROTATIONAL INSTABILITY; DEAD-ZONE; NONLINEAR EVOLUTION;
CONVECTIVE OVERSTABILITY; CIRCUMSTELLAR DISKS; DYNAMICAL STABILITY;
PLANET INTERACTIONS
AB Context. Rossby wave instability (RWI) at dead zone boundaries may play an important role in planet formation. Viscous hydrodynamics results suggest RWI is excited only when the viscosity changes over a radial distance less than two density scale heights. However in the disks around Solar-mass T Tauri stars, it is not viscosity but magnetic forces that provide the accretion stress beyond about 10 AU, where surface densities are low enough so stellar X-rays and interstellar cosmic rays can penetrate.
Aims. We explore the conditions for RWI in the smooth transition with increasing distance, from resistive and magnetically-dead to conducting and magnetically-active.
Methods. We perform 3D unstratified MHD simulations with the Pencil code, using static resistivity profiles.
Results. We find that in MHD, contrary to viscous models, the RWI is triggered even with a gradual change in resistivity extending from 10 to 40 AU (i.e., spanning 15 scale heights for aspect ratio 0.1). This is because magneto-rotational turbulence sets in abruptly when the resistivity reaches a threshold level. At higher resistivities the longest unstable wavelength is quenched, resulting in a sharp decline of the Maxwell stress towards the star. The sharp gradient in the magnetic forces leads to a localized density bump, that is in turn Rossby wave unstable.
Conclusions. Even weak gradients in the resistivity can lead to sharp transitions in the Maxwell stress. As a result the RWI is more easily activated in the outer disk than previously thought. Rossby vortices at the outer dead zone boundary thus could underlie the dust asymmetries seen in the outer reaches of transition disks.
C1 [Lyra, W.; Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lyra, W.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[McNally, C. P.] Niels Bohr Int Acad, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
RP Lyra, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM wlyra@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); European Union
[327995]
FX This work was performed in part at the Jet Propulsion Laboratory, under
contract with the California Institute of Technology funded by the
National Aeronautics and Space Administration (NASA) through the Sagan
Fellowship Program executed by the NASA Exoplanet Science Institute. The
research leading to these results has received funding from the People
Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme (FP7/2007-2013) under REA grant agreement 327995. We
acknowledge discussions with Min-Kai Lin and Zhaohuan Zhu.
NR 59
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A10
DI 10.1051/0004-6361/201424919
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000010
ER
PT J
AU Muller, C
Krauss, F
Dauser, T
Kreikenbohm, A
Beuchert, T
Kadler, M
Ojha, R
Wilms, J
Bock, M
Carpenter, B
Dutka, M
Markowitz, A
McConville, W
Pottschmidt, K
Stawarz, L
Taylor, GB
AF Mueller, C.
Krauss, F.
Dauser, T.
Kreikenbohm, A.
Beuchert, T.
Kadler, M.
Ojha, R.
Wilms, J.
Boeck, M.
Carpenter, B.
Dutka, M.
Markowitz, A.
McConville, W.
Pottschmidt, K.
Stawarz, L.
Taylor, G. B.
TI Redshifted Fe K alpha line from the unusual gamma-ray source PMN
J1603-4904
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: jets; galaxies: individual: PMN J1603-4904;
X-rays: galaxies; gamma rays: galaxies
ID ACTIVE GALACTIC NUCLEI; COMPACT STEEP-SPECTRUM; LARGE-AREA TELESCOPE;
EXTRAGALACTIC RADIO-SOURCES; PHOTON IMAGING CAMERA; XMM-NEWTON;
SYMMETRIC OBJECTS; TIMING-EXPLORER; FERMI-LAT; EMISSION
AB Context. Multiwavel ngth observations have revealed the highly unusual properties of the gamma-ray source PIYIN J1603-4904, which are difficult to reconcile with any other well established gamma-ray source class. The object either a very atypical blazar or a compact jet source seen at a larger angle to the line of sight.
Aims. To determine the physical origin of the high-energy emission processes in PMNJ1603-4904, we study the X-ray spectrum in detail,
Methods. We performed quasi simultaneous X-ray observations with XMM -Newton and Suzaku in 2013 September. This resulted in the first high signal-to-noise X-ray spectrum of this source.
Results. The 2-10 keV X-ray spectrum can be well described by an absorbed power law with an emission line at 5.44 +/- 0.05 key (observed frame). We interpret this feature as a Ka line from neutral iron and accordingly determine the redshift of PMNJ1603-4904 to be z = 0.18 +/- 0.01, which corresponds to a luminosity distance of 872 +/- 54 Mpc.
Conclusions. The detection of a redshiftecl X-ray emission line further challenges the original BL Lac classification of PMN J1603-4904. This result suggests that the source is observed at a larger angle to the line of sight than expected for blazars. and thus the source would add to the elusive class of gamma-ray loud misaligned jet objects, possibly a gamma-ray bright young radio galaxy.
C1 [Mueller, C.; Krauss, F.; Kreikenbohm, A.; Beuchert, T.; Kadler, M.; Boeck, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Mueller, C.; Krauss, F.; Dauser, T.; Kreikenbohm, A.; Beuchert, T.; Wilms, J.; Boeck, M.; Markowitz, A.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte, D-96049 Bamberg, Germany.
[Mueller, C.; Krauss, F.; Dauser, T.; Kreikenbohm, A.; Beuchert, T.; Wilms, J.; Boeck, M.; Markowitz, A.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Ojha, R.; Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Ojha, R.; Carpenter, B.; Dutka, M.; McConville, W.; Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Ojha, R.; Carpenter, B.; Dutka, M.; McConville, W.; Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Carpenter, B.] Catholic Univ Amer, Washington, DC 20064 USA.
[Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Markowitz, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Stawarz, L.] Inst Space & Astronaut Sci JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
RP Muller, C (reprint author), Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
EM cornelia.mueller@astro.uni-wuerzburg.de
RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410;
FU Bundesministerium fur Wirtschaft und Technologie (BMWi) through
Deutsches Zentrum fur Luftund Raumfahrt (DLR) [50 OR 1404];
Studienstiftung des Deutschen Volkes; National Aeronautics and Space
Administration (NASA) through Fermi Guest Investigator [NNH09ZDA001N,
NNH10ZDA001N, NNH12ZDA001N]; BMWi through DLR [50 OR 1311]; Deutsche
Forschungsgemeinschaft [WI1860/10-1]
FX We thank the referee for the helpful comments, and R. Schulz and PG.
Edwards for the useful discussions that improved the manuscript. C.M.
acknowledges the support of the Bundesministerium fur Wirtschaft und
Technologie (BMWi) through Deutsches Zentrum fur Luftund Raumfahrt (DLR)
grant 50 OR 1404 and of the Studienstiftung des Deutschen Volkes. This
research was funded in part by the National Aeronautics and Space
Administration (NASA) through Fermi Guest Investigator grants
NNH09ZDA001N, NNH10ZDA001N, and NNH12ZDA001N, by BMWi through DLR grant
50 OR 1311, by Deutsche Forschungsgemeinschaft grant WI1860/10-1, and by
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. We thank J. E. Davis for the development of the
slxfig module that has been used to prepare figure in this work. This
research has made use of ISIS functions provided by ECAP/Dr. Karl
Remeis-Observatoty (Bamberg, Germany) and MIT
(http://www.sternwarte.uni-erlangen.de/isis/)
NR 60
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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 FEB
PY 2015
VL 574
AR A117
DI 10.1051/0004-636/201425442
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000117
ER
PT J
AU Parmentier, V
Guillot, T
Fortney, JJ
Marley, MS
AF Parmentier, Vivien
Guillot, Tristan
Fortney, Jonathan J.
Marley, Mark S.
TI A non-grey analytical model for irradiated atmospheres II. Analytical
vs. numerical solutions
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiative transfer; planets and satellites: atmospheres; stars:
atmospheres; planet-star interactions
ID EXTRASOLAR GIANT PLANETS; HOT JUPITERS; HD 209458B; THERMAL STRUCTURE;
MEAN OPACITIES; SPECTRA; CLOUDS; STARS; TIO; ABSORPTION
AB Context. The recent discovery and characterization of the diversity of the atmospheres of exoplanets and brown dwarfs calls for the development of fast and accurate analytical models.
Aims. We wish to assess the goodness of the different approximations used to solve the radiative transfer problem in irradiated atmospheres analytically, and we aim to provide a useful tool for a fast computation of analytical temperature profiles that remains correct over a wide range of atmospheric characteristics.
Methods. We quantify the accuracy of the analytical solution derived in paper I for an irradiated, non-grey atmosphere by comparing it to a state-of-the-art radiative transfer model. Then, using a grid of numerical models, we calibrate the different coefficients of our analytical model for irradiated solar-composition atmospheres of giant exoplanets and brown dwarfs.
Results. We show that the so-called Eddington approximation used to solve the angular dependency of the radiation field leads to relative errors of up to similar to 5% on the temperature profile. For grey or semi-grey atmospheres (i.e., when the visible and thermal opacities, respectively, can be considered independent of wavelength), we show that the presence of a convective zone has a limited effect on the radiative atmosphere above it and leads to modifications of the radiative temperature profile of approximately similar to 2%. However, for realistic non-grey planetary atmospheres, the presence of a convective zone that extends to optical depths smaller than unity can lead to changes in the radiative temperature profile on the order of 20% or more. When the convective zone is located at deeper levels (such as for strongly irradiated hot Jupiters), its effect on the radiative atmosphere is again on the same order (similar to 2%) as in the semi-grey case. We show that the temperature inversion induced by a strong absorber in the optical, such as TiO or VO is mainly due to non-grey thermal effects reducing the ability of the upper atmosphere to cool down rather than an enhanced absorption of the stellar light as previously thought. Finally, we provide a functional form for the coefficients of our analytical model for solar-composition giant exoplanets and brown dwarfs. This leads to fully analytical pressure-temperature profiles for irradiated atmospheres with a relative accuracy better than 10% for gravities between 2.5 m s(-2) and 250 m s(-2) and effective temperatures between 100 K and 3000 K. This is a great improvement over the commonly used Eddington boundary condition.
C1 [Parmentier, Vivien; Guillot, Tristan] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab J L Lagrange, F-06304 Nice, France.
[Parmentier, Vivien; Guillot, Tristan; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Parmentier, V (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab J L Lagrange, BP 4229, F-06304 Nice, France.
EM vivien.parmentier@oca.eu
OI Marley, Mark/0000-0002-5251-2943
FU Fulbright Fellowship; Jet Propulsion Laboratory (JPL); NASA
FX We acknowledge the anonymous referee for his general comments that
increased the quality of this manuscript. This work was performed in
part thanks to a joint Fulbright Fellowship to V.P. and T.G. The whole
project would not have been possible without the help and support of
Douglas Lin. We also acknowledge University of California Santa Cruz for
hosting us while this work was carried out. During the last part of this
work, V.P. was under contract with the Jet Propulsion Laboratory (JPL)
funded by NASA through the Sagan Fellowship Program executed by the NASA
Exoplanet Science Institute.
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FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A35
DI 10.1051/0004-6361/201323127
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000035
ER
PT J
AU Pereira, TMD
Uitenbroek, H
AF Pereira, Tiago M. D.
Uitenbroek, Han
TI RH 1.5D: a massively parallel code for multi-level radiative transfer
with partial frequency redistribution and Zeeman polarisation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE line: formation; methods: numerical; radiative transfer; polarization;
stars: atmospheres
ID SPECTRAL-LINE FORMATION; RED GIANT STARS; SOLAR PHOTOSPHERE; K LINES; MG
II; SIMULATIONS; CONVECTION; ABUNDANCE; ATMOSPHERES; MAGNETOCONVECTION
AB The emergence of three-dimensional magneto-hydrodynamic simulations of stellar atmospheres has sparked a need for efficient radiative transfer codes to calculate detailed synthetic spectra. We present RH 1.5D, a massively parallel code based on the RH code and capable of performing Zeeman polarised multi-level non-local thermodynamical equilibrium calculations with partial frequency redistribution for an arbitrary amount of chemical species. The code calculates spectra from 3D, 2D or 1D atmospheric models on a column-by-column basis (or 1.5D). While the 1.5D approximation breaks down in the cores of very strong lines in an inhomogeneous environment, it is nevertheless suitable for a large range of scenarios and allows for faster convergence with finer control over the iteration of each simulation column. The code scales well to at least tens of thousands of CPU cores, and is publicly available. In the present work we briefly describe its inner workings, strategies for convergence optimisation, its parallelism, and some possible applications.
C1 [Pereira, Tiago M. D.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Pereira, Tiago M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pereira, Tiago M. D.] Lockheed Martin Adv Technol Ctr, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Uitenbroek, Han] Natl Solar Observ, Sunspot, NM 88349 USA.
RP Pereira, TMD (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
EM tiago.pereira@astro.uio.no
FU NASA High-End Computing (HEC) Program through NASA Advanced
Supercomputing (NAS) Division at Ames Research Center [s1061]; Notur
project through Research Council of Norway; European Research Council
under the European Union / ERC [291058]; NASA Postdoctoral Program at
Ames Research Center [NNH06CC03B]
FX We are grateful to Jorrit Leenaarts for his extensive contributions to
the code (in particular the PRD switching, approximate angle-dependent
PRD, and support for many collisional processes). We would also like to
thank Bhavna Rathore, Mats Carlsson, and Hsiao-Hsuan Lin for their
contributions to the code. 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 (project s1061) and from the Notur project through
grants from the Research Council of Norway. This work was supported by
the European Research Council under the European Union's Seventh
Framework Programme (FP7/2007-2013) / ERC Grant agreement No. 291058.
T.M.D.P. was supported by the NASA Postdoctoral Program at Ames Research
Center (grant NNH06CC03B).
NR 42
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A3
DI 10.1051/0004-6361/201424785
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000003
ER
PT J
AU Rots, AH
Bunclark, PS
Calabretta, MR
Allen, SL
Manchester, RN
Thompson, WT
AF Rots, Arnold H.
Bunclark, Peter S.
Calabretta, Mark R.
Allen, Steven L.
Manchester, Richard N.
Thompson, William T.
TI Representations of time coordinates in FITS Time and relative dimension
in space
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE time; standards; methods: data analysis; techniques: miscellaneous;
astronomical databases: miscellaneous; reference systems
ID SOLAR
AB Context. In a series of three previous papers, formulation and specifics of the representation of world coordinate transformations in FITS data have been presented. This fourth paper deals with encoding time.
Aims. Time on all scales and precisions known in astronomical datasets is to be described in an unambiguous, complete, and self-consistent manner.
Methods. Employing the well-established World Coordinate System (WCS) framework, and maintaining compatibility with the FITS conventions that are currently in use to specify time, the standard is extended to describe rigorously the time coordinate.
Results. World coordinate functions are defined for temporal axes sampled linearly and as specified by a lookup table. The resulting standard is consistent with the existing FITS WCS standards and specifies a metadata set that achieves the aims enunciated above.
C1 [Rots, Arnold H.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Bunclark, Peter S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Calabretta, Mark R.; Manchester, Richard N.] CSIRO, Astron & Space Sci, Epping, NSW 1710, Australia.
[Allen, Steven L.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Thompson, William T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA.
RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St MS 67, Cambridge, MA 02138 USA.
EM arots@cfa.harvard.edu
OI Rots, Arnold/0000-0003-2377-2356
FU NASA [NAS 8-03060]
FX The authors want to express their deep gratitude and appreciation for
the dedication and tireless efforts of their colleague and friend Peter
Bunclark in moving the work on this paper forward. We received his last
email on 8 December 2008, just two days before his untimely death. We
miss Pete dearly, not only as a great co-author who kept us on the
straight and narrow, but especially as a very good friend. It was a
privilege to have collaborated with him. We are also very much indebted
to former IAU FITS Working Group chair Bill Pence, who provided valuable
comments and kept exhorting us to finally finish this paper. A.H.R.
gratefully acknowledges the many helpful discussions he had with
Jonathan McDowell and the support by NASA under contract NAS 8-03060 to
the Smithsonian Astrophysical Observatory for operation of the Chandra
X-ray Center. We thank an anonymous referee for helpful comments that
resulted in improved clarity. And we thank Patrick Wallace, Ken
Seidelmann, and George Kaplan for their comments and suggestions.
NR 46
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A36
DI 10.1051/0004-6361/201424653
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000036
ER
PT J
AU Schaerer, D
Boone, F
Zamojski, M
Staguhn, J
Dessauges-Zavadsky, M
Finkelstein, S
Combes, F
AF Schaerer, D.
Boone, F.
Zamojski, M.
Staguhn, J.
Dessauges-Zavadsky, M.
Finkelstein, S.
Combes, F.
TI New constraints on dust emission and UV attenuation of z=6.5-7.5
galaxies from millimeter observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: high-redshift; galaxies: starburst; dust, extinction;
galaxies: ISM; submillimeter: galaxies
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; SIMILAR-TO 7; HERSCHEL
LENSING SURVEY; FORMATION RATE DENSITY; LY-ALPHA EMITTER; GREATER-THAN
6.5; C II LINE; HIGH-REDSHIFT; FORMATION HISTORIES
AB Context. Determining the dust properties and UV attenuation of distant star-forming galaxies is of great interest for our understanding of galaxy formation and cosmic star formation in the early Universe. However, few direct measurements exist so far.
Aims. To shed new light on these questions, we have targeted two recently discovered Lyman-break galaxies (LBGs) at z approximate to 6.8 and z = 7.508 to search for dust continuum and [C II] 1158 pm line emission.
Methods. The strongly lensed z approximate to 6.8 LBG A1703-zD1 behind the galaxy cluster Abell 1703 and the spectroscopically confirmed z = 7.508 LBG z8-GND-5296 in the GOODS-N field were observed with the Plateau de Bure Interferometer (PdBI) at 1.2 mm. These observations were combined with those of three z > 6.5 Ly alpha emitters (HCM6A, Himiko, and IOK-1), for which deep measurements were recently obtained with the PdBI and ALMA.
Results. [C II] is undetected in both galaxies, providing a deep upper limit of L-[C II] < 2.8 x 10(7) L for A1703-zD1, comparable to the nondetections of Himiko and IOK-1 with ALMA. Dust continuum emission from A1703-zD1 and z8-GND-5296 is not detected with an rms of 0.12 and 0.16 mJy/beam. From these nondetections and earlier multiwavelength observations we derive upper limits on their IR luminosity and star formation rate, dust mass, and UV attenuation. Thanks to strong gravitational lensing, the achieved limit for A1703-zDI is similar to those achieved with ALMA, probing below the luminous infrared galaxy (LIRG) regime (L-IR < 8.1 x 10(10) L-circle dot) and very low dust masses (M-d < 1.6 x 10(7) M-circle dot). We find that all five galaxies are compatible with the Calzetti IRX-beta relation, their UV attenuation is compatible with several indirect estimates from other methods (the UV slope, extrapolation of the attenuation measured from the IR/UV ratio at lower redshift, and spectral energy distribution fits), and the dust-to-stellar mass ratio is compatible with that of galaxies from z = 0 to 3. From their stellar mass, the high-z galaxies studied here have an attenuation below the one expected from the mean relation of low-redshift (z less than or similar to 1.5) galaxies.
Conclusions. More and deeper (sub-)mm data are clearly needed to directly determine the UV attenuation and dust content of the dominant population of high-z star-forming galaxies and to establish their dependence on stellar mass, redshift, and other properties more firmly.
C1 [Schaerer, D.; Zamojski, M.; Finkelstein, S.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland.
[Schaerer, D.; Boone, F.] CNRS, IRAP, F-31400 Toulouse, France.
[Staguhn, J.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Staguhn, J.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Finkelstein, S.] Univ Texas Austin, Austin, TX 78712 USA.
[Combes, F.] Observ Paris, LERMA, F-75014 Paris, France.
RP Schaerer, D (reprint author), Univ Geneva, Observ Geneva, 51 Ch Maillettes, CH-1290 Versoix, Switzerland.
EM daniel.schaerer@unige.ch
OI Combes, Francoise/0000-0003-2658-7893
FU Swiss National Science Foundation; NSF ATI [1020981, 1106284]
FX We thank IRAM, in particular Tessel van der Laan, for efficient
observations and help with data reduction. This work was supported by
the Swiss National Science Foundation. J.S. and the GISMO observations
were supported through NSF ATI grants 1020981 and 1106284. We made use
of the public Cosmolopy python package from Roban Kramer
(http://roban.github.com/CosmoloPy/), the python version of Ned Wright's
cosmology calculator, from James Schombert, TOPCAT (Taylor 2005), and
the NASA ADS services. This paper makes use of the following ALMA data:
ADS/JAO. ALMA#2011.0.00115.S and ADS/JAO. ALMA#2011.0.00767.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.
NR 72
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A19
DI 10.1051/0004-6361/201424649
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000019
ER
PT J
AU Werner, K
Rauch, T
Kucas, S
Kruk, JW
AF Werner, K.
Rauch, T.
Kucas, S.
Kruk, J. W.
TI The prospective search for highly ionized technetium in hot (pre-) white
dwarfs
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: evolution; stars: AGB and post-AGB; white
dwarfs; atomic data; line: identification
ID CONSISTENT DIFFUSION-MODELS; OSCILLATOR-STRENGTHS; STELLAR LABORATORIES;
RE 0503-289; G191-B2B; ABUNDANCES; VALIDATION; SEQUENCES; SPECTRA; STARS
AB The discovery of technetium (Tc) in the atmospheres of red giants by Merrill (1952, ApJ, 116, 21) constituted convincing proof that s-process nucleosynthesis is indeed occurring in evolved stars. In principle, Tc should still be present in the atmospheres of hot post-AGB stars and (pre-) white dwarfs although, due to radioactive decay, it should be present in decreasing quantities along post-AGB evolution. The recent discovery of a large number of trans-iron group elements in hot white dwarfs with atomic numbers in the range A = 30-56 (Zn to Ba) raises the prospect that Tc (A = 43) may also be detected. However, this is currently not feasible because no atomic data exist for ionization stages beyond Tc II. As an initial step, we calculated atomic energy levels and oscillator strengths of Tc IV-VI and used these data to compute non-local thermodynamic equilibrium (NLTE) model atmospheres to estimate at which minimum abundance level Tc could be detected. We show that Tc lines can be found in ultraviolet spectra of hot white dwarfs provided Tc is as abundant as other detected trans-Fe elements. We find that radiative levitation can keep Tc in large, easily detectable quantities in the atmosphere. A direct identification of Tc lines is still not feasible because wavelength positions cannot be computed with necessary precision. Laboratory measurements are necessary to overcome this problem. Our results suggest that such efforts are beneficial to the astrophysical community.
C1 [Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Kucas, S.] Vilnius Univ, Inst Theoret Phys & Astron, LT-01108 Vilnius, Lithuania.
[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) [05 OR 1402]; Federal Ministry of
Education and Research (BMBF) [05 AC 6 VTB, 05 AC 11 VTB]; NASA
[NAS5-26555]; NASA Office of Space Science [NNX09AF08G]
FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR
1402). The spectral energy distributions that were calculated for this
analysis are available via the registered virtual-observatory (VO)
service TheoSSA (Theoretical Stellar Spectra Access,
http://dc.g-vo.org/theossa) that was developed within a German
Astrophysical Virtual Observatory (GAVO, http://dc.g-vo.org) project at
Tubingen. The GAVO project at Tubingen had been supported by the Federal
Ministry of Education and Research (BMBF, grants 05 AC 6 VTB, 05 AC 11
VTB). This research has made use of the SIMBAD database, operated at
CDS, Strasbourg, France. Some of the data presented in this paper were
obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data
is provided by the NASA Office of Space Science via grant NNX09AF08G and
by other grants and contracts.
NR 24
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2015
VL 574
AR A29
DI 10.1051/0004-6361/201424199
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB2OJ
UT WOS:000349467000029
ER
PT J
AU Grady, C
Fukagawa, M
Maruta, Y
Ohta, Y
Wisniewski, J
Hashimoto, J
Okamoto, Y
Momose, M
Currie, T
McElwain, M
Muto, T
Kotani, T
Kusakabe, N
Feldt, M
Sitko, M
Follette, K
Bonnefoy, M
Henning, T
Takami, M
Karr, J
Kwon, J
Kudo, T
Abe, L
Brandner, W
Brandt, T
Carson, J
Egner, S
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, G
Kuzuhara, M
Matsuo, T
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Grady, C.
Fukagawa, M.
Maruta, Y.
Ohta, Y.
Wisniewski, J.
Hashimoto, J.
Okamoto, Y.
Momose, M.
Currie, T.
McElwain, M.
Muto, T.
Kotani, T.
Kusakabe, N.
Feldt, M.
Sitko, M.
Follette, K.
Bonnefoy, M.
Henning, T.
Takami, M.
Karr, J.
Kwon, J.
Kudo, T.
Abe, L.
Brandner, W.
Brandt, T.
Carson, J.
Egner, S.
Goto, M.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Hodapp, K.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G.
Kuzuhara, M.
Matsuo, T.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, E.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y. H.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI The outer disks of Herbig stars from the UV to NIR
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Review
DE Stars: pre-main sequence; Stars: Herbig Ae/Be; Protoplanetary disks;
Planet-disk interactions
ID INTERMEDIATE-MASS STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR
OBJECTS; AE/BE STARS; PROTOPLANETARY DISKS; X-RAY; HIGH-RESOLUTION;
CIRCUMSTELLAR DISK; SCATTERED-LIGHT; AE SYSTEMS
AB Spatially-resolved imaging of Herbig stars and related objects began with HST, but intensified with commissioning of high-contrast imagers on 8-m class telescopes. The bulk of the data taken from the ground have been polarized intensity imagery at H-band, with the majority of the sources observed as part of the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) survey. Sufficiently many systems have been imaged that we discuss disk properties in scattered, polarized light in terms of groups defined by the IR spectral energy distribution. We find novel phenomena in many of the disks, including spiral density waves, and discuss the disks in terms of clearing mechanisms. Some of the disks have sufficient data to map the dust and gas components, including water ice dissociation products.
C1 [Grady, C.] Eureka Sci & Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
[Fukagawa, M.; Maruta, Y.; Ohta, Y.] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 560004, Japan.
[Wisniewski, J.; Hashimoto, J.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA.
[Okamoto, Y.; Momose, M.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Currie, T.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[McElwain, M.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Kotani, T.; Kusakabe, N.; Kudo, T.; Hayashi, M.; Ishii, M.; Iye, M.; Morino, J. -I.; Suenaga, T.; Suto, H.; Suzuki, R.; Takahashi, Y. H.; Takami, H.; Usuda, T.; Tamura, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Follette, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Feldt, M.; Bonnefoy, M.; Henning, T.; Brandner, W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Sitko, M.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Takami, M.; Karr, J.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Knapp, G.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Currie, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Kandori, R.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kwon, J.; Takahashi, Y. H.; Tamura, M.] Univ Tokyo, Dept Astron, Tokyo 1130033, Japan.
[Abe, L.] Univ Nice, Lab Lagrange, CNRS, Observ Cote Azur,UMR 7293, F-06108 Nice 2, France.
[Brandt, T.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, M.] Univ Munich, D-81679 Munich, Germany.
[Hodapp, K.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Suenaga, T.] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Thalmann, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Janson, M.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden.
RP Grady, C (reprint author), Eureka Sci & Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
EM Carol.A.Grady@nasa.gov
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU World Premier International Research Center Initiative, MEXT, Japan; NSF
AST [1008440]; NASA Origins of Solar Systems program [NNG13PB64P]; NASA
RTOP through the NASA Origins of Solar Systems program [12-OSS12-0045];
NSF-AST [1009314]; NASA Origins of Solar System program [NNX13AK17G];
NASA ADP [SOF-0026, NNX09AC73G]
FX We wish to thank the referee, Glenn Schneider, for helpful comments
which improved the quality of this chapter. This research is based in
part on data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan. This research has been
supported in part by the World Premier International Research Center
Initiative, MEXT, Japan. This research has made use of the SIMBAD
database and Vizier service, operated at CDS, Strasbourg, France. The
authors wish to recognize and acknowledge the very significant cultural
role and reverence that the summit of Mauna Kea has always had within
the indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. CAG has been
supported by NSF AST 1008440 and through the NASA Origins of Solar
Systems program on NNG13PB64P, as well as by SOF-0026. MWMcE is
supported under NASA RTOP 12-OSS12-0045 through the NASA Origins of
Solar Systems program. JPW is supported under NSF-AST 1009314 and the
NASA Origins of Solar System program under NNX13AK17G. MLS was supported
under NASA ADP grant NNX09AC73G and SOF-0026.
NR 124
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
EI 1572-946X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD FEB
PY 2015
VL 355
IS 2
BP 253
EP 266
DI 10.1007/s10509-014-2214-2
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC2WV
UT WOS:000350206600007
ER
PT J
AU Daloz, AS
Camargo, SJ
Kossin, JP
Emanuel, K
Horn, M
Jonas, JA
Kim, D
LaRow, T
Lim, YK
Patricola, CM
Roberts, M
Scoccimarro, E
Shaevitz, D
Vidale, PL
Wang, H
Wehner, M
Zhao, M
AF Daloz, Anne S.
Camargo, S. J.
Kossin, J. P.
Emanuel, K.
Horn, M.
Jonas, J. A.
Kim, D.
LaRow, T.
Lim, Y. -K.
Patricola, C. M.
Roberts, M.
Scoccimarro, E.
Shaevitz, D.
Vidale, P. L.
Wang, H.
Wehner, M.
Zhao, M.
TI Cluster Analysis of Downscaled and Explicitly Simulated North Atlantic
Tropical Cyclone Tracks
SO JOURNAL OF CLIMATE
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; GLOBAL ATMOSPHERIC MODEL; SEA-SURFACE
TEMPERATURE; AFRICAN EASTERLY WAVES; HIGH-RESOLUTION; CLIMATE MODELS;
CMIP5 MODELS; INTENSITY; FREQUENCY; GCM
AB A realistic representation of the North Atlantic tropical cyclone tracks is crucial as it allows, for example, explaining potential changes in U.S. landfalling systems. Here, the authors present a tentative study that examines the ability of recent climate models to represent North Atlantic tropical cyclone tracks. Tracks from two types of climate models are evaluated: explicit tracks are obtained from tropical cyclones simulated in regional or global climate models with moderate to high horizontal resolution (1 degrees-0.25 degrees), and downscaled tracks are obtained using a downscaling technique with large-scale environmental fields from a subset of these models. For both configurations, tracks are objectively separated into four groups using a cluster technique, leading to a zonal and a meridional separation of the tracks. The meridional separation largely captures the separation between deep tropical and subtropical, hybrid or baroclinic cyclones, while the zonal separation segregates Gulf of Mexico and Cape Verde storms. The properties of the tracks' seasonality, intensity, and power dissipation index in each cluster are documented for both configurations. The authors' results show that, except for the seasonality, the downscaled tracks better capture the observed characteristics of the clusters. The authors also use three different idealized scenarios to examine the possible future changes of tropical cyclone tracks under 1) warming sea surface temperature, 2) increasing carbon dioxide, and 3) a combination of the two. The response to each scenario is highly variable depending on the simulation considered. Finally, the authors examine the role of each cluster in these future changes and find no preponderant contribution of any single cluster over the others.
C1 [Daloz, Anne S.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53704 USA.
[Camargo, S. J.; Kim, D.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Kossin, J. P.] NOAA Natl Climat Data Ctr, Asheville, NC USA.
[Emanuel, K.] MIT, Cambridge, MA 02139 USA.
[Horn, M.] Univ Melbourne, Sch Earth, Melbourne, Vic, Australia.
[Jonas, J. A.] Columbia Univ, Ctr Climate Syst, New York, NY USA.
[Jonas, J. A.; Lim, Y. -K.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Jonas, J. A.; Lim, Y. -K.] NASA Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res IM Syst Grp, Greenbelt, MD USA.
[LaRow, T.] Florida State Univ, Tallahassee, FL 32306 USA.
[Patricola, C. M.] Texas A&M Univ, College Stn, TX USA.
[Roberts, M.] Met Off Hadley Ctr, Exeter, Devon, England.
[Scoccimarro, E.] Ist Nazl Geofis & Vulcanol, Bologna, Italy.
[Scoccimarro, E.] Ctr Euromediterraneo Cambiamenti Climat, Lecce, Italy.
[Shaevitz, D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Vidale, P. L.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Wang, H.] NOAA NWS NCEP Climate Predict Ctr, College Pk, MD USA.
[Wang, H.] Innovim LLC, Greenbelt, MD USA.
[Wehner, M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Wehner, M.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Zhao, M.] NOAA Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Daloz, AS (reprint author), Univ Wisconsin, Space Sci & Engn Ctr, 1225 West Dayton St,11th Floor, Madison, WI 53704 USA.
EM adaloz@wisc.edu
RI Camargo, Suzana/C-6106-2009; Zhao, Ming/C-6928-2014; Kossin,
James/C-2022-2016; Patricola, Christina/L-9902-2016;
OI Camargo, Suzana/0000-0002-0802-5160; Kossin, James/0000-0003-0461-9794;
Patricola, Christina/0000-0002-3387-0307; Vidale, Pier
Luigi/0000-0002-1800-8460
FU NOAA [NA11OAR4310093]; NSF [AGS1143959]; NASA [NNX09AK34G]; Regional and
Global Climate Modeling Program of the Office of Biological and
Environmental Research in the Department of Energy Office of Science
[DE-AC02-05CH11231]
FX We acknowledge support from NOAA Grant NA11OAR4310093, NSF Grant
AGS1143959, and NASA Grant NNX09AK34G. The data were provided by the
U.S. CLIVAR Hurricane Working Group. We thank Naomi Henderson for her
support with the U.S. CLIVAR Hurricane Working Group dataset. Wehner was
supported by the Regional and Global Climate Modeling Program of the
Office of Biological and Environmental Research in the Department of
Energy Office of Science under Contract DE-AC02-05CH11231. CAM5
calculations were performed at the National Energy Research
Supercomputing Center (NERSC) at the Lawrence Berkeley National
Laboratory. We also would like to thank the three anonymous reviewers
for their helpful comments.
NR 89
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD FEB
PY 2015
VL 28
IS 4
BP 1333
EP 1361
DI 10.1175/JCLI-D-13-00646.1
PG 29
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB5LX
UT WOS:000349670000001
ER
PT J
AU Kubar, TL
Stephens, GL
Lebsock, M
Larson, VE
Bogenschutz, PA
AF Kubar, Terence L.
Stephens, Graeme L.
Lebsock, Matthew
Larson, Vincent E.
Bogenschutz, Peter A.
TI Regional Assessments of Low Clouds against Large-Scale Stability in CAM5
and CAM-CLUBB Using MODIS and ERA-Interim Reanalysis Data
SO JOURNAL OF CLIMATE
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; PROBABILITY DENSITY-FUNCTIONS; ORDER
TURBULENCE CLOSURE; BOUNDARY-LAYER CLOUDS; CLIMATE SIMULATIONS; SHALLOW
CONVECTION; VOCALS-REX; PART I; STRATOCUMULUS; CUMULUS
AB Daily gridded cloud data from MODIS and ERA- Interim reanalysis have been assessed to examine variations of low cloud fraction (CF) and cloud-top height and their dependence on large-scale dynamics and a measure of stability. To assess the stratocumulus (Sc) to cumulus (Cu) transition (STCT), the observations are used to evaluate two versions of the NCAR Community Atmosphere Model version 5 (CAM5), both the base model and a version that has implemented a new subgrid low cloud parameterization, Cloud Layers Unified by Binormals (CLUBB).
The ratio of moist static energy (MSE) at 700-1000 hPa (MSEtotal) is a skillful predictor of median CF of screened low cloud grids. Values of MSEtotal less than 1.00 represent either conditionally or absolutely unstable layers, and probability density functions of CF suggest a preponderance of either trade Cu (median CF < 0.4) or transitional Sc clouds (0.4 < CF < 0.9). With increased stability (MSEtotal > 1.00), an abundance of overcast or nearly overcast low clouds exists. While both MODIS and ERA-Interim indicate a fairly smooth transition between the low cloud regimes, CAM5-Base simulates an abrupt shift from trade Cu to Sc, with trade Cu covering both too much area and occurring over excessively strong stabilities. In contrast, CAM-CLUBB simulates a smoother trade Cu to Sc transition (CTST) as a function of MSEtotal, albeit with too extensive coverage of overcast Sc in the primary northeastern Pacific subsidence region. While the overall CF distribution in CAM-CLUBB is more realistic, too few transitional clouds are simulated for intermediate MSEtotal compared to observations.
C1 [Kubar, Terence L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Stephens, Graeme L.; Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Larson, Vincent E.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Bogenschutz, Peter A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Kubar, TL (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM terry.kubar@jpl.nasa.gov
FU National Science Foundation [AGS-098643, AGS-0968640]; National
Aeronautics and Space Administration
FX T. K. acknowledges support from the National Science Foundation Grant
AGS-098643. V. E. Larson acknowledges support from the National Science
Foundation under Grant AGS-0968640. 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 also thank Dr. Andrew Gettelman for
beneficial feedback of the manuscript, as well as Dr. Feiquin Xie for
his instructive dialogue about evaluation of boundary layer cloud
heights. Finally, the authors are grateful to the thorough comments from
three anonymous reviewers, which have significantly improved the content
and readability of this manuscript.
NR 36
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U1 3
U2 13
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD FEB
PY 2015
VL 28
IS 4
BP 1685
EP 1706
DI 10.1175/JCLI-D-14-00184.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB5LX
UT WOS:000349670000020
ER
PT J
AU Glotch, TD
Bandfield, JL
Lucey, PG
Hayne, PO
Greenhagen, BT
Arnold, JA
Ghent, RR
Paige, DA
AF Glotch, Timothy D.
Bandfield, Joshua L.
Lucey, Paul G.
Hayne, Paul O.
Greenhagen, Benjamin T.
Arnold, Jessica A.
Ghent, Rebecca R.
Paige, David A.
TI Formation of lunar swirls by magnetic field standoff of the solar wind
SO NATURE COMMUNICATIONS
LA English
DT Article
ID SURFACE-ROUGHNESS; THERMAL EMISSION; MOON; MERCURY; RADIOMETER; SPECTRA
AB Lunar swirls are high-albedo markings on the Moon that occur in both mare and highland terrains; their origin remains a point of contention. Here, we use data from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer to support the hypothesis that the swirls are formed as a result of deflection of the solar wind by local magnetic fields. Thermal infrared data from this instrument display an anomaly in the position of the silicate Christiansen Feature consistent with reduced space weathering. These data also show that swirl regions are not thermophysically anomalous, which strongly constrains their formation mechanism. The results of this study indicate that either solar wind sputtering and implantation are more important than micrometeoroid bombardment in the space-weathering process, or that micrometeoroid bombardment is a necessary but not sufficient process in space weathering, which occurs on airless bodies throughout the solar system.
C1 [Glotch, Timothy D.; Arnold, Jessica A.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Bandfield, Joshua L.] Space Sci Inst, Boulder, CO 80301 USA.
[Lucey, Paul G.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Hayne, Paul O.; Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ghent, Rebecca R.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada.
[Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Glotch, TD (reprint author), SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
EM timothy.glotch@stonybrook.edu
RI Greenhagen, Benjamin/C-3760-2016
FU Diviner Lunar Radiometer Experiment extended mission science
investigation; Remote, In Situ, and Synchrotron Studies
(RIS4E) team of NASA's Solar System Research Virtual
Institute (SSERVI)
FX Funding for this work was provided by the Diviner Lunar Radiometer
Experiment extended mission science investigation and the Remote, In
Situ, and Synchrotron Studies (RIS4E) team of NASA's Solar
System Research Virtual Institute (SSERVI). This is SSERVI publication
number SSERVI-2014-158.
NR 44
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U1 1
U2 13
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 FEB
PY 2015
VL 6
AR 6189
DI 10.1038/ncomms7189
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CC2UI
UT WOS:000350199700005
PM 25650225
ER
PT J
AU Konishi, M
Shibai, H
Sumi, T
Fukagawa, M
Matsuo, T
Samland, MS
Yamamoto, K
Sudo, J
Itoh, Y
Arimoto, N
Kajisawa, M
Abe, L
Brandner, W
Brandt, TD
Carson, J
Currie, T
Egner, SE
Feldt, M
Goto, M
Grady, CA
Guyon, O
Hashimoto, J
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kudo, T
Kusakabe, N
Kuzuhara, M
Kwon, J
McElwain, MW
Miyama, S
Morino, J
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, H
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Usuda, T
Watanabe, M
Wisniewski, JP
Yamada, T
Tamura, M
AF Konishi, Mihoko
Shibai, Hiroshi
Sumi, Takahiro
Fukagawa, Misato
Matsuo, Taro
Samland, Matthias S.
Yamamoto, Kodai
Sudo, Jun
Itoh, Yoichi
Arimoto, Nobuo
Kajisawa, Masaru
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Grady, Carol A.
Guyon, Olivier
Hashimoto, Jun
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Kuzuhara, Masayuki
Kwon, Jungmi
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
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Usuda, Tomonori
Watanabe, Makoto
Wisniewski, John P.
Yamada, Toru
Tamura, Motohide
TI Indications of M-dwarf deficits in the halo and thick disk of the Galaxy
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE Galaxy: disk; Galaxy: halo; stars: imaging; stars: low-mass
ID MASS BROWN DWARFS; SKY STAR COUNT; MILKY-WAY; ULTRACOOL DWARFS; COOL
NEIGHBORS; LUMINOSITY-FUNCTION; MAIN-SEQUENCE; DEEP FIELD; WHOLE SKY;
PLANETS
AB We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the H band is significantly smaller than the predicted number. This indicates that M-dwarfs, the major component, are fewer in the halo and the thick disk. We used archived data of several surveys in both the north and south field of GOODS (Great Observatories Origins Deep Survey), MODS (MOIRCS Deep Survey) in GOODS-N, and ERS (Early Release Science) and CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey) in GOODS-S. The number density of M-dwarfs in the halo has to be 20%+/- 13% relative to that in the solar vicinity, in order for the detected number of stars fainter than 20.5 mag in the H band to match with the predicted value from the model. In the thick disk, the number density of M-dwarfs must be reduced (52%+/- 13%) or the scale height must be decreased (similar to 600 pc). Alternatively, overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect, because our sample mainly consists of faint M-dwarfs. Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought. We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fitting number densities.
C1 [Konishi, Mihoko; Shibai, Hiroshi; Sumi, Takahiro; Fukagawa, Misato; Sudo, Jun] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Matsuo, Taro; Yamamoto, Kodai] Kyoto Univ, Fac Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Samland, Matthias S.] Heidelberg Univ, Dept Phys & Astron, D-69117 Heidelberg, Germany.
[Itoh, Yoichi] Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
[Arimoto, Nobuo; Currie, Thayne; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Ishii, Miki; Kudo, Tomoyuki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Subaru Telescope, Hilo, HI 96720 USA.
[Arimoto, Nobuo; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan.
[Kajisawa, Masaru] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06108 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, Carol A.; McElwain, Michael W.] ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Hashimoto, Jun; Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Kwon, Jungmi; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, Markus] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kuzuhara, Masayuki; Kwon, Jungmi; Takahashi, Yasuhiro H.; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Miyama, Shoken] Hiroshima Univ, Higashihiroshima, Hiroshima 7398526, Japan.
[Moro-Martin, Amaya] CSIC, CAB, INTA, Dept Astrophys, Madrid 28850, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosciences, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Konishi, M (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
EM konishi@iral.ess.sci.osaka-u.ac.jp
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
NR 56
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB
PY 2015
VL 67
IS 1
AR 1
DI 10.1093/pasj/psu125
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC1RN
UT WOS:000350120500002
ER
PT J
AU Nakano, T
Murakami, H
Makishima, K
Hiraga, JS
Uchiyama, H
Kaneda, H
Enoto, T
AF Nakano, Toshio
Murakami, Hiroaki
Makishima, Kazuo
Hiraga, Junoko S.
Uchiyama, Hideki
Kaneda, Hidehiro
Enoto, Teruaki
TI Suzaku studies of the supernova remnant CTB 109 hosting the magnetar 1E
2259+586
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM: supernova remnants; stars: magnetars; stars: magnetic fields;
stars: neutron; X-rays: individual (CTB 109, 1E 2259+586)
ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; NEUTRON-STARS; OPTICAL COUNTERPART;
PROPER MOTIONS; XMM-NEWTON; SPIN-DOWN; CANDIDATE 1E-2259+586; CTB-109
G109.1-1.0; SWIFT J1822.3-1606
AB Ages of the magnetar 1E 2259+586 and the associated supernova remnant CTB 109 were studied. Analyzing the Suzaku data of CTB 109, its age was estimated to be similar to 14 kyr, which is much younger than the measured characteristic age of 1E 2259+586, 230 kyr. This reconfirms the previously reported age discrepancy of this magnetar/remnant association, and suggests that the characteristic ages of magnetars are generally over-estimated as compared to their true ages. This discrepancy is thought to arise because the former are calculated without considering decay of the magnetic fields. This novel view is supported independently by much stronger Galactic-plane concentration of magnetars than other pulsars. The process of magnetic field decay in magnetars is mathematically modeled. It is implied that magnetars are much younger objects than previously considered, and can dominate new-born neutron stars.
C1 [Nakano, Toshio; Murakami, Hiroaki; Makishima, Kazuo] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Makishima, Kazuo] RIKEN, Inst Phys & Chem Res, MAXI Team, Wako, Saitama 3510198, Japan.
[Makishima, Kazuo; Hiraga, Junoko S.] Univ Tokyo, Res Ctr Early Univ, Bunkyo Ku, Tokyo 1130033, Japan.
[Uchiyama, Hideki] Shizuoka Univ, Fac Educ, Suruga Ku, Shizuoka 4228529, Japan.
[Kaneda, Hidehiro] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Enoto, Teruaki] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagakute, Aichi 4648602, Japan.
[Enoto, Teruaki] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan.
RP Nakano, T (reprint author), Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM nakano@juno.phys.s.u-tokyo.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU JSPS KAKENHI [12J09081]
FX This work was supported by JSPS KAKENHI Grant Number 12J09081.
NR 76
TC 4
Z9 4
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 FEB
PY 2015
VL 67
IS 1
AR 9
DI 10.1093/pasj/psu135
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC1RN
UT WOS:000350120500010
ER
PT J
AU Chronis, T
Carey, LD
Schultz, CJ
Schultz, EV
Calhoun, KM
Goodman, SJ
AF Chronis, T.
Carey, Lawrence D.
Schultz, Christopher J.
Schultz, Elise V.
Calhoun, Kristin M.
Goodman, Steven J.
TI Exploring Lightning Jump Characteristics
SO WEATHER AND FORECASTING
LA English
DT Article
DE Lightning
ID THUNDERSTORM ELECTRIFICATION; MAPPING ARRAY; SEVERE WEATHER; STORM;
ALGORITHM; PRECIPITATION; RADAR
AB This study is concerned with the characteristics of storms exhibiting an abrupt temporal increase in the total lightning flash rate [i.e., lightning jump (LJ)]. An automated storm tracking method is used to identify storm clusters and total lightning activity from three different lightning detection systems over Oklahoma, northern Alabama, and Washington, D.C. On average and for different employed thresholds, the clusters that encompass at least one LJ (LJ1) last longer and relate to higher maximum expected size of hail, vertical integrated liquid, and lightning flash rates (area normalized) than do the clusters without an LJ (LJ0). The respective mean radar-derived and lightning values for LJ1 (LJ0) clusters are 80 min (35 min), 14 mm (8 mm), 25 kg m(-2) (18 kg m(-2)), and 0.05 flash min(-1) km(-2) (0.01 flash min(-1) km(-2)). Furthermore, the LJ1 clusters are also characterized by slower-decaying autocorrelation functions, a result that implies a less random behavior in the temporal flash rate evolution. In addition, the temporal occurrence of the last LJ provides an estimate of the time remaining to the storm's dissipation. Depending on the LJ strength (i.e., varying thresholds), these values typically range between 20 and 60 min, with stronger jumps indicating more time until storm decay. This study's results support the hypothesis that the LJ is a proxy for the storm's kinematic and microphysical state rather than a coincidental value.
C1 [Chronis, T.; Schultz, Elise V.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
[Carey, Lawrence D.; Schultz, Christopher J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Schultz, Christopher J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Calhoun, Kristin M.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA.
[Calhoun, Kristin M.] Natl Severe Storms Lab, Norman, OK 73069 USA.
[Goodman, Steven J.] NOAA, Natl Environm Satellite Data & Informat Serv, Greenbelt, MD USA.
RP Chronis, T (reprint author), Univ Alabama, Ctr Earth Syst Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM themis.chronis@nsstc.uah.edu
FU GOES-R System Program as part of the Proving Ground and Risk Reduction
programs; UAH Individual Investigator Distinguished Research awards;
NASA Pathways Intern Program
FX We acknowledge the support by the GOES-R System Program as part of the
Proving Ground and Risk Reduction programs. The first and second authors
also acknowledge the support by the UAH Individual Investigator
Distinguished Research awards for 2014. CJS would like to acknowledge
the NASA Pathways Intern Program, which provided the funding for support
of this work. Sincere thanks to 1) Geoffrey Stano and the NASA
Short-Term Prediction Research and Transition Center (SPoRT) for the NA
LMA, 2) Earth Networks for the ENTLN data, 3) Vaisala for the NLDN data,
4) Donald R. MacGorman for the Oklahoma LMA data, and 5) Monte Bateman
for the ENTLN processing. We would also like to extend our sincere
thanks to the three anonymous reviewers who helped us improve this
paper.
NR 47
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Z9 11
U1 1
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
EI 1520-0434
J9 WEATHER FORECAST
JI Weather Forecast.
PD FEB
PY 2015
VL 30
IS 1
BP 23
EP 37
DI 10.1175/WAF-D-14-00064.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB8CU
UT WOS:000349856900003
ER
PT J
AU Zoghbi, A
Miller, JM
Walton, DJ
Harrison, FA
Fabian, AC
Reynolds, CS
Boggs, SE
Christensen, FE
Craig, W
Hailey, CJ
Stern, D
Zhang, WW
AF Zoghbi, A.
Miller, J. M.
Walton, D. J.
Harrison, F. A.
Fabian, A. C.
Reynolds, C. S.
Boggs, S. E.
Christensen, F. E.
Craig, W.
Hailey, C. J.
Stern, D.
Zhang, W. W.
TI NuSTAR REVEALS RELATIVISTIC REFLECTION BUT NO ULTRA-FAST OUTFLOW IN THE
QUASAR PG 1211+143
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars:
absorption lines; quasars: individual (PG 1211+143)
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; HOST GALAXIES; NGC
1365; DISK; LINE; MODELS; NARROW
AB We report on four epochs of observations of the quasar PG 1211+143 using NuSTAR. The net exposure time is 300 ks. Prior work on this source found suggestive evidence of an ultra-fast outflow ( UFO) in the Fe K band with a velocity of approximately 0.1c. The putative flow would carry away a high-mass flux and kinetic power, with broad implications for feedback and black hole-galaxy co-evolution. NuSTAR detects PG 1211+143 out to 30 keV, meaning that the continuum is well-defined both through and above the Fe K band. A characteristic relativistic disk reflection spectrum is clearly revealed via a broad Fe K emission line and Compton back-scattering curvature. The data offer only weak constraints on the spin of the black hole. A careful search for UFOs shows no significant absorption feature above 90% confidence. The limits are particularly tight when relativistic reflection is included. We discuss the statistics and the implications of these results in terms of connections between accretion onto quasars, Seyferts, and stellar-mass black holes, and feedback into their host environments.
C1 [Zoghbi, A.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walton, D. J.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boggs, S. E.; Craig, W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zoghbi, A (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA.
EM abzoghbi@umich.edu
RI Boggs, Steven/E-4170-2015; Zoghbi, Abderahmen/A-8445-2017
OI Boggs, Steven/0000-0001-9567-4224; Zoghbi,
Abderahmen/0000-0002-0572-9613
FU National Aeronautics and Space Administration
FX This work 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.
NR 29
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Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2015
VL 799
IS 2
AR L24
DI 10.1088/2041-8205/799/2/L24
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB0KS
UT WOS:000349315400010
ER
PT J
AU Li, JY
Cleveland, M
Ziemba, LD
Griffin, RJ
Barsanti, KC
Pankow, JF
Ying, Q
AF Li, Jingyi
Cleveland, Meredith
Ziemba, Luke D.
Griffin, Robert J.
Barsanti, Kelley C.
Pankow, James F.
Ying, Qi
TI Modeling regional secondary organic aerosol using the Master Chemical
Mechanism
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE MCMv3.2; CMAQ model; Isoprene epoxydiol; Glyoxal; Surface reactive
uptake
ID TORCH 2003 CAMPAIGN; MCM V3 PART; TROPOSPHERIC DEGRADATION;
MASS-SPECTROMETRY; MEXICO-CITY; MOLECULAR CONSTITUENTS;
AROMATIC-HYDROCARBONS; SOURCE APPORTIONMENT; ISOPRENE EPOXYDIOLS;
CONDENSED-PHASE
AB A modified near-explicit Master Chemical Mechanism (MCM, version 3.2) with 5727 species and 16,930 reactions and an equilibrium partitioning module was incorporated into the Community Air Quality Model (CMAQ) to predict the regional concentrations of secondary organic aerosol (SOA) from volatile organic compounds (VOCs) in the eastern United States (US). In addition to the semi-volatile SOA from equilibrium partitioning, reactive surface uptake processes were used to simulate SOA formation due to isoprene epoxydiol, glyoxal and methylglyoxal. The CMAQ-MCM-SOA model was applied to simulate SOA formation during a two-week episode from August 28 to September 7, 2006. The southeastern US has the highest SOA, with a maximum episode-averaged concentration of similar to 12 mu g m(-3). Primary organic aerosol (POA) and SOA concentrations predicted by CMAQ-MCM-SOA agree well with AMS-derived hydrocarbon-like organic aerosol (HOA) and oxygenated organic aerosol (OOA) urban concentrations at the Moody Tower at the University of Houston. Predicted molecular properties of SOA (O/C, H/C, N/C and OM/OC ratios) at the site are similar to those reported in other urban areas, and O/C values agree with measured O/C at the same site. Isoprene epoxydiol is predicted to be the largest contributor to total SOA concentration in the southeast US, followed by methylglyoxal and glyoxal. The semi-volatile SOA components are dominated by products from beta-caryophyllene oxidation, but the major species and their concentrations are sensitive to errors in saturation vapor pressure estimation. A uniform decrease of saturation vapor pressure by a factor of 100 for all condensable compounds can lead to a 150% increase in total SOA. A sensitivity simulation with UNIFAC-calculated activity coefficients (ignoring phase separation and water molecule partitioning into the organic phase) led to a 10% change in the predicted semivolatile SOA concentrations. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Li, Jingyi; Ying, Qi] Texas A&M Univ, Zachry Dept Civil Engn, College Stn, TX 77843 USA.
[Cleveland, Meredith] SRA Int, Washington, DC 20005 USA.
[Ziemba, Luke D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Griffin, Robert J.] Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA.
[Barsanti, Kelley C.; Pankow, James F.] Portland State Univ, Dept Civil & Environm Engn, Portland, OR 97021 USA.
RP Ying, Q (reprint author), Texas A&M Univ, Zachry Dept Civil Engn, College Stn, TX 77843 USA.
EM qying@civil.tamu.edu
FU State of Texas as part of the program of the Texas Air Research Center
[079ATM0099A, 078ATM2080A, 312ATM0126A]; Electric Power Research
Institute
FX This project has been funded with funds from the State of Texas as part
of the program of the Texas Air Research Center (Project Number
079ATM0099A, 078ATM2080A and 312ATM0126A). Support was also provided by
the Electric Power Research Institute. The contents do not necessarily
reflect the views and policies of the sponsors, nor does the mention of
trade names or commercial projects constitute endorsement or
recommendation for use. The authors would like to acknowledge the Texas
A&M Supercomputing Facility (http://sc.tamu.edu) and the Texas Advanced
Computing Center (TACC) at The University of Texas at Austin
(http://www.tacc.utexas.edu) for providing computing resources useful in
conducting the research reported in this paper. The authors would also
like to thank the two anonymous reviewers for their valuable comments
and suggestions.
NR 60
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Z9 12
U1 16
U2 92
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 FEB
PY 2015
VL 102
BP 52
EP 61
DI 10.1016/j.atmosenv.2014.11.054
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CB4IB
UT WOS:000349590300006
ER
PT J
AU Li, J
Carlson, BE
Lacis, AA
AF Li, Jing
Carlson, Barbara E.
Lacis, Andrew A.
TI How well do satellite AOD observations represent the spatial and
temporal variability of PM2.5 concentration for the United States?
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE PM2; Aerosol optical depth; Satellite remote sensing; Principal
component analysis; Spatial and temporal variability
ID AEROSOL OPTICAL DEPTH; COMPARE SPATIOTEMPORAL VARIABILITY;
SPECTRAL-ANALYSIS TECHNIQUES; GROUND-LEVEL PM2.5; AIR-QUALITY;
PARTICULATE MATTER; RETRIEVALS; SURFACE; MODIS; LAND
AB Due to their extensive spatial coverage, satellite Aerosol Optical Depth (AOD) observations have been widely used to estimate and predict surface PM2.5 concentrations. While most previous studies have focused on establishing relationships between collocated, hourly or daily AOD and PM2.5 measurements, in this study, we instead focus on the comparison of the large-scale spatial and temporal variability between satellite AOD and PM2.5 using monthly mean measurements. A newly developed spectral analysis technique Combined Maximum Covariance Analysis (CMCA) is applied to Moderate Resolution Imaging Spectroradiometer (MODIS), Multi-angle Imaging Spectroradiometer (MISR), Sea-viewing Wide Field-of-view Sensor (SeaWiFS) and Ozone Monitoring Instrument (OMI) AOD datasets and Environmental Protection Agency (EPA) PM2.5 data, in order to extract and compare the dominant modes of variability. Results indicate that AOD and PM2.5 agree well in terms of interannual variability. An overall decrease is found in both AOD and PM2.5 across the United States, with the strongest signal over the eastern US. With respect to seasonality, good agreement is found only for Eastern US, while for Central and Western US, AOD and PM2.5 seasonal cycles are largely different or even reversed. These results are verified using Aerosol Robotic Network (AERONET) AOD observations and differences between satellite and AERONET are also examined. MODIS and MISR appear to have the best agreement with AERONET. In order to explain the disagreement between AOD and PM2.5 seasonality, we further use Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) extinction profile data to investigate the effect of two possible contributing factors, namely aerosol vertical distribution and cloud-free sampling. We find that seasonal changes in aerosol vertical distribution, due to the seasonally varying mixing height, is the primary cause for the AOD and PM2.5 seasonal discrepancy, in particular, the low AOD but high PM2.5 observed during the winter season for Central and Western US. In addition, cloud-free sampling by passive sensors also induces some bias in AOD seasonality, especially for the Western US, where the largest seasonal change in cloud fraction is found. The seasonal agreement between low level (below 500 m AGL), all sky CALIOP AOD and PM2.5 is significantly better than column AOD from MODIS, MISR, SeaWiFS and OMI. In particular, the correlation between low level, all sky AOD and PM2.5 seasonal cycles increases to above 0.7 for Central and Western US, as opposed to near zero or negative correlation for column, clear sky AOD. This result highlights the importance of accounting for the seasonally varying aerosol profiles and cloud-free sampling bias when using column AOD measurements to infer surface PM2.5 concentrations. (C) 2014 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-SA license (http://creativecommons.org/licenses/by-nc-sat3.0/).
C1 [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Li, Jing] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
RP Li, J (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM Jing.li@nasa.gov
OI Li, Jing/0000-0002-0540-0412
FU NASA [509496.02.08.04.24]
FX The authors thank the MODIS, MISR, SeaWiFS and OMI aerosol retrieval
team for providing the satellite used in this study. We also thank the
AERONET team and EPA for providing the ground based AOD and
PM2.5 data. The CALIOP data is provide by the NASA Langley
Atmospheric Science Data Center. This study is funded by NASA climate
grant 509496.02.08.04.24. Jing Li also acknowledge Hal Maring and the
NASA Radiation Science program for providing funding for this
investigation.
NR 64
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U1 3
U2 56
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 FEB
PY 2015
VL 102
BP 260
EP 273
DI 10.1016/j.atmosenv.2014.12.010
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CB4IB
UT WOS:000349590300029
ER
PT J
AU Thomas, N
Lucas, R
Itoh, T
Simard, M
Fatoyinbo, L
Bunting, P
Rosenqvist, A
AF Thomas, Nathan
Lucas, Richard
Itoh, Takuya
Simard, Marc
Fatoyinbo, Lola
Bunting, Peter
Rosenqvist, Ake
TI An approach to monitoring mangrove extents through time-series
comparison of JERS-1 SAR and ALOS PALSAR data
SO WETLANDS ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Remote sensing; Radar; Mangroves; Change
ID REMOTE-SENSING TECHNIQUES; COASTAL VEGETATION; ELEVATION DATA;
FRENCH-GUIANA; RADAR DATA; FORESTS; AQUACULTURE; ECOSYSTEMS; BIOMASS;
ICESAT/GLAS
AB Between 2007 and 2010, Japan's Advanced Land Observing Satellite (ALOS) Phased Arrayed L-band Synthetic Aperture Radar (PALSAR) captured dual polarization HH and HV data across the tropics and sub-tropics. A pan tropical dataset of Japanese Earth Resources Satellite (JERS-1) SAR (HH) data was also acquired between 1995 and 1998. The provision of these comparable cloud-free datasets provided an opportunity for observing changes in the extent of coastal mangroves over more than a decade. Focusing on nine sites distributed through the tropics, this paper demonstrates how these data can be used to backdate and update existing baseline maps of mangrove extent. The benefits of integrating dense time-series of Landsat sensor data for both validating assessments of change and determining the causes of change are outlined. The approach is evaluated for wider application across the geographical range of mangroves in order to advance the development of JAXA's Global Mangrove Watch (GMW) program.
C1 [Thomas, Nathan; Bunting, Peter] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Ceredigion, Wales.
[Lucas, Richard] Univ New S Wales, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia.
[Itoh, Takuya] Remote Sensing Technol Ctr Japan RESTEC, Minato Ku, Tokyo 1060032, Japan.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 90039 USA.
[Fatoyinbo, Lola] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Rosenqvist, Ake] Solo Earth Observat soloEO, Chuo Ku, Tokyo 1040054, Japan.
RP Lucas, R (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, High St, Kensington, NSW 2052, Australia.
EM richard.lucas@unsw.edu.au
RI Fatoyinbo, Temilola/G-6104-2012; Simard, Marc/H-3516-2013; Bunting,
Pete/B-8678-2013
OI Fatoyinbo, Temilola/0000-0002-1130-6748; Simard,
Marc/0000-0002-9442-4562; Bunting, Pete/0000-0002-7435-0148
FU Japanese Space Exploration Agency
FX Japanese Space Exploration Agency.
NR 47
TC 0
Z9 0
U1 3
U2 24
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-4861
EI 1572-9834
J9 WETL ECOL MANAG
JI Wetl. Ecol. Manag.
PD FEB
PY 2015
VL 23
IS 1
SI SI
BP 3
EP 17
DI 10.1007/s11273-014-9370-6
PG 15
WC Environmental Sciences; Water Resources
SC Environmental Sciences & Ecology; Water Resources
GA CB4OL
UT WOS:000349607200002
ER
PT J
AU Ho, JC
AF Ho, Jimmy C.
TI Stiffness Constants of Homogeneous, Anisotropic, Prismatic Beams
SO AIAA JOURNAL
LA English
DT Article
ID SECTIONAL ANALYSIS; COMPOSITE BEAMS
AB This paper presents a complete set of analytical expressions for the stiffness constants of a generalized Euler-Bernoulli beam theory for homogeneous, anisotropic, prismatic beams with arbitrary cross-sectional shapes. These expressions are extracted from exact solutions of the linear equations of three-dimensional elasticity for the cases of loading by axial forces, torques, and bending moments about two orthogonal directions. Closed-form expressions are derived for the extensional stiffness and the extension-related coupling terms. Expressions for the remaining stiffness constants are derived in terms of the torsional stiffness: the expression of which is in terms of a function that needs to be obtained. The resulting expressions reveal both similarities and differences from its isotropic and orthotropic counterparts. For elliptical, anisotropic cross sections and rectangular, orthotropic cross sections, all stiffness constants are known in closed form. These closed-form expressions constitute a standard with which the ability of two-dimensional beam cross-sectional analyses to model material anisotropy may be assessed. The calculated stiffness constants, from one such cross-sectional analysis, are successfully validated in this manner.
C1 Sci & Technol Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ho, JC (reprint author), Sci & Technol Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jimmy.c.ho2.ctr@mail.mil
NR 14
TC 0
Z9 0
U1 1
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD FEB
PY 2015
VL 53
IS 2
BP 473
EP 478
DI 10.2514/1.J053194
PG 6
WC Engineering, Aerospace
SC Engineering
GA CB1DA
UT WOS:000349365700018
ER
PT J
AU Golbabaei-Asl, M
Knight, D
Wilkinson, S
AF Golbabaei-Asl, Mona
Knight, Doyle
Wilkinson, Stephen
TI Novel Technique to Determine SparkJet Efficiency
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 51st AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 06-11, 2013
CL Grapevine, TX
SP AIAA
ID DISCHARGE PLASMA; DRAG REDUCTION; HIGH-SPEED; AERODYNAMICS
C1 [Golbabaei-Asl, Mona; Knight, Doyle] Rutgers State Univ, New Brunswick, NJ 08903 USA.
[Wilkinson, Stephen] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA.
RP Golbabaei-Asl, M (reprint author), Rutgers State Univ, New Brunswick, NJ 08903 USA.
NR 8
TC 8
Z9 8
U1 0
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 FEB
PY 2015
VL 53
IS 2
BP 501
EP +
DI 10.2514/1.J053034
PG 4
WC Engineering, Aerospace
SC Engineering
GA CB1DA
UT WOS:000349365700022
ER
PT J
AU Reichardt, J
Reichardt, S
Hostetler, CA
Lucker, PL
McGee, TJ
Twigg, LW
Dornbrack, A
Schoeberl, MR
Yang, P
AF Reichardt, Jens
Reichardt, Susanne
Hostetler, Chris A.
Lucker, Patricia L.
McGee, Thomas J.
Twigg, Laurence W.
Doernbrack, Andreas
Schoeberl, Mark R.
Yang, Ping
TI Mother-of-pearl cloud particle size and composition from aircraft-based
photography of coloration and lidar measurements
SO APPLIED OPTICS
LA English
DT Article
ID POLAR STRATOSPHERIC CLOUDS; NITRIC-ACID TRIHYDRATE; LIQUID PARTICLES;
ICE CRYSTALS; MODEL; IRIDESCENCE; SCATTERING; MICROPHYSICS; SIMULATION;
DYNAMICS
AB During a Stratospheric Aerosol and Gas (SAGE)-III Ozone Loss and Validation Experiment (SOLVE)-II science flight on 4 February 2003, a mother-of-pearl cloud over Iceland was underflown by the NASA DC-8 and measured with the lidars onboard. In addition, color photos were taken during the approach. Aided by extensive modeling of cloud coloration, the main results of the analysis of this unique data set are: (1) the polar stratospheric cloud was mountain wave-induced and of type II; (2) the spectacular color display was caused by ice particles with sizes around 2 mu m. (C) 2014 Optical Society of America
C1 [Reichardt, Jens] Deutsch Wetterdienst, Richard Assmann Observ, D-15848 Lindenberg, Germany.
[Reichardt, Susanne] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Hostetler, Chris A.] NASA, Langley Res Ctr, Sci Directorate, Climate Sci Branch, Hampton, VA 23681 USA.
[Lucker, Patricia L.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[McGee, Thomas J.; Schoeberl, Mark R.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
[Twigg, Laurence W.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Doernbrack, Andreas] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, D-82234 Wessling, Germany.
[Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Reichardt, J (reprint author), Deutsch Wetterdienst, Richard Assmann Observ, Observ 12, D-15848 Lindenberg, Germany.
EM jens.reichardt@dwd.de
RI Yang, Ping/B-4590-2011
NR 45
TC 0
Z9 0
U1 1
U2 6
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 FEB 1
PY 2015
VL 54
IS 4
BP B140
EP B153
DI 10.1364/AO.54.00B140
PG 14
WC Optics
SC Optics
GA CA8II
UT WOS:000349161300018
PM 25967820
ER
PT J
AU Turner, W
Rondinini, C
Pettorelli, N
Mora, B
Leidner, AK
Szantoi, Z
Buchanan, G
Dech, S
Dwyer, J
Herold, M
Koh, LP
Leimgruber, P
Taubenboeck, H
Wegmann, M
Wikelski, M
Woodcock, C
AF Turner, W.
Rondinini, C.
Pettorelli, N.
Mora, B.
Leidner, A. K.
Szantoi, Z.
Buchanan, G.
Dech, S.
Dwyer, J.
Herold, M.
Koh, L. P.
Leimgruber, P.
Taubenboeck, H.
Wegmann, M.
Wikelski, M.
Woodcock, C.
TI Free and open-access satellite data are key to biodiversity conservation
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Satellite; Remote sensing; Biodiversity; Conservation; Monitoring;
Landsat
ID LANDSAT IMAGERY; COVER CHANGE; SCIENCE; OPPORTUNITIES; CHALLENGES;
SUPPORT; SYSTEM
AB Satellite remote sensing is an important tool for monitoring the status of biodiversity and associated environmental parameters, including certain elements of habitats. However, satellite data are currently underused within the biodiversity research and conservation communities. Three factors have significant impact on the utility of remote sensing data for tracking and understanding biodiversity change. They are its continuity, affordability, and access. Data continuity relates to the maintenance of long-term satellite data products. Such products promote knowledge of how biodiversity has changed over time and why. Data affordability arises from the cost of the imagery. New data policies promoting free and open access to government satellite imagery are expanding the use of certain imagery but the number of free and open data sets remains too limited. Data access addresses the ability of conservation biologists and biodiversity researchers to discover, retrieve, manipulate, and extract value from satellite imagery as well as link it with other types of information. Tools are rapidly improving access. Still, more cross-community interactions are necessary to strengthen ties between the biodiversity and remote sensing communities. (C) 2014 Published by Elsevier Ltd.
C1 [Turner, W.; Leidner, A. K.] NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA.
[Rondinini, C.] Univ Roma La Sapienza, Dept Biol & Biotechnol, Rome, Italy.
[Pettorelli, N.] Zool Soc London, Inst Zool, London, England.
[Mora, B.; Herold, M.] GOFC GOLD Land Cover Off, Wageningen, Netherlands.
[Leidner, A. K.] Univ Space Res Assoc, Houston, TX USA.
[Szantoi, Z.] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, Land Resources Management Unit, Ispra, Italy.
[Buchanan, G.] Royal Soc Protect Birds, Ctr Conservat Sci, Sandy, Beds, England.
[Dech, S.; Taubenboeck, H.] German Aerosp Ctr DLR, German Remote Sensing Data Ctr, Cologne, Germany.
[Dwyer, J.] US Geol Survey, Earth Resources Observat & Sci Ctr, Reston, VA USA.
[Koh, L. P.] Univ Adelaide, Inst Environm, Adelaide, SA 5005, Australia.
[Leimgruber, P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Wegmann, M.] Univ Wurzburg, German Aerosp Ctr DLR, CEOS Biodivers German Remote Sensing Data Ctr, Wurzburg, Germany.
[Wegmann, M.] Univ Wurzburg, Dept Remote Sensing, Wurzburg, Germany.
[Wikelski, M.] Univ Konstanz, Max Planck Inst Ornithol, Constance, Germany.
[Wikelski, M.] Univ Konstanz, Dept Biol, Constance, Germany.
[Woodcock, C.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
RP Turner, W (reprint author), NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA.
EM woody.turner@nasa.gov
RI Koh, Lian Pin/A-5794-2010; Trivedi, Kruti/E-7558-2015; Herold,
Martin/F-8553-2012; Leimgruber, Peter/O-1304-2015;
OI Koh, Lian Pin/0000-0001-8152-3871; Herold, Martin/0000-0003-0246-6886;
Leimgruber, Peter/0000-0002-3682-0153; Dwyer, John/0000-0002-8281-0896;
Szantoi, Zoltan/0000-0003-2580-4382
NR 25
TC 26
Z9 30
U1 6
U2 33
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
EI 1873-2917
J9 BIOL CONSERV
JI Biol. Conserv.
PD FEB
PY 2015
VL 182
BP 173
EP 176
DI 10.1016/j.biocon.2014.11.048
PG 4
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CB3AY
UT WOS:000349501400022
ER
PT J
AU Johnson-Roberson, M
Bryson, M
Douillard, B
Pizarro, O
Williams, SB
AF Johnson-Roberson, Matthew
Bryson, Mitch
Douillard, Bertrand
Pizarro, Oscar
Williams, Stefan B.
TI Discovering salient regions on 3D photo-textured maps: Crowdsourcing
interaction data from multitouch smartphones and tablets
SO COMPUTER VISION AND IMAGE UNDERSTANDING
LA English
DT Article
DE Crowdsourcing; Visual saliency; 3D maps; Multitouch interaction; HMM;
Gaze-tracking; Smartphones; Mobile devices
ID VISUAL-ATTENTION; RECOGNITION; ALGORITHMS; OBJECTS; MODELS
AB This paper presents a system for crowdsourcing saliency interest points for 3D photo-textured maps rendered on smartphones and tablets. An app was created that is capable of interactively rendering 3D reconstructions gathered with an Autonomous Underwater Vehicle. Through hundreds of thousands of logged user interactions with the models we attempt to data-mine salient interest points. To this end we propose two models for calculating saliency from human interaction with the data. The first uses the view frustum of the camera to track the amount of time points are on screen. The second uses the velocity of the camera as an indicator of saliency and uses a Hidden Markov model to learn the classification of salient and non-salient points. To provide a comparison to existing techniques several traditional visual saliency approaches are applied to orthographic views of the models' photo-texturing. The results of all approaches are validated with human attention ground truth gathered using a remote gaze-tracking system that recorded the locations of the person's attention while exploring the models. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Johnson-Roberson, Matthew] Univ Michigan, Ann Arbor, MI 48109 USA.
[Douillard, Bertrand] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
[Bryson, Mitch; Pizarro, Oscar; Williams, Stefan B.] Univ Sydney, Australian Ctr Field Robot, Sydney, NSW 2006, Australia.
RP Johnson-Roberson, M (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM mattjr@umich.edu; m.bryson@acfr.usyd.edu.au;
Bertrand.Douillard@jpl.nasa.gov; o.pizar-ro@acfr.usyd.edu.au;
stefanw@acfr.usyd.edu.au
OI Williams, Stefan/0000-0001-9416-5639
FU New South Wales State Government; Integrated Marine Observing System
(IMOS) through the DIISR National Collaborative Research Infrastructure
Scheme
FX This work is supported by the New South Wales State Government and the
Integrated Marine Observing System (IMOS) through the DIISR National
Collaborative Research Infrastructure Scheme. The authors of this work
would like to thank the Australian Institute for Marine Science and the
Tasmanian Aquaculture and Fisheries Institute (TAFI) for making ship
time available to support this study. The crews of the R/V Solander and
R/V Challenger were instrumental in facilitating successful deployment
and recovery of the AUV. We also acknowledge the help of all those who
have contributed to the development and operation of the AUV, Ian Mahon,
Stephen Barkby, Ritesh Lal, Paul Rigby, Jeremy Randle, Bruce Crundwell
and the late Alan Trinder, Duncan Mercer and George Powell. We also
thank Bryce Barlow for his help with running experiments.
NR 73
TC 1
Z9 1
U1 2
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1077-3142
EI 1090-235X
J9 COMPUT VIS IMAGE UND
JI Comput. Vis. Image Underst.
PD FEB
PY 2015
VL 131
BP 28
EP 41
DI 10.1016/j.cviu.2014.07.006
PG 14
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA CB4HN
UT WOS:000349588900003
ER
PT J
AU Ashley, JW
AF Ashley, James W.
TI THE STUDY OF EXOGENIC ROCKS ON MARS-AN EVOLVING SUBDISCIPLINE IN
METEORITICS
SO ELEMENTS
LA English
DT Editorial Material
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ashley, JW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.w.ashley@ipl.nasa.gov
NR 16
TC 1
Z9 1
U1 0
U2 0
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 1811-5209
EI 1811-5217
J9 ELEMENTS
JI Elements
PD FEB
PY 2015
VL 11
IS 1
BP 10
EP 11
PG 2
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CB5ES
UT WOS:000349650900003
ER
PT J
AU Grotzinger, JP
Crisp, JA
Vasavada, AR
AF Grotzinger, John P.
Crisp, Joy A.
Vasavada, Ashwin R.
CA MSL Sci Team
TI Curiosity's Mission of Exploration at Gale Crater, Mars
SO ELEMENTS
LA English
DT Article
DE Mars; Gale Crater; water; geochemistry; mineralogy; habitability
ID ROCKNEST; ORIGIN; ROCKS
AB Landed missions to the surface of Mars have long sought to determine the material properties of rocks and soils encountered during the course of surface exploration. Increasingly, emphasis is placed on the study of materials formed or altered in the presence of liquid water. Placed in the context of their geological environment, these materials are then used to help evaluate ancient habitability. The Mars Science Laboratory mission-with its Curiosity rover-seeks to establish the availability of elements that may have fueled microbial metabolism, including carbon, hydrogen, sulfur, nitrogen, phosphorus, and a host of others at the trace element level. These measurements are most valuable when placed in a geological framework of ancient environments as interpreted from mapping, combined with an understanding of the petrogenesis of the igneous rocks and derived sedimentary materials. In turn, the analysis of solid materials and the reconstruction of ancient environments provide the basis to assess past habitability.
C1 [Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Crisp, Joy A.; Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Grotzinger, JP (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM grotz@gps.caltech.edu
RI Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi, Jose/L-8001-2014;
Crisp, Joy/H-8287-2016; Ramos, Miguel/K-2230-2014
OI Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Crisp,
Joy/0000-0002-3202-4416; Ramos, Miguel/0000-0003-3648-6818
FU National Aeronautics and Space Administration
FX We are indebted to the Mars Science Laboratory Project engineering and
science teams for their exceptionally skilled and diligent efforts in
making the mission as effective as possible and enhancing science
operations. The manuscript was reviewed by Gordon Brown, Paul Mahaffy,
and Dave Vaniman, and help with figures was provided by Mike Baker, Fred
Calef, Caroline Freissinet, Jen Griffes Shechet, Scott McLennan, Ralph
Milliken, Kirsten Siebach, and Dave Vaniman. Some of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. Data presented in this paper, and in others of this
issue, are archived in the Planetary Data System (pds.nasa.gov).
NR 29
TC 6
Z9 6
U1 6
U2 43
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 1811-5209
EI 1811-5217
J9 ELEMENTS
JI Elements
PD FEB
PY 2015
VL 11
IS 1
BP 19
EP 26
DI 10.2113/gselements.11.1.19
PG 8
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CB5ES
UT WOS:000349650900006
ER
PT J
AU Mahaffy, PR
Conrad, PG
AF Mahaffy, Paul R.
Conrad, Pamela G.
CA MSL Sci Team
TI Volatile and Isotopic Imprints of Ancient Mars
SO ELEMENTS
LA English
DT Article
DE Mars; organics; Gale Crater; isotopes; habitability; Curiosity rover
ID MARTIAN ATMOSPHERE; NOBLE-GASES; ORIGIN; EVOLUTION; RATIOS; CURIOSITY;
WATER; SOIL
AB The science investigations enabled by Curiosity rover's Instruments focus on identifying and exploring the habitability of the Martian environment. Measurements of noble gases, organic and inorganic compounds, and the isotopes of light elements permit the study of the physical and chemical processes that have transformed Mars throughout its history. Samples of the atmosphere, volatiles released from soils, and rocks from the floor of Gale Crater have provided a wealth of new data and a window into conditions on ancient Mars.
C1 [Mahaffy, Paul R.; Conrad, Pamela G.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
RP Mahaffy, PR (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
EM Paul.R.Mahaffy@NASA.gov; pamela.g.conrad@nasa.gov
RI Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi, Jose/L-8001-2014;
Ramos, Miguel/K-2230-2014
OI Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Ramos,
Miguel/0000-0003-3648-6818
NR 31
TC 4
Z9 4
U1 5
U2 24
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 1811-5209
EI 1811-5217
J9 ELEMENTS
JI Elements
PD FEB
PY 2015
VL 11
IS 1
BP 51
EP 56
DI 10.2113/gselements.11.1.51
PG 6
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CB5ES
UT WOS:000349650900011
ER
PT J
AU Perdomo-Ortiz, A
Fluegemann, J
Narasimhan, S
Biswas, R
Smelyanskiy, VN
AF Perdomo-Ortiz, A.
Fluegemann, J.
Narasimhan, S.
Biswas, R.
Smelyanskiy, V. N.
TI A quantum annealing approach for fault detection and diagnosis of
graph-based systems
SO EUROPEAN PHYSICAL JOURNAL-SPECIAL TOPICS
LA English
DT Review
ID ISING SPIN-GLASS; ADIABATIC EVOLUTION; MODELS; OPTIMIZATION; COMPUTATION
AB Diagnosing the minimal set of faults capable of explaining a set of given observations, e.g., from sensor readouts, is a hard combinatorial optimization problem usually tackled with artificial intelligence techniques. We present the mapping of this combinatorial problem to quadratic unconstrained binary optimization (QUBO), and the experimental results of instances embedded onto a quantum annealing device with 509 quantum bits. Besides being the first time a quantum approach has been proposed for problems in the advanced diagnostics community, to the best of our knowledge this work is also the first research utilizing the route Problem -> QUBO -> Direct embedding into quantum hardware, where we are able to implement and tackle problem instances with sizes that go beyond previously reported toy-model proof-of-principle quantum annealing implementations; this is a significant leap in the solution of problems via direct-embedding adiabatic quantum optimization. We discuss some of the programmability challenges in the current generation of the quantum device as well as a few possible ways to extend this work to more complex arbitrary network graphs.
C1 [Perdomo-Ortiz, A.; Fluegemann, J.; Biswas, R.; Smelyanskiy, V. N.] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
[Perdomo-Ortiz, A.; Narasimhan, S.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Fluegemann, J.] San Jose State Res Fdn, 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.
EM alejandro.perdomoortiz@nasa.gov
FU AFRL Information Directorate [F4HBKC4162G001]; NASA Advanced Exploration
Systems program; NASA Ames Research Center
FX This work was supported by the AFRL Information Directorate under grant
F4HBKC4162G001. All opinions, findings, conclusions, and recommendations
expressed in this material are those of the authors and do not
necessarily reflect the views of AFRL. The authors would also like to
acknowledge support from the NASA Advanced Exploration Systems program
and NASA Ames Research Center.
NR 41
TC 12
Z9 12
U1 2
U2 9
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1951-6355
EI 1951-6401
J9 EUR PHYS J-SPEC TOP
JI Eur. Phys. J.-Spec. Top.
PD FEB
PY 2015
VL 224
IS 1
BP 131
EP 148
DI 10.1140/epjst/e2015-02347-y
PG 18
WC Physics, Multidisciplinary
SC Physics
GA CB2GZ
UT WOS:000349446400012
ER
PT J
AU O'Gorman, B
Babbush, R
Perdomo-Ortiz, A
Aspuru-Guzik, A
Smelyanskiy, V
AF O'Gorman, B.
Babbush, R.
Perdomo-Ortiz, A.
Aspuru-Guzik, A.
Smelyanskiy, V.
TI Bayesian network structure learning using quantum annealing
SO EUROPEAN PHYSICAL JOURNAL-SPECIAL TOPICS
LA English
DT Review
ID COMPUTATION; LATTICE; MODEL
AB We introduce a method for the problem of learning the structure of a Bayesian network using the quantum adiabatic algorithm. We do so by introducing an efficient reformulation of a standard posterior-probability scoring function on graphs as a pseudo-Boolean function, which is equivalent to a system of 2-body Ising spins, as well as suitable penalty terms for enforcing the constraints necessary for the reformulation; our proposed method requires oe"(n (2)) qubits for n Bayesian network variables. Furthermore, we prove lower bounds on the necessary weighting of these penalty terms. The logical structure resulting from the mapping has the appealing property that it is instance-independent for a given number of Bayesian network variables, as well as being independent of the number of data cases.
C1 [O'Gorman, B.; Perdomo-Ortiz, A.; Smelyanskiy, V.] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
[O'Gorman, B.; Babbush, R.; Aspuru-Guzik, A.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
RP O'Gorman, B (reprint author), NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
EM vadim.n.smelyanskiy@nasa.gov
FU AFRL Information Directorate [F4HBKC4162G001]; NASA Advanced Exploration
Systems program; NASA Ames Research Center; National Science Foundation
[NSF CHE-1152291]
FX This work was supported by the AFRL Information Directorate under grant
F4HBKC4162G001. All opinions, findings, conclusions, and recommendations
expressed in this material are those of the authors and do not
necessarily reflect the views of AFRL. The authors would also like to
acknowledge support from the NASA Advanced Exploration Systems program
and NASA Ames Research Center. R. B. and A. A.-G. were supported by the
National Science Foundation under award NSF CHE-1152291. The authors are
grateful to David Tempel, Ole Mengshoel, and Eleanor Rieffel for useful
discussions.
NR 36
TC 10
Z9 10
U1 5
U2 14
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1951-6355
EI 1951-6401
J9 EUR PHYS J-SPEC TOP
JI Eur. Phys. J.-Spec. Top.
PD FEB
PY 2015
VL 224
IS 1
BP 163
EP 188
DI 10.1140/epjst/e2015-02349-9
PG 26
WC Physics, Multidisciplinary
SC Physics
GA CB2GZ
UT WOS:000349446400014
ER
PT J
AU Barmatz, MB
Jackson, HW
Javeed, AS
Jamieson, CS
Steinfeld, DE
AF Barmatz, Martin B.
Jackson, Henry W.
Javeed, Aurya S.
Jamieson, Corey S.
Steinfeld, David E.
TI An Accurate Radially Stratified Approach for Determining the Complex
Permittivity of Liquids in a Cylindrical Microwave Cavity
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Article
DE Cavity perturbation; microwave; permittivity measurement; radially
stratified approach; resonant cylindrical cavity; wall losses
ID DIELECTRIC LOSS MEASUREMENTS; NONPOLAR LIQUIDS; REGION; GHZ
AB A complex permittivity measurement method is introduced that is applicable to radially stratified resonant microwave cavities excited by a TM0m0 eigenmode. This single-frequency approach is well suited to the measurement of the complex permittivity of liquids because it can accurately account for a supporting tube container. It can also be applied advantageously to solid rods or tubes. The frequency dependence, as well as the field configuration at the cavity walls are taken into account more accurately than in other approaches. Comparing our results with published measurements of well-known liquids validates this technique.
C1 [Barmatz, Martin B.; Steinfeld, David E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Javeed, Aurya S.] Cornell Univ, Ctr Appl Math, Ithaca, NY 14853 USA.
[Jamieson, Corey S.] SETI Inst, Mountain View, CA 94043 USA.
RP Barmatz, MB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM b.barmatz@jpl.nasa.gov; hw-jackson2@gmail.com; aj463@cornell.edu;
cjamieson@seti.org; David.E.Steinfeld@jpl.nasa.gov
FU NASA
FX The work, carried out at the Jet Propulsion Laboratory, California
Institute of Technology, was supported by NASA under a contract with
NASA. Copyright 2014.
NR 14
TC 1
Z9 1
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
EI 1557-9670
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD FEB
PY 2015
VL 63
IS 2
BP 504
EP 508
DI 10.1109/TMTT.2014.2387057
PN 1
PG 5
WC Engineering, Electrical & Electronic
SC Engineering
GA CB4UI
UT WOS:000349623300020
ER
PT J
AU Druyan, LM
Fulakeza, M
AF Druyan, Leonard M.
Fulakeza, Matthew
TI The impact of the Atlantic cold tongue on West African monsoon onset in
regional model simulations for 1998-2002
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Article
DE West African monsoon onset; Atlantic cold tongue; regional climate model
ID SEASONAL EVOLUTION; CLIMATE; VARIABILITY; RESOLUTION; PARAMETERIZATION;
SENSITIVITY; REANALYSIS; NCEP
AB The Atlantic cold tongue (ACT) develops during spring and early summer near the Equator in the Eastern Atlantic Ocean and Gulf of Guinea. The hypothesis that the ACT accelerates the timing of West African monsoon (WAM) onset is tested by comparing two regional climate model (RM3) simulation ensembles. Observed sea surface temperatures (SST) that include the ACT are used to force a control ensemble. An idealized, warm SST perturbation is designed to represent lower boundary forcing without the ACT for the experiment ensemble. Summer simulations forced by observed SST and reanalysis boundary conditions for each of five consecutive years are compared to five parallel runs forced by SST with the warm perturbation. The article summarizes the sequence of events leading to the onset of the WAM in the Sahel region. The representation of WAM onset in RM3 simulations is examined and compared to Tropical Rainfall Measuring Mission (TRMM), Global Precipitation Climatology Project (GPCP) and reanalysis data. The study evaluates the sensitivity of WAM onset indicators to the presence of the ACT by analysing the differences between the two simulation ensembles. Results show that the timing of major rainfall events and therefore the WAM onset in the Sahel are not sensitive to the presence of the ACT. However, the warm SST perturbation does increase downstream rainfall rates over West Africa as a consequence of enhanced specific humidity and enhanced northward moisture flux in the lower troposphere.
C1 [Druyan, Leonard M.; Fulakeza, Matthew] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
[Druyan, Leonard M.; Fulakeza, Matthew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Druyan, LM (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10027 USA.
EM ld12@columbia.edu
FU US National Science Foundation [AGS-10000874]; NASA [NNX11AR63A]
FX This research was supported by US National Science Foundation Grant
AGS-10000874 and the NASA Cooperative Agreement NNX11AR63A. TRMM data
were acquired using the GES-DISC Interactive Online Visualization and
Analysis Infrastructure (Giovanni), part of NASA's Goddard Earth
Sciences (GES) Data and Information Services Center (DISC). GPCP data
were obtained from NASA/GSFC/MAPL. NCEP/DOE reanalysis 2 data used in
the study were obtained from the NOAA-ESRL Physical Sciences Division,
Boulder CO online from www.esrl.noaa.gov/psd. The authors gratefully
acknowledge the constructive suggestions of two anonymous reviewers.
NR 29
TC 3
Z9 3
U1 0
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
EI 1097-0088
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD FEB
PY 2015
VL 35
IS 2
BP 275
EP 287
DI 10.1002/joc.3980
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB5JP
UT WOS:000349663600009
ER
PT J
AU Loikith, PC
Waliser, DE
Lee, H
Kim, J
Neelin, JD
Lintner, BR
McGinnis, S
Mattmann, CA
Mearns, LO
AF Loikith, Paul C.
Waliser, Duane E.
Lee, Huikyo
Kim, Jinwon
Neelin, J. David
Lintner, Benjamin R.
McGinnis, Seth
Mattmann, Chris A.
Mearns, Linda O.
TI Surface Temperature Probability Distributions in the NARCCAP Hindcast
Experiment: Evaluation Methodology, Metrics, and Results
SO JOURNAL OF CLIMATE
LA English
DT Article
ID REGIONAL CLIMATE MODEL; NORTH-AMERICA; SOIL-MOISTURE; DENSITY-FUNCTIONS;
DAILY MAXIMUM; HEAT WAVES; EXTREMES; PRECIPITATION; VARIABILITY;
REANALYSIS
AB Methodology is developed and applied to evaluate the characteristics of daily surface temperature distributions in a six-member regional climate model (RCM) hindcast experiment conducted as part of the North American Regional Climate Change Assessment Program (NARCCAP). A surface temperature dataset combining gridded station observations and reanalysis is employed as the primary reference. Temperature biases are documented across the distribution, focusing on the median and tails. Temperature variance is generally higher in the RCMs than reference, while skewness is reasonably simulated in winter over the entire domain and over the western United States and Canada in summer. Substantial differences in skewness exist over the southern and eastern portions of the domain in summer. Four examples with observed long-tailed probability distribution functions (PDFs) are selected for model comparison. Long cold tails in the winter are simulated with high fidelity for Seattle, Washington, and Chicago, Illinois. In summer, the RCMs are unable to capture the distribution width and long warm tails for the coastal location of Los Angeles, California, while long cold tails are poorly realized for Houston, Texas. The evaluation results are repeated using two additional reanalysis products adjusted by station observations and two standard reanalysis products to assess the impact of observational uncertainty. Results are robust when compared with those obtained using the adjusted reanalysis products as reference, while larger uncertainties are introduced when standard reanalysis is employed as reference. Model biases identified in this work will allow for further investigation into associated mechanisms and implications for future simulations of temperature extremes.
C1 [Loikith, Paul C.; Waliser, Duane E.; Lee, Huikyo; Mattmann, Chris A.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Waliser, Duane E.; Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Kim, Jinwon; Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Lintner, Benjamin R.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[McGinnis, Seth; Mearns, Linda O.] Natl Ctr Atmospher Res, Inst Math Applicat Geosci, Boulder, CO 80307 USA.
RP Loikith, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM paul.c.loikith@jpl.nasa.gov
OI McGinnis, Seth/0000-0001-8082-834X
FU NASA National Climate Assessment [11-NCA11-0028]; AIST
[AIST-QRS-12-0002]; NSF [Ex Arch 1125798]; NOAA [NA11OAR4310099]
FX Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Part of this research was funded
by NASA National Climate Assessment 11-NCA11-0028 and AIST
AIST-QRS-12-0002 projects and the NSF Ex Arch 1125798 (P.C.L., J.K.,
H.L., D.E.W., C.M.). Part of this research was funded by NOAA
NA11OAR4310099 (J.D.N.). We thank Jonathan Hobbs for his valuable advice
during this work. We also thank the NARCCAP team for production of the
model simulations and archiving of the data.
NR 58
TC 6
Z9 6
U1 4
U2 14
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 FEB 1
PY 2015
VL 28
IS 3
BP 978
EP 997
DI 10.1175/JCLI-D-13-00457.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA9WJ
UT WOS:000349275200005
ER
PT J
AU Muller, CL
Baker, A
Fairchild, IJ
Kidd, C
Boomer, I
AF Muller, Catherine L.
Baker, Andy
Fairchild, Ian J.
Kidd, Chris
Boomer, Ian
TI Intra-Event Trends in Stable Isotopes: Exploring Midlatitude
Precipitation Using a Vertically Pointing Micro Rain Radar
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID WATER-VAPOR; FLUORESCENCE SPECTROPHOTOMETRY; VARIABILITY; DELTA-O-18;
RAINWATER; MODEL; STORM; AUSTRALIA; DEUTERIUM
AB Annual, monthly, and daily analyses of stable isotopes in precipitation are commonly made worldwide, yet only a few studies have explored the variations occurring on short time scales within individual precipitation events, particularly at midlatitude locations. This study examines hydrogen isotope data from sequential, intra-event samples from 16 precipitation events during different seasons and a range of synoptic conditions over an 18-month period in Birmingham, United Kingdom. Precipitation events were observed simultaneously using a vertically pointing micro rain radar (MRR), which, for the first time at a midlatitude location, allowed high-resolution examination of the microphysical characteristics (e.g., rain rate, fall velocity, and drop size distributions) that may influence the local isotopic composition of rainwater. The range in the hydrogen isotope ratio (delta D, where D refers to deuterium) in 242 samples during 16 events was from -87.0 parts per thousand to +9.2 parts per thousand, while the largest variation observed in a single event was 55.4 parts per thousand. In contrast to previous work, the results indicate that some midlatitude precipitation events do indeed show significant intra-event trends that are strongly influenced by precipitation processes and parameters such as rain rate, melting-level height, and droplet sizes. Inverse relationships between rain rate and isotopic composition are observed, representing an example of a local type of "amount effect," a still poorly understood process occurring at different scales. For these particular events, the mean delta value may therefore not provide all the relevant information. This work has significance for the testing and development of isotope-enabled cloud-resolving models and land surface models at higher resolutions, and it provides improved insights into a range of environmental processes that are influenced by subsampled precipitation events.
C1 [Muller, Catherine L.; Fairchild, Ian J.; Boomer, Ian] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham, W Midlands, England.
[Baker, Andy] Univ New S Wales, Connected Waters Initiat Res Ctr, Sydney, NSW 2052, Australia.
[Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kidd, Chris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Baker, A (reprint author), Univ New S Wales, Connected Waters Initiat Res Ctr, Sydney, NSW 2052, Australia.
EM a.baker@unsw.edu.au
RI Boomer, Ian/C-5154-2009; Muller, Catherine L./E-9744-2011;
OI Muller, Catherine L./0000-0002-5176-5949; Fairchild,
Ian/0000-0003-4822-2895; Baker, Andy/0000-0002-1552-6166
FU University of Birmingham; Phillip Leverhulme Prize
FX Catherine Muller would like to thank the University of Birmingham for
financial support during this research. Andy Baker was supported by a
Phillip Leverhulme Prize. We thank Anne Ankcorn for her assistance with
sketching the schematic diagram in Fig. 1 and Guillaume Bertrand and the
two other anonymous reviewers for their comments, which have been
incorporated within this manuscript.
NR 59
TC 3
Z9 3
U1 5
U2 15
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 FEB
PY 2015
VL 16
IS 1
BP 194
EP 213
DI 10.1175/JHM-D-14-0038.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB1DR
UT WOS:000349367500014
ER
PT J
AU McNally, A
Husak, GJ
Brown, M
Carroll, M
Funk, C
Yatheendradas, S
Arsenault, K
Peters-Lidard, C
Verdin, JP
AF McNally, Amy
Husak, Gregory J.
Brown, Molly
Carroll, Mark
Funk, Chris
Yatheendradas, Soni
Arsenault, Kristi
Peters-Lidard, Christa
Verdin, James P.
TI Calculating Crop Water Requirement Satisfaction in the West Africa Sahel
with Remotely Sensed Soil Moisture
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SATELLITE ESTIMATED RAINFALL; LAND-SURFACE MODELS; DROUGHT;
EVAPOTRANSPIRATION; PRECIPITATION; ASSIMILATION; SYSTEM; MAIZE;
RETRIEVALS; SIMULATION
AB The Soil Moisture Active Passive (SMAP) mission will provide soil moisture data with unprecedented accuracy, resolution, and coverage, enabling models to better track agricultural drought and estimate yields. In turn, this information can be used to shape policy related to food and water from commodity markets to humanitarian relief efforts. New data alone, however, do not translate to improvements in drought and yield forecasts. New tools will be needed to transform SMAP data into agriculturally meaningful products. The objective of this study is to evaluate the possibility and efficiency of replacing the rainfall-derived soil moisture component of a crop water stress index with SMAP data. The approach is demonstrated with 0.1 degrees-resolution, similar to 10-day microwave soil moisture from the European Space Agency and simulated soil moisture from the Famine Early Warning Systems Network Land Data Assimilation System. Over a West Africa domain, the approach is evaluated by comparing the different soil moisture estimates and their resulting Water Requirement Satisfaction Index values from 2000 to 2010. This study highlights how the ensemble of indices performs during wet versus dry years, over different land-cover types, and the correlation with national-level millet yields. The new approach is a feasible and useful way to quantitatively assess how satellite-derived rainfall and soil moisture track agricultural water deficits. Given the importance of soil moisture in many applications, ranging from agriculture to public health to fire, this study should inspire other modeling communities to reformulate existing tools to take advantage of SMAP data.
C1 [McNally, Amy; Husak, Gregory J.; Funk, Chris] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[McNally, Amy; Husak, Gregory J.; Funk, Chris] Univ Calif Santa Barbara, Climate Hazards Grp, Santa Barbara, CA 93106 USA.
[McNally, Amy; Yatheendradas, Soni] Univ Maryland, ESSIC, College Pk, MD 20740 USA.
[McNally, Amy; Yatheendradas, Soni; Arsenault, Kristi; Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Carroll, Mark] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Brown, Molly] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Funk, Chris] Univ Calif Santa Barbara, US Geol Survey, Santa Barbara, CA 93106 USA.
[Arsenault, Kristi] SAIC Inc, Beltsville, MD USA.
[Verdin, James P.] US Geol Survey, Ctr Earth Resources Observat Sci, Sioux Falls, SD USA.
RP McNally, A (reprint author), Univ Maryland, ESSIC, 5825 Univ Res Ctr 4001, College Pk, MD 20740 USA.
EM amy.l.mcnally@nasa.gov
RI Peters-Lidard, Christa/E-1429-2012; Brown, Molly/E-2724-2010
OI Peters-Lidard, Christa/0000-0003-1255-2876; Brown,
Molly/0000-0001-7384-3314
FU USGS [G09AC000001]; NASA [NN10AN26I]; Center for Scientific Computing at
the CNSI [DMR-1121053]; NSF [CNS-0960316]; Center for Scientific
Computing at MRL [DMR-1121053]
FX This work was supported USGS Cooperative Agreement G09AC000001
"Monitoring and Forecasting Climate, Water and Land Use for Food
Production in the Developing World," with funding from the NASA Applied
Sciences Program, Award NN10AN26I for "A Land Data Assimilation System
for Famine Early Warning." We acknowledge support from the Center for
Scientific Computing at the CNSI and MRL for NSF MRSEC (DMR-1121053) and
NSF CNS-0960316. The authors thank Laura Harrison for assistance with
WRSI inputs; Pete Peterson for rainfall analysis; and Shraddhanand
Shukla, Libby White, and three anonymous reviewers for their helpful
comments.
NR 51
TC 5
Z9 5
U1 5
U2 32
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 FEB
PY 2015
VL 16
IS 1
BP 295
EP 305
DI 10.1175/JHM-D-14-0049.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB1DR
UT WOS:000349367500020
ER
PT J
AU Draper, C
Reichle, R
De Lannoy, G
Scarino, B
AF Draper, Clara
Reichle, Rolf
De Lannoy, Gabrielle
Scarino, Benjamin
TI A Dynamic Approach to Addressing Observation-Minus-Forecast Bias in a
Land Surface Skin Temperature Data Assimilation System
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID ENSEMBLE KALMAN FILTER; SOIL-MOISTURE; PREDICTION SYSTEM; SATELLITE
DATA; MODEL; RADIATION
AB In land data assimilation, bias in the observation-minus-forecast (O - F) residuals is typically removed from the observations prior to assimilation by rescaling the observations to have the same long-term mean (and higher-order moments) as the corresponding model forecasts. Such observation rescaling approaches require a long record of observed and forecast estimates and an assumption that the O - F residuals are stationary. A two-stage observation bias and state estimation filter is presented here, as an alternative to observation rescaling that does not require a long data record or assume stationary O - F residuals. The two-stage filter removes dynamic (nonstationary) estimates of the seasonal-scale mean O - F difference from the assimilated observations, allowing the assimilation to correct the model for subseasonal-scale errors without adverse effects from observation biases. The two-stage filter is demonstrated by assimilating geostationary skin temperature T-skin observations into the Catchment land surface model. Global maps of the estimated O - F biases are presented, and the two-stage filter is evaluated for one year over the Americas. The two-stage filter effectively removed the TskinO - F mean differences, for example, the Geostationary Operational Environmental Satellite (GOES)-West O - F mean difference at 2100 UTC was reduced from 5.1 K for a bias-blind assimilation to 0.3 K. Compared to independent in situ and remotely sensed T-skin observations, the two-stage assimilation reduced the unbiased root-mean-square difference (ubRMSD) of the modeled T-skin by 10% of the open-loop values.
C1 [Draper, Clara; Reichle, Rolf; De Lannoy, Gabrielle] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Draper, Clara; De Lannoy, Gabrielle] Univ Space Res Assoc, Columbia, MD USA.
[Scarino, Benjamin] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Draper, C (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM clara.draper@nasa.gov
RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016
OI Draper, Clara/0000-0002-8299-4939
FU NASA Modeling, Analysis, and Prediction program; NASA High-End Computing
program; NASA Satellite Calibration Interconsistency program
FX The research was supported by the NASA Modeling, Analysis, and
Prediction program, the NASA High-End Computing program, and the NASA
Satellite Calibration Interconsistency program. MODIS land surface data
were provided by NASA's Earth Observing System Data and Information
System, and the SURFRAD data were provided by the NOAA Earth System
Research Laboratory.
NR 39
TC 5
Z9 5
U1 2
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 FEB
PY 2015
VL 16
IS 1
BP 449
EP 464
DI 10.1175/JHM-D-14-0087.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB1DR
UT WOS:000349367500030
ER
PT J
AU Moran, MS
Doorn, B
Escobar, V
Brown, ME
AF Moran, M. Susan
Doorn, Bradley
Escobar, Vanessa
Brown, Molly E.
TI Connecting NASA Science and Engineering with Earth Science Applications
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SOIL-MOISTURE DATA; PASSIVE SMAP MISSION; ASSIMILATION; SATELLITE;
RAINFALL; DROUGHT
AB The National Research Council (NRC) recently highlighted the dual role of NASA to support both science and applications in planning Earth observations. This article reports the efforts of the NASA Applied Sciences Program and NASA Soil Moisture Active Passive (SMAP) mission to integrate applications with science and engineering in prelaunch planning. The SMAP Early Adopter program supported the prelaunch applied research that comprises the SMAP Special Collection of the Journal of Hydrometeorology. This research, in turn, has resulted in unprecedented prelaunch preparation for SMAP applications and critical feedback to the mission to improve product specifications and distribution for postlaunch applications. These efforts have been a learning experience that should provide direction for upcoming missions and set some context for the next NRC decadal survey.
C1 [Moran, M. Susan] USDA, ARS, Southwest Watershed Res Ctr, Tucson, AZ 85719 USA.
[Doorn, Bradley] NASA, Appl Sci Program, Washington, DC 20546 USA.
[Escobar, Vanessa] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Moran, MS (reprint author), USDA ARS, Southwest Watershed Res Ctr, 2000 E Allen Rd, Tucson, AZ 85719 USA.
EM susan.moran@ars.usda.gov
RI Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314
FU NASA [08-SMAPSDT08-0042]
FX This work has been supported in part by NASA (08-SMAPSDT08-0042), and
many ideas have been clarified though discussions with the NASA ASP
Applied Sciences Advisory Group (ASAG). The SMAP Early Adopter program
was a mission-wide effort by the SMAP project, NASA Headquarters, and
the SMAP Science Team.
NR 21
TC 2
Z9 2
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2015
VL 16
IS 1
BP 473
EP 483
DI 10.1175/JHM-D-14-0093.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB1DR
UT WOS:000349367500032
ER
PT J
AU Creager, C
Johnson, K
Plant, M
Moreland, S
Skonieczny, K
AF Creager, Colin
Johnson, Kyle
Plant, Mark
Moreland, Scott
Skonieczny, Krzysztof
TI Push-pull locomotion for vehicle extrication
SO JOURNAL OF TERRAMECHANICS
LA English
DT Article
DE Mobility; Articulation; Extrication; Sinkage; Entrapment; Locomotion;
Thrust; Wheel slip
AB For applications in which unmanned vehicles must traverse unfamiliar terrain, there often exists the risk of vehicle entrapment. Typically, this risk can be reduced by using feedback from on-board sensors that assess the terrain. This work addressed the situations where a vehicle has already become immobilized or the desired route cannot be traversed using conventional rolling. Specifically, the focus was on using push pull locomotion in high sinkage granular material. Push pull locomotion is an alternative mode of travel that generates thrust through articulated motion, using vehicle components as anchors to push or pull against. It has been revealed through previous research that push pull locomotion has the capacity for generating higher net traction forces than rolling, and a unique optical flow technique indicated that this is the result of a more efficient soil shearing method. It has now been found that push pull locomotion results in less sinkage, lower travel reduction, and better power efficiency in high sinkage material as compared to rolling. Even when starting from an "entrapped" condition, push pull locomotion was able to extricate the test vehicle. It is the authors' recommendation that push pull locomotion be considered as a reliable back-up mode of travel for applications where terrain entrapment is a possibility. Published by Elsevier Ltd. on behalf of ISTVS.
C1 [Creager, Colin; Johnson, Kyle] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Plant, Mark] Youngstown State Univ, Youngstown, OH 44555 USA.
[Moreland, Scott] NASA, Jet Prop Lab, Pasadena, CA 91011 USA.
[Skonieczny, Krzysztof] Concordia Univ, Montreal, PQ H4B 1R6, Canada.
RP Creager, C (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM colin.m.creager@nasa.gov; kyle.a.johnson@nasa.gov; maplant@ysu.edu;
scott.j.moreland@jpl.nasa.gov; kskoniec@encs.concordia.ca
NR 14
TC 0
Z9 0
U1 2
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4898
EI 1879-1204
J9 J TERRAMECHANICS
JI J. Terramech.
PD FEB
PY 2015
VL 57
BP 71
EP 80
DI 10.1016/j.jterra.2014.12.001
PG 10
WC Engineering, Environmental
SC Engineering
GA CB1ZK
UT WOS:000349426300005
ER
PT J
AU Wang, CX
Yang, P
Liu, X
AF Wang, Chenxi
Yang, Ping
Liu, Xu
TI A High-Spectral-Resolution Radiative Transfer Model for Simulating Multi
layered Clouds and Aerosols in the Infrared Spectral Region
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID PART I; OPTICAL-PROPERTIES; DELTA-4-STREAM APPROXIMATION;
SUCCESSIVE-ORDER; LIGHT-SCATTERING; DOUBLING METHOD; ICE CRYSTALS;
RETRIEVAL; CIRRUS; MODIS
AB A fast and flexible model is developed to simulate the transfer of thermal infrared radiation at wave-numbers from 700 to 1300 cm(-1) with a spectral resolution of 0.1 cm(-1) for scattering-absorbing atmospheres. In a single run and at multiple user-defined levels, the present model simulates radiances at different viewing angles and fluxes. Furthermore, the model takes into account complicated and realistic scenes in which ice cloud, water cloud, and mineral dust layers may coexist within an atmospheric column. The present model is compared to a rigorous reference model, the 32-stream Discrete Ordinate Radiative Transfer model (DISORT) code. For an atmosphere with three scattering layers (water, ice, and mineral dust), the rootmean-square error of the simulated brightness temperatures at the top of the atmosphere is approximately 0.05 K, and the relative flux errors at the boundary and internal levels are much smaller than 1%. Within the same computing environment, the fast model runs more than 10000, 6000, and 4000 times faster than DISORT under single-layer, two-layer, and three-layer cloud-aerosol conditions, respectively. With its computational efficiency and accuracy, the present model may optimally facilitate the forward radiative transfer simulations involved in remote sensing implementations based on high-spectral-resolution and narrowband infrared measurements and in the data assimilation applications of the weather forecasting system. The selected 0.1-cm(-1) spectral resolution is an obstacle to extending the present model to strongly absorptive bands (e.g., 600-700 cm(-1)). However, the present clear-sky module can be substituted by a more accurate model for specific applications involving spectral bands with strong absorption.
C1 [Wang, Chenxi; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Liu, Xu] NASA Langley Res Ctr, Sci Directorate, Hampton, VA USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM pyang@tamu.edu
RI Yang, Ping/B-4590-2011; Richards, Amber/K-8203-2015
FU NASA [NNX12AL90G, NNX11AK37G]
FX This study was partly supported by NASA grants (NNX12AL90G and
NNX11AK37G) and the endowment funds related to the David Bullock Harris
Chair in Geosciences at the College of Geosciences, Texas A&M
University.
NR 81
TC 0
Z9 0
U1 1
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 FEB
PY 2015
VL 72
IS 2
BP 926
EP 942
DI 10.1175/JAS-D-14-0046.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA5NU
UT WOS:000348955900025
ER
PT J
AU Koshak, WJ
Solakiewicz, RJ
Peterson, HS
AF Koshak, William J.
Solakiewicz, Richard J.
Peterson, Harold S.
TI A Return Stroke NOx Production Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID NUMERICAL-CALCULATION; OPTICAL RADIATION; THUNDERSTORMS; CHANNEL; ENERGY
AB A model is introduced for estimating the nitrogen oxides (NOx = NO + NO2) production from a lightning return stroke channel. A realistic modified transmission line model return stroke current is assumed to propagate vertically upward along a stepped leader channel of 0.1-cm radius. With additional assumptions about the initial radial expansion rate of the channel, the full nonlinear differential equation for the return stroke channel radius r(z, t) is solved numerically using Mathematica V9.0.1.0. Channel conductivity and channel air density are adjustable constants, and the model employs typical atmospheric profiles of temperature, pressure, and density. The channel pressure is modeled by a dynamic pressure expression. Channel temperature is extracted from the pressure by a minimization technique that involves a generalized gas law appropriate for high temperatures where dissociation and ionization are important. The altitude and time variations of the channel energy density are also obtained. Three model runs, each with different input parameters, are completed. Channel radii at sea level range from about 1.7 to 6.0 cm depending on the model inputs and are in good agreement with other investigators. The NOx production from each 1-m segment of the channel is computed using conservation of energy and equilibrium freeze-out-temperature chemistry. Because the NOx per meter of channel is computed as a function of altitude, extensions of the results to tortuous and branched channels are possible and lead to preliminary estimates of total return stroke NOx. These estimates are found to be smaller than the return stroke NOx values obtained from the NASA Lightning Nitrogen Oxides Model (LNOM).
C1 [Koshak, William J.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Solakiewicz, Richard J.] Chicago State Univ, Chicago, IL USA.
[Peterson, Harold S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Koshak, WJ (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Off, Mail Stop ZP11,320 Sparkman Dr, Huntsville, AL 35805 USA.
EM william.koshak@nasa.gov
FU NASA Marshall Space Flight Center Science Innovation Fund
FX This research has been supported by the NASA Marshall Space Flight
Center Science Innovation Fund, under the direction of the MSFC Science
and Technology Office Chief Scientist Dr. Melissa Mcgrath. We are
grateful to Dr. Mcgrath and Dr. Michael Lapointe of the National Space
Science and Technology Center for their helpful guidance and
encouragement throughout the term of this effort. In addition, we give
special thanks to the manager of the Earth Science Office at MSFC, Dr.
James Smoot, for his continued support and guidance during all phases of
this work.
NR 38
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U1 0
U2 8
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 FEB
PY 2015
VL 72
IS 2
BP 943
EP 954
DI 10.1175/JAS-D-14-0121.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA5NU
UT WOS:000348955900026
ER
PT J
AU Coy, L
Pawson, S
AF Coy, Lawrence
Pawson, Steven
TI The Major Stratospheric Sudden Warming of January 2013: Analyses and
Forecasts in the GEOS-5 Data Assimilation System
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID VARIATIONAL STATISTICAL-ANALYSIS; RECURSIVE FILTERS; NUMERICAL ASPECTS;
PART I; WAVES; CLIMATOLOGY; COVARIANCES; MODEL; PROPAGATION; VARIABILITY
AB The major stratospheric sudden warming (SSW) of 6 January 2013 is examined using output from the NASA Global Modeling and Assimilation Office (GMAO) Goddard Earth Observing System version 5 (GEOS-5) near-real-time data assimilation system(DAS). GEOS-5 analyses showed that the SSW of January 2013 was a major warming by 1200 UTC 6 January, with a wave-2 vortex-splitting pattern. Upward wave activity flux from the upper troposphere (similar to 23 December 2012) displaced the; 10-hPa polar vortex off the pole in a wave-1 pattern, enabling the poleward advection of subtropical values of Ertel potential vorticity (EPV) into a developing anticyclonic circulation region. While the polar vortex subsequently split (wave-2 pattern) the wave-2 forcing [upward Eliassen-Palm (EP) flux] was smaller than what was found in recent wave-2, SSW events, with most of the forcing located in the Pacific hemisphere. Investigation of a rapidly developing tropospheric weather system over the North Atlantic on 28-29 December 2012 showed strong transient upward wave activity flux from the storm with influences up to 10 hPa; however, the Pacific hemisphere wave forcing remained dominate at this time. Results from the GEOS-5 five-day forecasts showed that the forecasts accurately predicted the major SSW of January 2013. The overall success of the 5-day forecasts provides motivation to produce regular 10-day forecasts with GEOS-5, to better support studies of stratosphere-troposphere interaction.
C1 [Coy, Lawrence; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Coy, Lawrence] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Coy, L (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
EM lawrence.coy@nasa.gov
RI Pawson, Steven/I-1865-2014
OI Pawson, Steven/0000-0003-0200-717X
FU NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center; NASA Modeling,
Analysis and Prediction (MAP) program
FX 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 work was supported by the
NASA Modeling, Analysis and Prediction (MAP) program. We strongly thank
both anonymous reviewers for their detailed comments and ideas for
improvements on this manuscript.
NR 35
TC 8
Z9 8
U1 2
U2 12
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 FEB
PY 2015
VL 143
IS 2
BP 491
EP 510
DI 10.1175/MWR-D-14-00023.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CB1XX
UT WOS:000349422400006
ER
PT J
AU Saglamyurek, E
Jin, J
Verma, VB
Shaw, MD
Marsili, F
Nam, SW
Oblak, D
Tittel, W
AF Saglamyurek, Erhan
Jin, Jeongwan
Verma, Varun B.
Shaw, Matthew D.
Marsili, Francesco
Nam, Sae Woo
Oblak, Daniel
Tittel, Wolfgang
TI Quantum storage of entangled telecom-wavelength photons in an
erbium-doped optical fibre
SO NATURE PHOTONICS
LA English
DT Article
ID MEMORY; EFFICIENCY; LEVEL
AB The realization of a future quantum Internet requires the processing and storage of quantum information at local nodes and interconnecting distant nodes using free-space and fibreoptic links(1). Quantum memories for light(2) are key elements of such quantum networks. However, to date, neither an atomic quantum memory for non- classical states of light operating at a wavelength compatible with standard telecom fibre infrastructure, nor a fibre-based implementation of a quantum memory, has been reported. Here, we demonstrate the storage and faithful recall of the state of a 1,532 nm wavelength photon entangled with a 795 nm photon, in an ensemble of cryogenically cooled erbium ions doped into a 20-m-long silica fibre, using a photon-echo quantum memory protocol. Despite its currently limited efficiency and storage time, our broadband light-matter interface brings fibre-based quantum networks one step closer to reality.
C1 [Saglamyurek, Erhan; Jin, Jeongwan; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Inst Quantum Sci & Technol, Calgary, AB T2N 1N4, Canada.
[Saglamyurek, Erhan; Jin, Jeongwan; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Verma, Varun B.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA.
[Shaw, Matthew D.; Marsili, Francesco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tittel, W (reprint author), Univ Calgary, Inst Quantum Sci & Technol, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM wtittel@ucalgary.ca
RI Tittel, Wolfgang/A-1600-2011
FU Alberta Innovates Technology Futures (AITF); National Science and
Engineering Research Council of Canada (NSERC); Defense Advanced
Research Projects Agency (DARPA) Information in a Photon (InPho)
programme
FX E.S., J.J., D.O. and W. T. thank C. Thiel, N. Sinclair, M. Hedges, T.
Lutz, K. Heshami, M. Grimau Puigiber, L. Giner, A. Croteau, C. La Mela
and V. Kiselyov for technical help and/or discussions, and acknowledge
funding through Alberta Innovates Technology Futures (AITF) and the
National Science and Engineering Research Council of Canada (NSERC). W.
T. is a senior fellow of the Canadian Institute for Advanced Research
(CIFAR). V. B. V. and S. W. N. acknowledge partial funding for detector
development from the Defense Advanced Research Projects Agency (DARPA)
Information in a Photon (InPho) programme. Part of the research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 30
TC 48
Z9 49
U1 1
U2 32
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1749-4885
EI 1749-4893
J9 NAT PHOTONICS
JI Nat. Photonics
PD FEB
PY 2015
VL 9
IS 2
BP 83
EP 87
DI 10.1038/NPHOTON.2014.311
PG 5
WC Optics; Physics, Applied
SC Optics; Physics
GA CB0YT
UT WOS:000349354300012
ER
PT J
AU Sun, Y
Bowman, KP
Genton, MG
Tokay, A
AF Sun, Ying
Bowman, Kenneth P.
Genton, Marc G.
Tokay, Ali
TI A Matern model of the spatial covariance structure of point rain rates
SO STOCHASTIC ENVIRONMENTAL RESEARCH AND RISK ASSESSMENT
LA English
DT Article
DE Covariance model; Exponential covariance; Matern covariance; Point rain
rates; Spectral model; Time scales
ID MULTIVARIATE RANDOM-FIELDS; STOCHASTIC-MODEL; GAUGE
AB It is challenging to model a precipitation field due to its intermittent and highly scale-dependent nature. Many models of point rain rates or areal rainfall observations have been proposed and studied for different time scales. Among them, the spectral model based on a stochastic dynamical equation for the instantaneous point rain rate field is attractive, since it naturally leads to a consistent space-time model. In this paper, we note that the spatial covariance structure of the spectral model is equivalent to the well-known Matern covariance model. Using high-quality rain gauge data, we estimate the parameters of the Matern model for different time scales and demonstrate that the Matern model is superior to an exponential model, particularly at short time scales.
C1 [Sun, Ying] Ohio State Univ, Dept Stat, Columbus, OH 43210 USA.
[Bowman, Kenneth P.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Genton, Marc G.] King Abdulaziz Univ Sci & Technol, CEMSE Div, Thuwal 239556900, Saudi Arabia.
[Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Genton, MG (reprint author), King Abdulaziz Univ Sci & Technol, CEMSE Div, Thuwal 239556900, Saudi Arabia.
EM sunwards@stat.osu.edu; marc.genton@kaust.edu.sa
RI Bowman, Kenneth/A-1345-2012;
OI Bowman, Kenneth/0000-0002-2667-8632; Genton, Marc
Georges/0000-0001-6467-2998; Sun, Ying/0000-0001-6703-4270
FU King Abdullah University of Science and Technology (KAUST)
[KUSC1-016-04]; Spanish Ministry of Science and Innovation - FEDER
[MTM2011-22664]
FX The research in this article was partially supported by Award No.
KUSC1-016-04 made by King Abdullah University of Science and Technology
(KAUST) and by the Spanish Ministry of Science and Innovation (Project
MTM2011-22664) which is co-funded by FEDER.
NR 25
TC 4
Z9 4
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1436-3240
EI 1436-3259
J9 STOCH ENV RES RISK A
JI Stoch. Environ. Res. Risk Assess.
PD FEB
PY 2015
VL 29
IS 2
BP 411
EP 416
DI 10.1007/s00477-014-0923-2
PG 6
WC Engineering, Environmental; Engineering, Civil; Environmental Sciences;
Statistics & Probability; Water Resources
SC Engineering; Environmental Sciences & Ecology; Mathematics; Water
Resources
GA CA5DL
UT WOS:000348928200009
ER
PT J
AU Mckay, DS
Cooper, BL
Taylor, LA
James, JT
Thomas-Keprta, K
Pieters, CM
Wentworth, SJ
Wallace, WT
Lee, TS
AF Mckay, D. S.
Cooper, B. L.
Taylor, L. A.
James, J. T.
Thomas-Keprta, K.
Pieters, C. M.
Wentworth, S. J.
Wallace, W. T.
Lee, T. S.
TI Physicochemical properties of respirable-size lunar dust
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Lunar dust; Dust toxicity; Nanophase iron; Space weathering; Lunar
gardening; Lunar samples
ID FINEST FRACTION; SOIL; TOXICITY; REGOLITH; SIMULANT; SAMPLES
AB We separated the respirable dust and other size fractions from Apollo 14 bulk sample 14003,96 in a dry nitrogen environment. While our toxicology team performed in vivo and in vitro experiments with the respirable fraction, we studied the size distribution and shape, chemistry, mineralogy, spectroscopy, iron content and magnetic resonance of various size fractions. These represent the finest-grained lunar samples ever measured for either FMR np-Fe-0 index or precise bulk chemistry, and are the first instance we know of in which SEM/TEM samples have been obtained without using liquids.
The concentration of single-domain, nanophase metallic iron (np-Fe-0) increases as particle size diminishes to 2 mu m, confirming previous extrapolations. Size-distribution studies disclosed that the most frequent particle size was in the 0.1-0.2 mu m range suggesting a relatively high surface area and therefore higher potential toxicity.
Lunar dust particles are insoluble in isopropanol but slightly soluble in distilled water (similar to 0.2 wt%/3 days). The interaction between water and lunar fines, which results in both agglomeration and partial dissolution, is observable on a macro scale over time periods of less than an hour.
Most of the respirable grains were smooth amorphous glass. This suggests less toxicity than if the grains were irregular, porous, or jagged, and may account for the fact that lunar dust is less toxic than ground quartz. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Mckay, D. S.] NASA, Johnson Space Ctr, KA, Houston, TX 77058 USA.
[Cooper, B. L.; Lee, T. S.] Hanyang Univ, Int Space Explorat Res Inst, Ansan 426791, Gyeonggi Do, South Korea.
[Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[James, J. T.] NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
[Thomas-Keprta, K.; Wentworth, S. J.] Jacobs Technol ESCG, Astromat Res Grp, Houston, TX 77258 USA.
[Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Wallace, W. T.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
RP Cooper, BL (reprint author), Hanyang Univ, Int Space Explorat Res Inst, Ansan 426791, Gyeonggi Do, South Korea.
EM bcooper108@gmail.com
FU Hanyang University Korea via the International Space Exploration
Research Institute [HY-2013-N]; NASA Lyndon B. Johnson Space Center's
Human Research Program
FX This work was supported in part by the research fund of Hanyang
University Korea (HY-2013-N) via the International Space Exploration
Research Institute. The research was conducted under the auspices of
NASA Lyndon B. Johnson Space Center's Human Research Program.
NR 64
TC 1
Z9 1
U1 2
U2 13
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 FEB-MAR
PY 2015
VL 107
BP 163
EP 176
DI 10.1016/j.actaastro.2014.10.032
PG 14
WC Engineering, Aerospace
SC Engineering
GA CA6XQ
UT WOS:000349061200013
ER
PT J
AU Wagner, S
Wie, B
Barbee, BW
AF Wagner, Sam
Wie, Bong
Barbee, Brent W.
TI Target selection for a hypervelocity asteroid intercept vehicle flight
validation mission
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Asteroids; Near-Earth objects; Planetary defense; Trajectory
optimization
ID DEFLECTION
AB Asteroids and comets have collided with the Earth in the past and will do so again in the future. Throughout Earth's history these collisions have played a significant role in shaping Earth's biological and geological histories. The planetary defense community has been examining a variety of options for mitigating the impact threat of asteroids and comets that approach or cross Earth's orbit, known as near-Earth objects (NEOs). This paper discusses the preliminary study results of selecting small (100-m class) NEO targets and mission analysis and design trade-offs for validating the effectiveness of a Hypervelocity Asteroid Intercept Vehicle (HAIV) concept, currently being investigated for a NIAC (NASA Advanced Innovative Concepts) Phase 2 study. In particular this paper will focus on the mission analysis and design for single spacecraft direct impact trajectories, as well as several mission types that enable a secondary rendezvous spacecraft to observe the HAIV impact and evaluate it's effectiveness. Published by Elsevier Ltd. on behalf of IAA.
C1 [Wagner, Sam; Wie, Bong; Barbee, Brent W.] Iowa State Univ, Asteroid Deflect Res Ctr, Dept Aerosp Engn, Ames, IA 50011 USA.
[Barbee, Brent W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barbee, BW (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM thewags@iastate.edu; bongwie@iastate.edu; brent.w.barbee@nasa.gov
NR 38
TC 2
Z9 2
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD FEB-MAR
PY 2015
VL 107
BP 247
EP 261
DI 10.1016/j.actaastro.2014.11.037
PG 15
WC Engineering, Aerospace
SC Engineering
GA CA6XQ
UT WOS:000349061200020
ER
PT J
AU Li, X
Danell, RM
Brinckerhoff, WB
Pinnick, VT
van Amerom, F
Arevalo, RD
Getty, SA
Mahaffy, PR
Steininger, H
Goesmann, F
AF Li, Xiang
Danell, Ryan M.
Brinckerhoff, William B.
Pinnick, Veronica T.
van Amerom, Friso
Arevalo, Ricardo D., Jr.
Getty, Stephanie A.
Mahaffy, Paul R.
Steininger, Harald
Goesmann, Fred
TI Detection of Trace Organics in Mars Analog Samples Containing
Perchlorate by Laser Desorption/Ionization Mass Spectrometry
SO ASTROBIOLOGY
LA English
DT Article
ID X-RAY SPECTROMETER; MARTIAN ATMOSPHERE; SOILS; CHEMISTRY; CRATER; ROCKS;
SITE
AB Evidence from recent Mars missions indicates the presence of perchlorate salts up to 1 wt % level in the near-surface materials. Mixed perchlorates and other oxychlorine species may complicate the detection of organic molecules in bulk martian samples when using pyrolysis techniques. To address this analytical challenge, we report here results of laboratory measurements with laser desorption mass spectrometry, including analyses performed on both commercial and Mars Organic Molecule Analyzer (MOMA) breadboard instruments. We demonstrate that the detection of nonvolatile organics in selected spiked mineral-matrix materials by laser desorption/ionization (LDI) mass spectrometry is not inhibited by the presence of up to 1 wt % perchlorate salt. The organics in the sample are not significantly degraded or combusted in the LDI process, and the parent molecular ion is retained in the mass spectrum. The LDI technique provides distinct potential benefits for the detection of organics in situ on the martian surface and has the potential to aid in the search for signs of life on Mars. Mars-Mass spectrometry-Search for Mars' organics-Perchlorate reduction. Astrobiology 15, 104-110.
C1 [Li, Xiang; Pinnick, Veronica T.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21228 USA.
[Danell, Ryan M.] Danell Consulting Inc, Winterville, NC USA.
[Brinckerhoff, William B.; Arevalo, Ricardo D., Jr.; Getty, Stephanie A.; Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[van Amerom, Friso] Mini Mass Consulting Inc, St Pete Beach, FL USA.
[Steininger, Harald; Goesmann, Fred] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany.
RP Li, X (reprint author), Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21228 USA.
EM shawnli@umbc.edu; william.b.brinckerhoff@nasa.gov
RI Li, Xiang/F-4539-2012; Getty, Stephanie/D-7037-2012
FU Mars Exploration Program
FX MOMA is a collaboration between NASA and ESA. Funding for MOMA-MS was
provided by the Mars Exploration Program. We also thank Dr. Daniel P.
Glavin for the valuable discussion.
NR 22
TC 3
Z9 3
U1 3
U2 30
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 FEB 1
PY 2015
VL 15
IS 2
BP 104
EP 110
DI 10.1089/ast.2014.1203
PG 7
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CB0MV
UT WOS:000349321300002
PM 25622133
ER
PT J
AU Luger, R
Barnes, R
AF Luger, R.
Barnes, R.
TI Extreme Water Loss and Abiotic O-2 Buildup on Planets Throughout the
Habitable Zones of M Dwarfs
SO ASTROBIOLOGY
LA English
DT Review
ID MAIN-SEQUENCE STARS; LOW-MASS STARS; INNER SOLAR-SYSTEM; EARTH-LIKE
PLANETS; SUPER-EARTHS; X-RAY; HYDRODYNAMIC ESCAPE; THERMAL ESCAPE; MAGMA
OCEAN; KINETIC SIMULATIONS
AB We show that terrestrial planets in the habitable zones of M dwarfs older than similar to 1 Gyr could have been in runaway greenhouses for several hundred million years following their formation due to the star's extended pre-main sequence phase, provided they form with abundant surface water. Such prolonged runaway greenhouses can lead to planetary evolution divergent from that of Earth. During this early runaway phase, photolysis of water vapor and hydrogen/oxygen escape to space can lead to the loss of several Earth oceans of water from planets throughout the habitable zone, regardless of whether the escape is energy-limited or diffusion-limited. We find that the amount of water lost scales with the planet mass, since the diffusion-limited hydrogen escape flux is proportional to the planet surface gravity. In addition to undergoing potential desiccation, planets with inefficient oxygen sinks at the surface may build up hundreds to thousands of bar of abiotically produced O-2, resulting in potential false positives for life. The amount of O-2 that builds up also scales with the planet mass; we find that O-2 builds up at a constant rate that is controlled by diffusion: similar to 5 bar/Myr on Earth-mass planets and up to similar to 25 bar/Myr on super-Earths. As a result, some recently discovered super-Earths in the habitable zone such as GJ 667Cc could have built up as many as 2000 bar of O-2 due to the loss of up to 10 Earth oceans of water. The fate of a given planet strongly depends on the extreme ultraviolet flux, the duration of the runaway regime, the initial water content, and the rate at which oxygen is absorbed by the surface. In general, we find that the initial phase of high luminosity may compromise the habitability of many terrestrial planets orbiting low-mass stars. Key Words: Astrobiology-Biosignatures-Extrasolar terrestrial planets-Habitability-Planetary atmospheres. Astrobiology 15, 119-143.
C1 [Luger, R.; Barnes, R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Luger, R.; Barnes, R.] NASA, Astrobiol Inst, Virtual Planetary Lab Lead Team, Seattle, WA USA.
RP Luger, R (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM rodluger@uw.edu
FU NASA Astrobiology Institute's Virtual Planetary Laboratory [NNA13AA93A];
ARCS Seattle chapter
FX This work was supported by the NASA Astrobiology Institute's Virtual
Planetary Laboratory under Cooperative Agreement solicitation NNA13AA93A
and by a generous fellowship from the ARCS Seattle chapter.
NR 122
TC 43
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U1 8
U2 23
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 FEB 1
PY 2015
VL 15
IS 2
BP 119
EP 143
DI 10.1089/ast.2014.1231
PG 25
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CB0MV
UT WOS:000349321300004
PM 25629240
ER
PT J
AU Brown, A
Neff, JE
Ayres, TR
Kowalski, A
Hawley, S
Berdyugina, S
Harper, GM
Korhonen, H
Piskunov, N
Saar, S
Walkowicz, L
Wells, MA
AF Brown, Alexander
Neff, James E.
Ayres, Thomas R.
Kowalski, Adam
Hawley, Suzanne
Berdyugina, Svetlana
Harper, Graham M.
Korhonen, Heidi
Piskunov, Nikolai
Saar, Steven
Walkowicz, Lucianne
Wells, Mark A.
TI SERENDIPITOUS DISCOVERY OF A DWARF NOVA IN THE KEPLER FIELD NEAR THE G
DWARF KIC 5438845
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE stars: dwarf novae; stars: individual (KIC 5438845)
ID SU UMA-TYPE; V344 LYRAE; INSTABILITY; SUPERHUMPS; OUTBURSTS; MODEL
AB The Kepler satellite provides a unique window into stellar temporal variability by observing a wide variety of stars with multi-year, near-continuous, high precision, optical photometric time series. While most Kepler targets are faint stars with poorly known physical properties, many unexpected discoveries should result from a long photometric survey of such a large area of sky. During our Kepler Guest Observer programs that monitored late-type stars for starspot and flaring variability, we discovered a previously unknown dwarf nova that lies within a few arcseconds of the mid-G dwarf star KIC 5438845. This dwarf nova underwent nine outbursts over a 4 year time span. The two largest outbursts lasted similar to 17-18 days and show strong modulations with a 110.8 minute period and a declining amplitude during the outburst decay phase. These properties are characteristic of an SU UMa-type cataclysmic variable. By analogy with other dwarf nova light curves, we associate the 110.8 minute (1.847 hr) period with the superhump period, close to but slightly longer than the orbital period of the binary. No precursor outbursts are seen before the super-outbursts and the overall super-outburst morphology corresponds to Osaki & Meyer "Case B" outbursts, which are initiated when the outer edge of the disk reaches the tidal truncation radius. "Case B" outbursts are rare within the Kepler light curves of dwarf novae. The dwarf nova is undergoing relatively slow mass transfer, as evidenced by the long intervals between outbursts, but the mass transfer rate appears to be steady, because the smaller "normal" outbursts show a strong correlation between the integrated outburst energy and the elapsed time since the previous outburst. At super-outburst maximum the system was at V similar to 18, but in quiescence it is fainter than V similar to 22, which will make any detailed quiescent follow-up of this system difficult.
C1 [Brown, Alexander; Ayres, Thomas R.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Neff, James E.; Wells, Mark A.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Kowalski, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kowalski, Adam; Hawley, Suzanne] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Berdyugina, Svetlana] Univ Freiburg, Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Harper, Graham M.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland.
[Korhonen, Heidi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Korhonen, Heidi] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Piskunov, Nikolai] Uppsala Univ, Dept Astron & Space Phys, SE-75120 Uppsala, Sweden.
[Saar, Steven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walkowicz, Lucianne] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Wells, Mark A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Brown, A (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 593 UCB, Boulder, CO 80309 USA.
EM Alexander.Brown@colorado.edu
RI Korhonen, Heidi/E-3065-2016
OI Korhonen, Heidi/0000-0003-0529-1161
FU NASA Kepler Cycle 1/2/3/4 Guest Observer grants [NNX10AC51G, NNX11AC79G,
NNX12AC85, NNX13AC31G]; GALEX Cycle 4 Guest Observer grant [NNX09AM47
G]; NSF [AST-1109695]; South Carolina Space Grant consortium; NASA
Office of Space Science [NNX13AC07 G]
FX This work was supported by NASA Kepler Cycle 1/2/3/4 Guest Observer
grants NNX10AC51G, NNX11AC79G, NNX12AC85 G, and NNX13AC31G, and GALEX
Cycle 4 Guest Observer grant NNX09AM47 G to the University of Colorado.
We acknowledge support by NSF grant AST-1109695 to the College of
Charleston, and by the South Carolina Space Grant consortium. The Kepler
data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). Support to MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX13AC07 G and by other
grants and contracts. This paper is based in part on observations
obtained with the Apache Point Observatory 3.5 m telescope, which is
owned and operated by the Astrophysical Research Consortium.
NR 16
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2015
VL 149
IS 2
AR 67
DI 10.1088/0004-6256/149/2/67
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB1BA
UT WOS:000349360200032
ER
PT J
AU De Los Reyes, MA
Ly, C
Lee, JC
Salim, S
Peeples, MS
Momcheva, I
Feddersen, J
Dale, DA
Ouchi, M
Ono, Y
Finn, R
AF De Los Reyes, Mithi A.
Ly, Chun
Lee, Janice C.
Salim, Samir
Peeples, Molly S.
Momcheva, Ivelina
Feddersen, Jesse
Dale, Daniel A.
Ouchi, Masami
Ono, Yoshiaki
Finn, Rose
TI THE RELATIONSHIP BETWEEN STELLAR MASS, GAS METALLICITY, AND STAR
FORMATION RATE FOR H-alpha-SELECTED GALAXIES AT z approximate to 0.8
FROM THE NEWH alpha SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: evolution; galaxies: fundamental
parameters; galaxies: ISM; galaxies: starburst
ID EMISSION-LINE GALAXIES; DIGITAL SKY SURVEY; SUBARU DEEP FIELD;
DISTRIBUTED ELECTRON ENERGIES; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT
GALAXIES; LYMAN-BREAK GALAXIES; FORMING GALAXIES; LUMINOSITY FUNCTION;
POPULATION SYNTHESIS
AB Using a sample of 299 H alpha-selected galaxies at z approximate to 0.8, we study the relationship between galaxy stellar mass, gasphase metallicity, and star formation rate (SFR), and compare to previous results. We use deep optical spectra obtained with the IMACS spectrograph at the Magellan telescope to measure strong oxygen lines. We combine these spectra and metallicities with (1) rest-frame UV-to-optical imaging, which allows us to determine stellar masses and dust attenuation corrections, and (2) H alpha narrowband imaging, which provides a robust measurement of the instantaneous SFR. Our sample spans stellar masses of similar to 10(9)-6 x 10(11) M-circle dot, SFRs of 0.4-270 M-circle dot yr(-1), and metal abundances of 12 + log (O/H) approximate to 8.3-9.1 (approximate to 0.4-2.6 M-circle dot). The correlations that we find between the H-alpha-based SFR and stellar mass (i.e., the star-forming "main sequence") and between the stellar mass and metallicity are both consistent with previous z similar to 1 studies of star-forming galaxies. We then study the relationship between the three properties using various plane-fitting techniques and a curve-fitting projection. In all cases, we exclude strong dependence of the M*-Z relation on SFR, but are unable to distinguish between moderate and no dependence. Our results are consistent with previous mass-metallicity-SFR studies. We check whether data set limitations may obscure a strong dependence on the SFR by using mock samples drawn from the Sloan Digital Sky Survey. These experiments reveal that the adopted signal-to-noise ratio cuts may have a significant effect on the measured dependence. Further work is needed to investigate these results, and to test whether a "fundamental metallicity relation"or a "fundamental plane"describes star-forming galaxies across cosmic time.
C1 [De Los Reyes, Mithi A.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[De Los Reyes, Mithi A.; Ly, Chun; Lee, Janice C.; Peeples, Molly S.; Feddersen, Jesse] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ly, Chun] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Salim, Samir] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Momcheva, Ivelina; Feddersen, Jesse] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Dale, Daniel A.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Ouchi, Masami; Ono, Yoshiaki] Univ Tokyo, TODIAS, Inst Phys & Math Universe, Tokyo 1138654, Japan.
[Finn, Rose] Siena Coll, Phys Dept Phys & Astron, Loudonville, NY USA.
RP De Los Reyes, MA (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM madelosr@ncsu.edu
OI Feddersen, Jesse/0000-0003-3810-3323
FU project of CFHT at the CFHT; project of CEA/DAPNIA at the CFHT; GALEX
Guest Investigator program under NASA [NNG09EG72I, NNX10AF04G]
FX This work is based on observations obtained with Mega-Prime/MegaCam, a
joint project of CFHT and CEA/DAPNIA, at the CFHT, which is operated by
the National Research Council of Canada, the Institut National des
Sciences de l'Univers of the Centre National de la Recherche
Scientifique of France, and the University of Hawaii. We thank Sebastien
Foucaud for facilitating access to publicly available CFHT u-band data
in the SXDS field, Victor Villar for providing data from his paper, and
Robert Yates for providing their best-fit projection for their local
fundamental metallicity relation. We also thank Brett A. Andrews for his
insightful comments and discussion. Our work is based in part on
observations made with the NASA's GALEX mission. We acknowledge support
for this work from the GALEX Guest Investigator program under NASA
grants NNG09EG72I and NNX10AF04G.
NR 119
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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 FEB
PY 2015
VL 149
IS 2
AR 79
DI 10.1088/0004-6256/149/2/79
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB1BA
UT WOS:000349360200044
ER
PT J
AU Everett, ME
Barclay, T
Ciardi, DR
Horch, EP
Howell, SB
Crepp, JR
Silva, DR
AF Everett, Mark E.
Barclay, Thomas
Ciardi, David R.
Horch, Elliott P.
Howell, Steve B.
Crepp, Justin R.
Silva, David R.
TI HIGH-RESOLUTION MULTI-BAND IMAGING FOR VALIDATION AND CHARACTERIZATION
OF SMALL KEPLER PLANETS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: visual; planetary systems; planets and satellites: detection;
planets and satellites: fundamental parameters; surveys; techniques:
high angular resolution
ID POTENTIAL TRANSIT SIGNALS; CANDIDATE HOST STARS; EARTH-SIZED PLANET;
ADAPTIVE OPTICS; HABITABLE ZONE; INFRARED CAMERA; INPUT CATALOG; BINARY
STARS; MISSION DATA; SYSTEMS
AB High-resolution ground-based optical speckle and near-infrared adaptive optics images are taken to search for stars in close angular proximity to host stars of candidate planets identified by the NASA Kepler Mission. Neighboring stars are a potential source of false positive signals. These stars also blend into Kepler light curves, affecting estimated planet properties, and are important for an understanding of planets in multiple star systems. Deep images with high angular resolution help to validate candidate planets by excluding potential background eclipsing binaries as the source of the transit signals. A study of 18 Kepler Object of Interest stars hosting a total of 28 candidate and validated planets is presented. Validation levels are determined for 18 planets against the likelihood of a false positive from a background eclipsing binary. Most of these are validated at the 99% level or higher, including five newly validated planets in two systems: Kepler-430 and Kepler-431. The stellar properties of the candidate host stars are determined by supplementing existing literature values with new spectroscopic characterizations. Close neighbors of seven of these stars are examined using multi-wavelength photometry to determine their nature and influence on the candidate planet properties. Most of the close neighbors appear to be gravitationally bound secondaries, while a few are best explained as closely co-aligned field stars. Revised planet properties are derived for each candidate and validated planet, including cases where the close neighbors are the potential host stars.
C1 [Everett, Mark E.; Silva, David R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Barclay, Thomas; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst, West Sonoma, CA 95476 USA.
[Ciardi, David R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
RP Everett, ME (reprint author), Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA.
OI Ciardi, David/0000-0002-5741-3047
NR 58
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2015
VL 149
IS 2
AR 55
DI 10.1088/0004-6256/149/2/55
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB1BA
UT WOS:000349360200020
ER
PT J
AU Meixner, M
Panuzzo, P
Roman-Duval, J
Engelbracht, C
Babler, B
Seale, J
Hony, S
Montiel, E
Sauvage, M
Gordon, K
Misselt, K
Okumura, K
Chanial, P
Beck, T
Bernard, JP
Bolatto, A
Bot, C
Boyer, ML
Carlson, LR
Clayton, GC
Chen, CHR
Cormier, D
Fukui, Y
Galametz, M
Galliano, F
Hora, JL
Hughes, A
Indebetouw, R
Israel, FP
Kawamura, A
Kemper, F
Kim, S
Kwon, E
Lebouteiller, V
Li, A
Long, KS
Madden, SC
Matsuura, M
Muller, E
Oliveira, JM
Onishi, T
Otsuka, M
Paradis, D
Poglitsch, A
Reach, WT
Robitaille, TP
Rubio, M
Sargent, B
Sewilo, M
Skibba, R
Smith, LJ
Srinivasan, S
Tielens, AGGM
van Loon, JT
Whitney, B
AF Meixner, M.
Panuzzo, P.
Roman-Duval, J.
Engelbracht, C.
Babler, B.
Seale, J.
Hony, S.
Montiel, E.
Sauvage, M.
Gordon, K.
Misselt, K.
Okumura, K.
Chanial, P.
Beck, T.
Bernard, J. -P.
Bolatto, A.
Bot, C.
Boyer, M. L.
Carlson, L. R.
Clayton, G. C.
Chen, C. -H. R.
Cormier, D.
Fukui, Y.
Galametz, M.
Galliano, F.
Hora, J. L.
Hughes, A.
Indebetouw, R.
Israel, F. P.
Kawamura, A.
Kemper, F.
Kim, S.
Kwon, E.
Lebouteiller, V.
Li, A.
Long, K. S.
Madden, S. C.
Matsuura, M.
Muller, E.
Oliveira, J. M.
Onishi, T.
Otsuka, M.
Paradis, D.
Poglitsch, A.
Reach, W. T.
Robitaille, T. P.
Rubio, M.
Sargent, B.
Sewilo, M.
Skibba, R.
Smith, L. J.
Srinivasan, S.
Tielens, A. G. G. M.
van Loon, J. Th.
Whitney, B.
TI THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION (HERITAGE) IN
THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM (vol 146, 62,
2013)
SO ASTRONOMICAL JOURNAL
LA English
DT Correction
ID EXCESS EMISSION; SUBMILLIMETER; DUST; ORIGIN; GAS
C1 [Meixner, M.; Roman-Duval, J.; Seale, J.; Gordon, K.; Beck, T.; Boyer, M. L.; Long, K. S.; Sargent, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meixner, M.; Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Panuzzo, P.; Hony, S.; Sauvage, M.; Okumura, K.; Chanial, P.; Cormier, D.; Galliano, F.; Lebouteiller, V.; Madden, S. C.] CEA, Lab AIM, Irfu, SAp, F-91191 Gif Sur Yvette, France.
[Panuzzo, P.] CNRS, Observ Paris, Lab GEPI, F-92195 Meudon, France.
[Engelbracht, C.; Montiel, E.; Misselt, K.; Skibba, R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Engelbracht, C.] Raytheon Co, Tucson, AZ 85756 USA.
[Babler, B.; Whitney, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Montiel, E.; Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Bernard, J. -P.; Paradis, D.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Bernard, J. -P.; Paradis, D.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Bolatto, A.] Univ Maryland, Dept Astron, Lab Millimeter Wave Astron, College Pk, MD 20742 USA.
[Bot, C.] Univ Strasbourg, Observ Astron Strasbourg, F-67000 Strasbourg, France.
[Bot, C.] CNRS, Observ Astron Strasbourg, UMR7550, F-67000 Strasbourg, France.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Chen, C. -H. R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukui, Y.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Hora, J. L.] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA.
[Hughes, A.; Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Kawamura, A.; Muller, E.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Kemper, F.; Otsuka, M.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea.
[Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Onishi, T.] Osaka Prefecture Univ, Dept Phys Sci, Sakai, Osaka 5998531, Japan.
[Poglitsch, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Rubio, M.] Univ Chile, Dept Astron, Santiago, Chile.
[Sargent, B.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Sargent, B.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
[Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Smith, L. J.] European Space Agcy, Baltimore, MD 21218 USA.
[Srinivasan, S.] UPMC, CNRS, UMR7095, Inst Astrophys, F-75014 Paris, France.
RP Meixner, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM meixner@stsci.edu
RI Rubio, Monica/J-3384-2016; Kemper, Francisca/D-8688-2011
OI Kemper, Francisca/0000-0003-2743-8240
NR 6
TC 0
Z9 0
U1 0
U2 7
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 FEB
PY 2015
VL 149
IS 2
AR 88
DI 10.1088/0004-6256/149/2/88
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CB1BA
UT WOS:000349360200053
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Allafort, A
Amin, MA
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Bonamente, E
Borgland, AW
Bregeon, J
Brigida, M
Buehler, R
Bulmash, D
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Corbet, RHD
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Finke, J
Focke, WB
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Hughes, RE
Inoue, Y
Jackson, MS
Jogler, T
Johannesson, G
Johnson, AS
Kamae, T
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Mazziotta, MN
Mehault, J
Michelson, PF
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohno, M
Ohsugi, T
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reyes, LC
Ritz, S
Romoli, C
Roth, M
Parkinson, PMS
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Takahashi, H
Takeuchi, Y
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Tronconi, V
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Werner, M
Winer, BL
Wood, KS
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Amin, M. A.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brigida, M.
Buehler, R.
Bulmash, D.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Corbet, R. H. D.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Finke, J.
Focke, W. B.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Hughes, R. E.
Inoue, Y.
Jackson, M. S.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mazziotta, M. N.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohno, M.
Ohsugi, T.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reyes, L. C.
Ritz, S.
Romoli, C.
Roth, M.
Parkinson, P. M. Saz
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Takahashi, H.
Takeuchi, Y.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Tronconi, V.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Werner, M.
Winer, B. L.
Wood, K. S.
TI GAMMA-RAY FLARING ACTIVITY FROM THE GRAVITATIONALLY LENSED BLAZAR PKS
1830-211 OBSERVED BY Fermi LAT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: galaxies; gamma rays: general; gravitational lensing:
strong; quasars: individual (PKS 1830-211); radiation mechanisms:
non-thermal; X-rays: individual (PKS 1830-211)
ID LARGE-AREA TELESCOPE; EINSTEIN RING PKS-1830-211; MOLECULAR
ABSORPTION-LINES; RADIO-SOURCE PKS1830-211; X-RAY; TIME-DELAY; GALACTIC
NUCLEI; SOURCE CATALOG; LIGHT CURVES; 3C 454.3
AB The Large Area Telescope ( LAT) on board the FermiGamma- ray Space Telescope routinely detects the MeV- peaked flat- spectrum radio quasar PKS 1830- 211 ( z = 2.507). Its apparent isotropic. - ray luminosity ( E > 100 MeV), averaged over 3 years of observations and peaking on 2010 October 14/ 15 at 2.9 x 1050 erg s- 1, makes it among the brightest high- redshift Fermi blazars. No published model with a single lens can account for all of the observed characteristics of this complex system. Based on radio observations, one expects time- delayed variability to follow about 25 days after a primary flare, with flux about a factor of 1.5 less. Two large. - ray flares of PKS 1830- 211 have been detected by the LAT in the considered period, and no substantial evidence for such a delayed activity was found. This allows us to place a lower limit of about 6 on the. - ray flux ratio between the two lensed images. Swift XRT observations from a dedicated Target of Opportunity program indicate a hard spectrum with no significant correlation of X- ray flux with the. - ray variability. The spectral energy distribution can be modeled with inverse Compton scattering of thermal photons from the dusty torus. The implications of the LAT data in terms of variability, the lack of evident delayed flare events, and different radio and. - ray flux ratios are discussed. Microlensing effects, absorption, size and location of the emitting regions, the complex mass distribution of the system, an energy- dependent inner structure of the source, and flux suppression by the lens galaxy for one image path may be considered as hypotheses for understanding our results.
C1 [Abdo, A. A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ackermann, M.; Buehler, R.] DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Amin, M. A.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Amin, M. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Amin, M. A.; Bulmash, D.] MIT, Dept Phys, Cambridge, MA 02138 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Romoli, C.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bulmash, D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Caliandro, G. A.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy.
[Cheung, C. C.; Dermer, C. D.; Finke, J.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Rome, Italy.
[Conrad, J.; Larsson, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Corbet, R. H. D.; Nemmen, R.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Corbet, R. H. D.; Nemmen, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corbet, R. H. D.; Nemmen, R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Corbet, R. H. D.; Nemmen, R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[D'Ammando, F.; Giroletti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Fukazawa, Y.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Gehrels, N.; Guiriec, S.; Hays, E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grenier, I. A.] Univ Paris Diderot, Lab AIM, CEA IRFU CNRS, Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] KTH Royal Inst Technol, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Lott, B.; Mehault, J.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Tanaka, T.] Kyoto Univ, Dept Phys, Grad Sch Sci, Kyoto 606, Japan.
[Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ciprini, S (reprint author), Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy.
EM sara.buson@pd.infn.it; stefano.ciprini@asdc.asi.it;
dammando@ira.inaf.it; justin.finke@nrl.navy.mil
RI Nemmen, Rodrigo/O-6841-2014; Morselli, Aldo/G-6769-2011; Reimer,
Olaf/A-3117-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano,
Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko,
Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
OI Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852;
Baldini, Luca/0000-0002-9785-7726; Morselli, Aldo/0000-0002-7704-9553;
Reimer, Olaf/0000-0001-6953-1385; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Mazziotta, Mario /0000-0001-9325-4672; Gargano,
Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888;
Moskalenko, Igor/0000-0001-6141-458X; Torres, Diego/0000-0002-1522-9065;
Giordano, Francesco/0000-0002-8651-2394; Caraveo,
Patrizia/0000-0003-2478-8018
NR 95
TC 10
Z9 10
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 143
DI 10.1088/0004-637X/799/2/143
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900030
ER
PT J
AU Barriere, NM
Krivonos, R
Tomsick, JA
Bachetti, M
Boggs, SE
Chakrabarty, D
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Hong, J
Mori, K
Stern, D
Zhang, WW
AF Barriere, Nicolas M.
Krivonos, Roman
Tomsick, John A.
Bachetti, Matteo
Boggs, Steven E.
Chakrabarty, Deepto
Christensen, Finn E.
Craig, William W.
Hailey, Charles J.
Harrison, Fiona A.
Hong, Jaesub
Mori, Kaya
Stern, Daniel
Zhang, William W.
TI NuSTAR OBSERVATION OF A TYPE I X-RAY BURST FROM GRS 1741.9-2853
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; nuclear reactions; nucleosynthesis;
abundances; stars: neutron; X-rays: binaries; X-rays: bursts; X-rays:
individual (GRS 1741.9-2853)
ID GALACTIC-CENTER REGION; PHOTOSPHERIC RADIUS EXPANSION; ACCRETING
NEUTRON-STARS; ABSORPTION-LINES; SHELL FLASHES; EXO 0748-676; MILKY-WAY;
SPECTRA; BINARY; DISCOVERY
AB We report on two NuSTAR observations of GRS 1741.9-2853, a faint neutron star (NS) low-mass X-ray binary burster located 10 ' away from the Galactic center. NuSTAR detected the source serendipitously as it was emerging from quiescence: its luminosity was 6x10(34) erg s(-1) on 2013 July 31 and 5x10(35) erg s(-1) in a second observation on 2013 August 3. A bright, 800 s long, H-triggered mixed H/He thermonuclear Type I burst with mild photospheric radius expansion (PRE) was present during the second observation. Assuming that the luminosity during the PRE was at the Eddington level, an H mass fraction X = 0.7 in the atmosphere, and an NS mass M = 1.4 M-circle dot, we determine a new lower limit on the distance for this source of 6.3 +/- 0.5 kpc. Combining with previous upper limits, this places GRS 1741.9-2853 at a distance of 7 kpc. Energy independent (achromatic) variability is observed during the cooling of the NS, which could result from the disturbance of the inner accretion disk by the burst. The large dynamic range of this burst reveals a long power-law decay tail. We also detect, at a 95.6% confidence level (1.7 sigma), a narrow absorption line at 5.46 +/- 0.10 keV during the PRE phase of the burst, reminiscent of the detection by Waki et al. We propose that the line, if real, is formed in the wind above the photosphere of the NS by a resonant K alpha transition from H-like Cr gravitationally redshifted by a factor 1 + z = 1.09, corresponding to a radius range of 29.0-41.4 km for a mass range of 1.4-2.0 M-circle dot.
C1 [Barriere, Nicolas M.; Krivonos, Roman; Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bachetti, Matteo] Inst Rech Astrophys & Plantol, UMR 5277, Toulouse, France.
[Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, Copenhagen, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Barriere, NM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM barriere@ssl.berkeley.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337
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 (NuSTAR-DAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA). The authors thank Nevin Weinberg for
useful discussions, and the anonymous referee for constructive comments.
NR 69
TC 5
Z9 5
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 123
DI 10.1088/0004-637X/799/2/123
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900010
ER
PT J
AU Campante, TL
Barclay, T
Swift, JJ
Huber, D
Adibekyan, VZ
Cochran, W
Burke, CJ
Isaacson, H
Quintana, EV
Davies, GR
Aguirre, VS
Ragozzine, D
Riddle, R
Baranec, C
Basu, S
Chaplin, WJ
Christensen-Dalsgaard, J
Metcalfe, TS
Bedding, TR
Handberg, R
Stello, D
Brewer, JM
Hekker, S
Karoff, C
Kolbl, R
Law, NM
Lundkvist, M
Miglio, A
Rowe, JF
Santos, NC
Van Laerhoven, C
Arentoft, T
Elsworth, YP
Fischer, DA
Kawaler, SD
Kjeldsen, H
Lund, MN
Marcy, GW
Sousa, SG
Sozzetti, A
White, TR
AF Campante, T. L.
Barclay, T.
Swift, J. J.
Huber, D.
Adibekyan, V. Zh.
Cochran, W.
Burke, C. J.
Isaacson, H.
Quintana, E. V.
Davies, G. R.
Aguirre, V. Silva
Ragozzine, D.
Riddle, R.
Baranec, C.
Basu, S.
Chaplin, W. J.
Christensen-Dalsgaard, J.
Metcalfe, T. S.
Bedding, T. R.
Handberg, R.
Stello, D.
Brewer, J. M.
Hekker, S.
Karoff, C.
Kolbl, R.
Law, N. M.
Lundkvist, M.
Miglio, A.
Rowe, J. F.
Santos, N. C.
Van Laerhoven, C.
Arentoft, T.
Elsworth, Y. P.
Fischer, D. A.
Kawaler, S. D.
Kjeldsen, H.
Lund, M. N.
Marcy, G. W.
Sousa, S. G.
Sozzetti, A.
White, T. R.
TI AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: disk; planetary systems; stars: individual (HIP 94931); stars:
late-type; stars: oscillations; techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; STELLAR EVOLUTION CODE;
GENEVA-COPENHAGEN SURVEY; LASER ADAPTIVE OPTICS; CANDIDATE HOST STARS;
PROPER-MOTION STARS; GALACTIC THICK DISC; ALPHA-CENTAURI-B; G-DWARF
STARS
AB The chemical composition of stars hosting small exoplanets (with radii less than four Earth radii) appears to be more diverse than that of gas-giant hosts, which tend to be metal-rich. This implies that small, including Earth-size, planets may have readily formed at earlier epochs in the universe's history when metals were more scarce. We report Kepler spacecraft observations of Kepler-444, a metal-poor Sun-like star from the old population of the Galactic thick disk and the host to a compact system of five transiting planets with sizes between those of Mercury and Venus. We validate this system as a true five-planet system orbiting the target star and provide a detailed characterization of its planetary and orbital parameters based on an analysis of the transit photometry. Kepler-444 is the densest star with detected solar-like oscillations. We use asteroseismology to directly measure a precise age of 11.2 +/- 1.0Gyr for the host star, indicating that Kepler-444 formed when the universe was less than 20% of its current age and making it the oldest known system of terrestrial-size planets. We thus show that Earth-size planets have formed throughout most of the universe's 13.8 billion year history, leaving open the possibility for the existence of ancient life in the Galaxy. The age of Kepler-444 not only suggests that thick-disk stars were among the hosts to the first Galactic planets, but may also help to pinpoint the beginning of the era of planet formation.
C1 [Campante, T. L.; Davies, G. R.; Chaplin, W. J.; Handberg, R.; Miglio, A.; Elsworth, Y. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Campante, T. L.; Davies, G. R.; Aguirre, V. Silva; Chaplin, W. J.; Christensen-Dalsgaard, J.; Metcalfe, T. S.; Bedding, T. R.; Handberg, R.; Stello, D.; Hekker, S.; Karoff, C.; Lundkvist, M.; Miglio, A.; Arentoft, T.; Elsworth, Y. P.; Kjeldsen, H.; Lund, M. N.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Barclay, T.; Huber, D.; Burke, C. J.; Quintana, E. V.; Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, T.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Swift, J. J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Swift, J. J.] CALTECH, Dept Planetary Sci, Pasadena, CA 91125 USA.
[Huber, D.; Burke, C. J.; Quintana, E. V.; Rowe, J. F.] SETI Inst, Mountain View, CA 94043 USA.
[Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Adibekyan, V. Zh.; Santos, N. C.; Sousa, S. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Adibekyan, V. Zh.; Santos, N. C.; Sousa, S. G.] Univ Porto, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal.
[Cochran, W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Cochran, W.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Isaacson, H.; Kolbl, R.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Ragozzine, D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Riddle, R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Baranec, C.] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA.
[Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA.
[Brewer, J. M.; Fischer, D. A.] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
[Hekker, S.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Karoff, C.] Aarhus Univ, Dept Geosci, DK-8000 Aarhus C, Denmark.
[Law, N. M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Santos, N. C.; Sousa, S. G.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal.
[Van Laerhoven, C.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Sozzetti, A.] INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, Italy.
[White, T. R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
RP Campante, TL (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM campante@bison.ph.bham.ac.uk
RI Adibekyan, Vardan/I-5026-2013;
OI Adibekyan, Vardan/0000-0002-0601-6199; Sozzetti,
Alessandro/0000-0002-7504-365X; Davies, Guy/0000-0002-4290-7351;
Lundkvist, Mia Sloth/0000-0002-8661-2571; Brewer,
John/0000-0002-9873-1471; Metcalfe, Travis/0000-0003-4034-0416; Karoff,
Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661;
Handberg, Rasmus/0000-0001-8725-4502; Lund, Mikkel
Norup/0000-0001-9214-5642
FU NASA's Science Mission Directorate; Danish National Research Foundation
[DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler) - European Research Council [267864]; European Research Council
under the European Community's Seventh Framework Programme (FP7)/ERC
[338251]; UK Science and Technology Facilities Council (STFC); NASA Keck
PI Data Award; W.M. Keck Foundation; NASA grant [NNX14AB92G]; Australian
Research Council's Discovery Projects funding scheme [DE40101364];
European Research Council/European Community [239953]; FCT (Portugal)
through FEDER funds in program COMPETE; FCT (Portugal)
[SFRH/BPD/70574/2010, SFRH/BPD/47611/2008]; California Institute of
Technology; Inter-University Centre for Astronomy and Astrophysics;
National Science Foundation [AST-0906060, AST-0960343]; Mount Cuba
Astronomical Foundation; Alfred P. Sloan Foundation; NSF [AST-1105930];
NASA [NNX13AE70G, NNX13AE91G]; Villum Foundation; FCT/MCTES (Portugal)
[IF/00169/2012]; POPH/FSE (EC); [RECI/FIS-AST/0176/2012
(FCOMP-01-0124-FEDER-027493)]; [RECI/FIS-AST/0163/2012
(FCOMP-01-0124-FEDER-027492)]
FX Funding for the Kepler mission is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team, without whom
these results would not be possible. We thank David W. Latham for
helpful comments on the manuscript. Funding for the Stellar Astrophysics
Centre is provided by The Danish National Research Foundation (grant
DNRF106). The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement No. 267864). The research
leading to the presented results has received funding from the European
Research Council under the European Community's Seventh Framework
Programme (FP7/2007-2013)/ERC grant agreement No. 338251 (StellarAges).
This research made use of APLpy, an open-source plotting package for
Python hosted at http://aplpy.github.com. T.L.C., G.R.D., W.J.C., R.H.,
A.M., and Y.P.E. acknowledge the support of the UK Science and
Technology Facilities Council (STFC). T.B. was supported by a NASA Keck
PI Data Award, administered by the NASA Exoplanet Science Institute.
Some of the data presented herein were obtained at the W. M. Keck
Observatory from telescope time allocated to the National Aeronautics
and Space Administration through the agency's scientific partnership
with the California Institute of Technology and the University of
California. The Observatory was made possible by the generous financial
support of the W.M. Keck Foundation. The authors wish to recognize and
acknowledge the very significant cultural role and reverence that the
summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain. D.H. and E.V.Q. acknowledge support by
an appointment to the NASA Postdoctoral Program at Ames Research Center
administered by Oak Ridge Associated Universities. D.H. also
acknowledges NASA grant NNX14AB92G issued through the Kepler
Participating Scientist Program and support by the Australian Research
Council's Discovery Projects funding scheme (project No. DE40101364). V.
Zh.A., N.C.S., and S.G.S. acknowledge support from the European Research
Council/European Community under FP7 through Starting grant agreement
No. 239953, and from FCT (Portugal) through FEDER funds in program
COMPETE, as well as through national funds in the form of grants
RECI/FIS-AST/0176/2012 (FCOMP-01-0124-FEDER-027493) and
RECI/FIS-AST/0163/2012 (FCOMP-01-0124-FEDER-027492). V.Zh.A. and S.G.S.
also acknowledge grants SFRH/BPD/70574/2010 and SFRH/BPD/47611/2008 from
FCT (Portugal), respectively. The Robo-AO system is supported by
collaborating partner institutions, the California Institute of
Technology and the Inter-University Centre for Astronomy and
Astrophysics, and by the National Science Foundation under grant Nos.
AST-0906060 and AST-0960343, by the Mount Cuba Astronomical Foundation,
and by a gift from Samuel Oschin. C.B. acknowledges support from the
Alfred P. Sloan Foundation. S.B. acknowledges NSF grant AST-1105930 and
NASA grant NNX13AE70G. T.S.M. acknowledges NASA grant NNX13AE91G. C.K.
acknowledges support from the Villum Foundation. N.C.S. also
acknowledges support in the form of contract reference IF/00169/2012
funded by FCT/MCTES (Portugal) and POPH/FSE (EC).
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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 FEB 1
PY 2015
VL 799
IS 2
AR 170
DI 10.1088/0004-637X/799/2/170
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900057
ER
PT J
AU Fuentes, ML
Klimchuk, JA
AF Lopez Fuentes, Marcelo
Klimchuk, James A.
TI TWO-DIMENSIONAL CELLULAR AUTOMATON MODEL FOR THE EVOLUTION OF ACTIVE
REGION CORONAL PLASMAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: magnetic fields; Sun: X-rays, gamma
rays
ID EMISSION MEASURE DISTRIBUTIONS; SELF-ORGANIZED CRITICALITY; MAGNETIC
NEUTRAL SHEETS; SOLAR-FLARES; RAY TELESCOPE; ENERGY-DISTRIBUTION;
TRANSITION-REGION; NANOFLARE MODEL; EVOLVING FIELDS; QUIET SUN
AB We study a two-dimensional cellular automaton (CA) model for the evolution of coronal loop plasmas. The model is based on the idea that coronal loops are made of elementary magnetic strands that are tangled and stressed by the displacement of their footpoints by photospheric motions. The magnetic stress accumulated between neighbor strands is released in sudden reconnection events or nanoflares that heat the plasma. We combine the CA model with the Enthalpy Based Thermal Evolution of Loops model to compute the response of the plasma to the heating events. Using the known response of the X-Ray Telescope on board Hinode, we also obtain synthetic data. The model obeys easy-to-understand scaling laws relating the output (nanoflare energy, temperature, density, intensity) to the input parameters (field strength, strand length, critical misalignment angle). The nanoflares have a power-law distribution with a universal slope of -2.5, independent of the input parameters. The repetition frequency of nanoflares, expressed in terms of the plasma cooling time, increases with strand length. We discuss the implications of our results for the problem of heating and evolution of active region coronal plasmas.
C1 [Lopez Fuentes, Marcelo] UBA, Inst Astron & Fis Espacio, CONICET, RA-1428 Buenos Aires, DF, Argentina.
[Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fuentes, ML (reprint author), UBA, Inst Astron & Fis Espacio, CONICET, CC 67,Suc 28, RA-1428 Buenos Aires, DF, Argentina.
EM lopezf@iafe.uba.ar
RI Klimchuk, James/D-1041-2012;
OI Klimchuk, James/0000-0003-2255-0305; Lopez Fuentes,
Marcelo/0000-0001-8830-4022
FU NASA Supporting Research and Technology; Argentinean grant (ANPCyT)
[PICT 2012-0973]; Argentinean grant UBACyT [20020100100733]; Argentinean
grant (CONICET) [PIP 2009-100766]
FX The authors acknowledge useful comments and suggestions from the
anonymous referee. They also wish to thank Dr. Peter Cargill for useful
discussions. J.A.K.'s work was funded by the NASA Supporting Research
and Technology and Guest Investigator programs. M.L.F. acknowledges
financial support from the Argentinean grants PICT 2012-0973 (ANPCyT),
UBACyT 20020100100733, and PIP 2009-100766 (CONICET).
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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 FEB 1
PY 2015
VL 799
IS 2
AR 128
DI 10.1088/0004-637X/799/2/128
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900015
ER
PT J
AU Mackie, CJ
Peeters, E
Bauschlicher, CW
Cami, J
AF Mackie, C. J.
Peeters, E.
Bauschlicher, C. W., Jr.
Cami, J.
TI CHARACTERIZING THE INFRARED SPECTRA OF SMALL, NEUTRAL, FULLY
DEHYDROGENATED POLYCYCLIC AROMATIC HYDROCARBONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules;
methods: numerical; molecular data
ID SPITZER-SPACE-TELESCOPE; EMISSION FEATURES; SPECTROSCOPIC DATABASE;
INTERSTELLAR-MEDIUM; PLANETARY-NEBULAE; CHARGE STATES; C-60; FULLERENES;
MOLECULES; PAHS
AB We present the results of a computational study to investigate the infrared spectroscopic properties of a large number of polycyclic aromatic hydrocarbon (PAH) molecules and their fully dehydrogenated counterparts. We constructed a database of fully optimized geometries for PAHs that is complete for eight or fewer fused benzene rings, thus containing 1550 PAHs and 805 fully dehydrogenated aromatics. A large fraction of the species in our database have clearly non-planar or curved geometries. For each species, we determined the frequencies and intensities of their normal modes using density functional theory calculations. Whereas most PAH spectra are fairly similar, the spectra of fully dehydrogenated aromatics are much more diverse. Nevertheless, these fully dehydrogenated species show characteristic emission features at 5.2 mu m, 5.5 mu m, and 10.6 mu m; at longer wavelengths, there is a forest of emission features in the 16-30 mu m range that appears as a structured continuum, but with a clear peak centered around 19 mu m. We searched for these features in Spitzer-IRS spectra of various positions in the reflection nebula NGC 7023. We find a weak emission feature at 10.68 mu m in all positions except that closest to the central star. We also find evidence for a weak 19 mu m feature at all positions that is not likely due to C-60. We interpret these features as tentative evidence for the presence of a small population of fully dehydrogenated PAHs, and discuss our results in the framework of PAH photolysis and the formation of fullerenes.
C1 [Mackie, C. J.; Peeters, E.; Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Mackie, C. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Peeters, E.; Cami, J.] SETI Inst, Mountain View, CA 94043 USA.
[Bauschlicher, C. W., Jr.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mackie, CJ (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
EM mackie@strw.leidenuniv.nl
OI Mackie, Cameron/0000-0003-2885-2021
FU Academic Development Fund (ADF) from Western University; Natural
Sciences and Engineering Research Council (NSERC)
FX We thank Xander Tielens and Lou Allamandola for the stimulating and
helpful discussions. We also thank the anonymous referee for the
constructive comments. This work was supported by a grant from the
Academic Development Fund (ADF) from Western University, and by a
Discovery Grant from the Natural Sciences and Engineering Research
Council (NSERC). This work was made possible by the facilities of the
Shared Hierarchical Academic Research Computing Network (SHARCNET:
www.sharcnet.ca) and Compute/Calcul Canada.
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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 FEB 1
PY 2015
VL 799
IS 2
AR 131
DI 10.1088/0004-637X/799/2/131
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900018
ER
PT J
AU Metchev, SA
Heinze, A
Apai, D
Flateau, D
Radigan, J
Burgasser, A
Marley, MS
Artigau, E
Plavchan, P
Goldman, B
AF Metchev, Stanimir A.
Heinze, Aren
Apai, Daniel
Flateau, Davin
Radigan, Jacqueline
Burgasser, Adam
Marley, Mark S.
Artigau, Etienne
Plavchan, Peter
Goldman, Bertrand
TI WEATHER ON OTHER WORLDS. II. SURVEY RESULTS: SPOTS ARE UBIQUITOUS ON L
AND T DWARFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: low-mass; stars: rotation; starspots; stars:
variables: general; techniques: photometric
ID DIGITAL SKY SURVEY; VERY-LOW-MASS; PROPER-MOTION SURVEY; TIME-SERIES
OBSERVATIONS; SPITZER-SPACE-TELESCOPE; STAR ADAPTIVE OPTICS; ULTRA-COOL
DWARFS; PECULIAR L DWARFS; FIELD L-DWARFS; BLUE L DWARF
AB We present results from theWeather on OtherWorlds Spitzer Exploration Science program to investigate photometric variability in L and T dwarfs, usually attributed to patchy clouds. We surveyed 44 L3- T8 dwarfs, spanning a range of J - Ks colors and surface gravities. We find that 14/ 23 ( 61%+ 17% - 20%, 95% confidence) of our single L3- L9.5 dwarfs are variable with peak- to- peak amplitudes between 0.2% and 1.5%, and 5/ 16 ( 31%+ 25% - 17%) of our single T0- T8 dwarfs are variable with amplitudes between 0.8% and 4.6%. After correcting for sensitivity, we find that 80%+ 20% - 27% of L dwarfs vary by 0.2%, and 36%+ 26% - 17% of T dwarfs vary by 0.4%. Given viewing geometry considerations, we conclude that photospheric heterogeneities causing > 0.2% 3- 5 m flux variations are present on virtually all L dwarfs, and probably on most T dwarfs. A third of L dwarf variables show irregular light curves, indicating that L dwarfs may have multiple spots that evolve over a single rotation. Also, approximately a third of the periodicities are on timescales > 10 hr, suggesting that slowly rotating brown dwarfs may be common. We observe an increase in the maximum amplitudes over the entire spectral type range, revealing a potential for greater temperature contrasts in T dwarfs than in L dwarfs. We find a tentative association ( 92% confidence) between low surface gravity and high- amplitude variability among L3- L5.5 dwarfs. Although we can not confirm whether lower gravity is also correlated with a higher incidence of variables, the result is promising for the characterization of directly imaged young extrasolar planets through variability.
C1 [Metchev, Stanimir A.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Metchev, Stanimir A.; Heinze, Aren] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Apai, Daniel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Radigan, Jacqueline] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Burgasser, Adam] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Artigau, Etienne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Artigau, Etienne] Observ Astron Mt Megantic, Montreal, PQ H3C 3J7, Canada.
[Plavchan, Peter] Mississippi State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA.
[Goldman, Bertrand] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Metchev, SA (reprint author), Univ Western Ontario, Dept Phys & Astron, 1151 Richmond Ave, London, ON N6A 3K7, Canada.
EM smetchev@uwo.ca
OI Marley, Mark/0000-0002-5251-2943
NR 108
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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 FEB 1
PY 2015
VL 799
IS 2
AR 154
DI 10.1088/0004-637X/799/2/154
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900041
ER
PT J
AU Perrin, MD
Duchene, G
Millar-Blanchaer, M
Fitzgerald, MP
Graham, JR
Wiktorowicz, SJ
Kalas, PG
Macintosh, B
Bauman, B
Cardwell, A
Chilcote, J
De Rosa, RJ
Dillon, D
Doyon, R
Dunn, J
Erikson, D
Gavel, D
Goodsell, S
Hartung, M
Hibon, P
Ingraham, P
Kerley, D
Konapacky, Q
Larkin, JE
Maire, J
Marchis, F
Marois, C
Mittal, T
Morzinski, KM
Oppenheimer, BR
Palmer, DW
Patience, J
Poyneer, L
Pueyo, L
Rantakyro, FT
Sadakuni, N
Saddlemyer, L
Savransky, D
Soummer, R
Sivaramakrishnan, A
Song, I
Thomas, S
Wallace, JK
Wang, JJ
Wolff, SG
AF Perrin, Marshall D.
Duchene, Gaspard
Millar-Blanchaer, Max
Fitzgerald, Michael P.
Graham, James R.
Wiktorowicz, Sloane J.
Kalas, Paul G.
Macintosh, Bruce
Bauman, Brian
Cardwell, Andrew
Chilcote, Jeffrey
De Rosa, Robert J.
Dillon, Daren
Doyon, Rene
Dunn, Jennifer
Erikson, Darren
Gavel, Donald
Goodsell, Stephen
Hartung, Markus
Hibon, Pascale
Ingraham, Patrick
Kerley, Daniel
Konapacky, Quinn
Larkin, James E.
Maire, Jerome
Marchis, Franck
Marois, Christian
Mittal, Tushar
Morzinski, Katie M.
Oppenheimer, B. R.
Palmer, David W.
Patience, Jennifer
Poyneer, Lisa
Pueyo, Laurent
Rantakyroe, Fredrik T.
Sadakuni, Naru
Saddlemyer, Leslie
Savransky, Dmitry
Soummer, Remi
Sivaramakrishnan, Anand
Song, Inseok
Thomas, Sandrine
Wallace, J. Kent
Wang, Jason J.
Wolff, Schuyler G.
TI POLARIMETRY WITH THE GEMINI PLANET IMAGER: METHODS, PERFORMANCE AT FIRST
LIGHT, AND THE CIRCUMSTELLAR RING AROUND HR 4796A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; instrumentation: adaptive optics; instrumentation:
high angular resolution; instrumentation: polarimeters; polarization;
stars: individual (HR 4796A)
ID INTERSTELLAR LINEAR-POLARIZATION; COMPLEX ORGANIC MATERIALS; TAURI
CIRCUMBINARY RING; IMAGING POLARIMETRY; DEBRIS DISK; WAVELENGTH
DEPENDENCE; PROTOPLANETARY DISKS; BETA-PICTORIS; PERICENTER GLOW;
SPACE-TELESCOPE
AB We present the first results from the polarimetry mode of the Gemini Planet Imager (GPI), which uses a new integral field polarimetry architecture to provide high contrast linear polarimetry with minimal systematic biases between the orthogonal polarizations. We describe the design, data reduction methods, and performance of polarimetry with GPI. Point-spread function (PSF) subtraction via differential polarimetry suppresses unpolarized starlight by a factor of over 100, and provides sensitivity to circumstellar dust reaching the photon noise limit for these observations. In the case of the circumstellar disk around HR 4796A, GPI's advanced adaptive optics system reveals the disk clearly even prior to PSF subtraction. In polarized light, the disk is seen all the way in to its semi-minor axis for the first time. The disk exhibits surprisingly strong asymmetry in polarized intensity, with the west side greater than or similar to 9 times brighter than the east side despite the fact that the east side is slightly brighter in total intensity. Based on a synthesis of the total and polarized intensities, we now believe that the west side is closer to us, contrary to most prior interpretations. Forward scattering by relatively large silicate dust particles leads to the strong polarized intensity on the west side, and the ring must be slightly optically thick in order to explain the lower brightness in total intensity there. These findings suggest that the ring is geometrically narrow and dynamically cold, perhaps shepherded by larger bodies in the same manner as Saturn's F ring.
C1 [Perrin, Marshall D.; Pueyo, Laurent; Soummer, Remi; Sivaramakrishnan, Anand; Wolff, Schuyler G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Duchene, Gaspard; Graham, James R.; Kalas, Paul G.; Mittal, Tushar; Wang, Jason J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, Gaspard] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Duchene, Gaspard] CNRS, IPAG, F-38000 Grenoble, France.
[Millar-Blanchaer, Max; Maire, Jerome] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Fitzgerald, Michael P.; Chilcote, Jeffrey; Larkin, James E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Wiktorowicz, Sloane J.; Dillon, Daren; Gavel, Donald] UC Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Macintosh, Bruce; Bauman, Brian; Palmer, David W.; Poyneer, Lisa] Lawrence Livermore Natl Lab, Livermore, CA 94040 USA.
[Macintosh, Bruce; Ingraham, Patrick] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Cardwell, Andrew; Goodsell, Stephen; Hartung, Markus; Hibon, Pascale; Rantakyroe, Fredrik T.; Sadakuni, Naru] Gemini Observ, La Serena, Chile.
[De Rosa, Robert J.; Patience, Jennifer] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[De Rosa, Robert J.] Univ Exeter, Sch Phys, Coll Engn Math & Phys Sci, Exeter EX4 4QL, Devon, England.
[Doyon, Rene; Ingraham, Patrick] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Dunn, Jennifer; Erikson, Darren; Kerley, Daniel; Marois, Christian; Saddlemyer, Leslie] Natl Res Council Canada Herzberg, Victoria, BC V9E 2E7, Canada.
[Marchis, Franck] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Morzinski, Katie M.] Univ Arizona, Ctr Astron Adapt Opt, Steward Observ, Tucson, AZ 85721 USA.
[Oppenheimer, B. R.] Amer Museum Nat Hist, New York, NY 10024 USA.
[Savransky, Dmitry] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Thomas, Sandrine] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wallace, J. Kent] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wolff, Schuyler G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Perrin, MD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Fitzgerald, Michael/C-2642-2009; Savransky, Dmitry/M-1298-2014;
OI Fitzgerald, Michael/0000-0002-0176-8973; Savransky,
Dmitry/0000-0002-8711-7206; Oppenheimer, Rebecca/0000-0001-7130-7681;
Morzinski, Katie/0000-0002-1384-0063; Wang, Jason/0000-0003-0774-6502
FU U.S. Department of Energy by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]
FX We thank the international team of engineers and scientists who worked
to make GPI a reality. The Gemini Observatory is operated by the
Association of Universities for Research in Astronomy, Inc., under a
cooperative agreement with the NSF on behalf of the Gemini partnership:
the National Science Foundation (United States), the National Research
Council (Canada), CONICYT (Chile), the Australian Research Council
(Australia),Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and
Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina).
We acknowledge financial support from the Gemini Observatory, the
National Science Foundation (NSF) Center for Adaptive Optics at
University of California, SantaCruz, theNSF (AST-0909188; AST-1211562),
NASA (NNX11AD21G and NNX10AH31G), the University of California Office of
the President (LFRP-118057), and the Dunlap Institute, University of
Toronto. Portions of this work were performed under the auspices of the
U.S. Department of Energy by Lawrence Livermore National Laboratory
under Contract DE-AC52-07NA27344, and other portions under contract with
the California Institute of Technology Jet Propulsion Laboratory funded
by NASA through the Sagan Fellowship Program executed by the NASA
Exoplanet Science Institute. We also acknowledge support from the
Natural Science and Engineering Council of Canada. M. D. P. was
supported in part by a National Science Foundation Astronomy and
Astrophysics Postdoctoral Fellowship, NSFAST-0702933. M.D.P. also
acknowledges support from the STScI Director's Discretionary Research
Fund.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 182
DI 10.1088/0004-637X/799/2/182
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900069
ER
PT J
AU Rana, V
Harrison, FA
Bachetti, M
Walton, DJ
Furst, F
Barret, D
Miller, JM
Fabian, AC
Boggs, SE
Christensen, FC
Craig, WW
Grefenstette, BW
Hailey, CJ
Madsen, KK
Ptak, AF
Stern, D
Webb, NA
Zhang, WW
AF Rana, Vikram
Harrison, Fiona A.
Bachetti, Matteo
Walton, Dominic J.
Furst, Felix
Barret, Didier
Miller, Jon M.
Fabian, Andrew C.
Boggs, Steven E.
Christensen, Finn C.
Craig, William W.
Grefenstette, Brian W.
Hailey, Charles J.
Madsen, Kristin K.
Ptak, Andrew F.
Stern, Daniel
Webb, Natalie A.
Zhang, William W.
TI THE BROADBAND XMM-NEWTON AND NuSTAR X-RAY SPECTRA OF TWO ULTRALUMINOUS
X-RAY SOURCES IN THE GALAXY IC 342
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; black hole physics; X-rays: binaries;
X-rays: individual (IC 342 X-1, IC 342 X-2)
ID MASS BLACK-HOLES; COOL ACCRETION DISKS; HOLMBERG-IX X-1; NGC 1313 X-1;
VARIABILITY; MODELS; REFLECTION; OUTFLOWS; IC-342; STATES
AB We present results for two ultraluminous X-ray sources (ULXs), IC 342 X-1 and IC 342 X-2, using two epochs of XMM-Newton and NuSTAR observations separated by similar to 7 days. We observe little spectral or flux variability above 1 keV between epochs, with unabsorbed 0.3-30 keV luminosities being 1.04(-0.06)(+0.08) x 10(40) erg s(-1) for IC 342 X-1 and 7.40 +/- 0.20 x 10(39) erg s(-1) for IC 342 X-2, so that both were observed in a similar, luminous state. Both sources have a high absorbing column in excess of the Galactic value. Neither source has a spectrum consistent with a black hole binary in low/hard state, and both ULXs exhibit strong curvature in their broadband X-ray spectra. This curvature rules out models that invoke a simple reflection-dominated spectrum with a broadened iron line and no cutoff in the illuminating power-law continuum. X-ray spectrum of IC 342 X-1 can be characterized by a soft disk-like blackbody component at low energies and a cool, optically thick Comptonization continuum at high energies, but unique physical interpretation of the spectral components remains challenging. The broadband spectrum of IC 342 X-2 can be fit by either a hot (3.8 keV) accretion disk or a Comptonized continuum with no indication of a seed photon population. Although the seed photon component may be masked by soft excess emission unlikely to be associated with the binary system, combined with the high absorption column, it is more plausible that the broadband X-ray emission arises from a simple thin blackbody disk component. Secure identification of the origin of the spectral components in these sources will likely require broadband spectral variability studies.
C1 [Rana, Vikram; Harrison, Fiona A.; Walton, Dominic J.; Furst, Felix; Grefenstette, Brian W.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Bachetti, Matteo; Barret, Didier; Webb, Natalie A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Bachetti, Matteo; Barret, Didier; Webb, Natalie A.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn C.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Ptak, Andrew F.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rana, V (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337;
Madsen, Kristin/0000-0003-1252-4891; Rana, Vikram/0000-0003-1703-8796
FU NASA [NNG08FD60C]; Centre National d'Etudes Spatiales (CNES); National
Aeronautics and Space Administration and XMM-Newton, an ESA mission
FX This work was supported under NASA No. NNG08FD60C and made use of data
from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a
project led by Caltech, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration and
XMM-Newton, an ESA mission. We thank the anonymous referee for positive
comments that improved the quality of this paper. 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 Caltech (USA). D.B. and
M.B. are grateful to the Centre National d'Etudes Spatiales (CNES) for
funding their activities.
NR 47
TC 18
Z9 18
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 121
DI 10.1088/0004-637X/799/2/121
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900008
ER
PT J
AU Sonnett, S
Mainzer, A
Grav, T
Masiero, J
Bauer, J
AF Sonnett, S.
Mainzer, A.
Grav, T.
Masiero, J.
Bauer, J.
TI BINARY CANDIDATES IN THE JOVIAN TROJAN AND HILDA POPULATIONS FROM
NEOWISE LIGHT CURVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets; asteroids: general
ID KUIPER-BELT BINARIES; INFRARED-SURVEY-EXPLORER; WISE/NEOWISE
OBSERVATIONS; SOLAR-SYSTEM; LOW-MASS; ASTEROIDS; PLANETS; JUPITER;
CAPTURE; OBJECTS
AB Determining the binary fraction for a population of asteroids, particularly as a function of separation between the two components, helps describe the dynamical environment at the time the binaries formed, which in turn offers constraints on the dynamical evolution of the solar system. We searched the NEOWISE archival data set for close and contact binary Trojans and Hildas via their diagnostically large light curve amplitudes. We present 48 out of 554 Hilda and 34 out of 953 Trojan binary candidates in need of follow-up to confirm their large light curve amplitudes and subsequently constrain the binary orbit and component sizes. From these candidates, we calculate a preliminary estimate of the binary fraction without confirmation or debiasing of 14%-23% for Trojans larger than similar to 12 km and 30%-51% for Hildas larger than similar to 4 km. Once the binary candidates have been confirmed, it should be possible to infer the underlying, debiased binary fraction through estimation of survey biases.
C1 [Sonnett, S.; Mainzer, A.; Masiero, J.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
RP Sonnett, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sarah.Sonnett@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU Planetary Science Division of the National Aeronautics and Space
Administration; NASA; National Aeronautics and Space Administration
FX This publication makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the Planetary Science Division of the National
Aeronautics and Space Administration. This research has made use of the
NASA/IPAC Infrared Science Archive, which is operated by the California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. S.S. gratefully acknowledges the support of
the NASA Postdoctoral Program.
NR 45
TC 2
Z9 2
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 191
DI 10.1088/0004-637X/799/2/191
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900078
ER
PT J
AU Temim, T
Dwek, E
Tchernyshyov, K
Boyer, ML
Meixner, M
Gall, C
Roman-Duval, J
AF Temim, Tea
Dwek, Eli
Tchernyshyov, Kirill
Boyer, Martha L.
Meixner, Margaret
Gall, Christa
Roman-Duval, Julia
TI DUST DESTRUCTION RATES AND LIFETIMES IN THE MAGELLANIC CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: individual objects (MAGELLANIC
CLOUDS); ISM: supernova remnants
ID GIANT BRANCH STARS; KEPLERS SUPERNOVA REMNANT; SPITZER-SPACE-TELESCOPE;
HIGH-REDSHIFT UNIVERSE; INTERSTELLAR DUST; SOLAR NEIGHBORHOOD;
INFRARED-EMISSION; FORMATION HISTORY; X-RAY; CHEMICAL EVOLUTION
AB The dust budget in galaxies depends on the rate at which dust grains are created in different stellar sources and destroyed by interstellar shocks. Because of their extensive wavelength coverage, proximity, and nearly face-on geometry, the Magellanic Clouds (MCs) provide a unique opportunity to study these processes in great detail. In this paper, we use the complete sample of supernova remnants (SNRs) in the MCs to calculate the lifetimes and destruction efficiencies of silicate and carbon dust. We find dust lifetimes of 22 13 Myr (30 17 Myr) for silicate (carbon) grains in the LMC, and 54 32 Myr (72 43 Myr) for silicate (carbon) grains in the SMC. The corresponding dust destruction rates are 2.3 x 10-2M yr-1 (5.9 x 10-3M yr-1) and 3.0 x 10-3M yr-1 (5.6 x 10-4M yr-1) for silicate (carbon) grains in the LMC and SMC, respectively. The significantly shorter lifetimes in the MCs, as compared to the Milky Way, are explained as the combined effect of their lower total dust mass and preferentially higher dust-to-gas (D2G) mass ratios in the vicinity of the SNRs. We find that the maximum dust injection rates by asymptotic giant branch stars and core collapse supernovae are an order of magnitude lower than the dust destruction rates by the SNRs, suggesting that most of the dust may be reconstituted in dense molecular clouds. We also discuss the dependence of the dust destruction rate on the local D2G mass ratio, ambient gas density, and metallicity, as well as the application of our results to other galaxies and dust evolution models.
C1 [Temim, Tea; Dwek, Eli; Meixner, Margaret] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Tchernyshyov, Kirill] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Boyer, Martha L.] ORAU, Oak Ridge, TN 37831 USA.
[Meixner, Margaret; Roman-Duval, Julia] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gall, Christa] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Gall, Christa] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM tea.temim@nasa.gov
RI Gall, Christa/P-7630-2016;
OI Gall, Christa/0000-0002-8526-3963; Temim, Tea/0000-0001-7380-3144
NR 99
TC 11
Z9 11
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 158
DI 10.1088/0004-637X/799/2/158
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900045
ER
PT J
AU Walton, DJ
Harrison, FA
Bachetti, M
Barret, D
Boggs, SE
Christensen, FE
Craig, WW
Fuerst, F
Grefenstette, BW
Hailey, CJ
Madsen, KK
Middleton, MJ
Rana, V
Roberts, TP
Stern, D
Sutton, AD
Webb, N
Zhang, W
AF Walton, D. J.
Harrison, F. A.
Bachetti, M.
Barret, D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Fuerst, F.
Grefenstette, B. W.
Hailey, C. J.
Madsen, K. K.
Middleton, M. J.
Rana, V.
Roberts, T. P.
Stern, D.
Sutton, A. D.
Webb, N.
Zhang, W.
TI NUSTAR AND XMM-NEWTON OBSERVATIONS OF THE EXTREME ULTRALUMINOUS X-RAY
SOURCE NGC 5907 ULX1: A VANISHING ACT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: individual (NGC 5907 ULX1)
ID MASS BLACK-HOLE; HOLMBERG IX X-1; SUPER-EDDINGTON ACCRETION; PHOTON
IMAGING CAMERA; ESO 243-49; SOLAR MASSES; BINARY; CHANDRA; HLX-1;
VARIABILITY
AB We present results obtained from two broadband X-ray observations of the extreme ultraluminous X-ray source (ULX) NGC 5907 ULX1, known to have a peak X-ray luminosity of similar to 5 x 10(40) erg s(-1). These XMM-Newton and NuSTAR observations, separated by only similar to 4 days, revealed an extreme level of short-term flux variability. In the first epoch, NGC 5907 ULX1 was undetected by NuSTAR, and only weakly detected (if at all) with XMM-Newton, while in the second NGC 5907 ULX1 was clearly detected at high luminosity by both missions. This implies an increase in flux of similar to 2 orders of magnitude or more during this similar to 4 day window. We argue that this is likely due to a rapid rise in the mass accretion rate, rather than to a transition from an extremely obscured to an unobscured state. During the second epoch we observed the broadband 0.3-20.0 keV X-ray luminosity to be (1.55 +/- 0.06) x 10(40) erg s(-1), similar to the majority of the archival X-ray observations. The broadband X-ray spectrum obtained from the second epoch is inconsistent with the low/hard accretion state observed in Galactic black hole binaries, but is well modeled with a simple accretion disk model incorporating the effects of photon advection. This strongly suggests that when bright, NGC 5907 ULX1 is a high-Eddington accretor.
C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walton, D. J.; Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Rana, V.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Bachetti, M.; Barret, D.; Webb, N.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Bachetti, M.; Barret, D.; Webb, N.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Middleton, M. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Roberts, T. P.; Sutton, A. D.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337;
Rana, Vikram/0000-0003-1703-8796
FU French Space Agency (CNES); NASA; NASA's Chandra; Swift satellites; ESA
Member States
FX The authors would like to thank the reviewer for positive and useful
feedback, which helped improve the manuscript, as well as Diego
Altamarino for useful discussions. M. B. and D. B. acknowledge financial
support from the French Space Agency (CNES). 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, and has utilized the
NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI
Science Data Center (ASDC, Italy) and Caltech (USA). This research has
also made use of data obtained with XMM-Newton, an ESA science mission
with instruments and contributions directly funded by ESA Member States
and NASA, and NASA's Chandra and Swift satellites.
NR 71
TC 12
Z9 12
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2015
VL 799
IS 2
AR 122
DI 10.1088/0004-637X/799/2/122
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CA3QH
UT WOS:000348820900009
ER
PT J
AU Hanselman, DH
Heifetz, J
Echave, KB
Dressel, SC
AF Hanselman, Dana H.
Heifetz, Jonathan
Echave, Katy B.
Dressel, Sherri C.
TI Move it or lose it: movement and mortality of sablefish tagged in Alaska
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID ANOPLOPOMA-FIMBRIA; RECOVERY DATA; MIGRATION RATES; FISH POPULATION;
STOCK ASSESSMENT; YELLOWFIN TUNA; PACIFIC-OCEAN; TAGGING DATA; MODEL;
DYNAMICS
AB A basic step in understanding the dynamics of a fish population is to quantify movement and mortality rates. Conventional mark-recapture experiments have provided the foundation for studies on animal movement, particularly for fish. Previous studies have shown rapid mixing of sablefish (Anoplopoma fimbria) among fishery regulatory areas, with the pattern of movement related to fish size. Over 300 000 tag releases in Alaska and over 27 000 tag recoveries from 1979 to 2009 were analyzed. We used a Markov model to quantify annual movement probabilities among areas for three size groups of sablefish. The negative-binomial likelihood was used to model the tag-recovery data because of significant overdispersion. Annual movement probabilities were high, ranging from 10% to 88% depending on area of occupancy at each time step and size group. Overall, movement probabilities were very different between areas of occupancy and moderately different between size groups. Estimated annual movement of small sablefish from the central Gulf of Alaska had the reverse pattern of a previous study, with 29% moving westward and 39% moving eastward. Movement probabilities also varied annually, with decreasing movement until the late 1990s and increasing movement until 2009. Year-specific magnitude in movement probability of large fish was highly negatively correlated with female spawning biomass estimates from the federal stock assessment. Mean mortality estimates from time at liberty were similar to the federal stock assessment. Incorporating these tag-recovery and movement data into a fully age-structured spatial stock assessment model will inform harvest apportionment strategies to conserve spawning biomass and maximize future yields.
C1 [Hanselman, Dana H.; Heifetz, Jonathan; Echave, Katy B.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA.
[Dressel, Sherri C.] Alaska Dept Fish & Game, Div Commercial Fisheries, Juneau, AK 99811 USA.
RP Hanselman, DH (reprint author), Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA.
EM dana.hanselman@noaa.gov
NR 70
TC 1
Z9 1
U1 0
U2 15
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0706-652X
EI 1205-7533
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD FEB
PY 2015
VL 72
IS 2
BP 238
EP 251
DI 10.1139/cjfas-2014-0251
PG 14
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA CA3GX
UT WOS:000348795800009
ER
PT J
AU Shuman, JK
Tchebakova, NM
Parfenova, EI
Soja, AJ
Shugart, HH
Ershov, D
Holcomb, K
AF Shuman, Jacquelyn K.
Tchebakova, Nadezhda M.
Parfenova, Elena I.
Soja, Amber J.
Shugart, Herman H.
Ershov, Dmitry
Holcomb, Katherine
TI Forest forecasting with vegetation models across Russia
SO CANADIAN JOURNAL OF FOREST RESEARCH
LA English
DT Article
DE modeling; boreal forest; biomass; carbon; validation; gap model;
bioclimatic model
ID CLIMATE-CHANGE; GLOBAL CLIMATE; BOREAL FORESTS; CARBON-CYCLE; FEEDBACKS;
SYSTEM; SENSITIVITY; PERMAFROST; ECOSYSTEMS; MANAGEMENT
AB Vegetation models are essential tools for projecting large-scale land-cover response to changing climate, which is expected to alter the distribution of biomes and individual species. A large-scale bioclimatic envelope model (RuBCliM) and an individual species based gap model (UVAFME) are used to simulate the Russian forests under current and future climate for two greenhouse gas emissions scenarios. Results for current conditions are compared between models and assessed against two independent maps of Russian forest biomes and dominant tree species. Comparisons measured with kappa statistics indicate good agreement between the models (kappa values from 0.76 to 0.69), as well as between the model results and two observation-based maps for both species presence and absence (kappa values from 0.70 to 0.43). Agreement between these multiple types of data on forest distribution provides confidence in the projected forest response to changing climate. For future conditions, both models indicate a shift in the dominant biomes from conifers to deciduous leaved species. These projections have implications for feedbacks between the energy budget, carbon cycle, and land cover in the boreal system. The distinct biome and species changes emphasize the need for continued investigation of this landmass that has the size necessary to influence regional and global climate.
C1 [Shuman, Jacquelyn K.; Shugart, Herman H.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Tchebakova, Nadezhda M.; Parfenova, Elena I.] Russian Acad Sci, Sukachev Inst Forest, Krasnoyarsk, Russia.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Radiat & Aerosols Branch, Hampton, VA 23681 USA.
[Ershov, Dmitry] Russian Acad Sci, Ctr Problems Ecol & Prod Forests, Moscow, Russia.
[Holcomb, Katherine] Univ Virginia, Alliance Computat Sci & Engn, Charlottesville, VA 22904 USA.
RP Shuman, JK (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall,291 McCormick Rd,POB 400123, Charlottesville, VA 22904 USA.
EM jkshuman@virginia.edu
RI Shugart, Herman/C-5156-2009; Ershov, Dmitry/A-8187-2014
OI Ershov, Dmitry/0000-0001-8948-6470
FU NASA [10-CARBON10-0068, 09-IDS09-116]
FX This work was funded by NASA grants to H.H. Shugart (Terrestrial Ecology
10-CARBON10-0068) and A.J. Soja (Inter-Disciplinary Science
09-IDS09-116). We thank the anonymous reviewers and V.A. Seamster for
helpful comments on earlier versions of this manuscript, and Robert
Smith for figure preparation. We also appreciate the software packages
that made this work possible: IDRISI developed in 1987 by R.J. Eastman
at Clark University in Worcester, Massachusetts, USA, and ESRI 2008
(ESRI ArcGIS version 9.3, ESRI, Redlands, California, USA).
NR 53
TC 3
Z9 3
U1 3
U2 30
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0045-5067
EI 1208-6037
J9 CAN J FOREST RES
JI Can. J. For. Res.
PD FEB
PY 2015
VL 45
IS 2
BP 175
EP 184
DI 10.1139/cjfr-2014-0138
PG 10
WC Forestry
SC Forestry
GA AZ9IB
UT WOS:000348526000005
ER
PT J
AU Lantukh, D
Russell, RP
Broschart, S
AF Lantukh, Demyan
Russell, Ryan P.
Broschart, Stephen
TI Heliotropic orbits at oblate asteroids: balancing solar radiation
pressure and J2 perturbations
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Asteroid exploration; Oblateness; Solar radiation pressure; Frozen
orbit; Averaged solutions; Lagrange planetary equations (LPE)
ID SCIENCE ORBIT; SATELLITES; DYNAMICS; EUROPA; DESIGN; DUST
AB The combined effect of significant solar radiation pressure and perturbations on spacecraft orbits is investigated using both singly and doubly-averaged disturbing potentials with the Lagrange Planetary Equations. The resulting dynamics are applied to a spacecraft around an oblate asteroid. Several Sun-frozen families of orbits are identified using the singly-averaged potential, including two new families of orbits and a previously-discovered equatorial heliotropic orbit family. Families of both stable and unstable Sun-frozen orbits are mapped and characterized in the singly-averaged case. In addition, a heliotropic constraint is implemented to locate heliotropic orbits out of the equatorial plane using a constrained, doubly-averaged potential. Dynamic bounds for these 3D heliotropic orbits are shown to have an inclination limit of approximately 46 degrees for oblate bodies, and this limit is independent of the value of and radiation parameters. The resulting heliotropic and related periodic families of orbits are good candidates to consider for low-altitude science orbits around small oblate bodies with low or near-180 degree obliquity like Bennu, the target for the OSIRIS-REx mission.
C1 [Lantukh, Demyan; Russell, Ryan P.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Broschart, Stephen] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Russell, RP (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
EM demyan@utexas.edu; ryan.russell@utexas.edu
FU NASA Office of the Chief Technologist via a NASA Space Technology
Research Fellowship [NNX12AI77H]; W. M. Keck Foundation; National
Aeronautics and Space Administration
FX The presented work was supported 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 the National Aeronautics and Space Administration.
NR 24
TC 5
Z9 5
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
EI 1572-9478
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD FEB
PY 2015
VL 121
IS 2
BP 171
EP 190
DI 10.1007/s10569-014-9596-x
PG 20
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA CA5VV
UT WOS:000348976800004
ER
PT J
AU Scully, JEC
Russell, CT
Yin, A
Jaumann, R
Carey, E
Castillo-Ropz, J
McSween, HY
Raymond, CA
Reddy, V
Le Corre, L
AF Scully, Jennifer E. C.
Russell, Christopher T.
Yin, An
Jaumann, Ralf
Carey, Elizabeth
Castillo-Ropz, Julie
McSween, Harry Y.
Raymond, Carol A.
Reddy, Vishnu
Le Corre, Lucille
TI Geomorphological evidence for transient water flow on Vesta
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Vesta; geomorphology; gullies; lobate deposits; transient water flow;
volatiles
ID MARTIAN GULLIES; DARK MATERIAL; SURFACE-FEATURES; VOLATILE CONTENT;
IMPACT CRATER; ASTEROID BELT; MARS; DAWN; HYPOTHESIS; ORIGIN
AB Vesta, the second most massive asteroid, has long been perceived as anhydrous. Recent studies suggesting the presence of hydrated minerals and past subsurface water have challenged this long-standing perception. Yet, direct geologic indications of water activity on Vesta's surface were unexpected. Herein we show evidence that transient water flowed on the surface, in a debris-flow-like process, and left distinctive geomorphologic features. Based on detailed analysis of highest-resolution (similar to 20 m/pixel) images obtained by the Dawn spacecraft, we identify a class of locally occurring, interconnected and curvilinear gully networks on the walls of young (< hundreds of Ma) impact craters, ending in lobate deposits near the crater floors. As curvilinear systems only occur within impact craters, we propose that they formed by a particulate-dominated flow of transient water that was released from buried ice-bearing deposits by impact-induced heating and melting. This interpretation is in accordance with the occurrence of pitted terrain on lobate deposits and crater floors. Pitted terrain is proposed to result from the degassing of volatiles. The proposed buried ice-bearing deposits are likely localized in extent and may be currently extant in Vesta's subsurface. Together with the discovery of water evaporation on Ceres and water activity on several small asteroids, our results support the new paradigm that water is widespread in the asteroid belt. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Scully, Jennifer E. C.; Russell, Christopher T.; Yin, An] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Jaumann, Ralf] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Carey, Elizabeth; Castillo-Ropz, Julie; Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Reddy, Vishnu] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Reddy, Vishnu; Le Corre, Lucille] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Scully, JEC (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles Young Dr East,Box 951567, Los Angeles, CA 90095 USA.
EM jscully@ucla.edu; ctrussel@igpp.ucla.edu; yin@ess.ucla.edu;
ralf.jaumann@dlr.de; Elizabeth.M.Carey@jpl.nasa.gov;
julie.c.castillo@jpl.nasa.gov; mcsween@utk.edu;
carol.a.raymond@jpl.nasa.gov; reddy@psi.edu; lecorre@psi.edu
OI Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932
NR 77
TC 13
Z9 13
U1 5
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD FEB 1
PY 2015
VL 411
BP 151
EP 163
DI 10.1016/j.epsl.2014.12.004
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CA8UX
UT WOS:000349197500016
ER
PT J
AU Rueda, JC
Randall, AA
Davis, C
Franco, C
Yestrebsky, CL
AF Rueda, Juan Camilo
Randall, Andrew A.
Davis, Chuck
Franco, Carolina
Yestrebsky, Cherie L.
TI Toxicity Studies of AKGA/Hydrazines Degradation By-Products and Their
Compatibility with Sewage Treatment Plant Operation
SO ENVIRONMENTAL ENGINEERING SCIENCE
LA English
DT Article
DE hydrazine; PCA; aerobic degradation; activated sludge; mPCA; AKGA;
toxicity; monomethylhydrazine
ID TESTS
AB A new method to treat hydrazine and monomethylhydrazine (MMH) using alpha-ketoglutaric acid (AKGA) was proposed. From the reaction of AKGA with hydrazine or MMH, two stable products are formed, 1,4,5,6-tetrahydro-6-oxo-3-pyridazinecarboxylic acid (PCA) and 1-methyl-1,4,5,6-tetrahydro-6-oxo-3-pyridazinecarboxylic acid (mPCA), respectively. With a focus toward use at an industrial facility, tests were undertaken to determine whether waste streams produced from this reaction can be metered into a municipal wastewater facility for final disposal. PCA and mPCA were analyzed for acute toxicity using crustaceans (Ceriodaphnia dubia) and fish (Pimephales promelas) and their effect on the wastewater treatment efficiency and viability using activated sludge (AS) microbes, and their biodegradability by AS organisms. Acute toxicity on crustaceans and fish was investigated according to the methods for acute toxicity by USEPA Method EPA-821-R-02-012. The effect of mPCA and PCA in the treatment efficiency and viability were estimated from respiration inhibition tests (USEPA, 2012) and heterotrophic plate counts. Last, the biodegradability of PCA and mPCA was assessed using the Closed Bottle Method. The results of this study showed that mPCA is significantly more toxic to C. dubia and P. promelas than PCA at the high concentrations ranges used in this study (0.5-1.5 g/L). On the other hand, PCA and mPCA did not show a significant inhibition of carbonaceous respiration of AS microbes at concentrations ranging from 0.5 to 1.5 g/L, although both exhibited some inhibitory effects on nitrification. Under the conditions of this study, PCA was biodegradable by AS while mPCA was not.
C1 [Rueda, Juan Camilo; Randall, Andrew A.] Univ Cent Florida, Dept Civil Environm & Construct Engn, Orlando, FL 32816 USA.
[Davis, Chuck] NASA, Kennedy Space Ctr, Cocoa Beach, FL USA.
[Franco, Carolina; Yestrebsky, Cherie L.] Univ Cent Florida, Dept Chem, Orlando, FL 32816 USA.
RP Randall, AA (reprint author), Univ Cent Florida, Dept Civil Environm & Construct Engn, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
EM andrew.randall@ucf.edu
FU National Aeronautics and Space Administration (NASA); URS engineering
company [NNK08OC01C, E1274976]; NASA/URS
FX This work was supported by the National Aeronautics and Space
Administration (NASA), as well as the URS engineering company under
contract number NNK08OC01C, Project E1274976 with NASA/URS.
NR 21
TC 1
Z9 1
U1 1
U2 3
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1092-8758
EI 1557-9018
J9 ENVIRON ENG SCI
JI Environ. Eng. Sci.
PD FEB 1
PY 2015
VL 32
IS 2
BP 153
EP 162
DI 10.1089/ees.2014.0333
PG 10
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA CB0NE
UT WOS:000349322300009
ER
PT J
AU Martre, P
Wallach, D
Asseng, S
Ewert, F
Jones, JW
Rotter, RP
Boote, KJ
Ruane, AC
Thorburn, PJ
Cammarano, D
Hatfield, JL
Rosenzweig, C
Aggarwal, PK
Angulo, C
Basso, B
Bertuzzi, P
Biernath, C
Brisson, N
Challinor, AJ
Doltra, J
Gayler, S
Goldberg, R
Grant, RF
Heng, L
Hooker, J
Hunt, LA
Ingwersen, J
Izaurralde, RC
Kersebaum, KC
Muller, C
Kumar, SN
Nendel, C
O'leary, G
Olesen, JE
Osborne, TM
Palosuo, T
Priesack, E
Ripoche, D
Semenov, MA
Shcherbak, I
Steduto, P
Stockle, CO
Stratonovitch, P
Streck, T
Supit, I
Tao, FL
Travasso, M
Waha, K
White, JW
Wolf, J
AF Martre, Pierre
Wallach, Daniel
Asseng, Senthold
Ewert, Frank
Jones, James W.
Rotter, Reimund P.
Boote, Kenneth J.
Ruane, Alex C.
Thorburn, Peter J.
Cammarano, Davide
Hatfield, Jerry L.
Rosenzweig, Cynthia
Aggarwal, Pramod K.
Angulo, Carlos
Basso, Bruno
Bertuzzi, Patrick
Biernath, Christian
Brisson, Nadine
Challinor, Andrew J.
Doltra, Jordi
Gayler, Sebastian
Goldberg, Richie
Grant, Robert F.
Heng, Lee
Hooker, Josh
Hunt, Leslie A.
Ingwersen, Joachim
Izaurralde, Roberto C.
Kersebaum, Kurt Christian
Mueller, Christoph
Kumar, Soora Naresh
Nendel, Claas
O'leary, Garry
Olesen, Jorgen E.
Osborne, Tom M.
Palosuo, Taru
Priesack, Eckart
Ripoche, Dominique
Semenov, Mikhail A.
Shcherbak, Iurii
Steduto, Pasquale
Stoeckle, Claudio O.
Stratonovitch, Pierre
Streck, Thilo
Supit, Iwan
Tao, Fulu
Travasso, Maria
Waha, Katharina
White, Jeffrey W.
Wolf, Joost
TI Multimodel ensembles of wheat growth: many models are better than one
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE ecophysiological model; ensemble modeling; model intercomparison;
process-based model; uncertainty; wheat (Triticum aestivum L.)
ID CLIMATE-CHANGE; CROP PRODUCTION; IMPACTS; YIELD; SIMULATIONS;
CALIBRATION; AUSTRALIA; BILLION; EUROPE; GRAIN
AB Crop models of crop growth are increasingly used to quantify the impact of global changes due to climate or crop management. Therefore, accuracy of simulation results is a major concern. Studies with ensembles of crop models can give valuable information about model accuracy and uncertainty, but such studies are difficult to organize and have only recently begun. We report on the largest ensemble study to date, of 27 wheat models tested in four contrasting locations for their accuracy in simulating multiple crop growth and yield variables. The relative error averaged over models was 24-38% for the different end-of-season variables including grain yield (GY) and grain protein concentration (GPC). There was little relation between error of a model for GY or GPC and error for in-season variables. Thus, most models did not arrive at accurate simulations of GY and GPC by accurately simulating preceding growth dynamics. Ensemble simulations, taking either the mean (e-mean) or median (e-median) of simulated values, gave better estimates than any individual model when all variables were considered. Compared to individual models, e-median ranked first in simulating measured GY and third in GPC. The error of e-mean and e-median declined with an increasing number of ensemble members, with little decrease beyond 10 models. We conclude that multimodel ensembles can be used to create new estimators with improved accuracy and consistency in simulating growth dynamics. We argue that these results are applicable to other crop species, and hypothesize that they apply more generally to ecological system models.
C1 [Martre, Pierre] INRA, Genet Divers & Ecophysiol Cereals GDEC UMR1095, 5 Chemin Beaulieu, F-63100 Clermont Ferrand, France.
[Martre, Pierre] Univ Blaise Pascal, GDEC UMR1095, F-63170 Aubiere, France.
[Wallach, Daniel] INRA, Agrosyst & Dev Terr UMR1248, F-31326 Castanet Tolosan, France.
[Asseng, Senthold; Jones, James W.; Boote, Kenneth J.; Cammarano, Davide] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA.
[Ewert, Frank; Angulo, Carlos] Univ Bonn, Inst Crop Sci & Resource Conservat, D-53115 Bonn, Germany.
[Rotter, Reimund P.; Palosuo, Taru] MTT Agrifood Res Finland, Plant Prod Res, FI-50100 Mikkeli, Finland.
[Ruane, Alex C.; Rosenzweig, Cynthia; Goldberg, Richie] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Thorburn, Peter J.] Commonwealth Sci & Ind Res Org, Ecosyst Sci, Dutton Pk, Qld 4102, Australia.
[Hatfield, Jerry L.] Natl Lab Agr & Environm, Ames, IA 50011 USA.
[Aggarwal, Pramod K.] Int Water Management Inst, Consultat Grp Int Agr Res, Res Program Climate Change Agr & Food Secur, New Delhi 110012, India.
[Basso, Bruno; Shcherbak, Iurii] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48823 USA.
[Basso, Bruno; Shcherbak, Iurii] Michigan State Univ, Kellogg Biol Stn, E Lansing, MI 48823 USA.
[Bertuzzi, Patrick; Ripoche, Dominique] INRA, AgroClim US1116, F-84914 Avignon, France.
[Biernath, Christian; Priesack, Eckart] Helmholtz Zentrum Munchen, Inst Soil Ecol, German Res Ctr Environm Hlth, D-85764 Neuherberg, Germany.
[Brisson, Nadine] INRA, Agron UMR0211, F-78750 Thiverval Grignon, France.
[Brisson, Nadine] AgroParisTech, Agron UMR0211, F-78750 Thiverval Grignon, France.
[Challinor, Andrew J.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Challinor, Andrew J.] Ctr Int Agr Trop, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia.
[Doltra, Jordi] Cantabrian Agr Res & Training Ctr, Muriedas 39600, Spain.
[Gayler, Sebastian] Univ Tubingen, Water & Earth Syst Sci Competence Cluster, D-72074 Tubingen, Germany.
[Grant, Robert F.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2E3, Canada.
[Heng, Lee] IAEA, A-1400 Vienna, Austria.
[Hooker, Josh] Univ Reading, Sch Agr Policy & Dev, Reading RG6 6AR, Berks, England.
[Hunt, Leslie A.] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada.
[Ingwersen, Joachim; Streck, Thilo] Univ Stuttgart Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany.
[Izaurralde, Roberto C.] Univ Maryland, Dept Geog Sci, Hyattsville, MD 20782 USA.
[Kersebaum, Kurt Christian; Nendel, Claas] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany.
[Mueller, Christoph; Waha, Katharina] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Kumar, Soora Naresh] Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India.
[O'leary, Garry] Dept Primary Ind Landscape & Water Sci, Horsham, Vic 3400, Australia.
[Olesen, Jorgen E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark.
[Osborne, Tom M.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading RG6 6BB, Berks, England.
[Semenov, Mikhail A.; Stratonovitch, Pierre] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England.
[Steduto, Pasquale] Food & Agr Org United Nations, I-00153 Rome, Italy.
[Stoeckle, Claudio O.] Washington State Univ, Pullman, WA 99164 USA.
[Supit, Iwan; Wolf, Joost] Wageningen Univ, NL-6700 AA Wageningen, Netherlands.
[Tao, Fulu] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China.
[Travasso, Maria] INTA CIRN, Inst Climate & Water, RA-1712 Castelar, Argentina.
[White, Jeffrey W.] USDA, Arid Land Agr Res Ctr, Maricopa, AZ 85138 USA.
RP Martre, P (reprint author), INRA, Genet Divers & Ecophysiol Cereals GDEC UMR1095, 5 Chemin Beaulieu, F-63100 Clermont Ferrand, France.
EM pierre.martre@clermont.inra.fr
RI Challinor, Andrew/C-4992-2008; Palosuo, Taru/B-9593-2012; Doltra,
Jordi/C-2106-2015; Thorburn, Peter/A-6884-2011; Priesack,
Eckart/M-7341-2014; Martre, Pierre/G-5399-2013; Mueller,
Christoph/E-4812-2016; Olesen, Jorgen/C-2905-2016
OI Cammarano, Davide/0000-0003-0918-550X; Wallach,
Daniel/0000-0003-3500-8179; Grant, Robert/0000-0002-8890-6231; Boote,
Kenneth/0000-0002-1358-5496; Kersebaum, Kurt
Christian/0000-0002-3679-8427; Priesack, Eckart/0000-0002-5088-9528;
Stratonovitch, Pierre/0000-0002-5806-2066; Challinor,
Andrew/0000-0002-8551-6617; Palosuo, Taru/0000-0003-4322-3450; Martre,
Pierre/0000-0002-7419-6558; Mueller, Christoph/0000-0002-9491-3550;
Olesen, Jorgen/0000-0002-6639-1273
NR 45
TC 48
Z9 48
U1 13
U2 102
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD FEB
PY 2015
VL 21
IS 2
BP 911
EP 925
DI 10.1111/gcb.12768
PG 15
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CA1DE
UT WOS:000348652400033
PM 25330243
ER
PT J
AU Goldsmith, MB
Sankar, BV
Haftka, RT
Goldberg, RK
AF Goldsmith, Marlana B.
Sankar, Bhavani V.
Haftka, Raphael T.
Goldberg, Robert K.
TI Effects of microstructural variability on thermo-mechanical properties
of a woven ceramic matrix composite
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE Ceramic-matrix composites; mechanical properties; porosity voids;
statistical properties; methods
ID MICRO-COMPUTED-TOMOGRAPHY; TEXTILE COMPOSITES; MICROMECHANICS; GEOMETRY;
PLAIN
AB The objectives of this paper include identifying important architectural parameters that describe the SiC/SiC five-harness satin weave composite and characterizing the statistical distributions and correlations of those parameters from photomicrographs of various cross sections. In addition, realistic artificial cross sections of a 2D representative volume element (RVE) are generated reflecting the variability found in the photomicrographs and include explicitly modeled voids (something not routinely done for woven CMCs). These models are used to make preliminary observation of the effects of architectural variability on the thermo-mechanical properties (material constants). Lastly, information is obtained on the sensitivity of linear thermo-mechanical properties to architectural variations. Two-dimensional finite element analysis is used in combination with a response surface and it is shown that the present method is effective in determining the effects of architectural variability on thermo-mechanical properties and their variability.
C1 [Goldsmith, Marlana B.; Sankar, Bhavani V.; Haftka, Raphael T.] Univ Florida, Gainesville, FL 32611 USA.
[Goldberg, Robert K.] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Goldsmith, MB (reprint author), Univ Florida, 231 MAE A Bldg,POB 116250, Gainesville, FL 32611 USA.
EM marlanabuf@gmail.com
FU NASA Graduate Student Research Program [NNX10AM49H]
FX The funding for this work was provided by the NASA Graduate Student
Research Program (grant no. NNX10AM49H).
NR 26
TC 2
Z9 2
U1 3
U2 17
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
EI 1530-793X
J9 J COMPOS MATER
JI J. Compos Mater.
PD FEB
PY 2015
VL 49
IS 3
BP 335
EP 350
DI 10.1177/0021998313519151
PG 16
WC Materials Science, Composites
SC Materials Science
GA CA1XB
UT WOS:000348701100007
ER
PT J
AU Nettles, AT
AF Nettles, Alan Tate
TI Notched compression strength of 18-ply laminates with various
percentages of 0 degrees plies
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE Compression-After-Impact; open-hole compression; percent 0 degrees
plies; knock-down factors
ID IMPACT STRENGTH; PREDICTION; COMPOSITES; FAILURE
AB The use of knockdown factors (percent reduction of undamaged compression strength) to account for flaws such as impact damage or holes have been used to infer the notched strength of laminates. It has been observed that this criterion tends to over-predict the strength of laminates with a high percentage of 0 degrees plies. This paper examines some limited data from the literature and presents new data that compares knockdown calculated notched compression strength values with those measured experimentally for laminates with various percentages of 0 degrees plies. Results show that the trend of over-predicting the notched compression strength of laminates as the percentage of 0 degrees plies increases, based on a knockdown factor, is observed, but the difference can be within scatter except at very high percentages of 0 degrees plies.
C1 NASA, MSFC, Huntsville, AL 35812 USA.
RP Nettles, AT (reprint author), NASA, MSFC, Bldg 4610, Huntsville, AL 35812 USA.
EM alan.t.nettles@nasa.gov
FU National Aeronautics and Space Administration under the Upper Stage
Program Office at Marshall Space Flight Center [136905.08.05.12]
FX This work was funded by the National Aeronautics and Space
Administration under the auspices of the Upper Stage Program Office at
Marshall Space Flight Center (136905.08.05.12).
NR 15
TC 0
Z9 0
U1 1
U2 2
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
EI 1530-793X
J9 J COMPOS MATER
JI J. Compos Mater.
PD FEB
PY 2015
VL 49
IS 4
BP 495
EP 505
DI 10.1177/0021998314521063
PG 11
WC Materials Science, Composites
SC Materials Science
GA CA4CW
UT WOS:000348852800009
ER
PT J
AU Norsk, P
Asmar, A
Damgaard, M
Christensen, NJ
AF Norsk, Peter
Asmar, Ali
Damgaard, Morten
Christensen, Niels Juel
TI Fluid shifts, vasodilatation and ambulatory blood pressure reduction
during long duration spaceflight
SO JOURNAL OF PHYSIOLOGY-LONDON
LA English
DT Article
ID INTERNATIONAL-SPACE-STATION; CARDIAC-OUTPUT; CARDIOVASCULAR REGULATION;
WATER IMMERSION; HEART-RATE; SUSTAINED MICROGRAVITY; RENAL-RESPONSES;
POSTURE CHANGE; PLASMA-VOLUME; HUMANS
AB Key points Weightlessness in space induces initially an increase in stroke volume and cardiac output, accompanied by unchanged or slightly reduced blood pressure. It is unclear whether these changes persist throughout months of flight. Here, we show that cardiac output and stroke volume increase by 35-41% between 3 and 6months on the International Space Station, which is more than during shorter flights. Twenty-four hour ambulatory brachial blood pressure is reduced by 8-10mmHg by a decrease in systemic vascular resistance of 39%, which is not a result of the suppression of sympathetic nervous activity, and the nightly dip is maintained in space. It remains a challenge to explore what causes the systemic vasodilatation leading to a reduction in blood pressure in space, and whether the unexpectedly high stroke volume and cardiac output can explain some vision acuity problems encountered by astronauts on the International Space Station.
Acute weightlessness in space induces a fluid shift leading to central volume expansion. Simultaneously, blood pressure is either unchanged or decreased slightly. Whether these effects persist for months in space is unclear. Twenty-four hour ambulatory brachial arterial pressures were automatically recorded at 1-2h intervals with portable equipment in eight male astronauts: once before launch, once between 85 and 192days in space on the International Space Station and, finally, once at least 2months after flight. During the same 24h, cardiac output (rebreathing method) was measured two to five times (on the ground seated), and venous blood was sampled once (also seated on the ground) for determination of plasma catecholamine concentrations. The 24h average systolic, diastolic and mean arterial pressures (mean +/- se) in space were reduced by 8 +/- 2mmHg (P=0.01; ANOVA), 9 +/- 2mmHg (P<0.001) and 10 +/- 3mmHg (P=0.006), respectively. The nightly blood pressure dip of 8 +/- 3mmHg (P=0.015) was maintained. Cardiac stroke volume and output increased by 35 +/- 10% and 41 +/- 9% (P<0.001); heart rate and catecholamine concentrations were unchanged; and systemic vascular resistance was reduced by 39 +/- 4% (P<0.001). The increase in cardiac stroke volume and output is more than previously observed during short duration flights and might be a precipitator for some of the vision problems encountered by the astronauts. The spaceflight vasodilatation mechanism needs to be explored further.
C1 [Norsk, Peter] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Norsk, Peter] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
[Norsk, Peter; Asmar, Ali] Univ Copenhagen, Fac Hlth Sci, Dept Biomed Sci, Copenhagen, Denmark.
[Asmar, Ali] Bispebjerg Hosp, Dept Clin Physiol & Nucl Med, Copenhagen, Denmark.
[Damgaard, Morten] Koege Hosp, Dept Clin Physiol & Nucl Med, Koege, Denmark.
[Christensen, Niels Juel] Herlev Univ Hosp, Dept Internal Med & Endocrinol, DK-2730 Herlev, Denmark.
RP Norsk, P (reprint author), NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM peter.norsk@nasa.gov
FU Danish Research Agency [2105-04-0006, 272-07-0614]; Danish Agency for
Science, Technology and Innovation, Copenhagen, Denmark
FX This work was supported by grant numbers 2105-04-0006 and 272-07-0614
from the Danish Research Agency and the Danish Agency for Science,
Technology and Innovation, Copenhagen, Denmark.
NR 49
TC 12
Z9 12
U1 0
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-3751
EI 1469-7793
J9 J PHYSIOL-LONDON
JI J. Physiol.-London
PD FEB 1
PY 2015
VL 593
IS 3
BP 573
EP 584
DI 10.1113/jphysiol.2014.284869
PG 12
WC Neurosciences; Physiology
SC Neurosciences & Neurology; Physiology
GA CB0CP
UT WOS:000349292900010
PM 25774397
ER
PT J
AU Devi, VM
Benner, DC
Smith, MAH
Mantz, AW
Sung, K
Crawford, TJ
Predoi-Cross, A
AF Devi, V. Malathy
Benner, D. Chris
Smith, Mary Ann H.
Mantz, Arlan W.
Sung, Keeyoon
Crawford, Timothy J.
Predoi-Cross, Adriana
TI Self- and air-broadened line shape parameters in the nu(2)+nu(3) band of
(CH4)-C-12: 4500-4630 cm(-1)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Methane; Lorentz width; Pressure-shift; Temperature dependence; Speed
dependence; Relaxation matrix
ID 2.3 MU-M; MULTISPECTRUM ANALYSIS; TEMPERATURE DEPENDENCES; COEFFICIENTS
WIDTHS; DATABASE; REGION; SHIFTS; CO; FREQUENCIES; LASER
AB Accurate knowledge of spectral line shape parameters is important for infrared transmission and radiance calculations in the terrestrial atmosphere. In this paper, we report the self- and air-broadened Lorentz half-widths, pressure-induced shifts and line mixing coefficients (via off-diagonal relaxation matrix elements) along with their temperature dependences for methane nu(2)+nu(3) absorption lines in the 4500-4630 cm(-1) region of the Octad. For this, we recorded 14 high-resolution, high signal to noise ratio (S/N) spectra of high-purity (99.95% C-12-enriched) samples of pure methane and its dilute mixtures in dry air between 298 K and 148 K. A Bruker IFS 125HR Fourier transform spectrometer (FTS) at the Jet Propulsion Laboratory, Pasadena, California, was used to obtain the experimental data. The absorption cell used for this study was a specially built 20.38 cm long coolable cell installed in its sample compartment. The sample pressures for the pure (CH4)-C-12 spectra were 4.5 - 385 Torr; for the air-broadened spectra the total pressures ranged between 95 and 300 Torr with the methane volume mixing ratios between 0.04 and 0.097. All 14 spectra were fitted simultaneously using an interactive multispectrum nonlinear least-squares curve fitting technique. The results are compared to values reported in the literature. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, POB 8795, Williamsburg, VA 23187 USA.
[Smith, Mary Ann H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
[Sung, Keeyoon; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Predoi-Cross, Adriana] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, POB 8795, Williamsburg, VA 23187 USA.
EM malathy.d.venkataraman@nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU Natural Sciences and Engineering Research Council of Canada
FX The authors are very grateful and thank LR Brown from JPL for the
encouragement, several useful discussions and support provided
throughout the course of this work. The research performed at the
College of William and Mary, Connecticut College and NASA Langley
Research Center was supported by NASA's Atmospheric Composition
Laboratory Research (ACLAB) program. The research at the Jet Propulsion
Laboratory (JPL) is performed under contract with National Aeronautics
and Space Administration. A. Predoi-Cross is grateful for the support
for this project provided by the Natural Sciences and Engineering
Research Council of Canada.
NR 33
TC 5
Z9 5
U1 0
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD FEB
PY 2015
VL 152
BP 149
EP 165
DI 10.1016/j.jqsrt.2014.11.011
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CA5PG
UT WOS:000348959700013
ER
PT J
AU Diaz, JA
Pieri, D
Wright, K
Sorensen, P
Kline-Shoder, R
Arkin, CR
Fladeland, M
Bland, G
Buongiorno, MF
Ramirez, C
Corrales, E
Alan, A
Alegria, O
Diaz, D
Linick, J
AF Andres Diaz, Jorge
Pieri, David
Wright, Kenneth
Sorensen, Paul
Kline-Shoder, Robert
Arkin, C. Richard
Fladeland, Matthew
Bland, Geoff
Buongiorno, Maria Fabrizia
Ramirez, Carlos
Corrales, Ernesto
Alan, Alfredo
Alegria, Oscar
Diaz, David
Linick, Justin
TI Unmanned Aerial Mass Spectrometer Systems for In-Situ Volcanic Plume
Analysis
SO JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY
LA English
DT Article
DE Miniature mass spectrometer; In-situ gas analysis; Harsh environment;
Unmanned aerial system; Validation and calibration; Remote sensing
comparison; Volcanic plume analysis; Volcanic monitoring; Airborne
instrumentation; Volcanic emissions analysis
ID GAS-ANALYSIS; EMISSIONS; NASA
AB Technology advances in the field of small, unmanned aerial vehicles and their integration with a variety of sensor packages and instruments, such as miniature mass spectrometers, have enhanced the possibilities and applications of what are now called unmanned aerial systems (UAS). With such technology, in situ and proximal remote sensing measurements of volcanic plumes are now possible without risking the lives of scientists and personnel in charge of close monitoring of volcanic activity. These methods provide unprecedented, and otherwise unobtainable, data very close in space and time to eruptions, to better understand the role of gas volatiles in magma and subsequent eruption products. Small mass spectrometers, together with the world's smallest turbo molecular pump, have being integrated into NASA and University of Costa Rica UAS platforms to be field-tested for in situ volcanic plume analysis, and in support of the calibration and validation of satellite-based remote sensing data. These new UAS-MS systems are combined with existing UAS flight-tested payloads and assets, such as temperature, pressure, relative humidity, SO2, H2S, CO2, GPS sensors, on-board data storage, and telemetry. Such payloads are capable of generating real time 3D concentration maps of the Turrialba volcano active plume in Costa Rica, while remote sensing data are simultaneously collected from the ASTER and OMI space-borne instruments for comparison. The primary goal is to improve the understanding of the chemical and physical properties of emissions for mitigation of local volcanic hazards, for the validation of species detection and abundance of retrievals based on remote sensing, and to validate transport models.
C1 [Andres Diaz, Jorge; Corrales, Ernesto; Alan, Alfredo; Alegria, Oscar; Diaz, David] Univ Costa Rica, CICANUM, GasLab, Phys Sch, San Jose, Costa Rica.
[Pieri, David; Linick, Justin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wright, Kenneth] INFICON Inc, E Syracuse, NY USA.
[Sorensen, Paul; Kline-Shoder, Robert] CREARE LLC, Hanover, NH USA.
[Arkin, C. Richard] Kennedy Space Ctr, Engn Serv Contract, Cape Canaveral, FL USA.
[Fladeland, Matthew] NASA, Ames Res Ctr, Mountain View, CA USA.
[Bland, Geoff] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Buongiorno, Maria Fabrizia] INGV, Rome, Italy.
[Ramirez, Carlos] Univ Costa Rica, RSN, Ctr Invest Ciencias Geol, Escuela Ctr Amer Geol, San Jose, Costa Rica.
RP Diaz, JA (reprint author), Univ Costa Rica, CICANUM, GasLab, Phys Sch, San Jose, Costa Rica.
EM jorge.andres.diaz@gmail.com
FU CICANUM; Universidad de Costa Rica [915-A9-091]
FX The authors thank the ASTER team for acquisition and access to ASTER
images. The UCR authors thank the CICANUM Director Ralph Garcia for his
support and project coordination with the Dean of Research at University
of Costa Rica; to Sara Azofiefa and Yetty Madrigal from the GasLab for
their daily help and logistics support of the project. The authors thank
Sergio Achi at the CICANUM Electronic lab for his help in
troubleshooting the PCBs, and to Victor Rodriguez ("Gato") at the
Physics School mechanical shop for machining some of the UAS-MS
components.; The authors acknowledge the Dean of Research at the
Universidad de Costa Rica for the financial support of part of this
project under grant 915-A9-091. This research was also carried out, in
part, under contract to NASA at the Jet Propulsion Laboratory of the
California Institute of Technology in Pasadena.
NR 25
TC 3
Z9 3
U1 4
U2 24
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1044-0305
EI 1879-1123
J9 J AM SOC MASS SPECTR
JI J. Am. Soc. Mass Spectrom.
PD FEB
PY 2015
VL 26
IS 2
BP 292
EP 304
DI 10.1007/s13361-014-1058-x
PG 13
WC Biochemical Research Methods; Chemistry, Analytical; Chemistry,
Physical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA CA9EH
UT WOS:000349223000012
PM 25588720
ER
PT J
AU Conversano, RW
Goebel, DM
AF Conversano, Ryan W.
Goebel, Dan M.
TI Improved Model of Long-Term Gain Increases in Traveling-Wave Tubes
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Traveling-wave tubes (TWTs)
ID PLASMA EDGE
AB An improved model to predict the gain increases in traveling-wave tubes (TWTs) during long-term operation is presented. The conventional gain growth model describes the pressure variation in a TWT over its life using an exponential decrease from the initial outgassing level to a constant base pressure. This model often shows an inability to capture the gain change behavior of many tubes during the transition between early life burn-in and long-term operation, leading to a significant underprediction of long-term gain increases. The model is improved here first through the introduction of another pressure-related term associated with desorption of gas from the tube's inner surfaces that exhibits a t-1/2 time dependence. This new pressure dependence is governed by the behavior of a Langmuirian adsorption isotherm. Second, the exponential pressure decay term is separated into two terms associated with early life and long-term operation with different outgassing time constants. The improved model shows a significantly better matching of long-term TWT gain growth data compared to the conventional model. In addition, the improved model predicts a more physical pressure behavior in the TWT with time.
C1 [Conversano, Ryan W.] Univ Calif Los Angeles, Plasma & Space Prop Lab, Wirz Res Grp, Los Angeles, CA 90095 USA.
[Goebel, Dan M.] CALTECH, Elect Prop Grp, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Conversano, RW (reprint author), Univ Calif Los Angeles, Plasma & Space Prop Lab, Wirz Res Grp, Los Angeles, CA 90095 USA.
EM ryan.w.conversano@jpl.nasa.gov; dan.m.goebel@jpl.nasa.gov
FU School of Engineering and Applied Sciences, University of California at
Los Angeles, Los Angeles, CA, USA; Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, CA, USA, through the National
Aeronautics and Space Administration
FX Manuscript received September 24, 2014; revised November 20, 2014;
accepted December 4, 2014. Date of current version January 20, 2015.
This work was supported in part by the School of Engineering and Applied
Sciences, University of California at Los Angeles, Los Angeles, CA, USA,
and in part by the Jet Propulsion Laboratory, California Institute of
Technology, Pasadena, CA, USA, through the National Aeronautics and
Space Administration. The review of this paper was arranged by Editor R.
Carter.
NR 11
TC 0
Z9 0
U1 1
U2 7
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 FEB
PY 2015
VL 62
IS 2
BP 652
EP 658
DI 10.1109/TED.2014.2380996
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA AZ7FZ
UT WOS:000348386100057
ER
PT J
AU Stickle, WB
Lindeberg, M
Rice, SD
AF Stickle, William B.
Lindeberg, Mandy
Rice, Stanley D.
TI Comparative freeze tolerance and physiological adaptations of three
species of vertically distributed rocky intertidal gastropods from
southeast Alaska
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Colligative osmolyte; Free amino acids; Gastropods; Freeze tolerance;
Intertidal zonation freeze events; Supercooling point
ID MELAMPUS-BIDENTATUS SAY; LITTORINA-LITTOREA L; CLIMATE-CHANGE; PULMONATE
GASTROPOD; THERMAL-STRESS; ICE NUCLEATOR; SNAILS; INVERTEBRATES;
SALINITY; PATTERNS
AB Tidal emersion temperatures are ameliorated on the coast of the continental United States because of the timing of low spring tides but spring low tides occur during the day in the summer and during the night in the winter in the inside passage north of Seattle. Extreme low air temperatures during the emersion of intertidal organisms at the northern intertidal sites render them vulnerable to freezing. To quantify the effects of freezing air temperatures on the supercooling point and freeze tolerance of Littorina sitkana from the upper intertidal, Nucella lima from the mid-intertidal, and Nucella lamellosa from the low intertidal, ambient temperatures were monitored with Hobo probes in two transects encompassing their intertidal distribution. To simulate the range of their emersion time the 2 and 5 h supercooling and freeze tolerance of N. lamellosa, 5 h supercooling and freeze tolerance of N. lima, and 5 and 10 h freeze tolerance of L. sitkana were determined. Seasonal variability in the degree of hydration and free amino acid concentrations of these species was also determined. The number of days when emersion temperature fell below 0 C increased with intertidal height as did the number of hours per day when the emersion temperature was <0 degrees C. The freeze tolerance temperature of these species increased directly with their intertidal distribution in 5 hour emersion exposures and did not change with emersion temperature duration typical of their intertidal range. L. sitkana and N. lima were more tolerant of freezing in the winter than in the summer but there was no seasonal difference in the freeze tolerance of N. lamellosa. The supercooling point of the species varied directly with their intertidal distribution, did not vary seasonally and reduced the period of time during emersion when they were subject to freezing. Free amino acids contributed to the increased freeze tolerance of L. sitkana and N. lima in the winter. Although the total free amino acid pool of N. lamellosa was significantly higher by 30.6% in the winter than the summer, no single free amino acid was higher. There were significantly higher concentrations of total FAA (54.6% increase), taurine (22%) and glycine (2150%) in N. lima in the winter. There were significant increases of total FAA (27.6% increase), taurine and glycine in the winter compared to the summer in L. sitkana. These FAA are important compatible colligative osmolytes which enhance winter freeze tolerance. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Stickle, William B.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Lindeberg, Mandy; Rice, Stanley D.] Alaska Fisheries Sci Ctr, Natl Oceanog & Atmospher Adm, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
RP Stickle, WB (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
EM zostic@Isu.edu
FU Louisiana Sea Grant
FX WBS gratefully acknowledges Louisiana State University for granting him
a sabbatical leave for the spring semester of the 2006-07 academic year
which allowed him to begin this project. We are also thankful to
Louisiana Sea Grant for awarding an undergraduate research opportunities
(UROP) grant to Kevin Vu who assisted with the freeze tolerance,
supercooling, and snail activity experiments in June 2008 and in
performing temperature probe analysis of the Pro V2 Hobo temperature
probe transects placed in the rocky intertidal zone at Bridget Cove, AK.
Ms. Jinny Johnson of the Texas A&M University Protein Chemistry
Laboratory performed the free amino acid analysis in a cheerful and
professional manner. [SS]
NR 19
TC 3
Z9 3
U1 4
U2 44
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 FEB
PY 2015
VL 463
BP 17
EP 21
DI 10.1016/j.jembe.2014.10.027
PG 5
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA CA0TD
UT WOS:000348628400003
ER
PT J
AU Nowakowski, AJ
Dewoody, JA
Fagan, ME
Willoughby, JR
Donnelly, MA
AF Nowakowski, A. Justin
Dewoody, J. Andrew
Fagan, Matthew E.
Willoughby, Janna R.
Donnelly, Maureen A.
TI Mechanistic insights into landscape genetic structure of two tropical
amphibians using field-derived resistance surfaces
SO MOLECULAR ECOLOGY
LA English
DT Article
DE connectivity; field experiments; fragmentation; gene flow; land use;
microclimate
ID REPRODUCTIVE RESOURCE SUPPLEMENTATION; MICROSATELLITE NULL ALLELES;
NORTHEASTERN COSTA-RICA; POPULATION-STRUCTURE; DENDROBATES-PUMILIO;
COUNTRYSIDE BIOGEOGRAPHY; AMBYSTOMA-MACULATUM; COMMUNITY STRUCTURE;
SPATIAL-ANALYSIS; ECOLOGICAL DATA
AB Conversion of forests to agriculture often fragments distributions of forest species and can disrupt gene flow. We examined effects of prevalent land uses on genetic connectivity of two amphibian species in northeastern Costa Rica. We incorporated data from field surveys and experiments to develop resistance surfaces that represent local mechanisms hypothesized to modify dispersal success of amphibians, such as habitat-specific predation and desiccation risk. Because time lags can exist between forest conversion and genetic responses, we evaluated landscape effects using land-cover data from different time periods. Populations of both species were structured at similar spatial scales but exhibited differing responses to landscape features. Litter frog population differentiation was significantly related to landscape resistances estimated from abundance and experiment data. Model support was highest for experiment-derived surfaces that represented responses to microclimate variation. Litter frog genetic variation was best explained by contemporary landscape configuration, indicating rapid population response to land-use change. Poison frog genetic structure was strongly associated with geographic isolation, which explained up to 45% of genetic variation, and long-standing barriers, such as rivers and mountains. However, there was also partial support for abundance- and microclimate response-derived resistances. Differences in species responses to landscape features may be explained by overriding effects of population size on patterns of differentiation for poison frogs, but not litter frogs. In addition, pastures are likely semi-permeable to poison frog gene flow because the species is known to use pastures when remnant vegetation is present, but litter frogs do not. Ongoing reforestation efforts will probably increase connectivity in the region by increasing tree cover and reducing area of pastures.
C1 [Nowakowski, A. Justin; Donnelly, Maureen A.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
[Dewoody, J. Andrew; Willoughby, Janna R.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA.
[Dewoody, J. Andrew] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA.
[Fagan, Matthew E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donnelly, Maureen A.] Florida Int Univ, Coll Arts & Sci, Miami, FL 33199 USA.
RP Nowakowski, AJ (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
EM Nowakowskia@gmail.com
RI DeWoody, James/C-4909-2008;
OI DeWoody, James/0000-0002-7315-5631; Willoughby,
Janna/0000-0002-0176-1878
FU Florida International University; OTS; Tinker Foundation; ASIH; NCHS;
Idea Wild
FX We thank M. Veiman for help in the field and laboratory and members of
the DeWoody laboratory for valuable feedback and assistance. We are
grateful to S. Spear, A. Storfer and J. Watling for comments that
improved the analyses and quality of the manuscript, to the Costa Rican
government (MINAE-SINAC) for permits and to The Organization for
Tropical Studies for logistical support. AJN was supported by Florida
International University Dissertation Evidence Acquisition and
Dissertation Year Fellowships, as well as by grants from OTS, Tinker
Foundation, ASIH, NCHS, and Idea Wild. All experimental protocols
received IACUC approval (#s 09-007, 10-023, & 12-003). This is
contribution number 295 to the programme in Tropical Biology at Florida
International University.
NR 106
TC 8
Z9 8
U1 3
U2 58
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0962-1083
EI 1365-294X
J9 MOL ECOL
JI Mol. Ecol.
PD FEB
PY 2015
VL 24
IS 3
BP 580
EP 595
DI 10.1111/mec.13052
PG 16
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA AZ9EZ
UT WOS:000348516900005
PM 25533403
ER
PT J
AU Woodall, CW
Russell, MB
Walters, BF
D'Amato, AW
Zhu, K
Saatchi, SS
AF Woodall, C. W.
Russell, M. B.
Walters, B. F.
D'Amato, A. W.
Zhu, K.
Saatchi, S. S.
TI Forest production dynamics along a wood density spectrum in eastern US
forests
SO TREES-STRUCTURE AND FUNCTION
LA English
DT Article
DE Wood density; Forest productivity; Volume; Biomass; Tree; Relative
density
ID NORTHEASTERN UNITED-STATES; ECONOMICS SPECTRUM; FUNCTIONAL TRAITS;
TROPICAL TREES; PLANT TRAITS; INDEX; MORTALITY; BIOMASS; GROWTH; SCALE
AB Emerging plant economics spectrum theories were confirmed across temperate forest systems of the eastern US where the use of a forest stand's mean wood density elucidated forest volume and biomass production dynamics integrating aspects of climate, tree mortality/growth, and rates of site occupancy.
As a tree's functional trait of wood density has been used to refine models of tree competition, it may also aid in evaluating hypotheses of forest production such as declining growth and mortality across a spectrum of increasing wood density. The goal of this study was to examine trends in aboveground live tree production as related to mean wood density using a region-wide repeated forest inventory across eastern US forests. Using quantile regression, the 90th percentile of volume and biomass accretion was negatively related to the mean wood density of a stand's constituent tree species. This relationship was strongest on forest sites with the highest number of growing season degree days, as growing season length influences the rates of stand development. For these sites, variations in volume and biomass accretion were most pronounced in stands with low mean tree wood density, which also demonstrated the highest rates of site occupancy and mortality. This study confirmed aspects of the emerging theory of "fast-slow" plant economics spectrums across temperate forest ecosystems. Stands with relatively low wood density appear to occupy sites more rapidly leading to a concomitantly higher rate of tree mortality, but with less biomass accretion relative to volume due to allocating biomass or carbon to a greater tree volume. In contrast, stands with higher wood density exhibited slower site occupancy due to high wood density construction costs, but with increased biomass relative to volume accretion. These findings highlight the potential application of the plant economics spectrum theory in refining our understanding of general patterns of forest stand production, the role of plant traits in forest management, and knowledge gaps such a shifts in tree allometry during stand development.
C1 [Woodall, C. W.; Walters, B. F.] USDA Forest Serv, No Res Stn, Forest Inventory & Anal Program, St Paul, MN 55114 USA.
[Russell, M. B.; D'Amato, A. W.] Univ Minnesota, Dept Forest Resources, Minneapolis, MN USA.
[Zhu, K.] Carnegie Inst Sci, Dept Global Ecol, Washington, DC 20005 USA.
[Zhu, K.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA.
[Saatchi, S. S.] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Woodall, CW (reprint author), USDA Forest Serv, No Res Stn, Forest Inventory & Anal Program, 1992 Folwell Ave, St Paul, MN 55114 USA.
EM cwoodall@fs.fed.us; russellm@umn.edu; bwalters@fs.fed.us;
damato@umn.edu; kai.zhu@stanford.edu; saatchi@jpl.nasa.gov
RI Zhu, Kai/H-1022-2013
OI Zhu, Kai/0000-0003-1587-3317
FU NASA Carbon Monitoring Systems [NNH11ZDA001N-CMS]
FX This study was funded in part by a NASA Carbon Monitoring Systems
(NNH11ZDA001N-CMS) grant.
NR 49
TC 2
Z9 2
U1 6
U2 34
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0931-1890
EI 1432-2285
J9 TREES-STRUCT FUNCT
JI Trees-Struct. Funct.
PD FEB
PY 2015
VL 29
IS 1
BP 299
EP 310
DI 10.1007/s00468-014-1083-1
PG 12
WC Forestry
SC Forestry
GA AZ8FZ
UT WOS:000348451800027
ER
PT J
AU Silva, AP
Burleigh, S
Hirata, CM
Obraczka, K
AF Silva, Aloizio P.
Burleigh, Scott
Hirata, Celso M.
Obraczka, Katia
TI A survey on congestion control for delay and disruption tolerant
networks
SO AD HOC NETWORKS
LA English
DT Article
DE Delay and disruption tolerant networks; Interplanetary networks;
Congestion control; Intermittent connectivity
ID DTN
AB Delay and disruption tolerant networks (DTNs) may experience frequent and long-lived connectivity disruptions. Unlike traditional networks, such as the TCP/IP-based Internet, DTNs are often subject to high latency caused by very long propagation delays (e.g., interplanetary communication) and/or intermittent connectivity. Another feature that sets DTNs apart from conventional networks is that there is no guarantee of end-to-end connectivity between source and destination. Such distinct features pose a number of technical challenges in designing core network functions such as routing and congestion control. In this paper, we survey the state-of-the-art in DTN congestion control. We propose a taxonomy to map the DTN congestion control design space and use it to classify existing DTN congestion control mechanisms. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Silva, Aloizio P.; Hirata, Celso M.] Ist Tecnol Aeronaut, Dept Elect & Comp Engn, Porto Alegre, RS, Brazil.
[Obraczka, Katia] Univ Calif Santa Cruz, Dept Comp Engn, Santa Cruz, CA 95064 USA.
[Burleigh, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Silva, AP (reprint author), Ist Tecnol Aeronaut, Dept Elect & Comp Engn, Porto Alegre, RS, Brazil.
EM aloizio@ita.br; scott.c.burleigh@jpl.nasa.gov; hirata@ita.br;
katia@soe.ucsc.edu
FU NASA; NSF [CNS 1321151]
FX Part of the research discussed in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. This work was partially funded by NSF under Project
CNS 1321151.
NR 65
TC 11
Z9 12
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1570-8705
EI 1570-8713
J9 AD HOC NETW
JI Ad Hoc Netw.
PD FEB
PY 2015
VL 25
SI SI
BP 480
EP 494
DI 10.1016/j.adhoc.2014.07.032
PN B
PG 15
WC Computer Science, Information Systems; Telecommunications
SC Computer Science; Telecommunications
GA AY7RL
UT WOS:000347756600015
ER
PT J
AU Smialek, JL
AF Smialek, James L.
TI Oxygen diffusivity in alumina scales grown on Al-MAX phases
SO CORROSION SCIENCE
LA English
DT Article
DE Ceramic; Thermal cycling; Oxidation; High temperature corrosion
ID TEMPERATURE OXIDATION BEHAVIOR; POTENTIAL GRADIENTS; AL2O3 SCALES;
ALLOYS; AIR; 1200-DEGREES-C; MECHANISM; KINETICS; CR2ALC; TI2ALC
AB Ti3AlC2, Ti2AlC, and Cr2AlC are oxidation resistant MAX phase compounds distinguished by the formation of protective Al2O3 scales with well controlled kinetics. A modified Wagner treatment was used to calculate interfacial grain boundary diffusivity from scale growth rates and corresponding interfacial grain size, based on the pressure dependence of oxygen vacancies and diffusivity. MAX phase data from the literature yielded grain boundary diffusivity nearly coincident with that for Zr-doped FeCrAl (and many other FeCrAl alloys), suggesting similar oxidation mechanisms. The consolidated body of diffusivity data was consistent with an activation energy of 375 +/- 25 kJ/mol. Published by Elsevier Ltd.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM james.l.smialek@nasa.gov
NR 27
TC 12
Z9 12
U1 7
U2 49
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0010-938X
EI 1879-0496
J9 CORROS SCI
JI Corrosion Sci.
PD FEB
PY 2015
VL 91
BP 281
EP 286
DI 10.1016/j.corsci.2014.11.030
PG 6
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AZ5MJ
UT WOS:000348264700028
ER
PT J
AU Woebken, D
Burow, LC
Behnam, F
Mayali, X
Schintlmeister, A
Fleming, ED
Prufert-Bebout, L
Singer, SW
Cortes, AL
Hoehler, TM
Pett-Ridge, J
Spormann, AM
Wagner, M
Weber, PK
Bebout, BM
AF Woebken, Dagmar
Burow, Luke C.
Behnam, Faris
Mayali, Xavier
Schintlmeister, Arno
Fleming, Erich D.
Prufert-Bebout, Leslie
Singer, Steven W.
Lopez Cortes, Alejandro
Hoehler, Tori M.
Pett-Ridge, Jennifer
Spormann, Alfred M.
Wagner, Michael
Weber, Peter K.
Bebout, Brad M.
TI Revisiting N-2 fixation in Guerrero Negro intertidal microbial mats with
a functional single-cell approach
SO ISME JOURNAL
LA English
DT Article
ID SULFATE-REDUCING BACTERIA; IN-SITU HYBRIDIZATION; NITROGEN-FIXATION;
CYANOBACTERIAL MATS; OLIGONUCLEOTIDE MICROARRAY; COMMUNITY STRUCTURE;
BAJA-CALIFORNIA; GENE-EXPRESSION; LYNGBYA-SP; MARINE
AB Photosynthetic microbial mats are complex, stratified ecosystems in which high rates of primary production create a demand for nitrogen, met partially by N-2 fixation. Dinitrogenase reductase (nifH) genes and transcripts from Cyanobacteria and heterotrophic bacteria (for example, Deltaproteobacteria) were detected in these mats, yet their contribution to N-2 fixation is poorly understood. We used a combined approach of manipulation experiments with inhibitors, nifH sequencing and single-cell isotope analysis to investigate the active diazotrophic community in intertidal microbial mats at Laguna Ojo de Liebre near Guerrero Negro, Mexico. Acetylene reduction assays with specific metabolic inhibitors suggested that both sulfate reducers and members of the Cyanobacteria contributed to N-2 fixation, whereas N-15(2) tracer experiments at the bulk level only supported a contribution of Cyanobacteria. Cyanobacterial and nifH Cluster III (including deltaproteobacterial sulfate reducers) sequences dominated the nifH gene pool, whereas the nifH transcript pool was dominated by sequences related to Lyngbya spp. Single-cell isotope analysis of N-15(2)-incubated mat samples via high-resolution secondary ion mass spectrometry (NanoSIMS) revealed that Cyanobacteria were enriched in N-15, with the highest enrichment being detected in Lyngbya spp. filaments (on average 4.4 at% N-15), whereas the Deltaproteobacteria (identified by CARD-FISH) were not significantly enriched. We investigated the potential dilution effect from CARD-FISH on the isotopic composition and concluded that the dilution bias was not substantial enough to influence our conclusions. Our combined data provide evidence that members of the Cyanobacteria, especially Lyngbya spp., actively contributed to N-2 fixation in the intertidal mats, whereas support for significant N-2 fixation activity of the targeted deltaproteobacterial sulfate reducers could not be found.
C1 [Woebken, Dagmar; Burow, Luke C.; Spormann, Alfred M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA.
[Woebken, Dagmar; Burow, Luke C.; Spormann, Alfred M.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
[Woebken, Dagmar; Burow, Luke C.; Fleming, Erich D.; Prufert-Bebout, Leslie; Hoehler, Tori M.; Bebout, Brad M.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA USA.
[Woebken, Dagmar; Behnam, Faris; Wagner, Michael] Univ Vienna, Dept Microbiol & Ecosyst Sci, Div Microbial Ecol, A-1090 Vienna, Austria.
[Mayali, Xavier; Pett-Ridge, Jennifer; Weber, Peter K.] Lawrence Livermore Natl Lab, Phys & Life Sci Directorate, Livermore, CA USA.
[Schintlmeister, Arno; Wagner, Michael] Univ Vienna, Large Instrument Facil Adv Isotope Res, A-1090 Vienna, Austria.
[Singer, Steven W.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
[Lopez Cortes, Alejandro] Northwestern Ctr Biol Res CIBNOR, Lab Geomicrobiol & Biotechnol, La Paz, Mexico.
RP Woebken, D (reprint author), Univ Vienna, Dept Microbiol & Ecosyst Sci, Div Microbial Ecol, Waehringer Guertel 18, A-1090 Vienna, Austria.
EM dwoebken@gmail.com; brad.m.bebout@nasa.gov
RI Woebken, Dagmar/A-4447-2013; Wagner, Michael/A-7801-2011;
OI Wagner, Michael/0000-0002-9778-7684; Woebken, Dagmar/0000-0002-1314-9926
FU National Commission of Aquaculture and Fishery of the Ministry of
Agriculture, Livestock, Rural Development, Fisheries and Food (Mexico)
[DAPA/2/080310/734]; DOE [DE-AC52-07NA27344, DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science, Office of Biological and
Environmental Research, Genomic Sciences Program [SCW1039]; German
Research Foundation (Deutsche Forschungsgemeinschaft); Austrian Science
Fund (FWF) [P 25700-B20]; European Research Council [294343]
FX We thank Angela Detweiler, Jan Dolinsek, Mike Kubo and Christina Ramon
for their excellent technical assistance, Jose Q Garcia-Maldonado for
his assistance in the field, Andrew McDowell at UC Berkeley for IRMS
analyses, and Stephanie A Eichorst for helpful comments on the
manuscript. We are grateful for access to the field site and for the
logistical support provided by Exportadora de Sal, S.A. de C.V. This
work was performed under Fishery Permit DAPA/2/080310/734 granted by the
National Commission of Aquaculture and Fishery of the Ministry of
Agriculture, Livestock, Rural Development, Fisheries and Food (Mexico).
Work at LLNL was performed under the auspices of the DOE under contract
DE-AC52-07NA27344. Work at LBNL was performed under the auspices of the
DOE under contract DE-AC02-05CH11231. This material is based upon work
supported by the U.S. Department of Energy, Office of Science, Office of
Biological and Environmental Research, Genomic Sciences Program, under
contract number SCW1039. This work was further financially supported by
the German Research Foundation (Deutsche Forschungsgemeinschaft) (to DW)
and the Austrian Science Fund (FWF) (P 25700-B20 to DW). FB and MW were
supported by the European Research Council (Advanced Grant Nitrification
Reloaded (NITRI-CARE) 294343).
NR 53
TC 13
Z9 13
U1 11
U2 54
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 FEB
PY 2015
VL 9
IS 2
BP 485
EP 496
DI 10.1038/ismej.2014.144
PG 12
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA AZ4SQ
UT WOS:000348213600018
PM 25303712
ER
PT J
AU Ikeda, KT
Hirose, Y
Hiraoka, K
Noro, E
Fujishima, K
Tomita, M
Kanai, A
AF Ikeda, Kahori T.
Hirose, Yuka
Hiraoka, Kiriko
Noro, Emiko
Fujishima, Kosuke
Tomita, Masaru
Kanai, Akio
TI Identification, expression, and molecular evolution of microRNAs in the
"living fossil" Triops cancriformis (tadpole shrimp)
SO RNA-A PUBLICATION OF THE RNA SOCIETY
LA English
DT Article
DE microRNA; deep sequencing; development; evolution; T. cancriformis
ID ARGONAUTE PROTEINS; SEQUENCE ALIGNMENT; ANIMAL DEVELOPMENT; SMALL RNAS;
PREDICTION; GENOME; GENES; ANNOTATION; BIOGENESIS; ALGORITHMS
AB MicroRNAs have been identified and analyzed in various model species, but an investigation of miRNAs in nonmodel species is required for a more complete understanding of miRNA evolution. In this study, we investigated the miRNAs of the nonmodel species Triops cancriformis (tadpole shrimp), a "living fossil," whose morphological form has not changed in almost 200 million years. Dramatic ontogenetic changes occur during its development. To clarify the evolution of miRNAs, we comparatively analyzed its miRNAs and the components of its RNAi machinery. We used deep sequencing to analyze small RNA libraries from the six different developmental stages of T. cancriformis (egg, first-fourth instars, and adult), and also analyzed its genomic DNA with deep sequencing. We identified 180 miRNAs (87 conserved miRNAs and 93 novel candidate miRNAs), and deduced the components of its RNAi machinery: the DICER1, AGO1-3, PIWI, and AUB proteins. A comparative miRNA analysis of T. cancriformis and Drosophila melanogaster showed inconsistencies in the expression patterns of four conserved miRNAs. This suggests that although the miRNA sequences of the two species are very similar, their roles differ across the species. An miRNA conservation analysis revealed that most of the conserved T. cancriformis miRNAs share sequence similarities with those of arthropods, although T. cancriformis is called a "living fossil." However, we found that let-7 and DICER1 of T. cancriformis are more similar to those of the vertebrates than to those of the arthropods. These results suggest that miRNA systems of T. cancriformis have evolved in a unique fashion.
C1 [Ikeda, Kahori T.; Hirose, Yuka; Hiraoka, Kiriko; Noro, Emiko; Fujishima, Kosuke; Tomita, Masaru; Kanai, Akio] Keio Univ, Inst Adv Biosci, Tsuruoka, Yamagata 9970017, Japan.
[Ikeda, Kahori T.; Hirose, Yuka; Tomita, Masaru; Kanai, Akio] Keio Univ, Grad Sch Media & Governance, Syst Biol Program, Fujisawa, Kanagawa 2520882, Japan.
[Fujishima, Kosuke] NASA, Ames Res Ctr, Univ Affiliated Res Ctr, Moffett Field, CA 94043 USA.
[Tomita, Masaru; Kanai, Akio] Keio Univ, Fac Environm & Informat Studies, Fujisawa, Kanagawa 2520882, Japan.
RP Kanai, A (reprint author), Keio Univ, Inst Adv Biosci, Tsuruoka, Yamagata 9970017, Japan.
EM akio@sfc.keio.ac.jp
OI Kanai, Akio/0000-0002-6362-2419; Fujishima, Kosuke/0000-0002-8844-812X
FU Yamagata Prefectural Government; Tsuruoka City, Japan; Japan Society for
the Promotion of Science (JSPS)
FX We thank Keiji Igarashi (Tohoku University of Community Service and
Science, Japan) for sharing his extensive knowledge of the tadpole
shrimp. We also thank Dr. Yoshiki Ikeda (Institute for Advanced
Biosciences, Keio University, Japan) for valuable discussions and
technical assistance, and all the members of the RNA group at the
Institute for Advanced Biosciences, Keio University, Japan, for their
insightful discussions. This research was supported, in part, by
research funds from the Yamagata Prefectural Government and Tsuruoka
City, Japan, and a research grant from the Japan Society for the
Promotion of Science (JSPS).
NR 52
TC 4
Z9 4
U1 1
U2 10
PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT
PI COLD SPRING HARBOR
PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA
SN 1355-8382
EI 1469-9001
J9 RNA
JI RNA-Publ. RNA Soc.
PD FEB
PY 2015
VL 21
IS 2
BP 230
EP 242
DI 10.1261/rna.045799.114
PG 13
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA AZ2AG
UT WOS:000348036400008
PM 25525151
ER
PT J
AU Jones, SM
Anderson, MS
Davies, AG
Kirby, JP
Burchell, MJ
Cole, MJ
AF Jones, S. M.
Anderson, M. S.
Davies, A. G.
Kirby, J. P.
Burchell, M. J.
Cole, M. J.
TI Aerogel dust collection for in situ mass spectrometry analysis
SO ICARUS
LA English
DT Article
DE Interplanetary dust; Experimental techniques; Impact processes
ID HYPERVELOCITY IMPACTS; COMET 81P/WILD-2; SILICA AEROGEL; STARDUST;
MICROPARTICLES; PARTICLES; ANALYZER; CAPTURE; ION; PROJECTILES
AB The current technique for conducting in situ mass spectroscopic analysis of dust around extraterrestrial bodies is to have the dust impact a solid plate and analyze the atoms and molecular fragments resulting from the high speed impact. Due to the fact that the kinetic energy from the impact is converted primarily to thermal energy, much of the organic compounds present in the dust may be significantly altered or destroyed. To avoid this problem, aerogel could be used to capture the dust grains, largely intact, maintaining the integrity of the organic compounds in the interior of the dust grains. To demonstrate that organic molecules, present as minor components of silica particles, would survive hypervelocity capture in aerogel and can then be analyzed with mass spectrometry, several light gas gun impact tests and analyses were conducted. Fine particles containing polycyclic aromatic hydrocarbons (PAHs) were captured in aerogel at 5.5 km s(-1). The flow of metastable helium from a Direct Analysis Real Time (DART) source was used to desorb and ionize the organics, which were then analyzed with a mass spectrometer. The PAHs were detected and identified by the DART-MS, demonstrating that this method could be used on future flight instruments. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Jones, S. M.; Anderson, M. S.; Davies, A. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kirby, J. P.] Planetaty Sci Inst, Tucson, AZ 85719 USA.
[Kirby, J. P.] Univ Washington, Seattle, WA 98195 USA.
[Burchell, M. J.; Cole, M. J.] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England.
RP Jones, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Burchell, Mark/0000-0002-2680-8943
FU Chief Scientist's Office at JPL; STFC research council; National
Aeronautics and Space Administration
FX We would like to thank Pete Schultz at Brown University and the AVGR
facility at Ames Research Center for arranging for the impact tests to
be done under the PG&G program, Julie Castillo and Randy Mielke of JPL
for making some of the projectile particles and the Chief Scientist's
Office at JPL for providing funding to conduct this study.; The STFC
research council is thanked for funding impact work at the University of
Kent.; The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 36
TC 0
Z9 0
U1 1
U2 18
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 FEB
PY 2015
VL 247
BP 71
EP 76
DI 10.1016/j.icarus.2014.09.047
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1ER
UT WOS:000346691400005
ER
PT J
AU Li, F
Yan, JG
Xu, LY
Jin, SG
Rodriguez, JAP
Dohm, JH
AF Li, Fei
Yan, Jianguo
Xu, Luyuan
Jin, Shuanggen
Rodriguez, J. Alexis P.
Dohm, James H.
TI A 10 km-resolution synthetic Venus gravity field model based on
topography
SO ICARUS
LA English
DT Article
DE Venus; Interior; Geophysics
ID ISOSTATIC COMPENSATION; ORDER MODEL; SUPPORT
AB A high resolution gravity field model is extremely important in the exploration of Venus. In this paper, we present a 3-dimensional Venus gravity field VGM2014 constructed by using the latest gravity and topography models, residual terrain model (RTM) and the Airy-Heiskanen isostatic compensation model. The VGM2014 is the first 10 km scale Venus gravity field model; the final results are representations of the 3-dimensional surface gravity accelerations and gravity disturbances for Venus. We found that the optimal global compensation depth of Venus is about 60 km, and the crustal density is potentially less than the commonly accepted value of 2700-2900 kg m(-3). This model will be potentially beneficial for the precise orbit determination and landing navigation of spacecraft around Venus, and may be utilized as a priori model for Venus gravity field simulation and inversion studies. The VGM2014 does not incorporate direct gravity information beyond degree 70 and it is not recommended for small-scale geophysical interpretation. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Li, Fei; Yan, Jianguo] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
[Yan, Jianguo] Natl Astron Observ Japan, RISE Project, Oshu 0230861, Japan.
[Xu, Luyuan] Wuhan Univ, Chinese Antarctic Ctr Surveying & Mapping, Wuhan 430070, Peoples R China.
[Jin, Shuanggen] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 20030, Peoples R China.
[Rodriguez, J. Alexis P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dohm, James H.] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
RP Yan, JG (reprint author), Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
RI Jin, Shuanggen/B-8094-2008
OI Jin, Shuanggen/0000-0002-5108-4828
FU National Natural Science Foundation of China [41174019, 41374024];
National Keystone Basic Research Program [2012CB72000]
FX We used the Generic Mapping Tools (GMT) software for drawing the
figures. Our spherical harmonic analyses were performed using the freely
available software archive SHTOOLS (http://www.ipgp.fr/similar to
wieczor/SH/SH.html). Dr. Stephen McClure is appreciated for his
discussion on the manuscript. This research is supported by Grant of the
National Natural Science Foundation of China (41174019, 41374024) and
the National Keystone Basic Research Program (2012CB72000).
NR 24
TC 0
Z9 0
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD FEB
PY 2015
VL 247
BP 103
EP 111
DI 10.1016/j.icarus.2014.09.052
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1ER
UT WOS:000346691400009
ER
PT J
AU Bottke, WF
Vokrouhlicky, D
Walsh, KJ
Delbo, M
Michel, P
Lauretta, DS
Campins, H
Connolly, HC
Scheeres, DJ
Chelsey, SR
AF Bottke, William F.
Vokrouhlicky, David
Walsh, Kevin J.
Delbo, Marco
Michel, Patrick
Lauretta, Dante S.
Campins, Humberto
Connolly, Harold C., Jr.
Scheeres, Daniel J.
Chelsey, Steven R.
TI In search of the source of asteroid (101955) Bennu: Applications of the
stochastic YORP model
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, dynamics; Near-Earth objects; Celestial mechanics
ID NEAR-EARTH OBJECTS; MAIN-BELT ASTEROIDS; SPIN RATE DISTRIBUTION;
DYNAMICAL EVOLUTION; COLLISIONAL HISTORY; SIZE DISTRIBUTIONS; MASSIVE
ASTEROIDS; CLOSE ENCOUNTERS; POTENTIAL TARGET; BINARY ASTEROIDS
AB Asteroid (101955) Bennu, the target of NASA's OSIRIS-REx sample return mission, is a D approximate to 0.5 km diameter low albedo near-Earth object. It has a spectral signature consistent with primitive carbonaceous chondrites, and an orbit similar to that of the Earth. A plausible evolution scenario for Bennu is that it migrated inward across the inner main belt from a low albedo family by Yarkovsky thermal forces over many hundreds of Myr. Eventually, it entered a resonance that took it into the terrestrial planet region, where a combination of planetary encounters and resonances took it to its current orbit over a few Myr to tens of Myr. When it departed the main belt, Bennu probably had an eccentricity 0.1 < e < 0.2 and an inclination 1 degrees < i < 6 degrees. Several low albedo families have the appropriate dynamical, color, albedo, and broad spectral characteristics to produce Bennu: Clarissa, Erigone, Eulalia, New Polana, and Sulamitis.
Here we used a suite of numerical simulations to determine the ages of the families above, how Bennu reached its current orbit, and the most probable source family for Bennu. Specifically, we tracked test Bennu-like asteroids evolving in semimajor axis by the coupled Yarkovsky/YORP effects, incorporating a new formalism for how YORP torques modify the spin vector evolution of small asteroids. Using results and insights provided by Statler (Statler, T.S. [2009]. Icarus 202, 502-513), we assumed that modest shape changes to asteroids, produced by a variety of processes (e.g., crater formation, changes to asteroid rotational angular momentum by YORP), caused the test asteroids' spin rates, but not their obliquities, to undergo a random walk. This "stochastic YORP" mechanism slows down how often asteroids reach YORP endstates (i.e., spinning up so fast that the asteroid sheds mass, spinning down so much the asteroid enters into a tumbling rotation state). This new model allowed us to reproduce the semimajor axis distribution of observed family members from Clarissa, Erigone, Eulalia, New Polana, and Sulamitis. In the process, we derived model family formation ages of 60 Myr old, 130 30 Myr old, 830(-100)(+370) Myr old, 1400 150 Myr old, and 200 40 Myr, respectively.
Next, using a Monte-Carlo code to track millions of test asteroids from each of the families above to main belt escape routes capable of producing Bennu-like orbits, we found the most likely parent families for Bennu are Eulalia and New Polana. On average, more than twice as many 0.5 km objects from the New Polana family reach Bennu's orbit as those from the Eulalia family. This corresponds to the New Polana and Eulalia families having a 70(-4)(+8)% and 30(-8)(+4)% probability of producing Bennu, respectively. Comparable runs to deduce the source of the Hayabusa 2 target, the low albedo 0.87 km diameter near-Earth object (162173) 1999 JU3, produced similar probabilities for both families. The former Marco-Polo-R target, the 1.9 km asteroid (175706) 1996 FG3, however, has a 85(-83)(+4)% probability of coming from the Eulalia family and a 15(-4)(+83)% probability of coming from the New Polana family. The reason for this switch is that 1996 FG3 may have been part of Yarkovsky/YORP-produced wave of like-sized bodies that is only now reaching the terrestrial planet region. We suggest that the top-like shape of Bennu is a byproduct of mass wasting and/or mass shedding events produced by YORP spin up during its long journey across the inner main belt. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Bottke, William F.; Walsh, Kevin J.] Southwest Res Inst, Boulder, CO 80302 USA.
[Bottke, William F.; Walsh, Kevin J.] Inst Sci Explorat Targets, Boulder, CO 80302 USA.
[Vokrouhlicky, David] Charles Univ Prague, Inst Astron, CR-18000 Prague 8, Czech Republic.
[Delbo, Marco; Michel, Patrick] Univ Nice Sophia Antipolis, CNRS, Cote dAzur Observ, Nice, France.
[Lauretta, Dante S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Campins, Humberto] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Connolly, Harold C., Jr.] CUNY, Kingsborough Community Coll, Dept Phys Sci, Brooklyn, NY 10023 USA.
[Connolly, Harold C., Jr.] CUNY, Grad Ctr, New York, NY 10016 USA.
[Connolly, Harold C., Jr.] AMNH, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Scheeres, Daniel J.] Univ Colorado, Dept Aerosp Engn Sci, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Chelsey, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bottke, WF (reprint author), Southwest Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM bottke@boulder.swri.edu
FU NASA [NNM10AA11C]; Center for Lunar Origin and Evolution of NASA's Lunar
Science Institute; NASA's Solar System Evolution Research Virtual
Institute (SSERVI) program through a grant to the Institute for the
Science of Exploration Targets [NNA14ABO3A]; NASA's OSIRIS-REx mission;
Czech Grant Agency [P209-13-01308S]; French CNES; NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center
FX We thank Valerio Carruba and an anonymous referee for their careful and
constructive reviews that improved this paper. We also thank the
innumerable helpful comments and suggestions that came from members of
the OSIRIS-REx science team. Research funds for William Bottke were
provided by NASA's OSIRIS-REx mission; NASA Contract NNM10AA11C (D.S.
Lauretta, PI). Support for Kevin Walsh came from the Center for Lunar
Origin and Evolution of NASA's Lunar Science Institute, and NASA's Solar
System Evolution Research Virtual Institute (SSERVI) program through a
grant to the Institute for the Science of Exploration Targets
(NNA14ABO3A), at the Southwest Research Institute in Boulder. The work
of David Vokrouhlicky was partially supported by research grant
P209-13-01308S of the Czech Grant Agency. Marco Delbo and Patrick Michel
acknowledge support from the French CNES. 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 127
TC 23
Z9 23
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD FEB
PY 2015
VL 247
BP 191
EP 217
DI 10.1016/j.icarus.2014.09.046
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1ER
UT WOS:000346691400015
ER
PT J
AU Stevens, MH
Evans, JS
Lumpe, J
Westlake, JH
Ajello, JM
Bradley, ET
Esposito, LW
AF Stevens, Michael H.
Evans, J. Scott
Lumpe, Jerry
Westlake, Joseph H.
Ajello, Joseph M.
Bradley, E. Todd
Esposito, Larry W.
TI Molecular nitrogen and methane density retrievals from Cassini UVIS
dayglow observations of Titan's upper atmosphere
SO ICARUS
LA English
DT Article
DE Titan, atmosphere; Atmospheres, composition; Aeronomy; Spectroscopy
ID SOLAR EUV; ELECTRON-IMPACT; STELLAR OCCULTATIONS; THERMAL STRUCTURE;
CROSS-SECTIONS; ERROR ANALYSIS; MODEL; THERMOSPHERE; PHOTOELECTRON;
IRRADIANCE
AB We retrieve number densities of molecular nitrogen (N-2) and methane (CH4) from Titan's upper atmosphere using the UV dayglow. We use Cassini Ultraviolet Imaging Spectrograph (UVIS) limb observations from 800 to 1300 km of the N I 1493 A and N II 1085 angstrom multiplets, both produced directly from photo-fragmentation of N-2. UVIS N-2 and CH4 densities are in agreement with measurements from Cassini's Ion Neutral Mass Spectrometer (INMS) from the same flyby if INMS densities are scaled up by a factor of 3.0 as reported in previous studies. Analysis of three Cassini flybys of Titan shows that (1) the CH4 homopause on Titan is between 900 and 1100 km, (2) upper atmospheric temperatures vary by less than 10 K over 6 h at the same geographic location and (3) from 1100 to 1700 local solar time temperatures also vary by less than 10 K. The capability of retrieving the global-scale composition from these data complements existing techniques and significantly advances the study of upper atmospheric variability at Titan and for any other atmosphere with a detectable UV dayglow. Published by Elsevier Inc.
C1 [Stevens, Michael H.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Evans, J. Scott] Computat Phys Inc, Springfield, VA 22151 USA.
[Lumpe, Jerry] Computat Phys Inc, Boulder, CO 80301 USA.
[Westlake, Joseph H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Ajello, Joseph M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bradley, E. Todd] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Esposito, Larry W.] Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
RP Stevens, MH (reprint author), Naval Res Lab, Div Space Sci, 4555 Overlook Ave SW, Washington, DC 20375 USA.
RI Westlake, Joseph/G-2732-2015
OI Westlake, Joseph/0000-0003-0472-8640
FU NASA [NNH13AV62I]
FX MHS, JSE and JMA gratefully acknowledge the NASA Cassini Data Analysis
Program for supporting this work (#NNH13AV62I). We thank A. Jouchoux, R.
West and the UVIS Operations Team for their help in arranging the
observations presented herein and R. Meier for assistance with the solar
irradiance calculations for this work and for many useful discussions.
We also thank T. Koskinen and F.J. Capalbo for providing the occultation
data shown in this work.
NR 53
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD FEB
PY 2015
VL 247
BP 301
EP 312
DI 10.1016/j.icarus.2014.10.008
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1ER
UT WOS:000346691400021
ER
PT J
AU Schuet, S
Timucin, D
Wheeler, K
AF Schuet, Stefan
Timucin, Dogan
Wheeler, Kevin
TI Physics-Based Precursor Wiring Diagnostics for Shielded-Twisted-Pair
Cable
SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT
LA English
DT Article
DE Bayesian methods; electromagnetic modeling; fault diagnosis; measurement
uncertainty; optimization methods; probability; scattering parameters;
wiring
ID FAULT LOCATION; MEASUREMENT UNCERTAINTY; DOMAIN REFLECTOMETRY; INVERSE
SCATTERING; TRANSMISSION-LINE; PARAMETERS; SYSTEMS; GUM
AB The capability to locate and characterize precursor wiring faults, such as chafing or pinching potentially enables preventive maintenance well before hard failures occur, thus maximizing system functionality and safety while minimizing out-of-service time. Toward this goal, results are presented on the application of a deterministic Bayesian inference procedure well suited for detecting chafing and pinch faults through the use of a newly developed physics-based model for shielded-twisted-pair cable. This method is significantly faster than more traditional nondeterministic Bayesian methods, such as Markov chain Monte Carlo, and retains many of the desirable features inherent to the Bayesian approach. These include the ability to quantify estimation uncertainty and model evidence in probabilistic terms, which then enables the study and design of noise-tolerant fault detection algorithms capable of classifying different types of faults. The fault parameter estimation results from both laboratory and field measurements on a C17 jet engine are shown to demonstrate the achievable model fidelity and the overall viability of the approach.
C1 [Schuet, Stefan; Timucin, Dogan; Wheeler, Kevin] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Schuet, S (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM stefan.r.schuet@nasa.gov
FU NASA Aviation Safety Program through the Vehicle Systems Safety
Technologies Project
FX This work was supported by the NASA Aviation Safety Program through the
Vehicle Systems Safety Technologies Project. The Associate Editor
coordinating the review process was Dr. John Sheppard.
NR 48
TC 0
Z9 0
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9456
EI 1557-9662
J9 IEEE T INSTRUM MEAS
JI IEEE Trans. Instrum. Meas.
PD FEB
PY 2015
VL 64
IS 2
BP 378
EP 391
DI 10.1109/TIM.2014.2347216
PG 14
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AY3ZU
UT WOS:000347518800009
ER
PT J
AU Abel, PB
Eppell, SJ
Walker, AM
Zypman, FR
AF Abel, Phillip B.
Eppell, Steven J.
Walker, Abigail M.
Zypman, Fredy R.
TI Viscosity of liquids from the transfer function of microcantilevers
SO MEASUREMENT
LA English
DT Article
DE Microcantilever; Microfluids; Viscosity measurement
ID ATOMIC-FORCE MICROSCOPE; FREQUENCY-RESPONSE; VISCOUS FLUIDS;
CANTILEVERS; SURFACE
AB A method is presented to obtain the viscosity and density of a fluid from the mechanical frequency response of a microcantilever beam immersed in fluids. The technique is a practical solution to perform the measurement when only very small quantities of the fluid are available. A novel algorithm is described to measure the viscosity and density of an ambient fluid by comparing experimental results with the theory. The theoretical results are analytical with a closed form solution. The algorithm presented is easier to implement than the standard method currently used by most atomic force microscope practitioners. In addition, unlike the standard method, the new algorithm is applicable to high viscosity fluids that do not produce resonant peaks in the microcantilever power spectra. Experiments were carried out using standard cantilevers in a fluid cell filled with air, water, methanol and commercial oils. The result of comparing theory with experiment validates the algorithm and thus we propose the algorithm as a way to measure density and viscosity of uncharacterized fluids. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Abel, Phillip B.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Eppell, Steven J.; Walker, Abigail M.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Zypman, Fredy R.] Yeshiva Univ, New York, NY 10033 USA.
RP Zypman, FR (reprint author), Yeshiva Univ, New York, NY 10033 USA.
FU NASA Glenn Research Center; Gamson Fund
FX FZ thanks financial support from NASA Glenn Research Center and the
Gamson Fund.
NR 32
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U1 4
U2 16
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-2241
EI 1873-412X
J9 MEASUREMENT
JI Measurement
PD FEB
PY 2015
VL 61
BP 67
EP 74
DI 10.1016/j.measurement.2014.10.019
PG 8
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AY3UB
UT WOS:000347506700009
ER
PT J
AU Huang, GJ
Bringi, VN
Moisseev, D
Petersen, WA
Bliven, L
Hudak, D
AF Huang, Gwo-Jong
Bringi, V. N.
Moisseev, Dmitri
Petersen, W. A.
Bliven, L.
Hudak, David
TI Use of 2D-video disdrometer to derive mean density-size and Z(e)-SR
relations: Four snow cases from the light precipitation validation
experiment
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Snow rate; Snow density; Radar reflectivity; Disdrometer
ID RADAR REFLECTIVITY; VIDEO DISDROMETER; WEATHER RADAR; FALL VELOCITY;
PART II; VARIABILITY; DISTRIBUTIONS; HYDROMETEORS; SCATTERING; GEOMETRY
AB The application of the 2D-video disdrometer to measure fall speed and snow size distribution and to derive liquid equivalent snow rate, mean density-size and reflectivity-snow rate power law is described. Inversion of the methodology proposed by Bohm provides the pathway to use measured fall speed, area ratio and '3D' size measurement to estimate the mass of each particle. Four snow cases from the Light Precipitation Validation Experiment are analyzed with supporting data from other instruments such as the Precipitation Occurrence Sensor System (POSS), Snow Video Imager (SVI), a network of seven snow gauges and three scanning C-band radars. The radar-based snow accumulations using the 2DVD-derived Z(e)-SR relation are in good agreement with a network of seven snow gauges and outperform the accumulations derived from a climatological Z(e)-SR relation used by the Finnish Meteorological Institute (FMI). The normalized bias between radar-derived and gauge accumulation is reduced from 96% when using the fixed FMI relation to 28% when using the Z(e)-SR relations based on 2DVD data. The normalized standard error is also reduced significantly from 66% to 31%. For two of the days with widely different coefficients of the Z(e)-SR power law, the reflectivity structure showed significant differences in spatial variability. Liquid water path estimates from radiometric data also showed significant differences between the two cases. Examination of SVI particle images at the measurement site corroborated these differences in terms of unrimed versus rimed snow particles. The findings reported herein support the application of Bohm's methodology for deriving the mean density-size and Z(e)-SR power laws using data from 2D-video disdrometer. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Huang, Gwo-Jong; Bringi, V. N.] Colorado State Univ, Ft Collins, CO 80525 USA.
[Moisseev, Dmitri] Univ Helsinki, Helsinki, Finland.
[Moisseev, Dmitri] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Petersen, W. A.; Bliven, L.] NASA, GSFC, Wallops Flight Facil, Wallops Isl, VA USA.
[Hudak, David] Environm Canada, Downsview, ON, Canada.
RP Huang, GJ (reprint author), Colorado State Univ, Ft Collins, CO 80525 USA.
EM gh222106@engr.colostate.edu
RI Moisseev, Dmitri/A-3288-2008
OI Moisseev, Dmitri/0000-0002-4575-0409
FU NASA [NNX10AJ11G, NNX11AK32G]; Academy of Finland [263333]
FX Two of the authors VNB and GJH acknowledge the support from NASA grants
NNX10AJ11G and NNX11AK32G. DM acknowledges the support from the Academy
of Finland grant 263333. WAP and LB acknowledge support from NASA GPM
Flight Project and Dr. Ramesh Kakar, Program Manager for PMM. The
authors also acknowledge Dr. Andrew Newman of NCAR for his assistance in
visual classification of SVI snow images for two of the events. The SVI
and POSS were installed by Peter Rodriguez of Environment Canada.
NR 44
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U1 2
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD FEB
PY 2015
VL 153
BP 34
EP 48
DI 10.1016/j.atmosres.2014.07.013
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AY0CD
UT WOS:000347264600004
ER
PT J
AU Liu, Z
AF Liu, Zhong
TI Comparison of precipitation estimates between Version 7 3-hourly TRMM
Multi-Satellite Precipitation Analysis (TMPA) near-real-time and
research products
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Precipitation; Satellite; Remote sensing; Intercomparison
ID TROPICAL RAINFALL; PASSIVE MICROWAVE; SATELLITE; SYSTEM; VALIDATION;
RESOLUTION; ALGORITHM; FLOOD; GAUGE; VISUALIZATION
AB Over the years, blended methods that use multi-satellites and multi-sensors have been developed for estimating global precipitation and resulting products are widely used in applications. An example is the 3-hourly TRMM (Tropical Rainfall Measuring Mission) Multi-Satellite Precipitation Analysis (TMPA) that consists of two products; near-real-time (3B42RT) and research-grade (3B42). The former provides quick, less accurate estimates suitable for monitoring activities; the latter provides more accurate estimates more suitable for research. Both products have been widely used in research and applications. Nonetheless, to improve near-real-time applications, it is important to understand their difference. In this study, seasonal mean difference (MD), mean absolute difference (MAD), root mean square difference (RMSD), and their inter-annual variations in boreal (June, July and August or JJA) and austral (December, January and February or DJF) summers and in different rain regimes over two surface types are investigated on a large scale (50 degrees N-50 degrees S) from 2000 and 2012. Over land, positive MD values (3B42RT > 3B42) dominate, especially in western China, western United States, northwest Asia and over some oceanic regions of light rain in both JJA and DJF. Over ocean, negative MD values (3B42RT < 3B42) prevail, except over regions of light rain. In general, relative (to 3B42) MD values increase with rain rate. Variation of the individual differences between the two products is small (large) over regions of heavy (light) rain. There is no significant inter-annual variation in the seasonal mean statistics. The difference between the two products is likely due to the algorithms and further investigations are needed. (C) 2014 The Author. Published by Elsevier B.V.
C1 [Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA.
[Liu, Zhong] NASA, Goddard Space Flight Ctr, GES DISC, Greenbelt, MD 20771 USA.
RP Liu, Z (reprint author), George Mason Univ, CSISS, 4400 Univ Dr, Fairfax, VA 22030 USA.
EM Zhong.Liu@nasa.gov
FU NASA [NNH10ZDA001N-ESDRERR]; NASA GES DISC
FX This project is supported by NASA Research Opportunities in Space and
Earth Science-2010 (ROSES-2010), NNH10ZDA001N-ESDRERR, Appendix A.32:
"Earth System Data Records Uncertainty Analysis" and the NASA GES DISC.
Special thanks to the GES DISC Giovanni development team. The TMPA data
were provided by the NASA Goddard Space Flight Center's Mesoscale
Atmospheric Processes Laboratory and Precipitation Processing System
(PPS), which develop and compute the TMPA as a contribution to TRMM.
Thanks extend to two anonymous reviewers who provided thought-provoking
comments and suggestions.
NR 36
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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 FEB
PY 2015
VL 153
BP 119
EP 133
DI 10.1016/j.atmosres.2014.07.032
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AY0CD
UT WOS:000347264600010
ER
PT J
AU Konishi, C
Lee, H
Mudawar, I
Hasan, MM
Nahra, HK
Hall, NR
Wagner, JD
May, RL
Mackey, JR
AF Konishi, Christopher
Lee, Hyoungsoon
Mudawar, Issam
Hasan, Mohammad M.
Nahra, Henry K.
Hall, Nancy R.
Wagner, James D.
May, Rochelle L.
Mackey, Jeffrey R.
TI Flow boiling in microgravity: Part 1-Interfacial behavior and
experimental heat transfer results
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Microgravity; Flow boiling; Interfacial behavior
ID FALLING LIQUID-FILMS; TRANSFER COEFFICIENT; MOMENTUM TRANSPORT; TRIGGER
MECHANISM; EARTH GRAVITY; CHF MECHANISM; WATER-FLOW; FLUX CHF;
ORIENTATION; MODEL
AB Space agencies worldwide are being confronted with the challenges of more distant manned space missions, which will demand greater energy efficiency and reduced weight and volume. One method being considered to reduce the weight and volume of a long duration mission spacecraft is to replace present single-phase Thermal Control Systems (TCSs) with ones that rely on flow boiling and condensation. This transition will require a thorough understanding of the influence of reduced gravity on flow boiling and condensation, and the development of predictive tools for both. This study is the first part of a two-part study investigating flow boiling of FC-72 in microgravity, which is simulated in a series of parabolic flight maneuvers. Flow boiling experiments are conducted in a rectangular channel fitted with two opposite heating walls. The operating conditions include liquid inlet velocities of 0.1-1.9 m/s, liquid mass velocities of 224.2-3347.5 kg/m(2) s, and inlet subcoolings ranging from 2.8 to 8.1 degrees C. The study includes both high-speed video analysis of interfacial features and heat transfer measurements. A dominant wavy vapor layer behavior is encountered for most operating conditions. Boiling is sustained mostly in 'wetting fronts' corresponding to contact regions between the wave troughs and the wall, and abated near the wave peaks. During a flight parabola, the heated wall temperatures decrease slightly as the aircraft enters the hypergravity ascent phase, then increase slightly during the microgravity phase, and decrease once again during the hypergravity descent. These temperature variations point to enhancement in flow boiling heat transfer with increasing gravity, and conversely a reduction with microgravity. (C) 2014 Published by Elsevier Ltd.
C1 [Konishi, Christopher; Lee, Hyoungsoon; Mudawar, Issam] Purdue Univ, Sch Mech Engn, Boiling & Twophase Flow Lab PU BTPFL, W Lafayette, IN 47907 USA.
[Hasan, Mohammad M.; Nahra, Henry K.; Hall, Nancy R.; Wagner, James D.; May, Rochelle L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Mackey, Jeffrey R.] Vantage Partners LLC, Brookpark, OH 44142 USA.
RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, Boiling & Twophase Flow Lab PU BTPFL, 585 Purdue Mall, W Lafayette, IN 47907 USA.
EM mudawar@ecn.purdue.edu
FU National Aeronautics and Space Administration (NASA) - United States
[NNX13AB01G]
FX The authors are grateful for the support of this project by the National
Aeronautics and Space Administration (NASA) - United States under Grant
no. NNX13AB01G.
NR 45
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U1 5
U2 29
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD FEB
PY 2015
VL 81
BP 705
EP 720
DI 10.1016/j.ijheatmasstransfer.2014.10.049
PG 16
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA AX5FE
UT WOS:000346951400068
ER
PT J
AU Konishi, C
Lee, H
Mudawar, I
Hasan, MM
Nahra, HK
Hall, NR
Wagner, JD
May, RL
Mackey, JR
AF Konishi, Christopher
Lee, Hyoungsoon
Mudawar, Issam
Hasan, Mohammad M.
Nahra, Henry K.
Hall, Nancy R.
Wagner, James D.
May, Rochelle L.
Mackey, Jeffrey R.
TI Flow boiling in microgravity: Part 2-Critical heat flux interfacial
behavior, experimental data, and model
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Microgravity; Flow boiling; Interfacial behavior; Critical heat flux
ID CHANNEL COOLING SCHEME; PRESSURE-DROP; TRIGGER MECHANISM; CHF MECHANISM;
2-PHASE INLET; BODY FORCE; WATER-FLOW; ORIENTATION; GRAVITY; LIQUID
AB This study is the second part of a two-part investigation of flow boiling critical heat flux (CHF) in microgravity, which is simulated in parabolic flight experiments. Using FC-72 as working fluid, flow boiling experiments are conducted in a rectangular channel fitted with two opposite heated walls, allowing either one or both heated walls to be activated during a test. While the first part explored flow boiling conditions leading to CHF, this part addresses events just before CHF, during the CHF transient, and immediately following CHF. For both single-sided and double-sided heating, interfacial behavior just before CHF is characterized by dominant wavy vapor layers covering the heated walls, where liquid is able to access the walls only in wetting fronts corresponding to the wave troughs. CHF is associated with successive lift-off of wetting fronts from the walls, consistent with the Interfacial Lift-off Model, which has been validated extensively in past studies using single-sided heating in both mu g(e) and 1 - g(e). It is shown this model predicts mu g(e) double-sided flow boiling CHF with excellent accuracy. Additionally, the model points to convergence of CHF values for mu g(e) and 1 - g(e) for inlet velocities greater than about 1 m/s. Therefore, by maintaining velocities above this threshold allows designers of space systems to achieve inertia-dominated performance as well as to adopt prior data and correlations developed from terrestrial studies. (C) 2014 Published by Elsevier Ltd.
C1 [Konishi, Christopher; Lee, Hyoungsoon; Mudawar, Issam] Purdue Univ, Boiling & Twophase Flow Lab PU BTPFL, Sch Mech Engn, W Lafayette, IN 47907 USA.
[Hasan, Mohammad M.; Nahra, Henry K.; Hall, Nancy R.; Wagner, James D.; May, Rochelle L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Mackey, Jeffrey R.] Vantage Partners LLC, Brookpark, OH 44142 USA.
RP Mudawar, I (reprint author), Purdue Univ, Boiling & Twophase Flow Lab PU BTPFL, Sch Mech Engn, 585 Purdue Mall, W Lafayette, IN 47907 USA.
EM mudawar@ecn.purdue.edu
FU National Aeronautics and Space Administration (NASA) - United States
[NNX13AB01G]
FX The authors are grateful for the support of this project by the National
Aeronautics and Space Administration (NASA) - United States under grant
no. NNX13AB01G.
NR 56
TC 5
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U1 4
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD FEB
PY 2015
VL 81
BP 721
EP 736
DI 10.1016/j.ijheatmasstransfer.2014.10.052
PG 16
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA AX5FE
UT WOS:000346951400069
ER
PT J
AU Astone, P
Weinstein, A
Agathos, M
Bejger, M
Christensen, N
Dent, T
Graff, P
Klimenko, S
Mazzolo, G
Nishizawa, A
Robinet, F
Schmidt, P
Smith, R
Veitch, J
Wade, M
Aoudia, S
Bose, S
Bustillo, JC
Canizares, P
Capano, C
Clark, J
Colla, A
Cuoco, E
Costa, CDS
Dal Canton, T
Evangelista, E
Goetz, E
Gupta, A
Hannam, M
Keitel, D
Lackey, B
Logue, J
Mohapatra, S
Piergiovanni, F
Privitera, S
Prix, R
Purrer, M
Re, V
Serafinelli, R
Wade, L
Wen, LQ
Wette, K
Whelan, J
Palomba, C
Prodi, G
AF Astone, Pia
Weinstein, Alan
Agathos, Michalis
Bejger, Michal
Christensen, Nelson
Dent, Thomas
Graff, Philip
Klimenko, Sergey
Mazzolo, Giulio
Nishizawa, Atsushi
Robinet, Florent
Schmidt, Patricia
Smith, Rory
Veitch, John
Wade, Madeline
Aoudia, Sofiane
Bose, Sukanta
Bustillo, Juan Calderon
Canizares, Priscilla
Capano, Colin
Clark, James
Colla, Alberto
Cuoco, Elena
Costa, Carlos Da Silva
Dal Canton, Tito
Evangelista, Edgar
Goetz, Evan
Gupta, Anuradha
Hannam, Mark
Keitel, David
Lackey, Benjamin
Logue, Joshua
Mohapatra, Satyanarayan
Piergiovanni, Francesco
Privitera, Stephen
Prix, Reinhard
Purrer, Michael
Re, Virginia
Serafinelli, Roberto
Wade, Leslie
Wen, Linqing
Wette, Karl
Whelan, John
Palomba, C.
Prodi, G.
TI Gravitational waves: search results, data analysis and parameter
estimation
SO GENERAL RELATIVITY AND GRAVITATION
LA English
DT Review
DE Gravitational waves; Parameter estimation; Tests of general relativity;
Compact binary merger; Neutron stars; Stochastic background
ID BLACK-HOLES
AB The Amaldi 10 Parallel Session C2 on gravitational wave(GW) search results, data analysis and parameter estimation included three lively sessions of lectures by 13 presenters, and 34 posters. The talks and posters covered a huge range of material, including results and analysis techniques for ground-based GW detectors, targeting anticipated signals from different astrophysical sources: compact binary inspiral, merger and ringdown; GW bursts from intermediate mass binary black hole mergers, cosmic string cusps, core-collapse supernovae, and other unmodeled sources; continuous waves from spinning neutron stars; and a stochastic GW background. There was considerable emphasis on Bayesian techniques for estimating the parameters of coalescing compact binary systems from the gravitational waveforms extracted from the data from the advanced detector network. This included methods to distinguish deviations of the signals from what is expected in the context of General Relativity.
C1 [Astone, Pia; Piergiovanni, Francesco; Palomba, C.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Weinstein, Alan; Privitera, Stephen] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Agathos, Michalis; Veitch, John] Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands.
[Bejger, Michal] N Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
[Christensen, Nelson] Carleton Coll, Northfield, MN 55057 USA.
[Dent, Thomas; Mazzolo, Giulio; Dal Canton, Tito; Goetz, Evan; Keitel, David; Prix, Reinhard; Wette, Karl] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Graff, Philip] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Klimenko, Sergey] Univ Florida, Gainesville, FL 32611 USA.
[Mazzolo, Giulio] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Nishizawa, Atsushi] Kyoto Univ, Kyoto 6068502, Japan.
[Robinet, Florent] Univ Paris 11, LAL Orsay, F-91898 Orsay, France.
[Schmidt, Patricia; Hannam, Mark; Purrer, Michael] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Smith, Rory] Univ Birmingham, Edgbaston B15 2TT, England.
[Wade, Madeline; Wade, Leslie] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Aoudia, Sofiane] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Bose, Sukanta] Washington State Univ, Pullman, WA 99164 USA.
[Bustillo, Juan Calderon] Univ Balearic Isl, Palma De Mallorca, Spain.
[Canizares, Priscilla] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Capano, Colin] Univ Maryland, College Pk, MD 20742 USA.
[Clark, James] Univ Massachusetts, Amherst, MA 01003 USA.
[Colla, Alberto; Serafinelli, Roberto] Univ Rome Sapienza, I-00185 Rome, Italy.
[Cuoco, Elena] EGO, I-56021 Pisa, Italy.
[Costa, Carlos Da Silva; Evangelista, Edgar] INPE, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, Brazil.
[Gupta, Anuradha] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Lackey, Benjamin] Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Logue, Joshua] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Mohapatra, Satyanarayan] Syracuse Univ, Syracuse, NY 13244 USA.
[Re, Virginia] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Re, Virginia] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Wen, Linqing] Univ Western Australia, Perth, WA 6009, Australia.
[Whelan, John] Rochester Inst Technol, Rochester, NY 14623 USA.
[Prodi, G.] Ist Nazl Fis Nucl, Grp Coll Trento, I-38050 Povo, Trento, Italy.
[Prodi, G.] Univ Trento, I-38050 Povo, Trento, Italy.
RP Weinstein, A (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM ajw@caltech.edu
OI Veitch, John/0000-0002-6508-0713
FU Australian Research Council; International Science Linkages program of
the Commonwealth of Australia; Council of Scientific and Industrial
Research of India; Istituto Nazionale di Fisica Nucleare of Italy;
Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia
Hisenda i Innovacio of the Govern de les Illes Balears; Netherlands
Organisation for Scientific Research; Foundation for Fundamental
Research; Polish Ministry of Science and Higher Education; FOCUS
Programme of Foundation for Polish Science; Royal Society; Scottish
Funding Council; Scottish Universities Physics Alliance; National
Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of
Origins (LIO); National Research Foundation of Korea; Industry Canada;
Province of Ontario through Ministry of Economic Development and
Innovation; National Science and Engineering Research Council Canada;
Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation;
Research Corporation; Alfred P. Sloan Foundation; Marie Curie
Intra-European Fellowship within 7th European Community Framework
Programme [PIEF-GA-2011-299190]; NSF grant [PHY-1204371]; IMPRS on
Gravitational Wave Astronomy; DOC-fFORTE-fellowship of the Austrian
Academy of Sciences; STFC [ST/H008438/1, ST/I001085/1]; Foundation for
Fundamental Research on Matter (FOM); Netherlands Organisation for
Scientific Research (NWO); NSF [PHY-0970074, PHY-1307429]; Wisconsin
Space Grant Consortium; NASA Postdoctoral Program at the Goddard Space
Flight Center
FX We wish to thank the organizers of the GR 20/Amaldi 10 conference, and
our hosts at the University of Warsaw, for an excellently organized,
smoothly run and extremely stimulating meeting. The authors gratefully
acknowledge the support of the United States National Science Foundation
for the construction and operation of the LIGO Laboratory, the Science
and Technology Facilities Council of the United Kingdom, the
Max-Planck-Society, and the State of Niedersachsen/Germany for support
of the construction and operation of the GEO600 detector, and the
Italian Istituto Nazionale di Fisica Nucleare and the French Centre
National de la Recherche Scientifique for the construction and operation
of the Virgo detector. The authors also gratefully acknowledge the
support of the research by these agencies and by the Australian Research
Council, the International Science Linkages program of the Commonwealth
of Australia, the Council of Scientific and Industrial Research of
India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish
Ministerio de Economia y Competitividad, the Conselleria d'Economia
Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation
for Fundamental Research on Matter supported by the Netherlands
Organisation for Scientific Research, the Polish Ministry of Science and
Higher Education, the FOCUS Programme of Foundation for Polish Science,
the Royal Society, the Scottish Funding Council, the Scottish
Universities Physics Alliance, The National Aeronautics and Space
Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO),
the National Research Foundation of Korea, Industry Canada and the
Province of Ontario through the Ministry of Economic Development and
Innovation, the National Science and Engineering Research Council
Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile
Packard Foundation, the Research Corporation, and the Alfred P. Sloan
Foundation. P. Canizares acknowledges support from a Marie Curie
Intra-European Fellowship within the 7th European Community Framework
Programme (PIEF-GA-2011-299190). N. Christensen acknowledges support
from NSF grant PHY-1204371. T. Dal Canton acknowledges support from the
IMPRS on Gravitational Wave Astronomy. P. Schmidt is a recipient of a
DOC-fFORTE-fellowship of the Austrian Academy of Sciences and was also
partially supported by the STFC. M Hannam acknowledges support from STFC
grants ST/H008438/1 and ST/I001085/1". J. Veitch acknowledges support
from the research programme of the Foundation for Fundamental Research
on Matter (FOM), which is partially supported by the Netherlands
Organisation for Scientific Research (NWO). M. Wade would acknowledges
support from NSF Grants No. PHY-0970074, No. PHY-1307429, and the
Wisconsin Space Grant Consortium. Philip Graff acknowledges support from
the NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. L. Wen acknowledges support from the Australian Research
Council.
NR 45
TC 1
Z9 1
U1 1
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0001-7701
EI 1572-9532
J9 GEN RELAT GRAVIT
JI Gen. Relativ. Gravit.
PD FEB
PY 2015
VL 47
IS 2
AR 11
DI 10.1007/s10714-014-1796-x
PG 26
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA DX2TR
UT WOS:000384224400001
ER
PT J
AU Guerra, JA
Pulkkinen, A
Uritsky, VM
Yashiro, S
AF Guerra, J. A.
Pulkkinen, A.
Uritsky, V. M.
Yashiro, S.
TI Spatio-Temporal Scaling of Turbulent Photospheric Line-of-Sight Magnetic
Field in Active Region NOAA 11158
SO SOLAR PHYSICS
LA English
DT Article
DE Active regions; Flares; relation to magnetic field; Magnetic fields;
photosphere; Photospheric turbulence
ID DYNAMICS-OBSERVATORY SDO; CORONAL MASS EJECTIONS; 2011 FEBRUARY 15; X2.2
FLARE; MAGNETOGRAMS; PRODUCTIVITY; SPECTRUM; IMAGER; SUN
AB We studied the structure and dynamics of the turbulent photospheric magnetic field in active region NOAA 11158 by characterizing spatial and temporal scaling properties of the line-of-sight (LOS) component. Using high-resolution high-cadence LOS magnetograms from SDO/HMI, we measured the power-law exponents alpha and beta that describe Fourier power spectra in wavenumber (k) and frequency (f) domains, and we investigated their evolution during the passage of the active region through the field of view of HMI. The flaring active region NOAA 11158 produces a one-dimensional spatial power spectral density that approximately follows a k (-2) power law - a spectrum that suggests parallel MHD fluctuations in an anisotropic turbulent medium. In addition, we found that the values of alpha capture systematically change in the configuration of the LOS photospheric magnetic field during flaring activity in the corona. Position-dependent values of the temporal scaling exponent beta showed that, on an average, the core of the active region scales with beta > 3 surrounded by a diffusive region with an approximately f (-2)-type spectrum. Our results indicate that only about 1 -aEuro parts per thousand 3 % of the studied LOS photospheric magnetic flux displays beta a parts per thousand alpha, implying that Taylor's hypothesis of frozen-in-flow turbulence is typically invalid for this scalar field in the presence of turbulent photospheric flows. In consequence, both spatial and temporal variations of the plasma and magnetic field must be included in a complete description of the turbulent evolution of active regions.
C1 [Guerra, J. A.; Uritsky, V. M.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Guerra, J. A.; Pulkkinen, A.; Uritsky, V. M.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Guerra, JA (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.
EM 94guerraagui@cardinalmail.cua.edu
NR 42
TC 2
Z9 2
U1 0
U2 2
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 FEB
PY 2015
VL 290
IS 2
BP 335
EP 350
DI 10.1007/s11207-014-0636-1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX0LN
UT WOS:000346644000003
ER
PT J
AU Lepping, RP
Wu, CC
Berdichevsky, DB
AF Lepping, R. P.
Wu, C. -C.
Berdichevsky, D. B.
TI Yearly Comparison of Magnetic Cloud Parameters, Sunspot Number, and
Interplanetary Quantities for the First 18 Years of the Wind Mission
SO SOLAR PHYSICS
LA English
DT Article
DE Magnetic Cloud; Sun spot number; Solar wind; Coronal Mass Ejection;
Interplanetary magnetic field; MC fitting model
ID CORONAL MASS EJECTIONS; SOLAR-WIND; GEOMAGNETIC STORMS; INTERACTION
REGION; INNER HELIOSPHERE; FLUX ROPES; AU; VOYAGER; FIELDS; ERRORS
AB In the scalar part of this study, we determine various statistical relationships between estimated magnetic cloud (MC) model fit-parameters and sunspot number (SSN) for the interval defined by the Wind mission, i.e., early 1995 until the end of 2012, all in terms of yearly averages. The MC-fitting model used is that of Lepping, Jones, and Burlaga (J. Geophys. Res. 95, 11957 -aEuro parts per thousand 11965, 1990). We also statistically compare the MC fit-parameters and other derived MC quantities [e.g., axial magnetic flux (I broken vertical bar(O)) and total axial current density (J (O))] with some associated ambient interplanetary quantities (including the interplanetary magnetic field (B (IMF)), proton number density (N (P)), and others). Some of the main findings are that the minimum SSN is nearly simultaneous with the minimum in the number of MCs per year (N (MC)), which occurs in 2008. There are various fluctuations in N (MC) and the MC model-fit quality (Q') throughout the mission, but the last four years (2009 -aEuro parts per thousand 2012) are markedly different from the others; Q' is low and N (MC) is large over these four years. N (MC) is especially large for 2012. The linear correlation coefficient (c.c.a parts per thousand 0.75) between the SSN and each of the three quantities J (O), MC diameter (2R (O)), and B (IMF), is moderately high, but none of the MC parameters track the SSN well in the sense defined in this article. However, there is good statistical tracking among the following: MC axial field, B (IMF), 2R (O), average MC speed (V (MC)), and yearly average solar wind speed (V (SW)) with relatively high c.c.s among most of these. From the start of the mission until late 2005, J (O) gradually increases, with a slight violation in 2003, but then a dramatic decrease (by more than a factor of five) occurs to an almost steady and low value of a parts per thousand aEuro parts per thousand 3 mu A km(-2) until the end of the interval of interest, i.e., lasting for at least seven years. This tends to split the overall 18-year interval into two phases with a separator at the end of 2005. There is good tracking between 2R (O) and the total axial current density, as expected. The MC duration is also correlated well with these two quantities. I broken vertical bar(O) shows marked variations throughout the mission, but has no obvious trend. N (P), B (IMF), V (MC), Q', and V (SW) are all quite steady over the full 18 years and have markedly low relative variation. Concerning vector quantities, we examine the distribution of MC type for the 18 years, where type refers to the field directional change through a given MC starting at first encounter (i.e., North-to-South, or South-to-North, All South, All North, etc.). Combining all 18 years of MC types shows that the occurrence rate varies strongly across the various MC types, with N-to-S being most prevalent, with a 27 % occurrence rate (of all MCs), and S-to-N being second, with a 23 % occurrence. Then All N and All S come next at 16 % and 10 % occurrence rate, respectively. All others are at 7 % or lower. For the variation of MC types with time, the southern types (i.e., those that start with a southern magnetic field, a negative B (Z) in geocentric-solar-ecliptic coordinates) decrease, as the northern types (i.e.
, those that start with a northern field) increase, apparently consistent with the specific timing of the polarity change of the solar magnetic field, as predicted by Bothmer and Rust (in Crooker, N., Joselyn, J., Feynman J. (eds), Geophys. Monogr., 139 -aEuro parts per thousand 146, 1997).
C1 [Lepping, R. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wu, C. -C.] Naval Res Lab, Washington, DC 20375 USA.
[Berdichevsky, D. B.] Univ Dist Columbia, Dept Elect & Comp Engn, Washington, DC USA.
RP Wu, CC (reprint author), Naval Res Lab, Washington, DC 20375 USA.
EM Chin-Chun.Wu@nrl.navy.mil
FU NASA [NNG10PB25P]; ONR 6.1 program
FX We thank the Wind/MFI and SWE teams for the care they employ in
producing the plasma and field data used for this work, and in
particular, we thank Keith Ogilvie, the principal investigator of SWE,
and Adam Szabo (PI) and Franco Mariani (instrument calibrations), both
of the MFI team. We are grateful to the referee for comments that
significantly added to the proper interpretation of our analysis and for
finding a mistake. This work was supported by a NASA program under grant
number NNG10PB25P. CCW was partially supported by the ONR 6.1 program.
NR 42
TC 7
Z9 7
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD FEB
PY 2015
VL 290
IS 2
BP 553
EP 578
DI 10.1007/s11207-014-0622-7
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX0LN
UT WOS:000346644000015
ER
PT J
AU Walsh, BM
Di Bartolo, B
AF Walsh, Brian M.
Di Bartolo, Baldassare
TI On the analysis of the thermal line shift and thermal line width of ions
in solids
SO JOURNAL OF LUMINESCENCE
LA English
DT Article
DE Debye function; Rational approximation; Thermal line shift; Thermal line
width; Transition metal ions; Rare earth ions
AB A method of analysis for the thermally induced line shift and line width of spectral lines regarding the Raman process of ions in solids utilizing rational approximations for the Debye functions is presented. The E-2 level unsplit R-line in V2+:MgO is used as an example to illustrate the utility of the methods discussed here in providing a new analytical tool for researchers. Published by Elsevier B.V.
C1 [Walsh, Brian M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Di Bartolo, Baldassare] Boston Coll, Dept Phys, Chestnut Hill, MA 23667 USA.
RP Walsh, BM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM brian.m.walsh@nasa.gov; baldassare.dibartolo@bc.edu
NR 10
TC 0
Z9 1
U1 1
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-2313
EI 1872-7883
J9 J LUMIN
JI J. Lumines.
PD FEB
PY 2015
VL 158
BP 265
EP 267
DI 10.1016/j.jlumin.2014.10.015
PG 3
WC Optics
SC Optics
GA AW8WR
UT WOS:000346540700044
ER
PT J
AU Chen, XM
Zhang, LY
Zheng, M
Park, C
Wang, XQ
Ke, CH
AF Chen, Xiaoming
Zhang, Liuyang
Zheng, Meng
Park, Cheol
Wang, Xianqiao
Ke, Changhong
TI Quantitative nanomechanical characterization of the van der Waals
interfaces between carbon nanotubes and epoxy
SO CARBON
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATIONS; POLYMER MATRIX; FRACTURE ENERGY; SINGLE;
COMPOSITES; STRENGTH; CRYSTALLIZATION; NANOCOMPOSITES;
POLYACRYLONITRILE; PERFORMANCE
AB Interfacial interactions between carbon nanotubes (CNTs) and polymer matrices play a critical role in the bulk mechanical performance of CNT-reinforced polymer nanocomposites, but their mechanisms remain elusive after over a decade of research. Here we present an in situ electron microscopy nanomechanical study of the non-covalent van der Waals interfaces between individual CNTs and epoxy resins in conjunction with atomistic simulations. By pulling out individual double-walled CNTs from Epon 828 films inside a high resolution electron microscope, the nanomechanical measurements capture the shear lag effect on CNT-epoxy interfaces. The maximum pull-out load of CNT-epoxy interfaces is found to be about 44% higher than the recently reported value for CNT-poly(methyl methacrylate) (PMMA) interfaces that were characterized using the same experimental technique and the same batch of dispersed CNTs. The higher interfacial strength of CNT-epoxy interfaces is partially attributed to the forced molecular deformations of aromatic rings in epoxy chains in the vicinity of the binding interface, which is supported by molecular dynamics simulations of the CNT-polymer interfacial interactions. The research findings contribute to a better understanding of the local load transfer on the tube-polymer interface and the tube's reinforcing mechanism, and ultimately the optimal design and performance of nanotube-reinforced polymer nanocomposites. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Chen, Xiaoming; Zheng, Meng; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
[Zhang, Liuyang; Wang, Xianqiao] Univ Georgia, Coll Engn, Athens, GA 30602 USA.
[Park, Cheol] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Wang, XQ (reprint author), Univ Georgia, Coll Engn, Athens, GA 30602 USA.
EM xqwang@uga.edu; cke@binghamton.edu
RI Wang, Xianqiao/E-5252-2010; Ke, Changhong/C-4064-2008; CHEN,
XIAOMING/A-1377-2016; Zhang, Liuyang/C-2987-2017
OI Wang, Xianqiao/0000-0003-2461-3015; Zhang, Liuyang/0000-0001-7170-5452
FU US Air Force Office of Scientific Research
FX This work was funded by US Air Force Office of Scientific Research. The
single-tube nanomechanical pull-out measurements were performed using
the facilities in the Analytical and Diagnostics Laboratory at
Binghamton University's Small Scale Systems Integration and Packaging
Center (S3IP). The facility support for molecular dynamics simulations
from the Georgia Advanced Computing Resource Center at University of
Georgia was greatly appreciated.
NR 55
TC 10
Z9 10
U1 7
U2 98
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0008-6223
EI 1873-3891
J9 CARBON
JI Carbon
PD FEB
PY 2015
VL 82
BP 214
EP 228
DI 10.1016/j.carbon.2014.10.065
PG 15
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA AU5ZZ
UT WOS:000345683100024
ER
PT J
AU Sankararaman, S
AF Sankararaman, Shankar
TI Significance, interpretation, and quantification of uncertainty in
prognostics and remaining useful life prediction
SO MECHANICAL SYSTEMS AND SIGNAL PROCESSING
LA English
DT Article
DE Prognostics; CBM; Uncertainty; Frequentist; Subjective; Filtering
ID BAYESIAN NETWORKS; STATE ESTIMATION; RELIABILITY; PROBABILITY; MODEL;
MACHINE; HEALTH; ALGORITHM; SYSTEMS
AB This paper analyzes the significance, interpretation, and quantification of uncertainty in prognostics, with an emphasis on predicting the remaining useful life of engineering systems and components. Prognostics deals with predicting the future behavior of engineering systems, and is affected by various sources of uncertainty. In order to facilitate meaningful prognostics-based decision-making, it is important to analyze how these sources of uncertainty affect prognostics, and thereby, compute the overall uncertainty in the remaining useful life prediction. This paper investigates the classical (frequentist) and subjective (Bayesian) interpretations of uncertainty and their implications on prognostics, and argues that the Bayesian interpretation of uncertainty is more suitable for condition-based prognostics and health monitoring. It is also demonstrated that uncertainty quantification in remaining useful life prediction needs to be approached as an uncertainty propagation problem. Several uncertainty propagation methods are discussed in this context, and the practical challenges involved in such uncertainty quantification are outlined. (C) 2014 Elsevier Ltd. All rights reserved.
C1 NASA, SGT Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sankararaman, S (reprint author), NASA, SGT Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM shankar.sankararaman@nasa.gov
FU NASA System-wide Safety Assurance Technologies (SSAT) project under the
Aviation Safety (AvSafe) Program of the Aeronautics Research Mission
Directorate (ARMD); NASA Automated Cryogenic Loading Operations (ACLO)
project under the Office of the Chief Technologist (OCT) of Advanced
Exploration Systems (AES)
FX The work reported herein was in part funded by the NASA System-wide
Safety Assurance Technologies (SSAT) project under the Aviation Safety
(AvSafe) Program of the Aeronautics Research Mission Directorate (ARMD),
and by the NASA Automated Cryogenic Loading Operations (ACLO) project
under the Office of the Chief Technologist (OCT) of Advanced Exploration
Systems (AES).
NR 79
TC 10
Z9 10
U1 1
U2 33
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0888-3270
J9 MECH SYST SIGNAL PR
JI Mech. Syst. Signal Proc.
PD FEB
PY 2015
VL 52-53
BP 228
EP 247
DI 10.1016/j.ymssp.2014.05.029
PG 20
WC Engineering, Mechanical
SC Engineering
GA AU2UI
UT WOS:000345472500016
ER
PT J
AU Tabatabaeenejad, A
Burgin, M
Duan, XY
Moghaddam, M
AF Tabatabaeenejad, Alireza
Burgin, Mariko
Duan, Xueyang
Moghaddam, Mahta
TI P-Band Radar Retrieval of Subsurface Soil Moisture Profile as a
Second-Order Polynomial: First AirMOSS Results
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne Microwave Observatory of Subcanopy and Subsurface (AirMOSS);
discrete scattering model; quadratic function; radar; remote sensing;
second-order polynomial; simulated annealing; soil moisture profile
ID SURFACES; ASSIMILATION; TEMPERATURE; SCATTERING; SUBCANOPY; MISSION;
MODEL
AB We propose a new model for estimating subsurface soil moisture using P-band radar data over barren, shrubland, and vegetated terrains. The unknown soil moisture profile is assumed to have a second-order polynomial form as a function of subsurface depth with three unknown coefficients that we estimate using the simulated annealing algorithm. These retrieved coefficients produce the value of soil moisture at any given depth up to a prescribed depth of validity. We use a discrete scattering model to calculate the radar backscattering coefficients of the terrain. The retrieval method is tested and developed with synthetic radar data and is validated with measured radar data and in situ soil moisture measurements. Both forward and inverse models are briefly explained. The radar data used in this paper have been collected during the Airborne Microwave Observatory of Subcanopy and Subsurface (AirMOSS) mission flights in September and October of 2012 over a 100 km by 25 km area in Arizona, including the Walnut Gulch Experimental Watershed. The study area and the ancillary data layers used to characterize each radar pixel are explained. The inversion results are presented, and it is shown that the RMSE between the retrieved and measured soil moisture profiles ranges from 0.060 to 0.099 m(3)/m(3), with a Root Mean Squared Error (RMSE) of 0.075 m(3)/m(3) over all sites and all acquisition dates. We show that the accuracy of retrievals decreases as depth increases. The profiles used in validation are from a fairy dry season in Walnut Gulch and so are the accuracy conclusions.
C1 [Tabatabaeenejad, Alireza; Moghaddam, Mahta] Univ So Calif, Ming Hsieh Dept Elect Engn, Los Angeles, CA 90089 USA.
[Burgin, Mariko; Duan, Xueyang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tabatabaeenejad, A (reprint author), Univ So Calif, Ming Hsieh Dept Elect Engn, Los Angeles, CA 90089 USA.
NR 40
TC 9
Z9 11
U1 3
U2 58
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 FEB
PY 2015
VL 53
IS 2
BP 645
EP 658
DI 10.1109/TGRS.2014.2326839
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AQ6HG
UT WOS:000342910800006
ER
PT J
AU Treuhaft, R
Goncalves, F
dos Santos, JR
Keller, M
Palace, M
Madsen, SN
Sullivan, F
Graca, PMLA
AF Treuhaft, Robert
Goncalves, Fabio
dos Santos, Joao Roberto
Keller, Michael
Palace, Michael
Madsen, Soren N.
Sullivan, Franklin
Graca, Paulo M. L. A.
TI Tropical-Forest Biomass Estimation at X-Band From the Spaceborne
TanDEM-X Interferometer
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Biomass; interferometric synthetic aperture radar (InSAR); lidar;
tropical forest
ID SAR INTERFEROMETRY; CARBON; LIDAR; BALANCE; RADAR
AB This letter reports the sensitivity of X-band interferometric synthetic aperture radar (InSAR) data from the first dual-spacecraft radar interferometer, TanDEM-X, to variations in tropical-forest aboveground biomass (AGB). It also reports the first tropical-forest AGB estimates from TanDEM-X data. Tropical forests account for about 50% of the world's forested biomass and play critical roles in the control of atmospheric carbon dioxide by emission through deforestation and uptake through forest growth. The TanDEM-X InSAR data used in this analysis were taken over the Tapajos National Forest, Par, Brazil, where field measurements from 30 stands were acquired. The magnitude of the InSAR normalized complex correlation, which is called coherence, decreases by about 25% as AGB increases from 2 to 430 Mg-ha(-1), suggesting more vertically distributed return-power profiles with increasing biomass. Comparison of InSAR coherences to those of small-spot (15 cm) lidar suggests that lidar penetrates deeper into the canopies than InSAR. Modeling InSAR profiles from InSAR coherence and lidar profiles yields an estimate of 0.29 dB/m for the X-band extinction coefficient relative to that of lidar. Forest AGB estimated from InSAR observations on 0.25-ha plots shows RMS scatters about the field-estimated AGB between 52 and 62 Mg-ha(-1), which is between 29% and 35% of the average AGB of 179 Mg-ha(-1), depending on the data analysis mode. The sensitivity and biomass-estimation performance suggest the potential of TanDEM-X observations to contribute to global tropical-forest biomass monitoring.
C1 [Treuhaft, Robert; Madsen, Soren N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Goncalves, Fabio] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[dos Santos, Joao Roberto] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil.
[Keller, Michael] USDA, Forest Serv, Int Inst Trop Forestry, San Juan, PR 00926 USA.
[Keller, Michael] Empresa Brasileira Pesquisa Agropecuaria EM BRAPA, BR-13070115 Campinas, SP, Brazil.
[Keller, Michael; Palace, Michael; Sullivan, Franklin] Univ New Hampshire, Durham, NH 03824 USA.
[Graca, Paulo M. L. A.] Inst Nacl de Pesquisas da Amazonia, BR-69067375 Manaus, AM, Brazil.
RP Treuhaft, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.treuhaft@jpl.nasa.gov; fgoncalves@whrc.org; jroberto@dsr.inpe.br;
mkeller.co2@gmail.com; palace@guero.sr.unh.edu;
soren.n.madsen@jpl.nasa.gov; fsulliva@gmail.com; pmlag@inpa.gov.br
RI de Alencastro Graca, Paulo Mauricio/B-3375-2013; Keller,
Michael/A-8976-2012
OI Keller, Michael/0000-0002-0253-3359
NR 25
TC 14
Z9 14
U1 3
U2 101
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 FEB
PY 2015
VL 12
IS 2
BP 239
EP 243
DI 10.1109/LGRS.2014.2334140
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 AO7YA
UT WOS:000341567600005
ER
PT J
AU Gong, XH
Paige, DA
Siegler, MA
Jin, YQ
AF Gong, Xiaohui
Paige, David A.
Siegler, Matthew A.
Jin, Ya-Qiu
TI Inversion of Dielectric Properties of the Lunar Regolith Media With
Temperature Profiles Using Chang'e Microwave Radiometer Observations
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Apollo heat flow; brightness temperature (Tb); Chang'e 1 and 2 (CE-1 and
CE-2); dielectric properties; Diviner; radiative transfer; regolith
media; temperature profile
ID TITANIUM ABUNDANCE; SPECTRUM; IRON
AB As ground truth to utilize the surface temperature measurements from the Diviner Lunar IR Radiometer and the subsurface thermal properties from the Apollo heat-flow probes, we create a forward model to predict brightness temperatures (Tbs) from lunar regolith media in the microwave (MW) spectrum. These models can be then directly compared with and matched to the data from the MW radiometers flown aboard the Chang'e 1 and 2 (CE-1 and CE-2) missions. Based on an MW radiative transfer model and the least-mean-square method, the effective surface reflectivity and absorption coefficient of the lunar regolith are retrieved from multichannel MW Tbs. The effective complex dielectric constant of the lunar regolith as a function of the depth at different frequency channels is derived. Meanwhile, we find that the maximum penetration depth of the MW radiation at the Apollo 15 site ranges from about 30 cm at 37.0 GHz to 230 cm at 3.0 GHz and from 30 cm at 37.0 GHz to 560 cm at 3.0 GHz in the equatorial highlands, which are much lower than the previous results that were simply derived from FeO and TiO2 abundance.
C1 [Gong, Xiaohui; Jin, Ya-Qiu] Fudan Univ, Minist Educ, Key Lab Informat Sci Electromagnet Waves, Shanghai 200433, Peoples R China.
[Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Siegler, Matthew A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jin, YQ (reprint author), Fudan Univ, Minist Educ, Key Lab Informat Sci Electromagnet Waves, Shanghai 200433, Peoples R China.
EM yqjin@fudan.edu.cn
NR 15
TC 1
Z9 2
U1 1
U2 58
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 FEB
PY 2015
VL 12
IS 2
BP 384
EP 388
DI 10.1109/LGRS.2014.2343617
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 AO7YA
UT WOS:000341567600034
ER
PT J
AU Vaidehi, N
Jain, A
AF Vaidehi, Nagarajan
Jain, Abhinandan
TI Internal Coordinate Molecular Dynamics: A Foundation for Multiscale
Dynamics
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID PROTEIN-STRUCTURE PREDICTION; CLASSICAL STATISTICAL-MECHANICS; LINKED
RIGID BODIES; BROWNIAN DYNAMICS; STRUCTURE REFINEMENT; POLYMER-CHAIN;
CONFORMATIONAL DYNAMICS; CONSTRAINED DYNAMICS; CALMODULIN STRUCTURE;
SIMULATION
AB Internal coordinates such as bond lengths, bond angles, and torsion angles (BAT) are natural coordinates for describing a bonded molecular system. However, the molecular dynamics (MD) simulation methods that are widely used for proteins, DNA, and polymers are based on Cartesian coordinates owing to the mathematical simplicity of the equations of motion. However, constraints are often needed with Cartesian MD simulations to enhance the conformational sampling. This makes the equations of motion in the Cartesian coordinates differential-algebraic, which adversely impacts the complexity and the robustness of the simulations. On the other hand, constraints can be easily placed in BAT coordinates by removing the degrees of freedom that need to be constrained. Thus, the internal coordinate MD (ICMD) offers an attractive alternative to Cartesian coordinate MD for developing multiscale MD method. The torsional MD method is a special adaptation of the ICMD method, where all the bond lengths and bond angles are kept rigid. The advantages of ICMD simulation methods are the longer time step size afforded by freezing high frequency degrees of freedom and performing a conformational search in the more important low frequency torsional degrees of freedom. However, the advancements in the ICMD simulations have been slow and stifled by long-standing mathematical bottlenecks. In this review, we summarize the recent mathematical advancements we have made based on spatial operator algebra, in developing a robust long time scale ICMD simulation toolkit useful for various applications. We also present the applications of ICMD simulations to study conformational changes in proteins and protein structure refinement. We review the advantages of the ICMD simulations over the Cartesian simulations when used with enhanced sampling methods and project the future use of ICMD simulations in protein dynamics.
C1 [Vaidehi, Nagarajan] Beckman Res Inst City Hope, Dept Immunol, Duarte, CA 91010 USA.
[Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vaidehi, N (reprint author), Beckman Res Inst City Hope, Dept Immunol, Duarte, CA 91010 USA.
EM nvaidehi@coh.org; Abhi.Jain@jpl.nasa.gov
FU National Institute of Health [RO1GM082896-01A2]; National Aeronautics
and Space Administration
FX We thank Mr. Adrien Larsen and Mr. Saugat Kandel for their help with the
manuscript preparation. This work was supported in part by Grant Number
RO1GM082896-01A2 from the National Institute of Health. The research
described in this paper was also performed in part at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration. Government
sponsorship is acknowledged.
NR 73
TC 1
Z9 1
U1 4
U2 17
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 JAN 29
PY 2015
VL 119
IS 4
BP 1233
EP 1242
DI 10.1021/jp509136y
PG 10
WC Chemistry, Physical
SC Chemistry
GA CA2QY
UT WOS:000348753600001
PM 25517406
ER
PT J
AU Ehlmann, BL
Buz, J
AF Ehlmann, Bethany L.
Buz, Jennifer
TI Mineralogy and fluvial history of the watersheds of Gale, Knobel, and
Sharp craters: A regional context for the Mars Science Laboratory
Curiosity's exploration
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE clay mineralogy; chlorides; fluvial activity; olivine bedrock; sediment
provenance; MSL
ID LANDING SITE; EVOLUTION; CONSTRAINTS; ORIGIN; MOUND; AREA
AB A 500km long network of valleys extends from Herschel crater to Gale, Knobel, and Sharp craters. The mineralogy and timing of fluvial activity in these watersheds provide a regional framework for deciphering the origin of sediments of Gale crater's Mount Sharp, an exploration target for the Curiosity rover. Olivine-bearing bedrock is exposed throughout the region, and its erosion contributed to widespread olivine-bearing sand dunes. Fe/Mg phyllosilicates are found in both bedrock and sediments, implying that materials deposited in Gale crater may have inherited clay minerals, transported from the watershed. While some topographic lows of the Sharp-Knobel watershed host chloride salts, the only salts detected in the Gale watershed are sulfates within Mount Sharp, implying regional or temporal differences in water chemistry. Crater counts indicate progressively more spatially localized aqueous activity: large-scale valley network activity ceased by the early Hesperian, though later Hesperian/Amazonian fluvial activity continued near Gale and Sharp craters.
C1 [Ehlmann, Bethany L.; Buz, Jennifer] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Ehlmann, BL (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM ehlmann@caltech.edu
FU MSL Participating Scientist grant; Rose Hills Foundation
FX All data used in this paper are available in the NASA Planetary Data
System; derived products are available by request. Work was partially
funded by an MSL Participating Scientist grant to B.L.E. and by a Rose
Hills Foundation fellowship to J.B. Thanks to A. Oshagan for
construction of the CTX mosaics used, C. Fassett for sharing a
spreadsheet for incremental crater statistics, and N. Warner and M.
Golombek for discussions of crater counting methodology. Thanks also to
reviewers J. Grant and B. Thomson for their constructive, critical
comments.
NR 38
TC 4
Z9 5
U1 2
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2015
VL 42
IS 2
BP 264
EP 273
DI 10.1002/2014GL062553
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CB9MO
UT WOS:000349956000011
ER
PT J
AU Jolivet, R
Simons, M
Agram, PS
Duputel, Z
Shen, ZK
AF Jolivet, R.
Simons, M.
Agram, P. S.
Duputel, Z.
Shen, Z. -K.
TI Aseismic slip and seismogenic coupling along the central San Andreas
Fault
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE InSAR; GPS; San Andreas Fault; aseismic slip; Bayesian inversion
ID GREAT 1857 EARTHQUAKE; CENTRAL CALIFORNIA; FRANCISCO EARTHQUAKE;
NORTHERN CALIFORNIA; CREEPING SECTION; OKI EARTHQUAKE; SEISMIC CYCLE;
GEODETIC DATA; INSAR; SYSTEM
AB We use high-resolution Synthetic Aperture Radar- and GPS-derived observations of surface displacements to derive the first probabilistic estimates of fault coupling along the creeping section of the San Andreas Fault, in between the terminations of the 1857 and 1906 magnitude 7.9 earthquakes. Using a fully Bayesian approach enables unequaled resolution and allows us to infer a high probability of significant fault locking along the creeping section. The inferred discreet locked asperities are consistent with evidence for magnitude 6+ earthquakes over the past century in this area and may be associated with the initiation phase of the 1857 earthquake. As creeping segments may be related to the initiation and termination of seismic ruptures, such distribution of locked and creeping asperities highlights the central role of the creeping section on the occurrence of major earthquakes along the San Andreas Fault.
C1 [Jolivet, R.; Simons, M.; Duputel, Z.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
[Agram, P. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Duputel, Z.] Inst Phys Globe Strasbourg, UdS, Strasbourg, France.
[Duputel, Z.] EOST CNRS UMR, Strasbourg, France.
[Shen, Z. -K.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
RP Jolivet, R (reprint author), Univ Cambridge, Dept Earth Sci, Bullard Labs, Cambridge CB2 3EQ, England.
EM rpj29@cam.ac.uk
RI Duputel, Zacharie/C-2906-2016;
OI Duputel, Zacharie/0000-0002-8809-451X; Jolivet,
Romain/0000-0002-9896-3651; Simons, Mark/0000-0003-1412-6395
FU National Science Foundation [EAR-1118239]; United States Geological
Survey [G11AP20044]; Southern California Earthquake Center; NSF
[EAR-1033462]; USGS [G12AC20038]
FX Advanced Land Observing Satellite (ALOS) data were acquired by the
Japanese space agency (JAXA) and provided by the Alaska SAR Facility
(ASF). This study was funded by National Science Foundation grant
EAR-1118239 and United States Geological Survey grant G11AP20044. This
research was supported by the Southern California Earthquake Center.
SCEC is funded by NSF cooperative agreement EAR-1033462 and USGS
Cooperative Agreement G12AC20038. The SCEC contribution for this paper
is 1975. This study contributed from fruitful discussions with H.
Kanamori, T. Heaton, J. Stock, K. Scharer, L. Rivera, S. Minson, M.
Aivazis, and H. Zhang. We thank the Editor and two anonymous reviewers
for providing insightful comments that helped improve this manuscript.
NR 50
TC 15
Z9 15
U1 5
U2 21
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 JAN 28
PY 2015
VL 42
IS 2
BP 297
EP 306
DI 10.1002/2014GL062222
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CB9MO
UT WOS:000349956000015
ER
PT J
AU Santer, BD
Solomon, S
Bonfils, C
Zelinka, MD
Painter, JF
Beltran, F
Fyfe, JC
Johannesson, G
Mears, C
Ridley, DA
Vernier, JP
Wentz, FJ
AF Santer, Benjamin D.
Solomon, Susan
Bonfils, Celine
Zelinka, Mark D.
Painter, Jeffrey F.
Beltran, Francisco
Fyfe, John C.
Johannesson, Gardar
Mears, Carl
Ridley, David A.
Vernier, Jean-Paul
Wentz, Frank J.
TI Observed multivariable signals of late 20th and early 21st century
volcanic activity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Volcanic forcing; Climate change; Signal detection
ID GLOBAL CLIMATE-CHANGE; STRATOSPHERIC AEROSOL; DECADAL CHANGES;
WATER-VAPOR; TEMPERATURE; TRENDS; VARIABILITY; MODEL; ENSO
AB The relatively muted warming of the surface and lower troposphere since 1998 has attracted considerable attention. One contributory factor to this warming hiatus is an increase in volcanically induced cooling over the early 21st century. Here we identify the signals of late 20th and early 21st century volcanic activity in multiple observed climate variables. Volcanic signals are statistically discernible in spatial averages of tropical and near-global SST, tropospheric temperature, net clear-sky short-wave radiation, and atmospheric water vapor. Signals of late 20th and early 21st century volcanic eruptions are also detectable in near-global averages of rainfall. In tropical average rainfall, however, only a Pinatubo-caused drying signal is identifiable. Successful volcanic signal detection is critically dependent on removal of variability induced by the El Nino-Southern Oscillation.
C1 [Santer, Benjamin D.; Bonfils, Celine; Zelinka, Mark D.; Painter, Jeffrey F.; Beltran, Francisco; Johannesson, Gardar] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA.
[Solomon, Susan; Ridley, David A.] MIT, Cambridge, MA 02139 USA.
[Fyfe, John C.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Mears, Carl; Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA USA.
[Vernier, Jean-Paul] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Santer, BD (reprint author), Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA.
EM santer1@llnl.gov
RI Santer, Benjamin/F-9781-2011; Zelinka, Mark/C-4627-2011
OI Zelinka, Mark/0000-0002-6570-5445
FU US Department of Energy [DE-AC52-07NA27344]; DOE/OBER Early Career
Research Program Award [SCW1295]; NSF [AGS-1342810]
FX All observational climate data used here are in the public domain,
available at the following locations: (1) http://www.remss.com/data (for
TMT, TLT, and PW); (2) http://www.ncdc.noaa.gov/oa/climate/research/sst
(for SST); (3) http://ceres-tool.larc.nasa.gov/ord-tool/ (for SW); and
(4) http://www.esrl.noaa.gov/psd/data/gridded/data.gpcp.html (for PR).
We thank Tom Wigley (University of Adelaide) for valuable comments and
suggestions. At Lawrence Livermore National Laboratory, work by B.D.S.,
J.P., and M.Z. was performed under the auspices of the US Department of
Energy under contract DE-AC52-07NA27344; C.B. was supported by the
DOE/OBER Early Career Research Program Award SCW1295. S.S. was supported
in part by NSF grant AGS-1342810.
NR 36
TC 15
Z9 15
U1 4
U2 29
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 JAN 28
PY 2015
VL 42
IS 2
BP 500
EP 509
DI 10.1002/2014GL062366
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CB9MO
UT WOS:000349956000040
ER
PT J
AU Chae, Y
Kang, SM
Jeong, SJ
Kim, B
Frierson, DMW
AF Chae, Yoojeong
Kang, Sarah M.
Jeong, Su-Jong
Kim, Baekmin
Frierson, Dargan M. W.
TI Arctic greening can cause earlier seasonality of Arctic amplification
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Arctic greening; Arctic amplification; seasonality; CO2 doubling
ID CLIMATE-CHANGE; VEGETATION; FEEDBACKS; CO2; TEMPERATURE; MODEL
AB As global temperatures rise, vegetation types will change, particularly in the northern high latitudes. Under a warming scenario, shrub and grasslands over the Arctic are expected to shift to boreal forests. This study compares the impact of such a change in Arctic vegetation type with that of CO2 doubling on the seasonality of Arctic warming. Even though vegetation is changed throughout the year, the effect of the surface albedo change is maximum in boreal summer when the incoming solar radiation is largest. Evapotranspiration changes are also maximized in the summer, when the photosynthesis rate is highest. As a result, when Arctic vegetation change is considered in addition to doubled CO2, Arctic amplification is maximized earlier in the annual cycle.
C1 [Chae, Yoojeong; Kang, Sarah M.] UNIST, Sch Urban & Environm Engn, Ulsan, South Korea.
[Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kim, Baekmin] Korea Polar Res Inst, Div Polar Climate Change Res, Inchon, South Korea.
[Frierson, Dargan M. W.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
RP Kang, SM (reprint author), UNIST, Sch Urban & Environm Engn, Ulsan, South Korea.
EM skang@unist.ac.kr
RI Jeong, Su-Jong/J-4110-2014; Frierson, Dargan/F-1763-2010
OI Frierson, Dargan/0000-0001-8952-5644
FU Ulsan National Institute of Science and Technology (UNIST) [1.140014]
FX S.M.K. is supported by the Creativity and Innovation Research Fund
1.140014 of Ulsan National Institute of Science and Technology (UNIST).
The output of the CAM3 experiments can be obtained by sending a written
request to the corresponding author.
NR 24
TC 2
Z9 2
U1 7
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2015
VL 42
IS 2
BP 536
EP 541
DI 10.1002/2014GL061841
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CB9MO
UT WOS:000349956000043
ER
PT J
AU Smeltzer, CC
Lukinova, NN
Towcimak, ND
Mann, D
Drohan, WN
Griko, YV
AF Smeltzer, Claudia C.
Lukinova, Nina N.
Towcimak, Nicole D.
Mann, David
Drohan, William N.
Griko, Yuri V.
TI Effect of Gamma Radiation on the Structural and Functional Integrity of
IgG
SO BIOPHYSICAL JOURNAL
LA English
DT Meeting Abstract
CT 59th Annual Meeting of the Biophysical-Society
CY FEB 07-11, 2015
CL Baltimore, MD
SP Biophys Soc
C1 [Smeltzer, Claudia C.; Lukinova, Nina N.; Towcimak, Nicole D.; Mann, David; Drohan, William N.] Clearant Inc, Gaithersburg, MD USA.
[Griko, Yuri V.] NASA Ames Res Ctr, Space Biosci, Mountain View, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0006-3495
EI 1542-0086
J9 BIOPHYS J
JI Biophys. J.
PD JAN 27
PY 2015
VL 108
IS 2
SU 1
MA 2613-Pos
BP 517A
EP 517A
PG 1
WC Biophysics
SC Biophysics
GA CT5KV
UT WOS:000362849600221
ER
PT J
AU Chronis, T
Cummins, K
Said, R
Koshak, W
McCaul, E
Williams, ER
Stano, GT
Grant, M
AF Chronis, T.
Cummins, K.
Said, R.
Koshak, W.
McCaul, E.
Williams, E. R.
Stano, G. T.
Grant, M.
TI Climatological diurnal variation of negative CG lightning peak current
over the continental United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE lightning peak current; diurnal variation
ID GLOBAL ELECTRIC-CIRCUIT; ELECTROMAGNETIC-FIELDS; FLORIDA THUNDERSTORMS;
RETURN STROKES; CLOUD; NLDN; VARIABILITY; EVENTS; CHARGE; CLIMATOGRAPHY
AB This study provides an 11year climatology of the diurnal variability of the cloud-to-ground (CG) lightning peak current. The local diurnal variation of peak current for negative polarity CG (-CG) flashes exhibits a highly consistent behavior, with increasing magnitudes between the late night to early morning hours and decreasing magnitudes during the afternoon. Over most regions, an inverse relationship exists between the -CG peak current and the corresponding -CG activity, although specific details can depend on region and time of day. Overall, the diurnal variation of the -CG peak current appears to reflect fundamental differences between morning and afternoon storms, but additional studies are required to clearly identify the primary cause(s).
C1 [Chronis, T.] Univ Alabama, ESSC, Huntsville, AL 35899 USA.
[Cummins, K.] Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA.
[Said, R.] Vaisala Inc, Boulder Operat, Louisville, CO USA.
[Koshak, W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[McCaul, E.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Williams, E. R.] MIT, Cambridge, MA 02139 USA.
[Stano, G. T.] ENSCO Inc, NASA, Short Term Predict Res & Transit Ctr, Huntsville, AL USA.
[Grant, M.] Univ Witwatersrand, Sch Elect & Informat Engn, Johannesburg, South Africa.
RP Chronis, T (reprint author), Univ Alabama, ESSC, Huntsville, AL 35899 USA.
EM themis.chronis@nsstc.uah.edu
OI Cummins, Kenneth/0000-0001-9871-691X
FU GOES-R Proving Ground; Risk Reduction programs
FX The first author acknowledges the support by Steve Goodman, Lawrence
Carey and the GOES-R Proving Ground and Risk Reduction programs. A
particular thanks to Philip Krider for the insightful comments.
Discussions with Rich Blakeslee, Hugh Christian, Walter Lyons, and
anonymous reviewers are much appreciated. The help by David Fanning on
IDL issues is always highly appreciated. The NLDN data were provided by
Vaisala Inc., through a UAH/ESSC memorandum of agreement, for research
purposes only. The NLDN data are available at
http://thunderstorm.vaisala.com.
NR 66
TC 7
Z9 7
U1 2
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2015
VL 120
IS 2
BP 582
EP 589
DI 10.1002/2014JD022547
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC1QQ
UT WOS:000350117100013
ER
PT J
AU Li, ZJ
Feng, S
Liu, YG
Lin, WY
Zhang, MH
Toto, T
Vogelmann, AM
Endo, S
AF Li, Zhijin
Feng, Sha
Liu, Yangang
Lin, Wuyin
Zhang, Minghua
Toto, Tami
Vogelmann, Andrew M.
Endo, Satoshi
TI Development of fine-resolution analyses and expanded large-scale forcing
properties: 1. Methodology and evaluation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE fine-resolution analyses; data assimilation; high-resolution
observations
ID COMMUNITY ATMOSPHERE MODEL; CLOUD MICROPHYSICS SCHEME; DATA ASSIMILATION
SYSTEM; SINGLE-COLUMN MODELS; VARIATIONAL ANALYSIS; RESOLVING MODEL;
KALMAN FILTER; RADIATION; SMOOTHER; PROGRAM
AB We produce fine-resolution, three-dimensional fields of meteorological and other variables for the U.S. Department of Energy's Atmospheric Radiation Measurement (ARM) Southern Great Plains site. The Community Gridpoint Statistical Interpolation system is implemented in a multiscale data assimilation (MS-DA) framework that is used within the Weather Research and Forecasting model at a cloud-resolving resolution of 2km. The MS-DA algorithm uses existing reanalysis products and constrains fine-scale atmospheric properties by assimilating high-resolution observations. A set of experiments show that the data assimilation analysis realistically reproduces the intensity, structure, and time evolution of clouds and precipitation associated with a mesoscale convective system. Evaluations also show that the large-scale forcing derived from the fine-resolution analysis has an overall accuracy comparable to the existing ARM operational product. For enhanced applications, the fine-resolution fields are used to characterize the contribution of subgrid variability to the large-scale forcing and to derive hydrometeor forcing, which are presented in companion papers.
C1 [Li, Zhijin; Feng, Sha] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Li, Zhijin; Feng, Sha] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Liu, Yangang; Lin, Wuyin; Toto, Tami; Vogelmann, Andrew M.; Endo, Satoshi] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA.
[Zhang, Minghua] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA.
RP Li, ZJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Zhijin.Li@jpl.nasa.gov
RI Liu, Yangang/H-6154-2011; Vogelmann, Andrew/M-8779-2014
OI Vogelmann, Andrew/0000-0003-1918-5423
FU U.S. Department of Energy Earth System Modeling (ESM) program via the
FAst-physics System TEstbed and Research (FASTER)
FX The research described in this publication was supported by the U.S.
Department of Energy Earth System Modeling (ESM) program via the
FAst-physics System TEstbed and Research (FASTER) project
www.bnl.gov/faster. The research was carried out, in part, at Jet
Propulsion Laboratory (JPL) California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
The authors thank the ARM program for providing the SGP observations.
The authors are grateful to Ann Fridlind (NASA Goddard Institute for
Space Studies) for numerous stimulating discussions, insightful
suggestions, and strong support. The authors thank the anonymous
reviewers for comments that were very helpful in improving the
manuscript.
NR 48
TC 4
Z9 4
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2015
VL 120
IS 2
BP 654
EP 666
DI 10.1002/2014JD022245
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC1QQ
UT WOS:000350117100017
ER
PT J
AU Feng, S
Li, ZJ
Liu, YG
Lin, WY
Zhang, MH
Toto, T
Vogelmann, AM
Endo, S
AF Feng, Sha
Li, Zhijin
Liu, Yangang
Lin, Wuyin
Zhang, Minghua
Toto, Tami
Vogelmann, Andrew M.
Endo, Satoshi
TI Development of fine-resolution analyses and expanded large-scale forcing
properties: 2. Scale awareness and application to single-column model
experiments
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE scale-aware forcing; subgrid-scale dynamic process; single-column model
ID COMMUNITY ATMOSPHERE MODEL; CLOUD MICROPHYSICS SCHEME; RESOLVING MODEL;
CLIMATE; SYSTEM; RADIATION; PROGRAM; WEATHER; TESTS; CAM3
AB Fine-resolution three-dimensional fields have been produced using the Community Gridpoint Statistical Interpolation (GSI) data assimilation system for the U.S. Department of Energy's Atmospheric Radiation Measurement Program (ARM) Southern Great Plains region. The GSI system is implemented in a multiscale data assimilation framework using the Weather Research and Forecasting model at a cloud-resolving resolution of 2km. From the fine-resolution three-dimensional fields, large-scale forcing is derived explicitly at grid-scale resolution; a subgrid-scale dynamic component is derived separately, representing subgrid-scale horizontal dynamic processes. Analyses show that the subgrid-scale dynamic component is often a major component over the large-scale forcing for grid scales larger than 200km. The single-column model (SCM) of the Community Atmospheric Model version 5 is used to examine the impact of the grid-scale and subgrid-scale dynamic components on simulated precipitation and cloud fields associated with a mesoscale convective system. It is found that grid-scale size impacts simulated precipitation, resulting in an overestimation for grid scales of about 200km but an underestimation for smaller grids. The subgrid-scale dynamic component has an appreciable impact on the simulations, suggesting that grid-scale and subgrid-scale dynamic components should be considered in the interpretation of SCM simulations.
C1 [Feng, Sha; Li, Zhijin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Feng, Sha; Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Liu, Yangang; Lin, Wuyin; Toto, Tami; Vogelmann, Andrew M.; Endo, Satoshi] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA.
[Zhang, Minghua] SUNY Stony Brook, Stony Brook, NY 11794 USA.
RP Feng, S (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM sfeng@jifresse.ucla.edu
RI Liu, Yangang/H-6154-2011; Vogelmann, Andrew/M-8779-2014
OI Vogelmann, Andrew/0000-0003-1918-5423
FU U.S. Department of Energy Earth System Modeling program via the FASTER
project
FX The research described in this publication was supported by the U.S.
Department of Energy Earth System Modeling program via the FASTER
project (http://www.bnl.gov/faster). 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 (NASA). The authors are grateful to Ann Fridlind (NASA
Goddard Institute for Space Studies) and Leo J. Donner (Geophysical
Fluid Dynamics Laboratory) for stimulating the discussions and
insightful suggestions. Data from the U.S. Department of Energy's SGP
ARM Climate Research Facility (http://www.arm.gov/) are used in this
article. The authors thank the anonymous reviewers for their comments
that were very helpful in improving the manuscript.
NR 28
TC 3
Z9 3
U1 0
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 JAN 27
PY 2015
VL 120
IS 2
BP 667
EP 677
DI 10.1002/2014JD022254
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC1QQ
UT WOS:000350117100018
ER
PT J
AU Ott, LE
Pawson, S
Collatz, GJ
Gregg, WW
Menemenlis, D
Brix, H
Rousseaux, CS
Bowman, KW
Liu, JJ
Eldering, A
Gunson, MR
Kawa, SR
AF Ott, Lesley E.
Pawson, Steven
Collatz, George J.
Gregg, Watson W.
Menemenlis, Dimitris
Brix, Holger
Rousseaux, Cecile S.
Bowman, Kevin W.
Liu, Junjie
Eldering, Annmarie
Gunson, Michael R.
Kawa, Stephan R.
TI Assessing the magnitude of CO2 flux uncertainty in atmospheric CO2
records using products from NASA's Carbon Monitoring Flux Pilot Project
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CO2; GOSAT; modeling; ocean; CMS; biosphere
ID GENERAL-CIRCULATION MODEL; COLUMN OBSERVING NETWORK; REGIONAL CO2;
INTERANNUAL VARIABILITY; RETRIEVAL ALGORITHM; GREENHOUSE GASES;
TRANSPORT MODEL; FIRE EMISSIONS; FINITE-VOLUME; IN-SITU
AB NASA's Carbon Monitoring System Flux Pilot Project (FPP) was designed to better understand contemporary carbon fluxes by bringing together state-of-the art models with remote sensing data sets. Here we report on simulations using NASA's Goddard Earth Observing System Model, version 5 (GEOS-5) which was used to evaluate the consistency of two different sets of observationally informed land and ocean fluxes with atmospheric CO2 records. Despite the observation inputs, the average difference in annual terrestrial biosphere flux between the two land (NASA Ames Carnegie-Ames-Stanford-Approach (CASA) and CASA-Global Fire Emissions Database version 3 (GFED)) models is 1.7 Pg C for 2009-2010. Ocean models (NASA's Ocean Biogeochemical Model (NOBM) and Estimating the Circulation and Climate of the Ocean Phase II (ECCO2)-Darwin) differ by 35% in their global estimates of carbon flux with particularly strong disagreement in high latitudes. Based upon combinations of terrestrial and ocean fluxes, GEOS-5 reasonably simulated the seasonal cycle observed at Northern Hemisphere surface sites and by the Greenhouse gases Observing SATellite (GOSAT) while the model struggled to simulate the seasonal cycle at Southern Hemisphere surface locations. Though GEOS-5 was able to reasonably reproduce the patterns of XCO2 observed by GOSAT, it struggled to reproduce these aspects of Atmospheric Infrared Sounder observations. Despite large differences between land and ocean flux estimates, resulting differences in atmospheric mixing ratio were small, typically less than 5ppm at the surface and 3ppm in the XCO2 column. A statistical analysis based on the variability of observations shows that flux differences of these magnitudes are difficult to distinguish from inherent measurement variability, regardless of the measurement platform.
C1 [Ott, Lesley E.; Pawson, Steven; Gregg, Watson W.; Rousseaux, Cecile S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Collatz, George J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Menemenlis, Dimitris; Bowman, Kevin W.; Liu, Junjie; Eldering, Annmarie; Gunson, Michael R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Brix, Holger] Univ Calif Los Angeles, Los Angeles, CA USA.
[Rousseaux, Cecile S.] Univ Space Res Assoc, Greenbelt, MD USA.
[Kawa, Stephan R.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
RP Ott, LE (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM lesley.e.ott@nasa.gov
RI collatz, george/D-5381-2012; Pawson, Steven/I-1865-2014; Ott,
Lesley/E-2250-2012; Rousseaux, Cecile/E-8811-2012
OI Menemenlis, Dimitris/0000-0001-9940-8409; Pawson,
Steven/0000-0003-0200-717X; Rousseaux, Cecile/0000-0002-3022-2988
FU NASA's CMS FPP and Phase One activities
FX This work was supported by funding from NASA's CMS FPP and Phase One
activities. MERRA data used during the CMS FPP have been provided by the
GMAO at NASA Goddard Space Flight Center through the NASA GES DISC
online archive. Surface observations were provided by NOAA ESRL. TCCON
data were obtained from the TCCON Data Archive, operated by the
California Institute of Technology from the website at
http://tccon.ipac.caltech.edu/. HIPPO data were retrieved from the HIPPO
data archive at http://hippo.ornl.gov/dataaccess. AIRS is managed by
NASA's Jet Propulsion Laboratory with data provided through the NASA GES
DISC. ACOS data were provided by Chris O'Dell from Colorado State
University. Selected monthly average CO2 fields from the GEOS-5
simulations described above are available at
ftp://gmaoftp.gsfc.nasa.gov/pub/data/lott/CMS_monthly_average/.
Additional GEOS-5 CO2 fields will be provided upon request.
NR 110
TC 6
Z9 6
U1 6
U2 37
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2015
VL 120
IS 2
BP 734
EP 765
DI 10.1002/2014JD022411
PG 32
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC1QQ
UT WOS:000350117100023
ER
PT J
AU Schwartz, MJ
Manney, GL
Hegglin, MI
Livesey, NJ
Santee, ML
Daffer, WH
AF Schwartz, M. J.
Manney, G. L.
Hegglin, M. I.
Livesey, N. J.
Santee, M. L.
Daffer, W. H.
TI Climatology and variability of trace gases in extratropical
double-tropopause regions from MLS, HIRDLS, and ACE-FTS measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE double tropopause; composition; UTLS; satellite data
ID STRATOSPHERIC WATER-VAPOR; FOURIER-TRANSFORM SPECTROMETER; EDDY-DRIVEN
JET; POTENTIAL VORTICITY; UPPER TROPOSPHERE; INTERANNUAL VARIABILITY;
SOUTHERN-HEMISPHERE; INVERSION LAYER; SATELLITE DATA; WESTERLY JET
AB Upper tropospheric and lower stratospheric measurements from the Aura Microwave Limb Sounder (MLS), the Aura High Resolution Dynamics Limb Sounder (HIRDLS), and the Atmospheric Chemistry Experiment-Fourier transform spectrometer (ACE-FTS) are used to present the first global climatological comparison of extratropical, nonpolar trace gas distributions in double-tropopause (DT) and single-tropopause (ST) regions. Stratospheric tracers, O-3, HNO3, and HCl, have lower mixing ratios approximate to 2-8 km above the primary (lowermost) tropopause in DT than in ST regions in all seasons, with maximum Northern Hemisphere (NH) differences near 50% in winter and 30% in summer. Southern Hemisphere winter differences are somewhat smaller, but summer differences are similar in the two hemispheres. H2O in DT regions of both hemispheres shows strong negative anomalies in November through February and positive anomalies in July through October, reflecting the strong seasonal cycle in H2O near the tropical tropopause. CO and other tropospheric tracers examined have higher DT than ST values 2-7 km above the primary tropopause, with the largest differences in winter. Large DT-ST differences extend to high NH latitudes in fall and winter, with longitudinal maxima in regions associated with enhanced wave activity and subtropical jet variations. Results for O-3 and HNO3 agree closely between MLS and HIRDLS, and differences from ACE-FTS are consistent with its sparse and irregular midlatitude sampling. Consistent signatures in climatological trace gas fields provide strong evidence that transport from the tropical upper troposphere into the layer between double tropopauses is an important pathway for stratosphere-troposphere exchange.
C1 [Schwartz, M. J.; Livesey, N. J.; Santee, M. L.; Daffer, W. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Manney, G. L.] Northwest Res Associates, Socorro, NM USA.
[Manney, G. L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Hegglin, M. I.] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Schwartz, MJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM michael.j.schwartz@jpl.nasa.gov
RI Schwartz, Michael/F-5172-2016; Hegglin, Michaela/D-7528-2017
OI Schwartz, Michael/0000-0001-6169-5094; Hegglin,
Michaela/0000-0003-2820-9044
NR 94
TC 5
Z9 6
U1 2
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2015
VL 120
IS 2
BP 843
EP 867
DI 10.1002/2014JD021964
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CC1QQ
UT WOS:000350117100028
ER
PT J
AU Smith, LC
Chu, VW
Yang, K
Gleason, CJ
Pitcher, LH
Rennermalm, AK
Legleiter, CJ
Behar, AE
Overstreet, BT
Moustafa, SE
Tedesco, M
Forster, RR
LeWinter, AL
Finnegan, DC
Sheng, YW
Balog, J
AF Smith, Laurence C.
Chu, Vena W.
Yang, Kang
Gleason, Colin J.
Pitcher, Lincoln H.
Rennermalm, Asa K.
Legleiter, Carl J.
Behar, Alberto E.
Overstreet, Brandon T.
Moustafa, Samiah E.
Tedesco, Marco
Forster, Richard R.
LeWinter, Adam L.
Finnegan, David C.
Sheng, Yongwei
Balog, James
TI Efficient meltwater drainage through supraglacial streams and rivers on
the southwest Greenland ice sheet
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Greenland ice sheet; supraglacial hydrology; meltwater runoff; mass
balance; remote sensing
ID SURFACE MASS-BALANCE; WEST GREENLAND; CLIMATE MODEL; LAKES; FLOW;
ACCELERATION; VARIABILITY; IMAGERY; BUDGET
AB Thermally incised meltwater channels that flow each summer across melt-prone surfaces of the Greenland ice sheet have received little direct study. We use high-resolution WorldView-1/2 satellite mapping and in situ measurements to characterize supraglacial water storage, drainage pattern, and discharge across 6,812 km(2) of southwest Greenland in July 2012, after a record melt event. Efficient surface drainage was routed through 523 high-order stream/river channel networks, all of which terminated in moulins before reaching the ice edge. Low surface water storage (3.6 +/- 0.9 cm), negligible impoundment by supraglacial lakes or topographic depressions, and high discharge to moulins (2.54-2.81 cm.d(-1)) indicate that the surface drainage system conveyed its own storage volume every < 2 d to the bed. Moulin discharges mapped inside similar to 52% of the source ice watershed for Isortoq, a major proglacial river, totaled similar to 41-98% of observed proglacial discharge, highlighting the importance of supraglacial river drainage to true outflow from the ice edge. However, Isortoq discharges tended lower than runoff simulations from the Modele Atmospherique Regional (MAR) regional climate model (0.056-0.112 km(3).d(-1) vs. similar to 0.103 km(3).d(-1)), and when integrated over the melt season, totaled just 37-75% of MAR, suggesting nontrivial subglacial water storage even in this melt-prone region of the ice sheet. We conclude that (i) the interior surface of the ice sheet can be efficiently drained under optimal conditions, (ii) that digital elevation models alone cannot fully describe supraglacial drainage and its connection to subglacial systems, and (iii) that predicting outflow from climate models alone, without recognition of subglacial processes, may overestimate true meltwater export from the ice sheet to the ocean.
C1 [Smith, Laurence C.; Chu, Vena W.; Yang, Kang; Gleason, Colin J.; Pitcher, Lincoln H.; Sheng, Yongwei] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Rennermalm, Asa K.; Moustafa, Samiah E.] Rutgers State Univ, Dept Geog, Piscataway, NJ 08854 USA.
[Legleiter, Carl J.; Overstreet, Brandon T.] Univ Wyoming, Dept Geog, Laramie, WY 82071 USA.
[Behar, Alberto E.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tedesco, Marco] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Forster, Richard R.] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[LeWinter, Adam L.; Finnegan, David C.] US Army, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA.
[Balog, James] Earth Vis Trust, Boulder, CO 80304 USA.
RP Smith, LC (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
EM lsmith@geog.ucla.edu
RI Tedesco, Marco/F-7986-2015; Smith, Laurence/E-7785-2012;
OI Smith, Laurence/0000-0001-6866-5904; Legleiter,
Carl/0000-0003-0940-8013; Overstreet, Brandon/0000-0001-7845-6671
FU NASA Cryosphere Program [NNX11AQ38G]
FX This research is dedicated to the memory of Dr. Alberto Behar, who
tragically passed away January 9, 2015. This research was supported by
the NASA Cryosphere Program (Grant NNX11AQ38G), managed by Dr. Thomas
Wagner. P. Morin and C. Porter of the Polar Geospatial Center,
University of Minnesota, provided WorldView-2 satellite images, tasking,
and code for data processing. Updated surface and basal topography
datasets were kindly provided by I. Howat (Ohio State University) and J.
Bamber (University of Bristol). Careful, constructive reviews by the
external readers led to substantial improvements in the finished
manuscript. Field logistical support was provided by CH2M Hill Polar
Field Services, the Kangerlussuaq International Science Station, and Air
Greenland.
NR 33
TC 35
Z9 35
U1 7
U2 36
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 JAN 27
PY 2015
VL 112
IS 4
BP 1001
EP 1006
DI 10.1073/pnas.1413024112
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ7SB
UT WOS:000348417000028
PM 25583477
ER
PT J
AU Zahnle, K
AF Zahnle, Kevin
TI Play it again, SAM
SO SCIENCE
LA English
DT Editorial Material
ID MARS; VOLATILES; METHANE; ORIGIN; LIFE
C1 NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zahnle, K (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM kevin.j.zahnle@nasa.gov
NR 12
TC 5
Z9 5
U1 2
U2 18
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 JAN 23
PY 2015
VL 347
IS 6220
BP 370
EP 371
DI 10.1126/science.aaa3687
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800015
PM 25613875
ER
PT J
AU Gibbs, HK
Rausch, L
Munger, J
Schelly, I
Morton, DC
Noojipady, P
Soares-Filho, B
Barreto, P
Micol, L
Walker, NF
AF Gibbs, H. K.
Rausch, L.
Munger, J.
Schelly, I.
Morton, D. C.
Noojipady, P.
Soares-Filho, B.
Barreto, P.
Micol, L.
Walker, N. F.
TI Brazil's Soy Moratorium
SO SCIENCE
LA English
DT Editorial Material
ID DEFORESTATION; AMAZON
C1 [Gibbs, H. K.; Rausch, L.; Munger, J.; Schelly, I.] Univ Wisconsin, Madison, WI 53726 USA.
[Morton, D. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Noojipady, P.] Univ Maryland, College Pk, MD 20742 USA.
[Noojipady, P.; Walker, N. F.] Natl Wildlife Federat, Washington, DC 20006 USA.
[Soares-Filho, B.] Univ Fed Minas Gerais, BR-31270901 Belo Horizonte, MG, Brazil.
[Barreto, P.] IMAZON Amazon Inst People & Environm, BR-66060162 Belem, Para, Brazil.
[Micol, L.] Inst Ctr Vida, BR-78045055 Cuiaba, Mato Grosso, Brazil.
RP Gibbs, HK (reprint author), Univ Wisconsin, Madison, WI 53726 USA.
EM hkgibbs@wisc.edu
RI Morton, Douglas/D-5044-2012
NR 12
TC 59
Z9 61
U1 14
U2 71
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 JAN 23
PY 2015
VL 347
IS 6220
BP 377
EP 378
DI 10.1126/science.aaa0181
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800019
PM 25613879
ER
PT J
AU Taylor, MGGT
Alexander, C
Altobelli, N
Fulle, M
Fulchignoni, M
Grun, E
Weissman, P
AF Taylor, M. G. G. T.
Alexander, C.
Altobelli, N.
Fulle, M.
Fulchignoni, M.
Gruen, E.
Weissman, P.
TI Rosetta begins its COMET TALE
SO SCIENCE
LA English
DT Editorial Material
C1 [Taylor, M. G. G. T.] European Space Agcy, European Space Res & Technol Ctr, Sci & Robot Explorat Directorate, NL-2200 AG Noordwijk, Netherlands.
[Alexander, C.; Weissman, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Altobelli, N.] European Space Agcy, Sci & Robot Explorat Directorate, European Space Astron Ctr, Madrid, Spain.
[Fulle, M.] INAF Osservatorio Astron, Trieste, Italy.
[Fulchignoni, M.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, Paris, France.
[Gruen, E.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
RP Taylor, MGGT (reprint author), European Space Agcy, European Space Res & Technol Ctr, Sci & Robot Explorat Directorate, NL-2200 AG Noordwijk, Netherlands.
EM mtaylor@cosmos.esa.int
OI fulle, marco/0000-0001-8435-5287
NR 0
TC 13
Z9 13
U1 0
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 23
PY 2015
VL 347
IS 6220
BP 387
EP 387
DI 10.1126/science.aaa4542
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800026
PM 25613884
ER
PT J
AU Mahaffy, PR
Webster, CR
Stern, JC
Brunner, AE
Atreya, SK
Conrad, PG
Domagal-Goldman, S
Eigenbrode, JL
Flesch, GJ
Christensen, LE
Franz, HB
Freissinet, C
Glavin, DP
Grotzinger, JP
Jones, JH
Leshin, LA
Malespin, C
McAdam, AC
Ming, DW
Navarro-Gonzalez, R
Niles, PB
Owen, T
Pavlov, AA
Steele, A
Trainer, MG
Williford, KH
Wray, JJ
AF Mahaffy, P. R.
Webster, C. R.
Stern, J. C.
Brunner, A. E.
Atreya, S. K.
Conrad, P. G.
Domagal-Goldman, S.
Eigenbrode, J. L.
Flesch, G. J.
Christensen, L. E.
Franz, H. B.
Freissinet, C.
Glavin, D. P.
Grotzinger, J. P.
Jones, J. H.
Leshin, L. A.
Malespin, C.
McAdam, A. C.
Ming, D. W.
Navarro-Gonzalez, R.
Niles, P. B.
Owen, T.
Pavlov, A. A.
Steele, A.
Trainer, M. G.
Williford, K. H.
Wray, J. J.
CA Msl Sci Team
TI The imprint of atmospheric evolution in the D/H of Hesperian clay
minerals on Mars
SO SCIENCE
LA English
DT Article
ID MARTIAN ATMOSPHERE; TERRESTRIAL PLANETS; HYDROGEN ISOTOPES; WATER
RESERVOIRS; GALE CRATER; ORIGIN; FRACTIONATION; CONSTRAINTS; DEUTERIUM;
ABUNDANCE
AB The deuterium-to-hydrogen (D/H) ratio in strongly bound water or hydroxyl groups in ancient martian clays retains the imprint of the water of formation of these minerals. Curiosity's Sample Analysis at Mars (SAM) experiment measured thermally evolved water and hydrogen gas released between 550 degrees and 950 degrees C from samples of Hesperian-era Gale crater smectite to determine this isotope ratio. The D/H value is 3.0 (+/- 0.2) times the ratio in standard mean ocean water. The D/H ratio in this similar to 3-billion-year-old mudstone, which is half that of the present martian atmosphere but substantially higher than that expected in very early Mars, indicates an extended history of hydrogen escape and desiccation of the planet.
C1 [Mahaffy, P. R.; Stern, J. C.; Brunner, A. E.; Conrad, P. G.; Domagal-Goldman, S.; Eigenbrode, J. L.; Franz, H. B.; Freissinet, C.; Glavin, D. P.; Malespin, C.; McAdam, A. C.; Pavlov, A. A.; Trainer, M. G.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Webster, C. R.; Flesch, G. J.; Christensen, L. E.; Williford, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brunner, A. E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA.
[Brunner, A. E.; Franz, H. B.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, College Pk, MD 20742 USA.
[Atreya, S. K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Freissinet, C.] Oak Ridge Associated Univ, NASA, Postdoctoral Program, Oak Ridge, TN 37831 USA.
[Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Jones, J. H.; Ming, D. W.; Niles, P. B.] NASA, Johnson Space Flight Ctr, Houston, TX 77058 USA.
[Leshin, L. A.] Worcester Polytech Inst, Off President, Worcester, MA 01609 USA.
[Malespin, C.] NASA, Goddard Earth Sci Technol & Res GESTAR, Univ Space Res Assoc USRA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico.
[Owen, T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Wray, J. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
RP Mahaffy, PR (reprint author), NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM paul.r.mahaffy@nasa.gov
RI Ramos, Miguel/K-2230-2014; Zorzano, Maria-Paz/F-2184-2015; Dworkin,
Jason/C-9417-2012; Trainer, Melissa/E-1477-2012; Lemmon,
Mark/E-9983-2010; Merikallio, Sini/C-7812-2014; szopa,
cyril/C-6865-2015; Gonzalez, Rafael/D-1748-2009; Martin-Torres,
Francisco Javier/G-6329-2015; Rodriguez-Manfredi, Jose/L-8001-2014;
Glavin, Daniel/D-6194-2012; Harri, Ari-Matti/C-7142-2012; Wray,
James/B-8457-2008; Zorzano, Maria-Paz/C-5784-2015
OI Ramos, Miguel/0000-0003-3648-6818; Zorzano,
Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997;
Lemmon, Mark/0000-0002-4504-5136; Merikallio, Sini/0000-0001-7120-6127;
szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco
Javier/0000-0001-6479-2236; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Glavin, Daniel/0000-0001-7779-7765; Harri,
Ari-Matti/0000-0001-8541-2802; Wray, James/0000-0001-5559-2179; Zorzano,
Maria-Paz/0000-0002-4492-9650
FU NASA's Mars Exploration Program
FX This work was supported by NASA's Mars Exploration Program. The
dedicated teams that developed the SAM suite of instruments are
acknowledged. All data described can be found in NASA's the Planetary
Data System archive pds.nasa.gov.
NR 45
TC 28
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U1 7
U2 81
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 JAN 23
PY 2015
VL 347
IS 6220
BP 412
EP 414
DI 10.1126/science.1260291
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800040
PM 25515119
ER
PT J
AU Webster, CR
Mahaffy, PR
Atreya, SK
Flesch, GJ
Mischna, MA
Meslin, PY
Farley, KA
Conrad, PG
Christensen, LE
Pavlov, AA
Martin-Torres, J
Zorzano, MP
McConnochie, TH
Owen, T
Eigenbrode, JL
Glavin, DP
Steele, A
Malespin, CA
Archer, PD
Sutter, B
Coll, P
Freissinet, C
McKay, CP
Moores, JE
Schwenzer, SP
Bridges, JC
Navarro-Gonzalez, R
Gellert, R
Lemmon, MT
AF Webster, Christopher R.
Mahaffy, Paul R.
Atreya, Sushil K.
Flesch, Gregory J.
Mischna, Michael A.
Meslin, Pierre-Yves
Farley, Kenneth A.
Conrad, Pamela G.
Christensen, Lance E.
Pavlov, Alexander A.
Martin-Torres, Javier
Zorzano, Maria-Paz
McConnochie, Timothy H.
Owen, Tobias
Eigenbrode, Jennifer L.
Glavin, Daniel P.
Steele, Andrew
Malespin, Charles A.
Archer, P. Douglas, Jr.
Sutter, Brad
Coll, Patrice
Freissinet, Caroline
McKay, Christopher P.
Moores, John E.
Schwenzer, Susanne P.
Bridges, John C.
Navarro-Gonzalez, Rafael
Gellert, Ralf
Lemmon, Mark T.
CA MSL Sci Team
TI Mars methane detection and variability at Gale crater
SO SCIENCE
LA English
DT Article
ID MARTIAN DUST DEVILS; OXIDANT ENHANCEMENT; ATMOSPHERE; LIFE;
HABITABILITY; SEARCH; ORIGIN; STORMS
AB Reports of plumes or patches of methane in the martian atmosphere that vary over monthly time scales have defied explanation to date. From in situ measurements made over a 20-month period by the tunable laser spectrometer of the Sample Analysis at Mars instrument suite on Curiosity at Gale crater, we report detection of background levels of atmospheric methane of mean value 0.69 +/- 0.25 parts per billion by volume (ppbv) at the 95% confidence interval (CI). This abundance is lower than model estimates of ultraviolet degradation of accreted interplanetary dust particles or carbonaceous chondrite material. Additionally, in four sequential measurements spanning a 60-sol period (where 1 sol is a martian day), we observed elevated levels of methane of 7.2 +/- 2.1 ppbv (95% CI), implying that Mars is episodically producing methane from an additional unknown source.
C1 [Webster, Christopher R.; Flesch, Gregory J.; Mischna, Michael A.; Christensen, Lance E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mahaffy, Paul R.; Conrad, Pamela G.; Pavlov, Alexander A.; Eigenbrode, Jennifer L.; Glavin, Daniel P.; Malespin, Charles A.; Freissinet, Caroline] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Atreya, Sushil K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Meslin, Pierre-Yves] CNRS, UPS, Inst Rech Astrophys & Planetol, OMP, F-31028 Toulouse, France.
[Farley, Kenneth A.] CALTECH, Pasadena, CA 91125 USA.
[Martin-Torres, Javier] Univ Granada, CSIC, Inst Andaluz Ciencias Tierra, Granada, Spain.
[Martin-Torres, Javier] Lulea Univ Technol, Div Space Technol, Kiruna, Sweden.
[Zorzano, Maria-Paz] CSIC, Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, Madrid, Spain.
[McConnochie, Timothy H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Owen, Tobias] Univ Hawaii, Honolulu, HI 96822 USA.
[Steele, Andrew] Carnegie Inst Sci, Washington, DC 20015 USA.
[Archer, P. Douglas, Jr.; Sutter, Brad] NASA, Jacobs Technol, Johnson Space Ctr, Houston, TX 77058 USA.
[Coll, Patrice] CNRS, Lab Interuniv Syst Atmospher LISA, UMR 7583, Paris, France.
[McKay, Christopher P.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Moores, John E.] York Univ, Toronto, ON M3J 1P3, Canada.
[Schwenzer, Susanne P.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Bridges, John C.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England.
[Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Gellert, Ralf] Univ Guelph, Guelph, ON N1G 2W1, Canada.
[Lemmon, Mark T.] Texas A&M Univ, College Stn, TX 77843 USA.
RP Webster, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chris.r.webster@jpl.nasa.gov
RI Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Zorzano,
Maria-Paz/C-5784-2015; Lemmon, Mark/E-9983-2010; Merikallio,
Sini/C-7812-2014; szopa, cyril/C-6865-2015; Gonzalez,
Rafael/D-1748-2009; Martin-Torres, Francisco Javier/G-6329-2015;
Rodriguez-Manfredi, Jose/L-8001-2014; Glavin, Daniel/D-6194-2012; Harri,
Ari-Matti/C-7142-2012; Ramos, Miguel/K-2230-2014
OI Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin,
Jason/0000-0002-3961-8997; Schwenzer, Susanne Petra/0000-0002-9608-0759;
Kashyap, Srishti/0000-0003-4950-9636; Zorzano,
Maria-Paz/0000-0002-4492-9650; Lemmon, Mark/0000-0002-4504-5136;
Merikallio, Sini/0000-0001-7120-6127; szopa, cyril/0000-0002-0090-4056;
Martin-Torres, Francisco Javier/0000-0001-6479-2236; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Glavin, Daniel/0000-0001-7779-7765; Harri,
Ari-Matti/0000-0001-8541-2802; Ramos, Miguel/0000-0003-3648-6818
FU NASA; Spanish Ministry of Economy and Competiveness; UK Space Agency;
Canadian Space Agency
FX The research described here was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. Data described in the paper are further described in
the supplementary materials and have been submitted to NASA's Planetary
Data System (PDS) under an arrangement with the Mars Science Laboratory
(MSL) project. Funding is acknowledged for J.M.-T. and M.-P.Z. from the
Spanish Ministry of Economy and Competiveness, J.C.B. from the UK Space
Agency, and R.G. from the Canadian Space Agency.
NR 41
TC 67
Z9 68
U1 20
U2 135
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 JAN 23
PY 2015
VL 347
IS 6220
BP 415
EP 417
DI 10.1126/science.1261713
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800041
PM 25515120
ER
PT J
AU Capaccioni, F
Coradini, A
Filacchione, G
Erard, S
Arnold, G
Drossart, P
De Sanctis, MC
Bockelee-Morvan, D
Capria, MT
Tosi, F
Leyrat, C
Schmitt, B
Quirico, E
Cerroni, P
Mennella, V
Raponi, A
Ciarniello, M
McCord, T
Moroz, L
Palomba, E
Ammannito, E
Barucci, MA
Bellucci, G
Benkhoff, J
Bibring, JP
Blanco, A
Blecka, M
Carlson, R
Carsenty, U
Colangeli, L
Combes, M
Combi, M
Crovisier, J
Encrenaz, T
Federico, C
Fink, U
Fonti, S
Ip, WH
Irwin, P
Jaumann, R
Kuehrt, E
Langevin, Y
Magni, G
Mottola, S
Orofino, V
Palumbo, P
Piccioni, G
Schade, U
Taylor, F
Tiphene, D
Tozzi, GP
Beck, P
Biver, N
Bonal, L
Combe, JP
Despan, D
Flamini, E
Fornasier, S
Frigeri, A
Grassi, D
Gudipati, M
Longobardo, A
Markus, K
Merlin, F
Orosei, R
Rinaldi, G
Stephan, K
Cartacci, M
Cicchetti, A
Giuppi, S
Hello, Y
Henry, F
Jacquinod, S
Noschese, R
Peter, G
Politi, R
Reess, JM
Semery, A
AF Capaccioni, F.
Coradini, A.
Filacchione, G.
Erard, S.
Arnold, G.
Drossart, P.
De Sanctis, M. C.
Bockelee-Morvan, D.
Capria, M. T.
Tosi, F.
Leyrat, C.
Schmitt, B.
Quirico, E.
Cerroni, P.
Mennella, V.
Raponi, A.
Ciarniello, M.
McCord, T.
Moroz, L.
Palomba, E.
Ammannito, E.
Barucci, M. A.
Bellucci, G.
Benkhoff, J.
Bibring, J. P.
Blanco, A.
Blecka, M.
Carlson, R.
Carsenty, U.
Colangeli, L.
Combes, M.
Combi, M.
Crovisier, J.
Encrenaz, T.
Federico, C.
Fink, U.
Fonti, S.
Ip, W. H.
Irwin, P.
Jaumann, R.
Kuehrt, E.
Langevin, Y.
Magni, G.
Mottola, S.
Orofino, V.
Palumbo, P.
Piccioni, G.
Schade, U.
Taylor, F.
Tiphene, D.
Tozzi, G. P.
Beck, P.
Biver, N.
Bonal, L.
Combe, J. -Ph.
Despan, D.
Flamini, E.
Fornasier, S.
Frigeri, A.
Grassi, D.
Gudipati, M.
Longobardo, A.
Markus, K.
Merlin, F.
Orosei, R.
Rinaldi, G.
Stephan, K.
Cartacci, M.
Cicchetti, A.
Giuppi, S.
Hello, Y.
Henry, F.
Jacquinod, S.
Noschese, R.
Peter, G.
Politi, R.
Reess, J. M.
Semery, A.
TI The organic-rich surface of comet 67P/Churyumov-Gerasimenko as seen by
VIRTIS/Rosetta
SO SCIENCE
LA English
DT Article
ID SPECTRAL REFLECTANCE PROPERTIES; CARBONACEOUS CHONDRITES; WATER ICE;
81P/WILD-2; MICROMETEORITES; SPECTROSCOPY; NUCLEUS; ANALOGS; MATTER;
SNOW
AB The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 +/- 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% k angstrom(-1)), and the broad absorption feature in the 2.9-to-3.6-micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.
C1 [Capaccioni, F.; Coradini, A.; Filacchione, G.; De Sanctis, M. C.; Capria, M. T.; Tosi, F.; Cerroni, P.; Raponi, A.; Ciarniello, M.; Palomba, E.; Bellucci, G.; Magni, G.; Piccioni, G.; Frigeri, A.; Grassi, D.; Longobardo, A.; Rinaldi, G.; Cartacci, M.; Cicchetti, A.; Giuppi, S.; Noschese, R.; Politi, R.] Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Erard, S.; Drossart, P.; Bockelee-Morvan, D.; Leyrat, C.; Barucci, M. A.; Combes, M.; Crovisier, J.; Encrenaz, T.; Tiphene, D.; Biver, N.; Despan, D.; Fornasier, S.; Merlin, F.; Hello, Y.; Henry, F.; Jacquinod, S.; Reess, J. M.; Semery, A.] Univ Paris Diderot, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,CNRS, Meudon, France.
[Arnold, G.; Moroz, L.; Carsenty, U.; Jaumann, R.; Kuehrt, E.; Mottola, S.; Markus, K.; Stephan, K.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, Berlin, Germany.
[Schmitt, B.; Quirico, E.; Beck, P.; Bonal, L.] Univ Grenoble Alpes, CNRS, Inst Planetol & Astrophys Grenoble, Grenoble, France.
[Mennella, V.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[McCord, T.; Combe, J. -Ph.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Ammannito, E.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Benkhoff, J.; Colangeli, L.] European Space Agcy ESA, European Space Res & Technol Ctr ESTEC, Noordwijk, Netherlands.
[Bibring, J. P.; Langevin, Y.] CNRS, Inst Astrophys Spatial, F-91405 Orsay, France.
[Blanco, A.; Fonti, S.; Orofino, V.] Univ Salento, Dipartimento Matemat & Fis Ennio De Giorgi, Lecce, Italy.
[Blecka, M.] Polish Acad Sci, Ctr Space Res, Warsaw, Poland.
[Carlson, R.; Gudipati, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Combi, M.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Federico, C.] Univ Perugia, I-06100 Perugia, Italy.
[Fink, U.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
[Ip, W. H.] Natl Cent Univ, Taipei, Taiwan.
[Irwin, P.; Taylor, F.] Univ Oxford, Dept Phys, Oxford, England.
[Jaumann, R.] Free Univ Berlin, Inst Geosci, D-12249 Berlin, Germany.
[Palumbo, P.] Univ Parthenope, Naples, Italy.
[Schade, U.] Helmholtz Zentrum Berlin Mat & Energie, Berlin, Germany.
[Tozzi, G. P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Flamini, E.] Agenzia Spaziale Italiana, Rome, Italy.
[Gudipati, M.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Orosei, R.] CNR, Ist Radioastron, INAF, I-40126 Bologna, Italy.
[Peter, G.] DLR, Inst Opt Sensorsyst, Berlin, Germany.
RP Capaccioni, F (reprint author), Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
EM fabrizio.capaccioni@iaps.inaf.it
RI quirico, eric/K-9650-2013; Combi, Michael/J-1697-2012; Schmitt,
Bernard/A-1064-2009; Gudipati, Murthy/F-7575-2011; Beck,
Pierre/F-3149-2011; Frigeri, Alessandro/F-2151-2010;
OI Tosi, Federico/0000-0003-4002-2434; capria, maria
teresa/0000-0002-9814-9588; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Cerroni, Priscilla/0000-0003-0239-2741;
Bellucci, Giancarlo/0000-0003-0867-8679; Capaccioni,
Fabrizio/0000-0003-1631-4314; Filacchione, Gianrico/0000-0001-9567-0055;
Irwin, Patrick/0000-0002-6772-384X; Grassi, Davide/0000-0003-1653-3066;
Palomba, Ernesto/0000-0002-9101-6774; quirico, eric/0000-0003-2768-0694;
Piccioni, Giuseppe/0000-0002-7893-6808; Ciarniello,
Mauro/0000-0002-7498-5207; Politi, Romolo/0000-0002-9793-9780; Combi,
Michael/0000-0002-9805-0078; Schmitt, Bernard/0000-0002-1230-6627;
Frigeri, Alessandro/0000-0002-9140-3977; Cartacci,
Marco/0000-0001-9825-1817; CICCHETTI, ANDREA/0000-0002-9588-6531;
Noschese, Raffaella/0000-0003-0502-0337
FU Italian Space Agency (ASI, Italy); Centre National d'Etudes Spatiales
(CNES, France); DLR (Germany); NASA (USA) Rosetta Program; Science and
Technology Facilities Council (UK); CNES; ASI; Rosetta Science Ground
Segment; Rosetta Mission Operations Centre
FX We thank the following institutions and agencies for support of this
work: Italian Space Agency (ASI, Italy), Centre National d'Etudes
Spatiales (CNES, France), DLR (Germany), NASA (USA) Rosetta Program, and
Science and Technology Facilities Council (UK). VIRTIS was built by a
consortium, which includes Italy, France, and Germany, under the
scientific responsibility of the Istituto di Astrofisica e Planetologia
Spaziali of INAF, Italy, which also guides the scientific operations.
The VIRTIS instrument development has been funded and managed by ASI,
with contributions from Observatoire de Meudon financed by CNES, and
from DLR. We thank the Rosetta Science Ground Segment and the Rosetta
Mission Operations Centre for their support throughout the early phases
of the mission. The VIRTIS calibrated data will be available through the
ESA's Planetary Science Archive Website
(www.rssd.esa.int/index.php?project=PSA&page=index) and is available
upon request until posted to the archive. The VIRTIS Team wishes to
dedicate this paper to the memory of Angioletta Coradini, conceiver of
the instrument, our leader, and friend.
NR 31
TC 43
Z9 45
U1 9
U2 45
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 JAN 23
PY 2015
VL 347
IS 6220
AR aaa0628
DI 10.1126/science.aaa0628
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800031
PM 25613895
ER
PT J
AU Gulkis, S
Allen, M
von Allmen, P
Beaudin, G
Biver, N
Bockelee-Morvan, D
Choukroun, M
Crovisier, J
Davidsson, BJR
Encrenaz, P
Encrenaz, T
Frerking, M
Hartogh, P
Hofstadter, M
Ip, WH
Janssen, M
Jarchow, C
Keihm, S
Lee, S
Lellouch, E
Leyrat, C
Rezac, L
Schloerb, FP
Spilker, T
AF Gulkis, Samuel
Allen, Mark
von Allmen, Paul
Beaudin, Gerard
Biver, Nicolas
Bockelee-Morvan, Dominique
Choukroun, Mathieu
Crovisier, Jacques
Davidsson, Bjoern J. R.
Encrenaz, Pierre
Encrenaz, Therese
Frerking, Margaret
Hartogh, Paul
Hofstadter, Mark
Ip, Wing-Huen
Janssen, Michael
Jarchow, Christopher
Keihm, Stephen
Lee, Seungwon
Lellouch, Emmanuel
Leyrat, Cedric
Rezac, Ladislav
Schloerb, F. Peter
Spilker, Thomas
TI Subsurface properties and early activity of comet
67P/Churyumov-Gerasimenko
SO SCIENCE
LA English
DT Article
ID RADIATIVE-TRANSFER
AB Heat transport and ice sublimation in comets are interrelated processes reflecting properties acquired at the time of formation and during subsequent evolution. The Microwave Instrument on the Rosetta Orbiter (MIRO) acquired maps of the subsurface temperature of comet 67P/Churyumov-Gerasimenko, at 1.6 mm and 0.5 mm wavelengths, and spectra of water vapor. The total H2O production rate varied from 0.3 kg s(-1) in early June 2014 to 1.2 kg s(-1) in late August and showed periodic variations related to nucleus rotation and shape. Water outgassing was localized to the "neck" region of the comet. Subsurface temperatures showed seasonal and diurnal variations, which indicated that the submillimeter radiation originated at depths comparable to the diurnal thermal skin depth. A low thermal inertia (similar to 10 to 50 J K-1 m(-2) s(-0.5)), consistent with a thermally insulating powdered surface, is inferred.
C1 [Gulkis, Samuel; Allen, Mark; von Allmen, Paul; Choukroun, Mathieu; Frerking, Margaret; Hofstadter, Mark; Janssen, Michael; Keihm, Stephen; Lee, Seungwon; Schloerb, F. Peter; Spilker, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beaudin, Gerard; Encrenaz, Pierre] Univ Paris 06, Observ Paris, PSL Res Univ, LERMA,CNRS,UMR8112, F-75014 Paris, France.
[Biver, Nicolas; Bockelee-Morvan, Dominique; Crovisier, Jacques; Encrenaz, Therese; Lellouch, Emmanuel; Leyrat, Cedric] Univ Paris Diderot, UPMC, CNRS, LESIA Observ Paris, F-92195 Meudon, France.
[Davidsson, Bjoern J. R.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
[Hartogh, Paul; Jarchow, Christopher; Rezac, Ladislav] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Ip, Wing-Huen] Natl Cent Univ, Taoyuan 32001, Taiwan.
[Schloerb, F. Peter] Univ Massachusetts, Amherst, MA 01003 USA.
RP Gulkis, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM samuel.gulkis@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
FU entire MIRO project teams at the Jet Propulsion Laboratory;
Max-Planck-Institut fur Sonnensystemforschung; LESIA-Observatoire de
Paris; LERMA-Observatoire de Paris-Meudon; MIRO; National Aeronautics
and Space Administration; Deutsches Zentrum fur Luft- und Raumfahrt;
Max-Planck-Gesellschaft; Centre National d'Etudes Spatiales (CNES);
CNRS/Institut National des Sciences de l'Univers (INSU); National
Central University; Taiwanese National Science Counsel
[101-2111-M-008-016]; University of Massachusetts, Amherst, USA; Uppsala
University; Swedish National Space Board; ESOC in Germany; European
Space Astronomy Center (ESAC) in Spain
FX The authors gratefully acknowledge the assistance and support of the
entire MIRO project teams at the Jet Propulsion Laboratory, the
Max-Planck-Institut fur Sonnensystemforschung, LESIA-Observatoire de
Paris, and LERMA-Observatoire de Paris-Meudon. We thank Y. Anderson, T.
Koch, R. Nowicki, and L. Pan for their efforts in scheduling,
operations, and support of the MIRO instrument. The authors recognize
here the enormous contributions that our friend and colleague, Lucas
Kamp, made to the MIRO science and engineering efforts before his recent
death. The authors acknowledge support from their institutions and
funding sources. A part of the research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. A part
of the research was carried out at the Max-Planck-Institut fur
Sonnensystemforschung with financial support from Deutsches Zentrum fur
Luft- und Raumfahrt and Max-Planck-Gesellschaft. Parts of the research
were carried out by LESIA and LERMA, Observatoire de Paris, with
financial support from Centre National d'Etudes Spatiales (CNES) and
CNRS/Institut National des Sciences de l'Univers (INSU); at the National
Central University with funding from the Taiwanese National Science
Counsel grant 101-2111-M-008-016; at the University of Massachusetts,
Amherst, USA; and at Uppsala University with financial support from the
Swedish National Space Board. We acknowledge personnel at ESA's European
Space Operations Center (ESOC) in Darmstadt, Germany, and at ESA and
NASA/JPL tracking stations for their professional work in communication
with and directing the Rosetta spacecraft, thereby making this mission
possible. We acknowledge the excellent support provided by the Rosetta
teams at the ESOC in Germany and the European Space Astronomy Center
(ESAC) in Spain. Special mention is made of C. Vallat, whose superb
efforts have made many difficult MIRO observing sequences possible; B.
Grieger, whose calculations and visualizations have enabled and
optimized our science return; and N. Altobelli and M. Kuppers, whose
early liaison support and later oversight responsibilities have greatly
benefited the mission as a whole. The authors thank Holger Sierks and
the OSIRIS team for permission to use the SHAP2 shape model for analysis
purposes and for permission to publish several images here. All MIRO
data are released through the PSA archive of ESA and the PDS archive of
NASA. The data reported here are scheduled for delivery to the archive
on 19 May 2015 and are available on request until then.
NR 10
TC 31
Z9 31
U1 1
U2 20
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 23
PY 2015
VL 347
IS 6220
AR aaa0709
DI 10.1126/science.aaa0709
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800034
PM 25613896
ER
PT J
AU Rotundi, A
Sierks, H
Della Corte, V
Fulle, M
Gutierrez, PJ
Lara, L
Barbieri, C
Lamy, PL
Rodrigo, R
Koschny, D
Rickman, H
Keller, HU
Lopez-Moreno, JJ
Accolla, M
Agarwal, J
A'Hearn, MF
Altobelli, N
Angrilli, F
Barucci, MA
Bertaux, JL
Bertini, I
Bodewits, D
Bussoletti, E
Colangeli, L
Cosi, M
Cremonese, G
Crifo, JF
Da Deppo, V
Davidsson, B
Debei, S
De Cecco, M
Esposito, F
Ferrari, M
Fornasier, S
Giovane, F
Gustafson, B
Green, SF
Groussin, O
Grun, E
Guttler, C
Herranz, ML
Hviid, SF
Ip, W
Ivanovski, S
Jernimo, JM
Jorda, L
Knollenberg, J
Kramm, R
Kuhrt, E
Kuppers, M
Lazzarin, M
Leese, MR
Lopez-Jimenez, AC
Lucarelli, F
Lowry, SC
Marzari, F
Epifani, EM
McDonnell, JAM
Mennella, V
Michalik, H
Molina, A
Morales, R
Moreno, F
Mottola, S
Naletto, G
Oklay, N
Ortiz, JL
Palomba, E
Palumbo, P
Perrin, JM
Rodriguez, J
Sabau, L
Snodgrass, C
Sordini, R
Thomas, N
Tubiana, C
Vincent, JB
Weissman, P
Wenzel, KP
Zakharov, V
Zarnecki, JC
AF Rotundi, Alessandra
Sierks, Holger
Della Corte, Vincenzo
Fulle, Marco
Gutierrez, Pedro J.
Lara, Luisa
Barbieri, Cesare
Lamy, Philippe L.
Rodrigo, Rafael
Koschny, Detlef
Rickman, Hans
Keller, Horst Uwe
Lopez-Moreno, Jose J.
Accolla, Mario
Agarwal, Jessica
A'Hearn, Michael F.
Altobelli, Nicolas
Angrilli, Francesco
Barucci, M. Antonietta
Bertaux, Jean-Loup
Bertini, Ivano
Bodewits, Dennis
Bussoletti, Ezio
Colangeli, Luigi
Cosi, Massimo
Cremonese, Gabriele
Crifo, Jean-Francois
Da Deppo, Vania
Davidsson, Bjoern
Debei, Stefano
De Cecco, Mariolino
Esposito, Francesca
Ferrari, Marco
Fornasier, Sonia
Giovane, Frank
Gustafson, Bo
Green, Simon F.
Groussin, Olivier
Gruen, Eberhard
Guettler, Carsten
Herranz, Miguel L.
Hviid, Stubbe F.
Ip, Wing
Ivanovski, Stavro
Jernimo, Jose M.
Jorda, Laurent
Knollenberg, Joerg
Kramm, Rainer
Kuehrt, Ekkehard
Kueppers, Michael
Lazzarin, Monica
Leese, Mark R.
Lopez-Jimenez, Antonio C.
Lucarelli, Francesca
Lowry, Stephen C.
Marzari, Francesco
Epifani, Elena Mazzotta
McDonnell, J. Anthony M.
Mennella, Vito
Michalik, Harald
Molina, Antonio
Morales, Rafael
Moreno, Fernando
Mottola, Stefano
Naletto, Giampiero
Oklay, Nilda
Ortiz, Jose L.
Palomba, Ernesto
Palumbo, Pasquale
Perrin, Jean-Marie
Rodriguez, Julio
Sabau, Lola
Snodgrass, Colin
Sordini, Roberto
Thomas, Nicolas
Tubiana, Cecilia
Vincent, Jean-Baptiste
Weissman, Paul
Wenzel, Klaus-Peter
Zakharov, Vladimir
Zarnecki, John C.
TI Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound
to the Sun
SO SCIENCE
LA English
DT Article
ID ROSETTA MISSION; MODEL; PARTICLES; P/HALLEY; ORBITS; NUCLEI; GIOTTO;
WILD-2; SIZE
AB Critical measurements for understanding accretion and the dust/gas ratio in the solar nebula, where planets were forming 4.5 billion years ago, are being obtained by the GIADA (Grain Impact Analyser and Dust Accumulator) experiment on the European Space Agency's Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko. Between 3.6 and 3.4 astronomical units inbound, GIADA and OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) detected 35 outflowing grains of mass 10(-10) to 10(-7) kilograms, and 48 grains of mass 10(-5) to 10(-2) kilograms, respectively. Combined with gas data from the MIRO (Microwave Instrument for the Rosetta Orbiter) and ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instruments, we find a dust/gas mass ratio of 4 +/- 2 averaged over the sunlit nucleus surface. A cloud of larger grains also encircles the nucleus in bound orbits from the previous perihelion. The largest orbiting clumps are meter-sized, confirming the dust/gas ratio of 3 inferred at perihelion from models of dust comae and trails.
C1 [Rotundi, Alessandra; Della Corte, Vincenzo; Accolla, Mario; Ferrari, Marco; Ivanovski, Stavro; Palomba, Ernesto; Palumbo, Pasquale; Sordini, Roberto] Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, I-0133 Rome, Italy.
[Rotundi, Alessandra; Accolla, Mario; Bussoletti, Ezio; Ferrari, Marco; Lucarelli, Francesca; Palumbo, Pasquale] Uni Napoli Parthenope, Dipartimento Sci & Tecnol, CDN IC4, I-80143 Naples, Italy.
[Sierks, Holger; Agarwal, Jessica; Guettler, Carsten; Kramm, Rainer; Oklay, Nilda; Snodgrass, Colin; Tubiana, Cecilia; Vincent, Jean-Baptiste] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Fulle, Marco] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Gutierrez, Pedro J.; Lara, Luisa; Lopez-Moreno, Jose J.; Herranz, Miguel L.; Jernimo, Jose M.; Lopez-Jimenez, Antonio C.; Morales, Rafael; Moreno, Fernando; Ortiz, Jose L.; Rodriguez, Julio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Barbieri, Cesare; Lazzarin, Monica] Univ Padua, Dept Phys & Astron, I-35122 Padua, Italy.
[Lamy, Philippe L.; Groussin, Olivier; Jorda, Laurent] CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
[Lamy, Philippe L.; Groussin, Olivier; Jorda, Laurent] Aix Marseille Univ, F-13388 Marseille, France.
[Rodrigo, Rafael] CSIC, Inst Nacl Tecn Aerosp, Ctr Astrobiol, Madrid 28691, Spain.
[Rodrigo, Rafael; Zarnecki, John C.] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Koschny, Detlef; Wenzel, Klaus-Peter] European Space Agcy, Sci Support Off, NL-2201 Noordwijk, Netherlands.
[Rickman, Hans; Davidsson, Bjoern] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Rickman, Hans] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
[Keller, Horst Uwe] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[A'Hearn, Michael F.; Bodewits, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Altobelli, Nicolas; Kueppers, Michael] European Space Agcy, European Space Astron Ctr, Madrid 28692, Spain.
[Angrilli, Francesco; Debei, Stefano] Univ Padua, Dept Mech Engn, I-35131 Padua, Italy.
[Barucci, M. Antonietta; Fornasier, Sonia; Zakharov, Vladimir] Univ Paris Diderot, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astron, Observ Paris,CNRS, F-92195 Meudon, France.
[Bertaux, Jean-Loup; Crifo, Jean-Francois; Perrin, Jean-Marie] Univ Versailles St Quentin En Yvelines, Inst Pierre Simon Laplace, Lab Atmospheres, Observ Spatiales,CNRS, F-78280 Guyancourt, France.
[Bertini, Ivano] Univ Padua, Ctr Interdipartimentale Studi & Attivita Spaziali, I-35100 Padua, Italy.
[Colangeli, Luigi] ESA, European Space Res & Technol Ctr ESTEC, NL-2201 AZ Noordwijk, Netherlands.
[Cosi, Massimo] Selex ES, Florence, Italy.
[Cremonese, Gabriele] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Da Deppo, Vania] CNR, Ist Foton & Nanotecnol, Unita Operat Supporto Padova LUXOR, I-35131 Padua, Italy.
[De Cecco, Mariolino] Univ Trent, I-38100 Trento, Italy.
[Esposito, Francesca; Epifani, Elena Mazzotta; Mennella, Vito] Osserv Astron Capodimonte, INAF, I-80133 Naples, Italy.
[Giovane, Frank] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA.
[Gustafson, Bo] Univ Florida, Gainesville, FL 32611 USA.
[Green, Simon F.; Leese, Mark R.; McDonnell, J. Anthony M.; Snodgrass, Colin; Zarnecki, John C.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hviid, Stubbe F.; Knollenberg, Joerg; Kuehrt, Ekkehard; Mottola, Stefano] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Ip, Wing] Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan.
[Lowry, Stephen C.; McDonnell, J. Anthony M.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NZ, Kent, England.
[Marzari, Francesco] Univ Padua, Dept Phys, I-35131 Padua, Italy.
[McDonnell, J. Anthony M.] Unispacekent, Canterbury CT2 8EF, Kent, England.
[Michalik, Harald] Inst Datentech & Kommunikat Netze, D-38106 Braunschweig, Germany.
[Molina, Antonio] Univ Granada, Fac Ciencias, Dept Fis Aplicada, E-18071 Granada, Spain.
[Naletto, Giampiero] Univ Padua, Dept Informat Engn, I-35131 Padua, Italy.
[Perrin, Jean-Marie] Observ Haute Provence, OSU Pytheas, AMU, CNRS,UMS 2244, F-04870 St Michel lObservatoire, France.
[Sabau, Lola] Inst Nacl Tecn Aeroesp, Madrid 28850, Spain.
[Thomas, Nicolas] Univ Bern, Phys Inst, CH-3012 Bern, Switzerland.
[Weissman, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rotundi, A (reprint author), Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-0133 Rome, Italy.
EM rotundi@uniparthenope.it
RI Da Deppo, Vania/D-2897-2012; Lopez-Moreno, Jose Juan/C-7976-2011;
Herranz De La Revilla, Miguel Luis/L-5991-2014; Gutierrez,
Pedro/K-9637-2014; Lopez Jimenez, Antonio C./L-4738-2014; Naletto,
Giampiero/S-6329-2016; Green, Simon/C-7408-2009;
OI Da Deppo, Vania/0000-0001-6273-8738; Cremonese,
Gabriele/0000-0001-9021-1140; Lopez-Moreno, Jose
Juan/0000-0002-7946-2624; Herranz De La Revilla, Miguel
Luis/0000-0003-4343-6632; Gutierrez, Pedro/0000-0002-7332-6269; Lopez
Jimenez, Antonio C./0000-0002-6297-0681; Naletto,
Giampiero/0000-0003-2007-3138; Esposito, Francesca/0000-0001-9962-1648;
Ferrari, Marco/0000-0002-7447-6146; fulle, marco/0000-0001-8435-5287;
Snodgrass, Colin/0000-0001-9328-2905; Palomba,
Ernesto/0000-0002-9101-6774; Moreno, Fernando/0000-0003-0670-356X;
Rotundi, Alessandra/0000-0001-5467-157X; /0000-0002-2242-6147
FU GIADA; Spanish Ministry of Education and Science Ministerio de Educacion
y Ciencias (MEC); NASA through the U.S. Rosetta Project; Germany (DLR);
France (Centre National d'Etudes Spatiales); Italy (Italian Space
Agency); Spain (MEC); Sweden (Sweden National Science Board); ESA
Technical Directorate
FX GIADA was built by a consortium led by the Universita degli Studi di
Napoli "Parthenope" and INAF-Osservatorio Astronomico di Capodimonte, in
collaboration with the Instituto de Astrofisica de Andalucia, Selex-ES,
FI, and SENER. GIADA is presently managed and operated by Istituto di
Astrofisica e Planetologia Spaziali-INAF, Italy. GIADA was funded and
managed by the Agenzia Spaziale Italiana, with the support of the
Spanish Ministry of Education and Science Ministerio de Educacion y
Ciencias (MEC). GIADA was developed from a Principal Investigator
proposal from the University of Kent; science and technology
contributions were provided by CISAS, Italy; Laboratoire d'Astrophysique
Spatiale, France, and institutions from the UK, Italy, France, Germany,
and the USA. Science support was provided by NASA through the U.S.
Rosetta Project managed by the Jet Propulsion Laboratory/California
Institute of Technology. We would like to thank A. Coradini for her
contribution as a GIADA Co-Investigator. GIADA calibrated data will be
available through ESA's Planetary Science Archive (PSA) Web site
(www.rssd.esa.int/index.php?project=PSA&page=index). All data presented
here are available on request before archival in the PSA. OSIRIS was
built by a consortium led by the Max-Planck-Institut fur
Sonnensystemforschung, Katlenburg-Lindau, 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 (Centre National
d'Etudes Spatiales), Italy (Italian Space Agency), Spain (MEC), Sweden
(Sweden National Science Board), and the ESA Technical Directorate is
gratefully acknowledged. We thank the MIRO and ROSINA teams for sharing
their early results with us. We thank the Rosetta Science Ground Segment
at ESAC, the Rosetta Mission Operations Centre at ESOC (European Space
Operations Center), and the Rosetta Project at ESTEC (European Space
Technology Center) for their outstanding work enabling the science
return of the Rosetta Mission. We gratefully acknowledge the referees
for very constructive comments.
NR 25
TC 45
Z9 45
U1 2
U2 22
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 JAN 23
PY 2015
VL 347
IS 6220
AR aaa3905
DI 10.1126/science.aaa3905
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ4XZ
UT WOS:000348225800029
PM 25613898
ER
PT J
AU Andrews, RJ
Quintana, LM
AF Andrews, Russell J.
Quintana, Leonidas M.
TI Unpredictable, unpreventable and impersonal medicine: global disaster
response in the 21st century
SO EPMA JOURNAL
LA English
DT Review
DE Disaster response; Emergency response; Global health care; International
medicine; Medical evacuation; Mobile hospitals; Predictive preventive
personalized medicine; Trauma; Telemedicine
AB The United Nations has recognized the devastating consequences of "unpredictable, unpreventable and impersonal" disasters-at least US $2 trillion in economic damage and more than 1.3 million lives lost from natural disasters in the last two decades alone. In many disasters (both natural and man-made) hundreds-and in major earthquakes, thousands-of lives are lost in the first days following the event because of the lack of medical/surgical facilities to treat those with potentially survivable injuries. Disasters disrupt and destroy not only medical facilities in the disaster zone but also infrastructure (roads, airports, electricity) and potentially local healthcare personnel as well. To minimize morbidity and mortality from disasters, medical treatment must begin immediately, within minutes ideally, but certainly within 24 h (not the days to weeks currently seen in medical response to disasters). This requires that all resources-medical equipment and support, and healthcare personnel-be portable and readily available; transport to the disaster site will usually require helicopters, as military medical response teams in developed countries have demonstrated. Some of the resources available and in development for immediate medical response for disasters-from portable CT scanners to telesurgical capabilities-are described. For immediate deployment, these resources-medical equipment and personnel-must be ready for deployment on a moment's notice and not require administrative approvals or bureaucratic authorizations from numerous national and international agencies, as is presently the case. Following the "trauma center/stroke center" model, disaster response incorporating "disaster response centers" would be seamlessly integrated into the ongoing daily healthcare delivery systems worldwide, from medical education and specialty training (resident/registrar) to acute and subacute intensive care to long-term rehabilitation. The benefits of such a global disaster response network extend far beyond the lives saved: universal standards for medical education and healthcare delivery, as well as the global development of medical equipment and infrastructure, would follow. Capitalizing on the humanitarian nature of disaster response with its suspension of the cultural, socioeconomic and political barriers that often paralyze international cooperation and development-disaster response can be predictable, loss of life can be preventable and benefits can be both personal and societal.
C1 [Andrews, Russell J.] NASA, Ames Res Ctr, Nanotechnol & Smart Syst, Moffett Field, CA 94035 USA.
[Quintana, Leonidas M.] Univ Valparaiso, Med Ctr, Dept Neurosurg, Valparaiso, Chile.
RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Nanotechnol & Smart Syst, Moffett Field, CA 94035 USA.
EM rja@russelljandrews.org
NR 14
TC 2
Z9 2
U1 0
U2 11
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1878-5085
J9 EPMA J
JI EPMA J.
PD JAN 22
PY 2015
VL 6
AR UNSP 2
DI 10.1186/s13167-014-0024-9
PG 12
WC Medicine, General & Internal
SC General & Internal Medicine
GA CU6HB
UT WOS:000363631500002
PM 25663953
ER
PT J
AU Comer, J
Gumbart, JC
Henin, J
Lelievre, T
Pohorille, A
Chipot, C
AF Comer, Jeffrey
Gumbart, James C.
Henin, Jerome
Lelievre, Tony
Pohorille, Andrew
Chipot, Christophe
TI The Adaptive Biasing Force Method: Everything You Always Wanted To Know
but Were Afraid To Ask
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID FREE-ENERGY CALCULATIONS; MOLECULAR-DYNAMICS SIMULATIONS;
MONTE-CARLO-SIMULATION; COMPLEX-SYSTEMS; PERTURBATION CALCULATIONS;
COMPUTER-SIMULATIONS; BAYESIAN-INFERENCE; AVERAGE FORCE; MEAN FORCE;
THERMODYNAMIC INTEGRATION
AB In the host of numerical schemes devised to calculate free energy differences by way of geometric transformations, the adaptive biasing force algorithm has emerged as a promising route to map complex free-energy landscapes. It relies upon the simple concept that as a simulation progresses, a continuously updated biasing force is added to the equations of motion, such that in the long-time limit it yields a Hamiltonian devoid of an average force acting along the transition coordinate of interest. This means that sampling proceeds uniformly on a flat free-energy surface, thus providing reliable free-energy estimates. Much of the appeal of the algorithm to the practitioner is in its physically intuitive underlying ideas and the absence of any requirements for prior knowledge about free-energy landscapes. Since its inception in 2001, the adaptive biasing force scheme has been the subject of considerable attention, from in-depth mathematical analysis of convergence properties to novel developments and extensions. The method has also been successfully applied to many challenging problems in chemistry and biology. In this contribution, the method is presented in a comprehensive, self-contained fashion, discussing with a critical eye its properties, applicability, and inherent limitations, as well as introducing novel extensions. Through free-energy calculations of prototypical molecular systems, many methodological aspects are examined, from stratification strategies to overcoming the so-called hidden barriers in orthogonal space, relevant not only to the adaptive biasing force algorithm but also to other importance-sampling schemes. On the basis of the discussions in this paper, a number of good practices for improving the efficiency and reliability of the computed free-energy differences are proposed.
C1 [Comer, Jeffrey; Chipot, Christophe] Univ Lorraine, Lab Int Associe Ctr Natl Rech Sci & Univ Illinois, Unite Mixte Rech CNRS 7565, F-54506 Vandoeuvre Les Nancy, France.
[Gumbart, James C.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Gumbart, James C.] Georgia Inst Technol, Sch Chem, Atlanta, GA 30332 USA.
[Henin, Jerome] Inst Biol Physicochim, Lab Biochim Theor, F-75005 Paris, France.
[Lelievre, Tony] Ecole Ponts ParisTech, Ctr Enseignement & Rech Math & Calcul Sci, F-77455 Marne La Vallee 2, France.
[Pohorille, Andrew] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Pohorille, Andrew] Univ Calif San Francisco, San Francisco, CA 94143 USA.
[Chipot, Christophe] Univ Illinois, Beckman Inst Adv Sci & Technol, Theoret & Computat Biophys Grp, Urbana, IL 61801 USA.
[Chipot, Christophe] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Chipot, C (reprint author), Univ Lorraine, Lab Int Associe Ctr Natl Rech Sci & Univ Illinois, Unite Mixte Rech CNRS 7565, BP 70239, F-54506 Vandoeuvre Les Nancy, France.
EM chipot@ks.uiuc.edu
RI Lelievre, Tony/D-4420-2014; Henin, Jerome/A-7080-2008
OI Henin, Jerome/0000-0003-2540-4098
FU National Institutes of Health [K22-AI100927]; European Research Council;
NASA Exobiology Program; Direction Regionale a la Recherche et a la
Technologie de Lorraine; Fonds Europeen de Developpement Regional
FX J.C.G. gratefully acknowledges support from the National Institutes of
Health (K22-AI100927). T.L. gratefully acknowledges support of the
European Research Council. A.P. gratefully acknowledges support from the
NASA Exobiology Program. C.C. gratefully acknowledges support from the
Direction Regionale a la Recherche et a la Technologie de Lorraine and
the Fonds Europeen de Developpement Regional. The authors are indebted
to The Grand Equipement National de Calcul Informatique (GENCI) and to
the Centre Informatique National de l'Enseignement Superieur for
generous allocation of computer time.
NR 122
TC 32
Z9 32
U1 9
U2 58
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 JAN 22
PY 2015
VL 119
IS 3
SI SI
BP 1129
EP 1151
DI 10.1021/jp506633n
PG 23
WC Chemistry, Physical
SC Chemistry
GA CD8FA
UT WOS:000351329400046
PM 25247823
ER
PT J
AU Farr, WM
Gair, JR
Mandel, I
Cutler, C
AF Farr, Will M.
Gair, Jonathan R.
Mandel, Ilya
Cutler, Curt
TI Counting and confusion: Bayesian rate estimation with multiple
populations
SO PHYSICAL REVIEW D
LA English
DT Article
AB We show how to obtain a Bayesian estimate of the rates or numbers of signal and background events from a set of events when the shapes of the signal and background distributions are known, can be estimated, or approximated; our method works well even if the foreground and background event distributions overlap significantly and the nature of any individual event cannot be determined with any certainty. We give examples of determining the rates of gravitational-wave events in the presence of background triggers from a template bank when noise parameters are known and/or can be fit from the trigger data. We also give an example of determining globular-cluster shape, location, and density from an observation of a stellar field that contains a nonuniform background density of stars superimposed on the cluster stars.
C1 [Farr, Will M.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Dept Phys & Astron, Evanston, IL 60208 USA.
[Farr, Will M.; Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Gair, Jonathan R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cutler, Curt] CALTECH, Pasadena, CA 91125 USA.
RP Farr, WM (reprint author), Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA.
EM wfarr@star.sr.bham.ac.uk; jrg23@cam.ac.uk; imandel@star.sr.bham.ac.uk;
Curt.J.Cutler@jpl.nasa.gov
OI Mandel, Ilya/0000-0002-6134-8946
FU National Science Foundation under NSF Grant [PHY11-25915]; NSF
[PHY1068881]; Royal Society
FX We thank Kipp Cannon, Thomas Dent, Chad Hanna, Drew Keppel, Richard
O'Shaughnessy, David Hogg, and Ted von Hippel for discussions and
suggestions about this manuscript. I. M. and W. M. F. acknowledge the
hospitality of KITP, supported in part by the National Science
Foundation under NSF Grant No. PHY11-25915. C. C.'s work was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract to the National Aeronautics and Space Administration. C.
C. also gratefully acknowledges support from NSF Grant No. PHY1068881.
J. G.'s work is supported by the Royal Society.
NR 22
TC 7
Z9 7
U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 22
PY 2015
VL 91
IS 2
AR 023005
DI 10.1103/PhysRevD.91.023005
PG 14
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CA1CA
UT WOS:000348649400001
ER
PT J
AU Gerrits, T
Marsili, F
Verma, VB
Shalm, LK
Shaw, M
Mirin, RP
Nam, SW
AF Gerrits, T.
Marsili, F.
Verma, V. B.
Shalm, L. K.
Shaw, M.
Mirin, R. P.
Nam, S. W.
TI Spectral correlation measurements at the Hong-Ou-Mandel interference dip
SO PHYSICAL REVIEW A
LA English
DT Article
ID SINGLE-PHOTON DETECTORS; TELECOM WAVELENGTHS; CHIP; EFFICIENCY;
CIRCUITS; LIGHT
AB We present an efficient tool capable of measuring the spectral correlations between photons emerging from a Hong-Ou-Mandel interferometer. We show that for our spectrally factorizable spontaneous down-conversion source, the Hong-Ou-Mandel interference visibility decreases as the photons' frequency spread is increased to a maximum of 165 nm. Unfiltered, we obtained a visibility of 92.0% +/- 0.2%. The maximum visibility was 97% +/- 0.2% after applying filtering. We show that the tool can be useful for the study of spectral correlations that impair high-visibility and high-fidelity multisource interference applications. The nature of this tool also allows for arbitrary post-selective spectral filtering and high-rate multiphoton spectral correlation measurements.
C1 [Gerrits, T.; Verma, V. B.; Shalm, L. K.; Mirin, R. P.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
[Marsili, F.; Shaw, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gerrits, T (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA.
EM thomas.gerrits@nist.gov
OI Mirin, Richard/0000-0002-4472-4655
FU Quantum Information Science Initiative (QISI)
FX This work was supported by the Quantum Information Science Initiative
(QISI). T.G. thanks A. Fedrizzi, M.J. Stevens, A. White, and F. Wong for
discussions during the preparation of this manuscript. This work is a
contribution of NIST, an agency of the U.S. government, not subject to
copyright.
NR 31
TC 9
Z9 9
U1 1
U2 13
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 JAN 22
PY 2015
VL 91
IS 1
AR 013830
DI 10.1103/PhysRevA.91.013830
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA CA1BN
UT WOS:000348647800006
ER
PT J
AU D'Ammando, F
Orienti, M
Finke, J
Raiteri, CM
Hovatta, T
Larsson, J
Max-Moerbeck, W
Perkins, J
Readhead, ACS
Richards, JL
Beilicke, M
Benbow, W
Berger, K
Bird, R
Bugaev, V
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Dickinson, HJ
Eisch, JD
Errando, M
Falcone, A
Finley, JP
Fleischhack, H
Fortin, P
Fortson, L
Furniss, A
Gerard, L
Gillanders, GH
Griffiths, ST
Grube, J
Gyuk, G
Hakansson, N
Holder, J
Humensky, TB
Kar, P
Kertzman, M
Khassen, Y
Kieda, D
Krennrich, F
Kumar, S
Lang, MJ
Maier, G
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
de Bhroithe, AO
Ong, RA
Otte, AN
Pohl, M
Popkow, A
Prokoph, H
Pueschel, E
Quinn, J
Ragan, K
Reynolds, PT
Richards, GT
Roache, E
Rousselle, J
Santander, M
Sembroski, GH
Smith, AW
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
AF D'Ammando, F.
Orienti, M.
Finke, J.
Raiteri, C. M.
Hovatta, T.
Larsson, J.
Max-Moerbeck, W.
Perkins, J.
Readhead, A. C. S.
Richards, J. L.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Bugaev, V.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Dickinson, H. J.
Eisch, J. D.
Errando, M.
Falcone, A.
Finley, J. P.
Fleischhack, H.
Fortin, P.
Fortson, L.
Furniss, A.
Gerard, L.
Gillanders, G. H.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hakansson, N.
Holder, J.
Humensky, T. B.
Kar, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krennrich, F.
Kumar, S.
Lang, M. J.
Maier, G.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Pohl, M.
Popkow, A.
Prokoph, H.
Pueschel, E.
Quinn, J.
Ragan, K.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Rousselle, J.
Santander, M.
Sembroski, G. H.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
CA VERITAS Collaboration
TI The most powerful flaring activity from the NLSyl PMN J0948+0022
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active-galaxies: individual: PMN J0948+0022; galaxies: nuclei;
galaxies: Seyfert; gamma-rays: general
ID LINE SEYFERT 1; GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; QUASAR PKS
1510-089; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRUM RADIO QUASARS;
GALACTIC NUCLEI; X-RAY; MULTIWAVELENGTH OBSERVATIONS; RELATIVISTIC JETS
AB We report on multifrequency observations performed during 2012 December-2013 August of the first narrow-line Seyfert 1 galaxy detected in gamma-rays, PMN J0948+0022 (z = 0.5846). A y -ray flare was observed by the Large Area Telescope on board Fermi during 2012 December-2013 January, reaching a daily peak flux in the 0.1-100 GeV energy range of (155 31) x 10 8 ph cm(-2) S-1 on 2013 January 1, corresponding to an apparent isotropic luminosity of similar to 1.5 x 1048 erg s(-1). The y -ray flaring period triggered Swift and Very Energetic Radiation Imaging Telescope Array System (VERITAS) observations in addition to radio and optical monitoring by Owens Valley Radio Observatory, Monitoring Of Jets in Active galactic nuclei with VLBA Experiments, and Catalina Real-time Transient Survey. A strong flare was observed in optical, UV, and X-rays on 2012 December 30, quasi-simultaneously to the y -ray flare, reaching a record flux for this source from optical to y gamma-rays. VERITAS observations at very high energy (E > 100 GeV) during 2013 January 6-17 resulted in an upper limit of F>0.2 Trev < 4.0 x 10(-12) ph cm(-2) s(-1). We compared the spectral energy distribution (SED) of the flaring state in 2013 January with that of an intermediate state observed in 2011. The two SEDs, modelled as synchrotron emission and an external Compton scattering of seed photons from a dust torus, can be modelled by changing both the electron distribution parameters and the magnetic field.
C1 [D'Ammando, F.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[D'Ammando, F.] Inaf Ist Radioastron, I-40129 Bologna, Italy.
[Finke, J.] US Naval Res Lab, Washington, DC 20375 USA.
[Raiteri, C. M.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy.
[Hovatta, T.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Larsson, J.] KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, J.] KTH, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Max-Moerbeck, W.] Natl Radio Astron Observ NRAO, Socorro, NM 87801 USA.
[Perkins, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richards, J. L.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Beilicke, M.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Gerard, L.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Griffiths, S. T.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 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.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP D'Ammando, F (reprint author), Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
EM dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it;
dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it;
dammando@ira.inaf.it
RI Nieto, Daniel/J-7250-2015
OI Nieto, Daniel/0000-0003-3343-0755
FU US Department of Energy Office of Science; Smithsonian Institution;
NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748];
Science and Technology Facilities Council in the UK; NASA [NNX08AW31G,
NNX11A043G]; NSF [AST-0808050, AST-1109911]; US National Science
Foundation [AST-0909182]; Fermi Guest Investigator grants [NNX08AW56G,
NNX09AU10G, NNX12AO93G]
FX 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. The work of the VERITAS Collaboration 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 the Science and Technology Facilities Council 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.; We thank the Swift
team for making these observations possible, the duty scientists, and
science planners. The OVRO 40 m monitoring programme is supported in
part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants
AST-0808050 and AST-1109911. The CRTS survey is supported by the US
National Science Foundation under grants AST-0909182. This research has
made use of data from the MOJAVE data base that is maintained by the
MOJAVE team (Lister et al. 2009). Data from the Steward Observatory
spectropolarimetric monitoring project were used. This programme is
supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and
NNX12AO93G. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. We thank F. Schinzel, S. Digel, P. Bruel,
and the referee, Anthony M. Brown, for useful comments and suggestions.
NR 88
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U1 1
U2 11
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2015
VL 446
IS 3
BP 2456
EP 2467
DI 10.1093/mnras/stu2251
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TG
UT WOS:000350272300020
ER
PT J
AU Sbarrato, T
Ghisellini, G
Tagliaferri, G
Foschini, L
Nardini, M
Tavecchio, F
Gehrels, N
AF Sbarrato, T.
Ghisellini, G.
Tagliaferri, G.
Foschini, L.
Nardini, M.
Tavecchio, F.
Gehrels, N.
TI Blazar candidates beyond redshift 4 observed by Swift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: thermal; galaxies: active; quasars: general
X-rays: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; BLACK-HOLE; LUMINOSITY
FUNCTION; RX J1028.6-0844; DATA RELEASE; RAY SOURCES; TELESCOPE;
Q0906+6930; EVOLUTION
AB We have selected SDSS J222032.50+002537.5 and SDSS J142048.01+120545.9 as best blazar candidates out of a complete sample of extremely radio-loud quasars at z > 4, with highly massive black holes. We observed them and a third serendipitous candidate with similar features (PMN J2134-0419) in the X-rays with the Swift/XRT telescope, to confirm their blazar nature. We observed strong and hard X-ray fluxes (i.e. alpha(X) less than or similar to 0.6, where F(v) beta nu(-alpha X) in the 0.3-10 keV observed energy range, similar to 1-40 keV rest frame) in all three cases. This allowed us to classify our candidates as real blazars, being characterized by large Lorentz factors (similar to 13) and very small viewing angles (similar to 3 degrees). All three sources have black hole masses exceeding 10(9)M circle dot and their classification provides intriguing constraints on supermassive black hole formation and evolution models. We confirm our earlier suggestion that there are different formation epochs of extremely massive black holes hosted in jetted (z 4) and non-jetted systems (z similar to 2.5).
C1 [Sbarrato, T.] Univ Insubria, Dipartimento Sci & Alta Tecnol, I-22100 Como, Italy.
[Sbarrato, T.; Ghisellini, G.; Tagliaferri, G.; Foschini, L.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Nardini, M.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy.
[Gehrels, N.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Sbarrato, T (reprint author), Univ Insubria, Dipartimento Sci & Alta Tecnol, Via Valleggio 11, I-22100 Como, Italy.
EM tullia.sbarrato@brera.inaf.it
OI Ghisellini, Gabriele/0000-0002-0037-1974; Sbarrato,
Tullia/0000-0002-3069-9399; Foschini, Luigi/0000-0001-8678-0324
FU National Aeronautics and Space Administration
FX We thank the anonymous referee for useful comments. This research made
use of the NASA/IPAC Extragalactic Database (NED) and of the data
products from the Wide-field Infrared Survey Explorer, which are
operated by the Jet Propulsion Laboratory, Caltech, funded by the
National Aeronautics and Space Administration. Part of this work is
based on archival data, software and online services provided by the ASI
Science Data Center (ASDC). We made also use of data supplied by the UK
Swift Science Data Centre at the University of Leicester.
NR 36
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U1 1
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2015
VL 446
IS 3
BP 2483
EP 2489
DI 10.1093/mnras/stu2269
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TG
UT WOS:000350272300022
ER
PT J
AU Naslim, N
Kemper, F
Madden, SC
Hony, S
Chu, YH
Galliano, F
Bot, C
Yang, Y
Seok, J
Oliveira, JM
van Loon, JT
Meixner, M
Li, A
Hughes, A
Gordon, KD
Otsuka, M
Hirashita, H
Morata, O
Lebouteiller, V
Indebetouw, R
Srinivasan, S
Bernard, JP
Reach, WT
AF Naslim, N.
Kemper, F.
Madden, S. C.
Hony, S.
Chu, Y. -H.
Galliano, F.
Bot, C.
Yang, Y.
Seok, J.
Oliveira, J. M.
van Loon, J. Th
Meixner, M.
Li, A.
Hughes, A.
Gordon, K. D.
Otsuka, M.
Hirashita, H.
Morata, O.
Lebouteiller, V.
Indebetouw, R.
Srinivasan, S.
Bernard, J. -P.
Reach, W. T.
TI Molecular hydrogen emission in the interstellar medium of the Large
Magellanic Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: molecules; photodissociation region (PDR); galaxies: ISM;
Magellanic Cloud; infrared: ISM
ID INFRARED SPECTRAL ATLAS; FINE-STRUCTURE LINES; GALAXY EVOLUTION;
PHOTODISSOCIATION REGIONS; HERSCHEL INVENTORY; COMPACT SOURCES;
STAR-FORMATION; H-2 EMISSION; C-II; SPITZER
AB We present the detection and analysis of molecular hydrogen emission towards ten interstellar regions in the Large Magellanic Cloud. We examined low-resolution infrared spectral maps of 12 regions obtained with the Spitzer infrared spectrograph (IRS). The pure rotational 0-0 transitions of H-2 at 28.2 and 17.1 mu m are detected in the IRS spectra for 10 regions. The higher level transitions are mostly upper limit measurements except for three regions, where a 3 sigma detection threshold is achieved for lines at 12.2 and 8.6 p.m. The excitation diagrams of the detected IF transitions are used to determine the warm H-2 gas column density and temperature. The single-temperature fits through the lower transition lines give temperatures in the range 86-137 K. The bulk of the excited H-7 gas is found at these temperatures and contributes similar to 5-17 per cent to the total gas mass. We find a tight correlation of the H-2 surface brightness with polycyclic aromatic hydrocarbon and total infrared emission, which is a clear indication of photoelectric heating in photodissociation regions. We find the excitation of H-2 by this process is equally efficient in both atomic- and molecular-dominated regions. We also present the correlation of the warm H-2 physical conditions with dust properties. The warm H-2 mass fraction and excitation temperature show positive correlations with the average starlight intensity, again supporting H, excitation in photodissociation regions.
C1 [Naslim, N.; Kemper, F.; Chu, Y. -H.; Yang, Y.; Seok, J.; Otsuka, M.; Hirashita, H.; Morata, O.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Madden, S. C.; Galliano, F.; Indebetouw, R.] CEA Saclay, Lab AIM, CEA, DSM, F-91191 Gif Sur Yvette, France.
[Hony, S.; Hughes, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bot, C.] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France.
[Oliveira, J. M.; van Loon, J. Th] Keele Univ, Leonard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Meixner, M.; Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Bernard, J. -P.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Reach, W. T.] NASA, USRA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Naslim, N (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
EM naslimn@asiaa.sinica.edu.tw
RI Kemper, Francisca/D-8688-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Bot,
Caroline/0000-0001-6118-2985; Yang, Yao-Lun/0000-0001-8227-2816;
Lebouteiller, Vianney/0000-0002-7716-6223; Reach,
William/0000-0001-8362-4094
FU Taiwan's Ministry of Science and Technology (MoST)
[NSC100-2112-M-001-023-MY3, MoST 103-2112-M-001-033]
FX FK acknowledges funding from Taiwan's Ministry of Science and Technology
(MoST) under grants NSC100-2112-M-001-023-MY3 and MoST
103-2112-M-001-033. We thank the referee for fruitful comments.
NR 45
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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 JAN 21
PY 2015
VL 446
IS 3
BP 2490
EP 2504
DI 10.1093/mnras/stu2276
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TG
UT WOS:000350272300023
ER
PT J
AU Fumagalli, M
O'Meara, JM
Prochaska, JX
Rafelski, M
Kanekar, N
AF Fumagalli, Michele
O'Meara, John M.
Prochaska, J. Xavier
Rafelski, Marc
Kanekar, Nissim
TI Directly imaging damped Ly alpha galaxies at z > 2-III. The star
formation rates of neutral gas reservoirs at z similar to 2.7
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: atoms; galaxies: evolution; galaxies:
high-redshift; quasars: absorption lines; ultraviolet: galaxies
ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; MASS-METALLICITY RELATION;
MAGELLAN UNIFORM SURVEY; II-ASTERISK ABSORPTION; FORMATION RATE DENSITY;
DARK-MATTER UNIVERSE; FORMING GALAXIES; MOLECULAR GAS; DEEP FIELD
AB We present results from a survey designed to probe the star formation properties of 32 damped Lyman a systems (DLAs) at z similar to 2.7. By using the ` double-DLA' technique that eliminates the glare of the bright background quasars, we directly measure the rest-frame far-ultraviolet flux from DLAs and their neighbouring galaxies. At the position of the absorbing gas, we place stringent constraints on the unobscured star formation rates (SFRs) of DLAs to 2s limits of.. < 0.09-0.27M(circle dot) yr(-1), corresponding to SFR surface densities Sigma(sfr) < 10(-2.6)-10(-1.)5M(circle dot) yr(-1) kpc(-2). The implications of these limits for the star formation law, metal enrichment, and cooling rates of DLAs are examined. By studying the distribution of impact parameters as a function of SFRs for all the galaxies detected around these DLAs, we place new direct constraints on the bright end of the UV luminosity function of DLA hosts. We find that <= 13 per cent of the hosts have psi >= 2M(circle dot) yr(-1) at impact parameters b(dla) <= (psi/M-circle dot yr(-1))(0.8) + 6 kpc, differently from current samples of confirmed DLA galaxies. Our observations also disfavour a scenario in which the majority of DLAs arise from bright Lyman-break galaxies at distances 20 <= b(dla) < 100 kpc. These new findings corroborate a picture in which DLAs do not originate from highly star-forming systems that are coincident with the absorbers, and instead suggest that DLAs are associated with faint, possibly isolated, star-forming galaxies. Potential shortcomings of this scenario and future strategies for further investigation are discussed.
C1 [Fumagalli, Michele] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Fumagalli, Michele] Carnegie Observ, Pasadena, CA 91101 USA.
[O'Meara, John M.] St Michaels Coll, Dept Chem & Phys, Colchester 05439, Essex, England.
[Prochaska, J. Xavier] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Prochaska, J. Xavier] Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Rafelski, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kanekar, Nissim] Natl Ctr Radio Astrophys, TIFR, Pune 411007, Maharashtra, India.
RP Fumagalli, M (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, S Rd, Durham DH1 3LE, England.
EM michele.fumagalli@durham.ac.uk
RI Fumagalli, Michele/K-9510-2015
OI Fumagalli, Michele/0000-0001-6676-3842
FU Science and Technology Facilities Council [ST/L00075X/1]; NSF-AST
[1109447, 1109452]; Department of Science and Technology through
Ramanujan Fellowship; NASA from Space Telescope Science Institute
[11595, HST-GO-11595.001-A]; NASA [NAS5-26555, HST-GO-10878.05-A]
FX We thank J. Hennawi, M. Neeleman, and M. Rauch for useful comments and
suggestions on this work. We also thank J. Fynbo for providing a copy of
the code to compute the models presented in Fynbo et al. (2008). We
fondly remember discussions on the early stages of this work with Art
Wolfe. MF acknowledges support by the Science and Technology Facilities
Council [grant number ST/L00075X/1]. JXP acknowledges support from
NSF-AST 1109447 and 1109452 awards. MR acknowledges support from an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center. NK acknowledges support from the Department of Science and
Technology through a Ramanujan Fellowship. Support for Programme number
11595 was provided by NASA through a grant (HST-GO-11595.001-A) from the
Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Incorporated, under NASA
contract NAS5-26555. This work has been partially supported by NASA
grant HST-GO-10878.05-A. For access to the data used in this paper,
please contact the authors.
NR 138
TC 21
Z9 21
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 JAN 21
PY 2015
VL 446
IS 3
BP 3178
EP 3198
DI 10.1093/mnras/stu2325
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TG
UT WOS:000350272300077
ER
PT J
AU Meador, MAB
Aleman, CR
Hanson, K
Ramirez, N
Vivod, SL
Wilmoth, N
McCorkle, L
AF Meador, Mary Ann B.
Aleman, Christian R.
Hanson, Katrina
Ramirez, Nakaira
Vivod, Stephanie L.
Wilmoth, Nathan
McCorkle, Linda
TI Polyimide Aerogels with Amide Cross-Links: A Low Cost Alternative for
Mechanically Strong Polymer Aerogels
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE aerogel; polyimide; polyamide; mesoporous; cross-linked
ID NANOPOROUS POLYIMIDES
AB Polyimide aerogels combine high porosity, low thermal conductivity, flexibility, and low density with excellent mechanical properties. However, previously used cross-linkers, such as 1,3,5-triaminophenoxybenzene (TAB), 2,4,6-tris(4-aminophenyl)pyridine (TAPP), or octa(aminophenoxy)silsesquioxane (OAPS), either are not commercially available or are prohibitively expensive. Finding more cost efficient cross-linkers that are commercially available to synthesize these aerogels is crucial for making large scale manufacturing attractive. Herein, we describe an approach to making polyimide aerogels starting with amine capped oligomers that are cross-linked with 1,3,5-benzenetricarbonyl trichloride (BTC). BTC is a lower cost, commercially available alternative to TAB, TAPP, or OAPS. Aerogels made in this way have the same or higher modulus and higher surface area compared to those previously reported with either TAB or OAPS cross-links at the same density. While the cross-link structure is an amide, the thermal stability is not compromised most likely because the cross-link is only a small part of the composition of the aerogel. Onset of decomposition depends primarily on the backbone chemistry with 4,4'-oxidianiline (ODA) being more thermally stable than 2,2'-dimethylbenzidine (DMBZ), similar to those previously reported with other cross-links.
C1 [Meador, Mary Ann B.; Aleman, Christian R.; Hanson, Katrina; Ramirez, Nakaira; Vivod, Stephanie L.; Wilmoth, Nathan; McCorkle, Linda] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Meador, MAB (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
FU NASA Game Changing Development Program under Space Technology Mission
Directorate
FX We thank the NASA Game Changing Development Program under the Space
Technology Mission Directorate for funding this work. We also thank Dan
Scheiman (Ohio Aerospace Institute) for thermal analysis and pycnometry
measurements, Baochau Nguyen (Ohio Aerospace Institute) for solid NMR,
and Haiquan Guo (Ohio Aerospace Institute) for nitrogen sorption
measurements.
NR 20
TC 18
Z9 20
U1 30
U2 144
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 JAN 21
PY 2015
VL 7
IS 2
BP 1240
EP 1249
DI 10.1021/am507268c
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA AZ6MB
UT WOS:000348332700025
PM 25564878
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CA LIGO Sci Collaboration
Virgo Collaboration
TI Narrow-band search of continuous gravitational-wave signals from Crab
and Vela pulsars in Virgo VSR4 data
SO PHYSICAL REVIEW D
LA English
DT Article
ID SPIN-DOWN LIMIT; WIND TORI; EMISSION; STARS
AB In this paper we present the results of a coherent narrow-band search for continuous gravitational-wave signals from the Crab and Vela pulsars conducted on Virgo VSR4 data. In order to take into account a possible small mismatch between the gravitational-wave frequency and two times the star rotation frequency, inferred from measurement of the electromagnetic pulse rate, a range of 0.02 Hz around two times the star rotational frequency has been searched for both the pulsars. No evidence for a signal has been found and 95% confidence level upper limits have been computed assuming both that polarization parameters are completely unknown and that they are known with some uncertainty, as derived from x-ray observations of the pulsar wind torii. For Vela the upper limits are comparable to the spin-down limit, computed assuming that all the observed spin-down is due to the emission of gravitational waves. For Crab the upper limits are about a factor of 2 below the spin-down limit, and represent a significant improvement with respect to past analysis. This is the first time the spin-down limit is significantly overcome in a narrow-band search.
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[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Miller, A.; Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil.
[Nayak, R. K.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Ogin, G. H.] Whitman Coll, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[O'Shaughnessy, R.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Schnabel, R.] Univ Hamburg, D-22761 Hamburg, Germany.
[Sengupta, A. S.] Indian Inst Technol, Gandhinagar Ahmedabad 382424, Gujarat, India.
[Sengupta, A. S.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Ward, Robert/I-8032-2014; Howell, Eric/H-5072-2014; Costa,
Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016;
Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora
Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms,
Jan/J-4359-2012; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016;
Kumar, Prem/B-6691-2009; De Laurentis, Martina/L-3022-2016; Lazzaro,
Claudia/L-2986-2016; Pinto, Innocenzo/L-3520-2016; Ferrante,
Isidoro/F-1017-2012; Losurdo, Giovanni/K-1241-2014; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Martelli, Filippo/P-4041-2015; Branchesi,
Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao,
Haixing/O-1300-2013; Gammaitoni, Luca/B-5375-2009; Prokhorov,
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Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell,
Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri,
Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Steinlechner,
Sebastian/D-5781-2013; Shaddock, Daniel/A-7534-2011; Vicere,
Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Danilishin,
Stefan/K-7262-2012; Sigg, Daniel/I-4308-2015; Gorodetsky,
Michael/C-5938-2008; Gemme, Gianluca/C-7233-2008; McClelland,
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Xingjiang/0000-0001-7049-6468; Puppo, Paola/0000-0003-4677-5015; Tacca,
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prodi, giovanni/0000-0001-5256-915X; Papa,
M.Alessandra/0000-0002-1007-5298; Pinto, Innocenzo
M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Swinkels,
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Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Bondu,
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Gareth/0000-0002-4289-3439; Ricci, Fulvio/0000-0001-5475-4447; Vocca,
Helios/0000-0002-1200-3917; Scott, Jamie/0000-0001-6701-6515; Murphy,
David/0000-0002-8538-815X
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck Society; State of
Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare;
French Centre National de la Recherche Scientifique; Australian Research
Council; International Science Linkages program of the Commonwealth of
Australia; Council of Scientific and Industrial Research of India;
Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de
Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of
the Govern de les Illes Balears; Foundation for Fundamental Research;
Netherlands Organisation for Scientific Research; Polish Ministry of
Science and Higher Education; FOCUS Programme of Foundation for Polish
Science; Royal Society; Scottish Funding Council; Scottish Universities
Physics Alliance; National Aeronautics and Space Administration; OTKA of
Hungary; Lyon Institute of Origins (LIO); National Research Foundation
of Korea, Industry Canada; Province of Ontario through the Ministry of
Economic Development and Innovation; Natural Sciences and Engineering
Research Council of Canada; Carnegie Trust; Leverhulme Trust; David and
Lucile Packard Foundation; Research Corporation; Alfred P. Sloan
Foundation
FX The authors thank the anonymous referee for the careful reading of the
manuscript. They also gratefully acknowledge the support of the United
States National Science Foundation for the construction and operation of
the LIGO Laboratory, the Science and Technology Facilities Council of
the United Kingdom, the Max-Planck Society, and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organisation for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the Royal Society, the Scottish Funding
Council, the Scottish Universities Physics Alliance, The National
Aeronautics and Space Administration, OTKA of Hungary, the Lyon
Institute of Origins (LIO), the National Research Foundation of Korea,
Industry Canada and the Province of Ontario through the Ministry of
Economic Development and Innovation, the Natural Sciences and
Engineering Research Council of Canada, the Carnegie Trust, the
Leverhulme Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P. Sloan Foundation.
NR 21
TC 10
Z9 10
U1 4
U2 54
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 21
PY 2015
VL 91
IS 2
AR 022004
DI 10.1103/PhysRevD.91.022004
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CA2JF
UT WOS:000348734000002
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Atwood, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Favuzzi, C
Ferrara, EC
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Godfrey, G
Gomez-Vargas, GA
Grenier, IA
Guiriec, S
Gustafsson, M
Hadasch, D
Hayashi, K
Hays, E
Hewitt, JW
Ippoliti, P
Jogler, T
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Kataoka, J
Knodlseder, J
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Manfreda, A
Massaro, F
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohsugi, T
Omodei, N
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Romani, RW
Sanchez-Conde, M
Schaal, M
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Suson, DJ
Takahashi, H
Thayer, JG
Thayer, JB
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vianello, G
Werner, M
Winer, BL
Wood, KS
Wood, M
Zaharijas, G
Zimmer, S
AF Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Godfrey, G.
Gomez-Vargas, G. A.
Grenier, I. A.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hayashi, K.
Hays, E.
Hewitt, J. W.
Ippoliti, P.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Manfreda, A.
Massaro, F.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Ritz, S.
Romani, R. W.
Sanchez-Conde, M.
Schaal, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Suson, D. J.
Takahashi, H.
Thayer, J. G.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vianello, G.
Werner, M.
Winer, B. L.
Wood, K. S.
Wood, M.
Zaharijas, G.
Zimmer, S.
TI THE SPECTRUM OF ISOTROPIC DIFFUSE GAMMA-RAY EMISSION BETWEEN 100 MeV AND
820 GeV
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE diffuse radiation; gamma rays: diffuse background
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES;
FERMI-LAT; X-RAY; BACKGROUND-RADIATION; DARK-MATTER; EGRET DATA;
MILKY-WAY; CATALOG
AB The gamma-ray sky can be decomposed into individually detected sources, diffuse emission attributed to the interactions of Galactic cosmic rays with gas and radiation fields, and a residual all-sky emission component commonly called the isotropic diffuse gamma-ray background (IGRB). The IGRB comprises all extragalactic emissions too faint or too diffuse to be resolved in a given survey, as well as any residual Galactic foregrounds that are approximately isotropic. The first IGRB measurement with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi) used 10 months of sky-survey data and considered an energy range between 200 MeV and 100 GeV. Improvements in event selection and characterization of cosmic-ray backgrounds, better understanding of the diffuse Galactic emission (DGE), and a longer data accumulation of 50 months allow for a refinement and extension of the IGRB measurement with the LAT, now covering the energy range from 100 MeV to 820 GeV. The IGRB spectrum shows a significant high-energy cutoff feature and can be well described over nearly four decades in energy by a power law with exponential cutoff having a spectral index of 2.32 +/- 0.02 and a break energy of (279 +/- 52) GeV using our baseline DGE model. The total intensity attributed to the IGRB is (7.2 +/- 0.6) x 10(-6) cm(-2) s(-1) sr(-1) above 100 MeV, with an additional +15%/-30% systematic uncertainty due to the Galactic diffuse foregrounds.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, I-56127 Pisa, Italy.
[Ballet, J.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bechtol, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Bissaldi, E.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Bissaldi, E.; Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Hays, E.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, Lab Universe & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier, France.
[Bruel, P.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Conrad, J.; Larsson, S.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Cuoco, A.; Larsson, S.; Li, L.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Cuoco, A.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[D'Ammando, F.; Giroletti, M.; Ippoliti, P.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy.
[Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gomez-Vargas, G. A.; Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Gomez-Vargas, G. A.] Pontificia Univ Catolica Chile, Dept Fis, Santiago, Chile.
[Gustafsson, M.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Hayashi, K.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Hewitt, J. W.; Nemmen, R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Nemmen, R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Moiseev, A. A.; Nemmen, R.] CRESST, Greenbelt, MD 20771 USA.
[Hewitt, J. W.; Moiseev, A. A.; Nemmen, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, F-31400 Toulouse, France.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, E-08193 Barcelona, Spain.
[Li, L.] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Lott, B.; Reposeur, T.] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France.
[Massaro, F.] Yale Univ, Dept Phys, Dept Astron, New Haven, CT 06520 USA.
[Massaro, F.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, E-08028 Barcelona, Spain.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Zaharijas, G.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM markus.ackermann@desy.de; bechtol@kicp.uchicago.edu
RI Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando,
E/R-5594-2016; Gomez-Vargas, German/C-7138-2015; Moskalenko,
Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi,
Elisabetta/K-7911-2016; Nemmen, Rodrigo/O-6841-2014; Morselli,
Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015;
Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015;
Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto,
nicola/I-8951-2012
OI Gasparrini, Dario/0000-0002-5064-9495; Baldini,
Luca/0000-0002-9785-7726; Ajello, Marco/0000-0002-6584-1703; Massaro,
Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065;
giommi, paolo/0000-0002-2265-5003; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
Zaharijas, Gabrijela/0000-0001-8484-7791; SPINELLI,
Paolo/0000-0001-6688-8864; Giroletti, Marcello/0000-0002-8657-8852;
Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Moskalenko, Igor/0000-0001-6141-458X;
Bissaldi, Elisabetta/0000-0001-9935-8106; Morselli,
Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Funk,
Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036;
Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario
/0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto,
nicola/0000-0002-9021-2888
FU NASA [NNX09AC15G]
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT, as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States; the
Commissariat a l'EnergieAtomique 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. GALPROP
development is partially funded via NASA grant NNX09AC15G. Some of the
results in this paper have been derived using the HEALPix (Gorski et al.
2005) package.
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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 JAN 20
PY 2015
VL 799
IS 1
AR 86
DI 10.1088/0004-637X/799/1/86
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500084
ER
PT J
AU Aliu, E
Archer, A
Aune, T
Barnacka, A
Behera, B
Beilicke, M
Benbow, W
Berger, K
Bird, R
Buckley, JH
Bugaev, V
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Fortin, P
Fortson, L
Furniss, A
Galante, N
Gillanders, GH
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Hakansson, N
Hanna, D
Holder, J
Hughes, G
Humensky, TB
Johnson, CA
Kaaret, P
Kar, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Kumar, S
Lang, MJ
Madhavan, A
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Nieto, D
de Bhroithe, AO
Ong, RA
Orr, M
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
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Weinstein, A
Welsing, R
Wilhelm, A
Williams, DA
Zitzer, B
AF Aliu, E.
Archer, A.
Aune, T.
Barnacka, A.
Behera, B.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Fortin, P.
Fortson, L.
Furniss, A.
Galante, N.
Gillanders, G. H.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hakansson, N.
Hanna, D.
Holder, J.
Hughes, G.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Kumar, S.
Lang, M. J.
Madhavan, A.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
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.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Weinstein, A.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
TI VERITAS OBSERVATIONS OF THE BL LAC OBJECT PG 1553+113
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general
ID EXTRAGALACTIC BACKGROUND LIGHT; LACERTAE OBJECTS; GAMMA-RAYS; OPTICAL
SPECTROSCOPY; BLAZARS; TELESCOPE; RADIATION; SPECTRA; PG-1553+113; MODEL
AB We present results from VERITAS observations of the BL Lac object PG 1553+113 spanning the years 2010, 2011, and 2012. The time-averaged spectrum, measured between 160 and 560 GeV, is well described by a power law with a spectral index of 4.33 +/- 0.09. The time-averaged integral flux above 200 GeV measured for this period was (1.69 +/- 0.06) x 10(-11) photons cm(-2) s(-1), corresponding to 6.9% of the Crab Nebula flux. We also present the combined gamma-ray spectrum from the Fermi Large Area Telescope and VERITAS covering an energy range from 100 MeV to 560 GeV. The data are well fit by a power law with an exponential cutoff at 101.9 +/- 3.2 GeV. The origin of the cutoff could be intrinsic to PG 1553+113 or be due to the gamma-ray opacity of our universe through pair production off the extragalactic background light (EBL). Given lower limits to the redshift of z > 0.395 based on optical/UV observations of PG 1553+113, the cutoff would be dominated by EBL absorption. Conversely, the small statistical uncertainties of the VERITAS energy spectrum have allowed us to provide a robust upper limit on the redshift of PG 1553+113 of z <= 0.62. A strongly elevated mean flux of (2.50 +/- 0.14) x10(-11) photons cm(-2) s(-1) (10.3% of the Crab Nebula flux) was observed during 2012, with the daily flux reaching as high as (4.44 +/- 0.71) x10(-11) photons cm(-2) s(-1) (18.3% of the Crab Nebula flux) on MJD 56048. The light curve measured during the 2012 observing season is marginally inconsistent with a steady flux, giving a chi(2) probability for a steady flux of 0.03%.
C1 [Aliu, E.; Errando, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Behera, B.; Chen, X.; Federici, S.; Hughes, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany.
[Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Madhavan, A.; Orr, M.; Weinstein, A.] 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 Potsdam, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Univ Coll Galway, Sch Phys, 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.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755;
Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772; Bird,
Ralph/0000-0002-4596-8563
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the U.K.
FX 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. This research is supported by grants
from the U.S. Department of Energy Office of Science, the U.S. National
Science Foundation and the Smithsonian Institution, by NSERC in Canada,
by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the
U.K. 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.
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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 JAN 20
PY 2015
VL 799
IS 1
AR 7
DI 10.1088/0004-637X/799/1/7
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500007
ER
PT J
AU Barriere, NM
Tomsick, JA
Wik, DR
Chaty, S
Rodriguez, J
AF Barriere, Nicolas M.
Tomsick, John A.
Wik, Daniel R.
Chaty, Sylvain
Rodriguez, Jerome
TI SOURCE IDENTIFICATION IN THE IGR J17448-3232 FIELD: DISCOVERY OF THE
SCORPIUS GALAXY CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; galaxies: active; galaxies: clusters: individual
(CXOU J174453.4-323254); X-rays: individual (CXOU J174437.3-323222, IGR
J17448-3232)
ID PHOTON IMAGING CAMERA; RAY SURVEY CATALOG; XMM-NEWTON;
INTERSTELLAR-MEDIUM; INTRINSIC COLORS; GALACTIC-CENTER; X-RAYS; SAMPLE;
EXTINCTION; EMISSION
AB We use a 43 ks XMM-Newton observation to investigate the nature of sources first distinguished by a follow-up Chandra observation of the field surrounding INTEGRAL source IGR J17448-3232, which includes extended emission and a bright point source previously classified as a blazar. We establish that the extended emission is a heretofore unknown massive galaxy cluster hidden behind the Galactic bulge. The emission-weighted temperature of the cluster within the field of view is 8.8 keV, with parts of the cluster reaching temperatures of up to 12 keV; no cool core is evident. At a redshift of 0.055, the cluster is somewhat under-luminous relative to the X-ray luminosity-temperature relation, which may be attributable to its dynamical state. We present a preliminary analysis of its properties in this paper. We also confirm that the bright point source is a blazar, and we propose that it is either a flat spectrum radio quasar or a low-frequency peaked BL Lac object. We find four other fainter sources in the field, which we study and tentatively identify. Only one, which we propose is a foreground Galactic X-ray binary, is hard enough to contribute to IGR J17448-3232, but it is too faint to be significant. We thus determine that IGR J17448-3232 is in fact the galaxy cluster up to approximate to 45 keV and the blazar beyond.
C1 [Barriere, Nicolas M.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Wik, Daniel R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Chaty, Sylvain; Rodriguez, Jerome] Univ Paris Diderot, Irfu Serv Astrophys, Ctr Saclay, CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France.
RP Barriere, NM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
FU NASA through Astrophysics Data Analysis Program (ADAP) [NNX12AE71G]
FX Partial support for this work was provided by NASA through Astrophysics
Data Analysis Program (ADAP) grant NNX12AE71G. The authors are grateful
to Marco Ajello and Roman Krivonos for useful discussions.
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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 JAN 20
PY 2015
VL 799
IS 1
AR 24
DI 10.1088/0004-637X/799/1/24
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500023
ER
PT J
AU Cook, AM
Ricca, A
Mattioda, AL
Bouwman, J
Roser, J
Linnartz, H
Bregman, J
Allamandola, LJ
AF Cook, Amanda M.
Ricca, Alessandra
Mattioda, Andrew L.
Bouwman, Jordy
Roser, Joseph
Linnartz, Harold
Bregman, Jonathan
Allamandola, Louis J.
TI PHOTOCHEMISTRY OF POLYCYCLIC AROMATIC HYDROCARBONS IN COSMIC WATER ICE:
THE ROLE OF PAH IONIZATION AND CONCENTRATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; molecular
data; molecular processes
ID TELESCOPE PRIMOS SURVEY; ETHYL METHYL-ETHER; SAGITTARIUS B2(N);
INTERSTELLAR GLYCINE; RIGOROUS ATTEMPT; 3 MM; W51; GLYCOLALDEHYDE; CORES
AB Infrared spectroscopic studies of ultraviolet (UV) irradiated, water-rich, cosmic ice analogs containing small polycyclic aromatic hydrocarbons (PAHs) are described. The irradiation studies of anthracene: H2O, pyrene: H2O, and benzo[ghi]perylene: H2O ices (14 K) at various concentrations reported by Bouwman et al. are extended. While aromatic alcohols and ketones have been reported in residues after irradiated PAH:H2O ices were warmed to 270 K, it was not known if they formed during ice irradiation or during warm-up when reactants interact as H2O sublimes. Recent work has shown that they form in low temperature ice. Using DFT computed IR spectra to identify photoproducts and PAH cations, we tentatively identify the production of specific alcohols [PAH(OH)(n)] and quinones [PAH(O)(n)] for all PAH:H2O ices considered here. Little evidence is found for hydrogenation at 14 K, consistent with the findings of Gudipati & Yang. Addition of O and OH to the parent PAH is the dominant photochemical reaction, but PAH erosion to smaller PAHs (producing CO2 and H2CO) is also important. DFT spectra are used to assess the contribution of PAH-related species to interstellar absorption features from 5 to 9 mu m. The case is made that PAH cations are important contributors to the C2 component and PAH(OH)(n) and PAH(O)(n) to the C5 component described by Boogert et al. Thus, interstellar ices should contain neutral and ionized PAHs, alcohols, ketones and quinones at the similar to 2%-4% level relative to H2O. PAHs, their photoproducts, and ion-mediated processes should therefore be considered when modeling interstellar ice processes.
C1 [Cook, Amanda M.; Mattioda, Andrew L.; Roser, Joseph; Bregman, Jonathan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ricca, Alessandra; Allamandola, Louis J.] SETI Inst, Mountain View, CA 94043 USA.
[Bouwman, Jordy] Radboud Univ Nijmegen, Inst Mol & Mat, NL-6525 ED Nijmegen, Netherlands.
[Linnartz, Harold] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands.
RP Cook, AM (reprint author), NASA, Ames Res Ctr, POB 1,M-S 245-6, Moffett Field, CA 94035 USA.
FU NASA; NSF Graduate Research Fellowship; NSF University Radio
Observatories program [URO: AST-1140030]
FX We thank the anonymous referee for helpful comments. P.B.C and G.A.B.
gratefully acknowledge funding from the NASA Astrophysics Research and
Analysis and Herschel Guaranteed Time Observer programs. B.A.M.
gratefully acknowledges funding by an NSF Graduate Research Fellowship.
The Arizona Radio Observatory is operated by Steward Observatory,
University of Arizona, with partial support through the NSF University
Radio Observatories program (URO: AST-1140030). The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 21
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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 JAN 20
PY 2015
VL 799
IS 1
AR 14
DI 10.1088/0004-637X/799/1/14
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500014
ER
PT J
AU Defrere, D
Hinz, PM
Skemer, AJ
Kennedy, GM
Bailey, VP
Hoffmann, WF
Mennesson, B
Millan-Gabet, R
Danchi, WC
Absil, O
Arbo, P
Beichman, C
Brusa, G
Bryden, G
Downey, EC
Durney, O
Esposito, S
Gaspar, A
Grenz, P
Haniff, C
Hill, JM
Lebreton, J
Leisenring, JM
Males, JR
Marion, L
McMahon, TJ
Montoya, M
Morzinski, KM
Pinna, E
Puglisi, A
Rieke, G
Roberge, A
Serabyn, E
Sosa, R
Stapeldfeldt, K
Su, K
Vaitheeswaran, V
Vaz, A
Weinberger, AJ
Wyatt, MC
AF Defrere, D.
Hinz, P. M.
Skemer, A. J.
Kennedy, G. M.
Bailey, V. P.
Hoffmann, W. F.
Mennesson, B.
Millan-Gabet, R.
Danchi, W. C.
Absil, O.
Arbo, P.
Beichman, C.
Brusa, G.
Bryden, G.
Downey, E. C.
Durney, O.
Esposito, S.
Gaspar, A.
Grenz, P.
Haniff, C.
Hill, J. M.
Lebreton, J.
Leisenring, J. M.
Males, J. R.
Marion, L.
McMahon, T. J.
Montoya, M.
Morzinski, K. M.
Pinna, E.
Puglisi, A.
Rieke, G.
Roberge, A.
Serabyn, E.
Sosa, R.
Stapeldfeldt, K.
Su, K.
Vaitheeswaran, V.
Vaz, A.
Weinberger, A. J.
Wyatt, M. C.
TI FIRST-LIGHT LBT NULLING INTERFEROMETRIC OBSERVATIONS: WARM EXOZODIACAL
DUST RESOLVED WITHIN A FEW AU OF eta Crv
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: planetary systems; infrared: stars;
instrumentation: interferometers; stars: individual (eta Crv)
ID MAIN-SEQUENCE STARS; LATE-HEAVY BOMBARDMENT; SUN-LIKE STARS; DEBRIS
DISKS; HOT DUST; LUMINOSITY FUNCTION; PERFORMANCE; PLANETS; NULLER;
CORVI
AB We report on the first nulling interferometric observations with the Large Binocular Telescope Interferometer (LBTI), resolving the N' band (9.81-12.41 mu m) emission around the nearby main-sequence star eta Crv (F2V, 1-2 Gyr). The measured source null depth amounts to 4.40% +/- 0.35% over a field-of-view of 140 mas in radius (similar to 2.6AU for the distance of eta Crv) and shows no significant variation over 35 degrees of sky rotation. This relatively low null is unexpected given the total disk to star flux ratio measured by the Spitzer Infrared Spectrograph (IRS; similar to 23% across the N' band), suggesting that a significant fraction of the dust lies within the central nulled response of the LBTI (79 mas or 1.4AU). Modeling of the warm disk shows that it cannot resemble a scaled version of the solar zodiacal cloud unless it is almost perpendicular to the outer disk imaged by Herschel. It is more likely that the inner and outer disks are coplanar and the warm dust is located at a distance of 0.5-1.0AU, significantly closer than previously predicted by models of the IRS spectrum (similar to 3AU). The predicted disk sizes can be reconciled if the warm disk is not centrosymmetric, or if the dust particles are dominated by very small grains. Both possibilities hint that a recent collision has produced much of the dust. Finally, we discuss the implications for the presence of dust for the distance where the insolation is the same as Earth's (2.3AU).
C1 [Defrere, D.; Hinz, P. M.; Skemer, A. J.; Bailey, V. P.; Hoffmann, W. F.; Arbo, P.; Brusa, G.; Downey, E. C.; Durney, O.; Gaspar, A.; Grenz, P.; Leisenring, J. M.; Males, J. R.; McMahon, T. J.; Montoya, M.; Morzinski, K. M.; Rieke, G.; Sosa, R.; Su, K.; Vaitheeswaran, V.; Vaz, A.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Kennedy, G. M.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Mennesson, B.; Bryden, G.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Millan-Gabet, R.; Beichman, C.; Lebreton, J.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Danchi, W. C.; Roberge, A.; Stapeldfeldt, K.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Absil, O.; Marion, L.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Sart Tilman Par Liege, Belgium.
[Esposito, S.; Pinna, E.; Puglisi, A.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Haniff, C.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Hill, J. M.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
[Weinberger, A. J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Defrere, D (reprint author), Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
EM ddefrere@email.arizona.edu
RI Roberge, Aki/D-2782-2012
OI Roberge, Aki/0000-0002-2989-3725
FU National Aeronautics and Space Administration as part of its Exoplanet
Exploration Program; European Union through ERC [279973]
FX The Large Binocular Telescope Interferometer is funded by the National
Aeronautics and Space Administration as part of its Exoplanet
Exploration Program. The LBT is an international collaboration among
institutions in the United States, Italy, and Germany. LBT Corporation
partners are the University of Arizona on behalf of the Arizona
university system; Istituto Nazionale di Astrofisica, Italy; LBT
Beteiligungsgesellschaft, Germany, representing the Max-Planck Society,
the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio
State University; and the Research Corporation, on behalf of the
University of Notre Dame, the University of Minnesota, and the
University of Virginia. This work was supported by the European Union
through ERC grant number 279973 (G.M.K. and M.C.W.). The authors thank
C. Lisse for helpful advice. The LBTI team would like to dedicate this
paper to the memory of our colleague and friend, Vidhya Vaitheeswaran.
NR 50
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U1 2
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 42
DI 10.1088/0004-637X/799/1/42
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500041
ER
PT J
AU Gruesbeck, JR
Lepri, ST
Zurbuchen, TH
Christian, ER
AF Gruesbeck, Jacob R.
Lepri, Susan T.
Zurbuchen, Thomas H.
Christian, Eric R.
TI EVIDENCE FOR LOCAL ACCELERATION OF SUPRATHERMAL HEAVY ION OBSERVATIONS
DURING INTERPLANETARY CORONAL MASS EJECTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; Sun: coronal mass ejections (CMEs); Sun:
heliosphere
ID ADVANCED COMPOSITION EXPLORER; LARGE HELIOCENTRIC DISTANCES; SOLAR-WIND;
MAGNETIC-FIELD; ENERGETIC PARTICLES; COSMIC-RAYS; SPACECRAFT; SHOCK;
HELIOSPHERE; POPULATIONS
AB Suprathermal particles are an important seed population for a variety of energetic particles found throughout the heliosphere, but their origin is in debate. We present, for the first time, high-cadence observations of suprathermal heavy ions during interplanetary coronal mass ejections (ICMEs), from the Suprathermal Ion Composition Spectrometer on board the Wind spacecraft, and investigate their ionic composition and compare it to the bulk solar wind plasma composition, observed from the Solar Wind Ion Composition Spectrometer on board the Advanced Composition Explorer. We find that the composition of the suprathermal plasma is related to the local bulk solar wind plasma and not to the plasma upstream of the ICME. This implies that the suprathermal plasma is accelerated from the local bulk solar wind plasma and not the upstream solar wind plasma.
C1 [Gruesbeck, Jacob R.; Lepri, Susan T.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Christian, Eric R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gruesbeck, JR (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
FU NASA Graduate Student Research Program [NNX10AM41H]; NASA [NNX10AT73G,
NNX11AP01G]
FX This work was supported, in part, by the NASA Graduate Student Research
Program grant NNX10AM41H, and NASA grant NNX10AT73G. This paper was
enabled by discussions with L.A. Fisk who was supported by NASA grant
NNX11AP01G.
NR 47
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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 JAN 20
PY 2015
VL 799
IS 1
AR 57
DI 10.1088/0004-637X/799/1/57
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500055
ER
PT J
AU Hajra, R
Tsurutani, BT
Echer, E
Gonzalez, WD
Santolik, O
AF Hajra, Rajkumar
Tsurutani, Bruce T.
Echer, Ezequiel
Gonzalez, Walter D.
Santolik, Ondrej
TI RELATIVISTIC (E > 0.6, > 2.0, AND > 4.0 MeV) ELECTRON ACCELERATION AT
GEOSYNCHRONOUS ORBIT DURING HIGH-INTENSITY, LONG-DURATION, CONTINUOUS AE
ACTIVITY (HILDCAA) EVENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; magnetic reconnection; relativistic
processes; solar wind; waves
ID WHISTLER-MODE CHORUS; OUTER RADIATION BELT; INTERPLANETARY
MAGNETIC-FIELD; WAVE-PARTICLE INTERACTIONS; PITCH-ANGLE SCATTERING;
VAN-ALLEN BELT; SOLAR-CYCLE; INNER MAGNETOSPHERE; RESONANT DIFFUSION;
GEOMAGNETIC STORM
AB Radiation-belt relativistic (E > 0.6, > 2.0, and > 4.0 MeV) electron acceleration is studied for solar cycle 23 (1995-2008). High-intensity, long-duration, continuous AE activity (HILDCAA) events are considered as the basis of the analyses. All of the 35 HILDCAA events under study were found to be characterized by flux enhancements of magnetospheric relativistic electrons of all three energies compared to the pre-event flux levels. For the E > 2.0 MeV electron fluxes, enhancement of > 50% occurred during 100% of HILDCAAs. Cluster-4 passes were examined for electromagnetic chorus waves in the 5 < L < 10 and 0 < MLT < 12 region when wave data were available. Fully 100% of these HILDCAA cases were associated with enhanced whistler-mode chorus waves. The enhancements of E > 0.6, > 2.0, and > 4.0 MeV electrons occurred similar to 1.0 day, similar to 1.5 days, and similar to 2.5 days after the statistical HILDCAA onset, respectively. The statistical acceleration rates for the three energy ranges were similar to 1.8 x 10(5), 2.2 x 10(3), and 1.0 x 10(1) cm(-2) s(-1) sr(-1) d(-1), respectively. The relativistic electron-decay timescales were determined to be similar to 7.7, 5.5, and 4.0 days for the three energy ranges, respectively. The HILDCAAs were divided into short-duration (D <= 3 days) and long-duration (D > 3 days) events to study the dependence of relativistic electron variation on HILDCAA duration. For long-duration events, the flux enhancements during HILDCAAs with respect to pre-event fluxes were similar to 290%, 520%, and 82% for E > 0.6, > 2.0, and > 4.0 MeV electrons, respectively. The enhancements were similar to 250%, 400%, and 27% respectively, for short-duration events. The results are discussed with respect to the current understanding of radiation-belt dynamics.
C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Paulo, Brazil.
[Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Santolik, Ondrej] Inst Atmospher Phys AS CR, Prague, Czech Republic.
[Santolik, Ondrej] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Paulo, Brazil.
EM rajkumarhajra@yahoo.co.in
RI Hajra, Rajkumar/C-1246-2011; Santolik, Ondrej/F-7766-2014;
OI Hajra, Rajkumar/0000-0003-0447-1531
FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through a
postdoctoral research fellowship at INPE; Brazilian CNPq
[301233/2011-0]; NASA; [GACR205-10/2279]; [LH14010]
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. E.E. would like to thank the Brazilian CNPq
(301233/2011-0) agency for financial support. Portions of this research
were performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. O.S. acknowledges funding from
grants GACR205-10/2279 and LH14010. The Cluster data can be obtained
from ESA CFA. The GOES data used in this paper are collected from the
website http://www.ngdc.noaa.gov/stp/satellite/goes/dataaccess.html. The
OMNI data are collected from http://omniweb.gsfc.nasa.gov/.
NR 68
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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 JAN 20
PY 2015
VL 799
IS 1
AR 39
DI 10.1088/0004-637X/799/1/39
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500038
ER
PT J
AU Hashimoto, J
Tsukagoshi, T
Brown, JM
Dong, R
Muto, T
Zhu, Z
Wisniewski, J
Ohashi, N
Kudo, T
Kusakabe, N
Abe, L
Akiyama, E
Brandner, W
Brandt, T
Carson, J
Currie, T
Egner, S
Feldt, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, G
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Mayama, S
Mede, K
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, G
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Hashimoto, J.
Tsukagoshi, T.
Brown, J. M.
Dong, R.
Muto, T.
Zhu, Z.
Wisniewski, J.
Ohashi, N.
Kudo, T.
Kusakabe, N.
Abe, L.
Akiyama, E.
Brandner, W.
Brandt, T.
Carson, J.
Currie, T.
Egner, S.
Feldt, M.
Grady, C. A.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G.
Kuzuhara, M.
Kwon, J.
Matsuo, T.
McElwain, M. W.
Mayama, S.
Mede, K.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, G.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y.
Takami, M.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI THE STRUCTURE OF PRE-TRANSITIONAL PROTOPLANETARY DISKS. II. AZIMUTHAL
ASYMMETRIES, DIFFERENT RADIAL DISTRIBUTIONS OF LARGE AND SMALL DUST
GRAINS IN PDS 70
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; polarization; protoplanetary disks; stars: individual
(PDS 70); stars: pre-main sequence; submillimeter: general
ID T-TAURI DISKS; SPECTRAL ENERGY-DISTRIBUTIONS; PLANET-FORMING REGIONS;
YOUNG STELLAR OBJECTS; INDUCED GAP EDGES; TRANSITIONAL DISK; ACCRETION
DISKS; GIANT PLANET; SAO 206462; CIRCUMSTELLAR DISKS
AB The formation scenario of a gapped disk, i.e., transitional disk, and its asymmetry is still under debate. Proposed scenarios such as disk-planet interaction, photoevaporation, grain growth, anticyclonic vortex, eccentricity, and their combinations would result in different radial distributions of the gas and the small (sub-mu m size) and large (millimeter size) dust grains as well as asymmetric structures in a disk. Optical/near-infrared (NIR) imaging observations and (sub-)millimeter interferometry can trace small and large dust grains, respectively; therefore multi-wavelength observations could help elucidate the origin of complicated structures of a disk. Here we report Submillimeter Array observations of the dust continuum at 1.3 mm and (CO)-C-12 J = 2 -> 1 line emission of the pre-transitional protoplanetary disk around the solar-mass star PDS 70. PDS 70, a weak-lined T Tauri star, exhibits a gap in the scattered light from its disk with a radius of similar to 65 AU at NIR wavelengths. However, we found a larger gap in the disk with a radius of similar to 80 AU at 1.3 mm. Emission from all three disk components (the gas and the small and large dust grains) in images exhibits a deficit in brightness in the central region of the disk, in particular, the dust disk in small and large dust grains has asymmetric brightness. The contrast ratio of the flux density in the dust continuum between the peak position to the opposite side of the disk reaches 1.4. We suggest the asymmetries and different gap radii of the disk around PDS 70 are potentially formed by several (unseen) accreting planets inducing dust filtration.
C1 [Hashimoto, J.; Wisniewski, J.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA.
[Tsukagoshi, T.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dong, R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Zhu, Z.; Knapp, G.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Ohashi, N.; Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.] Subaru Telescope, Hilo, HI 96720 USA.
[Kusakabe, N.; Akiyama, E.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J. -I.; Suto, H.; Suzuki, R.; Takami, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Hippolyte Fizeau, UMR6525, F-06108 Nice 02, France.
[Brandner, W.; Carson, J.; Feldt, M.; Henning, T.; Janson, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, T.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Currie, T.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Hodapp, K.] Univ Hawaii, Hilo, HI 96720 USA.
[Janson, M.] Queens Univ Belfast, Astrophys Res Ctr, Belfast, Antrim, North Ireland.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kwon, J.; Mede, K.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Mayama, S.] Shonan Int Village, Grad Univ Adv Studies SOKENDAI, Hayama, Kanagawa 2400193, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima 7398511, Japan.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain.
[Serabyn, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suenaga, T.; Takahashi, Y.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Turner, E. L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Hashimoto, J (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA.
EM jun.hashimoto@ou.edu
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU MEXT Japan; Mitsubishi Foundation; U.S. National Science Foundation
[1009203, 1009314]; [25-8826]
FX We are grateful to an anonymous referee for providing useful comments
leading to an improved paper. We appreciate support from the SMA staff.
This work is partly supported by a Grant-in-Aid for Science Research in
a Priority Area from MEXT Japan, by the Mitsubishi Foundation, and by
the U.S. National Science Foundation under Award Nos. 1009203 and
1009314. This work is partially supported by Grant-in-Aid for JSPS
Fellows (No. 25-8826).
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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 JAN 20
PY 2015
VL 799
IS 1
AR 43
DI 10.1088/0004-637X/799/1/43
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500042
ER
PT J
AU Leggett, SK
Morley, CV
Marley, MS
Saumon, D
AF Leggett, S. K.
Morley, Caroline V.
Marley, M. S.
Saumon, D.
TI NEAR-INFRARED PHOTOMETRY OF Y DWARFS: LOW AMMONIA ABUNDANCE AND THE
ONSET OF WATER CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: atmospheres
ID HUBBLE-SPACE-TELESCOPE; COOLEST BROWN DWARFS; SURVEY-EXPLORER WISE;
DIGITAL SKY SURVEY; T-DWARFS; MULTIOBJECT SPECTROGRAPH; L/T TRANSITION;
STANDARD STARS; LOW-MASS; DISCOVERY
AB We present new near-infrared photometry for seven late-type T dwarfs and nine Y-type dwarfs, and lower limit magnitudes for a tenth Y dwarf, obtained at Gemini Observatory. We also present a reanalysis of H-band imaging data from the Keck Observatory Archive, for an 11th Y dwarf. These data are combined with earlier MKO-system photometry, Spitzer and WISE mid-infrared photometry, and available trigonometric parallaxes, to create a sample of late-type brown dwarfs that includes 10 T9-T9.5 dwarfs or dwarf systems, and 16 Y dwarfs. We compare the data to our models, which include updated H-2 and NH3 opacity, as well as low-temperature condensate clouds. The models qualitatively reproduce the trends seen in the observed colors; however, there are discrepancies of around a factor of two in flux for the Y0-Y1 dwarfs, with T-eff approximate to 350-400 K. At T-eff similar to 400 K, the problems could be addressed by significantly reducing the NH3 absorption, for example by halving the abundance of NH3 possibly by vertical mixing. At T-eff similar to 350 K, the discrepancy may be resolved by incorporating thick water clouds. The onset of these clouds might occur over a narrow range in T-eff, as indicated by the observed small change in 5 mu m flux over a large change in J -W2 color. Of the known Y dwarfs, the reddest in J-W2 are WISEP J182831.08 + 265037.8 and WISE J085510.83-071442.5. We interpret the former as a pair of identical 300-350 K dwarfs, and the latter as a 250 K dwarf. If these objects are similar to 3 Gyr old, their masses are similar to 10 and similar to 5 Jupiter-masses, respectively.
C1 [Leggett, S. K.] Gemini Observ, Northern Operat Ctr, Hilo, HI 96720 USA.
[Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, M. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Leggett, SK (reprint author), Gemini Observ, Northern Operat Ctr, 670 N Aohoku Pl, Hilo, HI 96720 USA.
EM sleggett@gemini.edu
OI Marley, Mark/0000-0002-5251-2943; Leggett, Sandy/0000-0002-3681-2989
FU NASA [NNH12AT89I]; Gemini Observatory; National Aeronautics and Space
Administration
FX D.S. is supported by NASA Origins NNH12AT89I. 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 Science and Technology
Facilities Council (United Kingdom), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina). S.K.L.'s
research is supported by Gemini Observatory. This publication makes use
of data products from the Wide-field Infrared Survey Explorer, which is
a joint project of the University of California, Los Angeles, and the
Jet Propulsion Laboratory/California Institute of Technology, funded by
the National Aeronautics and Space Administration. This research has
made use of the NASA/IPAC Infrared Science Archive, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research has made use of the Keck Observatory Archive (KOA), which is
operated by the W. M. Keck Observatory and the NASA Exoplanet Science
Institute (NExScI), under contract with the National Aeronautics and
Space Administration.
NR 69
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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 JAN 20
PY 2015
VL 799
IS 1
AR 37
DI 10.1088/0004-637X/799/1/37
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500036
ER
PT J
AU Milisavljevic, D
Margutti, R
Parrent, JT
Soderberg, AM
Fesen, RA
Mazzali, P
Maeda, K
Sanders, NE
Cenko, SB
Silverman, JM
Filippenko, AV
Kamble, A
Chakraborti, S
Drout, MR
Kirshner, RP
Pickering, TE
Kawabata, K
Hattori, T
Hsiao, EY
Stritzinger, MD
Marion, GH
Vinko, J
Wheeler, JC
AF Milisavljevic, D.
Margutti, R.
Parrent, J. T.
Soderberg, A. M.
Fesen, R. A.
Mazzali, P.
Maeda, K.
Sanders, N. E.
Cenko, S. B.
Silverman, J. M.
Filippenko, A. V.
Kamble, A.
Chakraborti, S.
Drout, M. R.
Kirshner, R. P.
Pickering, T. E.
Kawabata, K.
Hattori, T.
Hsiao, E. Y.
Stritzinger, M. D.
Marion, G. H.
Vinko, J.
Wheeler, J. C.
TI THE BROAD-LINED Type Ic SN 2012ap AND THE NATURE OF RELATIVISTIC
SUPERNOVAE LACKING A GAMMA-RAY BURST DETECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; supernovae: general; supernovae: individual
(SN 2012ap)
ID CORE-COLLAPSE SUPERNOVAE; DIFFUSE INTERSTELLAR BANDS; SOUTHERN
SPECTROPHOTOMETRIC STANDARDS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE;
CASSIOPEIA-A SUPERNOVA; LATE-TIME SPECTRA; H-II REGIONS;
STRIPPED-ENVELOPE; IB SUPERNOVAE; LIGHT CURVES
AB We present ultraviolet, optical, and near-infrared observations of SN 2012ap, a broad-lined Type Ic supernova in the galaxy NGC 1729 that produced a relativistic and rapidly decelerating outflow without a gamma-ray burst signature. Photometry and spectroscopy follow the flux evolution from -13 to +272 days past the B-band maximum of -17.4 +/- 0.5mag. The spectra are dominated by Fe II, OI, and Ca II absorption lines at ejecta velocities of nu approximate to 20,000 km s(-1) that change slowly over time. Other spectral absorption lines are consistent with contributions from photospheric He I, and hydrogen may also be present at higher velocities (nu greater than or similar to 27,000 km s(-1)). We use these observations to estimate explosion properties and derive a total ejecta mass of similar to 2.7 M-circle dot, a kinetic energy of similar to 1.0 x 10(52) erg, and a Ni-56 mass of 0.1-0.2 M-circle dot. Nebular spectra (t > 200 days) exhibit an asymmetric double-peaked [O I] lambda lambda 6300, 6364 emission profile that we associate with absorption in the supernova interior, although toroidal ejecta geometry is an alternative explanation. SN 2012ap joins SN2009bb as another exceptional supernova that shows evidence for a central engine (e. g., black hole accretion or magnetar) capable of launching a non-negligible portion of ejecta to relativistic velocities without a coincident gamma-ray burst detection. Defining attributes of their progenitor systems may be related to notable observed properties including environmental metallicities of Z greater than or similar to Z(circle dot), moderate to high levels of host galaxy extinction (E(B - V) > 0.4mag), detection of high-velocity helium at early epochs, and a high relative flux ratio of [Ca II]/[O I] > 1 at nebular epochs. These events support the notion that jet activity at various energy scales may be present in a wide range of supernovae.
C1 [Milisavljevic, D.; Margutti, R.; Parrent, J. T.; Soderberg, A. M.; Sanders, N. E.; Kamble, A.; Chakraborti, S.; Drout, M. R.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fesen, R. A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Mazzali, P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Mazzali, P.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Mazzali, P.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Maeda, K.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Maeda, K.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.
[Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. B.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Silverman, J. M.; Marion, G. H.; Vinko, J.; Wheeler, J. C.] Univ Texas Austin, Austin, TX 78712 USA.
[Pickering, T. E.] Southern African Large Telescope, ZA-7935 Cape Town, South Africa.
[Pickering, T. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kawabata, K.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Hattori, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Hsiao, E. Y.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile.
[Hsiao, E. Y.; Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary.
RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dmilisav@cfa.harvard.edu
OI stritzinger, maximilian/0000-0002-5571-1833
FU W.M. Keck Foundation; David and Lucile Packard Foundation; NSF Astronomy
and Astrophysics Postdoctoral Fellowship [AST-1302771]; NSF
[AST-1211196, AST-1109801, AST-1211916, AST-1008343, PHYS-1066293];
Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO
Foundation; World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan; Hungarian OTKA [NN-107637]; Danish Agency for
Science and Technology and Innovation; [23740141]; [26800100]
FX We thank an anonymous referee for helpful suggestions. Many of the
observations reported in this paper were obtained with the Southern
African Large Telescope. Additional 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. Some
observations also came from the MMT Observatory, a joint facility of the
Smithsonian Institution and the University of Arizona, as well as the
6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
Support was provided by the David and Lucile Packard Foundation
Fellowship for Science and Engineering awarded to A.M.S. J.M.S. is
supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship
under award AST-1302771. T.E.P. thanks the National Research Foundation
of South Africa. R.P.K. and J.C.W. are grateful for NSF grants
AST-1211196 and AST-1109801, respectively. A.V.F. and S.B.C. acknowledge
generous support from Gary and Cynthia Bengier, the Richard and Rhoda
Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation,
and NSF grant AST-1211916. K.M. acknowledges financial support by
Grant-in-Aid for Scientific Research for Young Scientists (23740141,
26800100). The work by K.M. is partly supported by World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan.
J.V. is supported by Hungarian OTKA grant NN-107637. M.D.S. and E.Y.H.
gratefully acknowledge generous support provided by the Danish Agency
for Science and Technology and Innovation realized through a Sapere Aude
Level 2 grant. E.Y.H. also acknowledges support from NSF grant
AST-1008343. D. Sahu and G. Pignata kindly provided archival spectra of
SN 2007ru and SN 2009bb, respectively. This paper made extensive use of
the SUSPECT database (www.nhn.ou.edu/similar to suspect/) and the
Weizmann interactive supernova data repository
(www.weizmann.ac.il/astrophysics/wiserep). This work was supported in
part by NSF grant No. PHYS-1066293 and the hospitality of the Aspen
Center for Physics.
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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 JAN 20
PY 2015
VL 799
IS 1
AR 51
DI 10.1088/0004-637X/799/1/51
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500049
ER
PT J
AU Ozak, N
Ofman, L
Vinas, AF
AF Ozak, N.
Ofman, L.
Vinas, A. -F.
TI ION HEATING IN INHOMOGENEOUS EXPANDING SOLAR WIND PLASMA: THE ROLE OF
PARALLEL AND OBLIQUE ION-CYCLOTRON WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; plasmas; solar wind; Sun: corona; Sun: magnetic fields;
waves
ID FREQUENCY ALFVEN WAVES; HYBRID SIMULATIONS; PROTON; CORONA;
ACCELERATION; INSTABILITY; TURBULENCE; ANISOTROPY; ULYSSES; FLUCTUATIONS
AB Remote sensing observations of coronal holes show that heavy ions are hotter than protons and their temperature is anisotropic. In-situ observations of fast solar wind streams provide direct evidence for turbulent Alfven wave spectrum, left-hand polarized ion-cyclotron waves, and He++ - proton drift in the solar wind plasma, which can produce temperature anisotropies by resonant absorption and perpendicular heating of the ions. Furthermore, the solar wind is expected to be inhomogeneous on decreasing scales approaching the Sun. We study the heating of solar wind ions in inhomogeneous plasma with a 2.5D hybrid code. We include the expansion of the solar wind in an inhomogeneous plasma background, combined with the effects of a turbulent wave spectrum of Alfvenic fluctuations and initial ion-proton drifts. We study the influence of these effects on the perpendicular ion heating and cooling and on the spectrum of the magnetic fluctuations in the inhomogeneous background wind. We find that inhomogeneities in the plasma lead to enhanced heating compared to the homogenous solar wind, and the generation of significant power of oblique waves in the solar wind plasma. The cooling effect due to the expansion is not significant for super-Alfvenic drifts, and is diminished further when we include an inhomogeneous background density. We reproduce the ion temperature anisotropy seen in observations and previous models, which is present regardless of the perpendicular cooling due to solar wind expansion. We conclude that small scale inhomogeneities in the inner heliosphere can significantly affect resonant wave ion heating.
C1 [Ozak, N.] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel.
[Ofman, L.] Catholic Univ Amer, Washington, DC 20064 USA.
[Ofman, L.; Vinas, A. -F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ozak, N (reprint author), Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel.
FU Helen Kimmel Center for Planetary Science; NASA [NNX10AC56G]
FX N.O. would like to acknowledge support by the Helen Kimmel Center for
Planetary Science. L.O. would like to acknowledge support by NASA grant
NNX10AC56G.
NR 42
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 77
DI 10.1088/0004-637X/799/1/77
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500075
ER
PT J
AU Pillai, T
Kauffmann, J
Tan, JC
Goldsmith, PF
Carey, SJ
Menten, KM
AF Pillai, T.
Kauffmann, J.
Tan, J. C.
Goldsmith, P. F.
Carey, S. J.
Menten, K. M.
TI MAGNETIC FIELDS IN HIGH-MASS INFRARED DARK CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: magnetic fields; polarization; stars: formation
ID STAR-FORMATION; MOLECULAR CLOUDS; GALACTIC-CENTER; DENSE CORES;
FRAGMENTATION; G11.11-0.12; POLARIMETRY; TURBULENT; MODELS; G0.253+0.016
AB High-mass stars are cosmic engines known to dominate the energetics in the Milky Way and other galaxies. However, their formation is still not well understood. Massive, cold, dense clouds, often appearing as infrared dark clouds (IRDCs), are the nurseries of massive stars. No measurements of magnetic fields in IRDCs in a state prior to the onset of high-mass star formation (HMSF) have previously been available, and prevailing HMSF theories do not consider strong magnetic fields. Here, we report observations of magnetic fields in two of the most massive IRDCs in the Milky Way. We show that IRDCs G11.11-0.12 and G0.253+0.016 are strongly magnetized and that the strong magnetic field is as important as turbulence and gravity for HMSF. The main dense filament in G11.11-0.12 is perpendicular to the magnetic field, while the lower density filament merging onto the main filament is parallel to the magnetic field. The implied magnetic field is strong enough to suppress fragmentation sufficiently to allow HMSF. Other mechanisms reducing fragmentation, such as the entrapment of heating from young stars via high-mass surface densities, are not required to facilitate HMSF.
C1 [Pillai, T.; Kauffmann, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Pillai, T.; Kauffmann, J.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Tan, J. C.] Univ Florida, Gainesville, FL 32611 USA.
[Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carey, S. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Pillai, T (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM tpillai.astro@gmail.com
RI Goldsmith, Paul/H-3159-2016;
OI Kauffmann, Jens/0000-0002-5094-6393
FU European Commission Seventh Framework Programme (FP7)
[PIRSES-GA-2012-31578 "EuroCal"]; Deutsche Forschungsgemeinschaft (DFG)
FX We thank P. Redman for his data on G11.11-0.12 and his discussion on the
observations. We thank Brenda Matthews for kindly checking the quality
of the re-processed SCUPOL data for this source. We thank the referee
for a very constructive review of the manuscript that improved the
quality of the manuscript. This work was carried out in part at the Jet
Propulsion Laboratory, which is operated for NASA by the California
Institute of Technology. T.P. and J.K. acknowledge support by the
European Commission Seventh Framework Programme (FP7) through grant
PIRSES-GA-2012-31578 "EuroCal". T.P. acknowledges support from the
Deutsche Forschungsgemeinschaft (DFG) via the SPP (priority program)
1573 'Physics of the ISM'.
NR 51
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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 JAN 20
PY 2015
VL 799
IS 1
AR 74
DI 10.1088/0004-637X/799/1/74
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500072
ER
PT J
AU Riddle, RL
Tokovinin, A
Mason, BD
Hartkopf, WI
Roberts, LC
Baranec, C
Law, NM
Bui, K
Burse, MP
Das, HK
Dekany, RG
Kulkarni, S
Punnadi, S
Ramaprakash, AN
Tendulkar, SP
AF Riddle, Reed L.
Tokovinin, Andrei
Mason, Brian D.
Hartkopf, William I.
Roberts, Lewis C., Jr.
Baranec, Christoph
Law, Nicholas M.
Bui, Khanh
Burse, Mahesh P.
Das, H. K.
Dekany, Richard G.
Kulkarni, Shrinivas
Punnadi, Sujit
Ramaprakash, A. N.
Tendulkar, Shriharsh P.
TI A SURVEY OF THE HIGH ORDER MULTIPLICITY OF NEARBY SOLAR-TYPE BINARY
STARS WITH Robo-AO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: general; instrumentation: adaptive optics;
stars: formation; techniques: high angular resolution
ID PHASES DIFFERENTIAL ASTROMETRY; USNO FLAGSTAFF STATION; LASER ADAPTIVE
OPTICS; VISUAL DOUBLE STARS; SPECKLE INTERFEROMETRY; ORBITAL ELEMENTS;
CD-ROM; SPECTROSCOPIC BINARIES; HIPPARCOS BINARIES; WIYN TELESCOPE
AB We conducted a survey of nearby binary systems composed of main sequence stars of spectral types F and G in order to improve our understanding of the hierarchical nature of multiple star systems. Using Robo-AO, the first robotic adaptive optics instrument, we collected high angular resolution images with deep and well-defined detection limits in the Sloan Digital Sky Survey i' band. A total of 695 components belonging to 595 systems were observed. We prioritized observations of faint secondary components with separations over 10 '' to quantify the still poorly constrained frequency of their subsystems. Of the 214 secondaries observed, 39 contain such subsystems; 19 of those were discovered with Robo-AO. The selection-corrected frequency of secondary subsystems with periods from 10(3.5) to 10(5) days is 0.12 +/- 0.03, the same as the frequency of such companions to the primary. Half of the secondary pairs belong to quadruple systems where the primary is also a close pair, showing that the presence of subsystems in both components of the outer binary is correlated. The relatively large abundance of 2+2 quadruple systems is a new finding, and will require more exploration of the formation mechanism of multiple star systems. We also targeted close binaries with periods less than 100 yr, searching for their distant tertiary components, and discovered 17 certain and 2 potential new triples. In a subsample of 241 close binaries, 71 have additional outer companions. The overall frequency of tertiary components is not enhanced, compared to all (non-binary) targets, but in the range of outer periods from 10(6) to 10(7.5) days (separations on the order of 500AU), the frequency of tertiary components is 0.16 +/- 0.03, exceeding the frequency of similar systems among all targets (0.09) by almost a factor of two. Measurements of binary stars with Robo-AO allowed us to compute first orbits for 9 pairs and to improve orbits of another 11 pairs.
C1 [Riddle, Reed L.; Bui, Khanh; Dekany, Richard G.; Kulkarni, Shrinivas; Tendulkar, Shriharsh P.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Tokovinin, Andrei] Cerro Tololo Interamer Observ, La Serena, Chile.
[Mason, Brian D.; Hartkopf, William I.] US Naval Observ, Washington, DC 20392 USA.
[Roberts, Lewis C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA.
[Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Burse, Mahesh P.; Das, H. K.; Punnadi, Sujit; Ramaprakash, A. N.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
RP Riddle, RL (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
OI Roberts, Lewis/0000-0003-3892-2900; Tokovinin,
Andrei/0000-0002-2084-0782
FU California Institute of Technology; Inter-University Centre for
Astronomy and Astrophysics; National Science Foundation [AST-0906060,
AST-0960343, AST-1207891]; Mount Cuba Astronomical Foundation; National
Aeronautics and Space Administration; Alfred P. Sloan Foundation
FX We acknowledge the input of the referee who read through this lengthy
paper and gave us comments to improve it. The Robo-AO system is
supported by collaborating partner institutions, the California
Institute of Technology and the Inter-University Centre for Astronomy
and Astrophysics, and by the National Science Foundation under grant
Nos. AST-0906060, AST-0960343, and AST-1207891, by the Mount Cuba
Astronomical Foundation, and by a gift from Samuel Oschin. We are
grateful to the Palomar Observatory staff for their ongoing support of
Robo-AO on the P60, particularly S. Kunsman, M. Doyle, J. Henning, R.
Walters, G. Van Idsinga, B. Baker, K. Dunscombe and D. Roderick.; A
portion of the research in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.; C.B.
acknowledges support from the Alfred P. Sloan Foundation.
NR 151
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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 JAN 20
PY 2015
VL 799
IS 1
AR 4
DI 10.1088/0004-637X/799/1/4
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500004
ER
PT J
AU Shrader, CR
Hamaguchi, K
Sturner, SJ
Oskinova, LM
Almeyda, T
Petre, R
AF Shrader, C. R.
Hamaguchi, K.
Sturner, S. J.
Oskinova, L. M.
Almeyda, T.
Petre, R.
TI HIGH-ENERGY PROPERTIES OF THE ENIGMATIC Be STAR gamma CASSIOPEIAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; stars: emission-line, Be; stars: individual (gamma
Cassiopeiae); white dwarfs; X-rays: binaries; X-rays: stars
ID X-RAY-EMISSION; MULTIWAVELENGTH CAMPAIGN; CATACLYSMIC VARIABLES;
CYCLICAL VARIABILITY; OPTICAL OBSERVATIONS; MASSIVE STAR; BINARIES;
SPECTRUM; CATALOG; SUZAKU
AB We present the results of a broadband X-ray study of the enigmatic Be star Gamma Cassiopeiae (herein gamma Cas) based on observations made with both the Suzaku and INTEGRAL observatories.. Cas has long been recognized as the prototypical example of a small subclass of Be stars with moderately strong X-ray emission dominated by a hot thermal component in the 0.5-12 keV energy range (L-x approximate to 10(32)-10(33) erg s(-1)). This places them at the high end of the known luminosity distribution for stellar emission, but several orders of magnitude below typical accretion-powered Be X-ray binaries. The INTEGRAL observations spanned an eight-year baseline and represent the deepest measurement to date at energies above similar to 50 keV. We find that the INTEGRAL data are consistent within statistics to a constant intensity source above 20 keV, with emission extending up to similar to 100 keV, and that searches for all of the previously reported periodicities of the system at lower energies led to null results. We further find that our combined Suzaku and INTEGRAL spectrum, which we suggest is the most accurate broadband X-ray measurement of gamma Cas to date, is fitted extremely well with a thermal plasma emission model with a single absorption component. We found no compelling need for an additional non-thermal high-energy component. We discuss these results in the context of a currently favored models for gamma Cas and its analogs.
C1 [Shrader, C. R.; Hamaguchi, K.; Sturner, S. J.; Petre, R.] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA.
[Shrader, C. R.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Hamaguchi, K.; Sturner, S. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Oskinova, L. M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Almeyda, T.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
RP Shrader, CR (reprint author), NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA.
EM Chris.R.Shrader@nasa.gov
RI XRAY, SUZAKU/A-1808-2009
FU DLR [50 OR 1302]
FX This project made use of observational data awarded to K.H. through the
Suzaku Guest Investigator program and INTEGRAL archival data obtained
from the HEASARC at the NASA Goddard Space Flight Center. C.R.S. thanks
Myron Smith for many useful discussions and for introducing him to this
topic many years ago. L.M.O. acknowledges support from DLR grant 50 OR
1302.
NR 65
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 84
DI 10.1088/0004-637X/799/1/84
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500082
ER
PT J
AU Sllowikowska, A
Stappers, BW
Harding, AK
O'Dell, SL
Elsner, RF
van der Horst, AJ
Weisskopf, MC
AF Sllowikowska, Agnieszka
Stappers, Benjamin W.
Harding, Alice K.
O'Dell, Stephen L.
Elsner, Ronald F.
van der Horst, Alexander J.
Weisskopf, Martin C.
TI HIGH-TIME-RESOLUTION MEASUREMENTS OF THE POLARIZATION OF THE CRAB PULSAR
AT 1.38 GHz
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; pulsars: general; pulsars: individual (Crab: PSR
B0531+21); stars: neutron
ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; LIGHT CURVES; OPTICAL
POLARIZATION; NEBULA PULSAR; GIANT PULSES; WIDE-BAND; RADIATION;
EMISSION; MODEL
AB Using the Westerbork Synthesis Radio Telescope, we obtained high-time-resolution measurements of the full polarization of the Crab pulsar. At a resolution of 1/8192 of the 34ms pulse period (i.e., 4.1 mu s), the 1.38 GHz linear-polarization measurements are in general agreement with previous lower-time-resolution 1.4 GHz measurements of linear polarization in the main pulse (MP), in the interpulse (IP), and in the low-frequency component (LFC). We find the MP and IP to be linearly polarized at about 24% and 21% with no discernible difference in polarization position angle. However, contrary to theoretical expectations and measurements in the visible, we find no evidence for significant variation (sweep) in the polarization position angle over the MP, the IP, or the LFC. We discuss the implications, which appear to be in contradiction to theoretical expectations. We also detect weak circular polarization in the MP and IP, and strong (approximate to 20%) circular polarization in the LFC, which also exhibits very strong (approximate to 98%) linear polarization at a position angle of 40 degrees from that of the MP or IP. The properties are consistent with the LFC, which is a low-altitude component, and the MP and IP, which are high-altitude caustic components. Current models for the MP and IP emission do not readily account for the absence of pronounced polarization changes across the pulse. We measure IP and LFC pulse phases relative to the MP consistent with recent measurements, which have shown that the phases of these pulse components are evolving with time.
C1 [Sllowikowska, Agnieszka] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland.
[Stappers, Benjamin W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Harding, Alice K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[O'Dell, Stephen L.; Elsner, Ronald F.; Weisskopf, Martin C.] NASA, Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[van der Horst, Alexander J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands.
RP Sllowikowska, A (reprint author), Univ Zielona Gora, Kepler Inst Astron, Lubuska 2, PL-65265 Zielona Gora, Poland.
OI O'Dell, Stephen/0000-0002-1868-8056
FU NWO, the Netherlands Foundation for Scientific Research; Polish National
Science Centre [DEC-2011/03/D/ST9/00656]; UK Science and Technology
Facilities Council; AKH, NASA [12-ATP12-0169, 11-FERMI11-0052]; AJvdH
from the European Research Council [247295]; NASA's Chandra Program
FX The Westerbork Synthesis Radio Telescope (WSRT) is operated by ASTRON,
the Netherlands Institute for Radio Astronomy, with support from NWO,
the Netherlands Foundation for Scientific Research. A.S. acknowledges
grant DEC-2011/03/D/ST9/00656 from the Polish National Science Centre;
BWS, a Consolidated Grant from the UK Science and Technology Facilities
Council; AKH, NASA grants Astrophysics Theory 12-ATP12-0169 and Fermi
Guest Investigator 11-FERMI11-0052; AJvdH, Advanced Investigator Grant
247295 (PI: R. A. M. J. Wijers) from the European Research Council; and
SLO, RFE, and MCW, support by NASA's Chandra Program.
NR 58
TC 2
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 70
DI 10.1088/0004-637X/799/1/70
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500068
ER
PT J
AU Viall, NM
Klimchuk, JA
AF Viall, Nicholeen M.
Klimchuk, James A.
TI THE TRANSITION REGION RESPONSE TO A CORONAL NANOFLARE: FORWARD MODELING
AND OBSERVATIONS IN SDO/AIA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: transition region; Sun: UV radiation
ID ACTIVE-REGION; LOOPS; EVOLUTION; PLASMA; WAVES; TRACE
AB The corona and transition region (TR) are fundamentally coupled through the processes of thermal conduction and mass exchange. It is not possible to understand one without the other. Yet the temperature-dependent emissions from the two locations behave quite differently in the aftermath of an impulsive heating event such as a coronal nanoflare. Whereas the corona cools sequentially, emitting first at higher temperatures and then at lower temperatures, the TR is multithermal and the emission at all temperatures responds in unison. We have previously applied the automated time lag technique of Viall & Klimchuk to disk observations of an active region (AR) made by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. Lines of sight passing through coronal plasma show clear evidence for post-nanoflare cooling, while lines of sight intersecting the TR footpoints of coronal strands show zero time lag. In this paper, we use the EBTEL hydrodynamics code to demonstrate that this is precisely the expected behavior when the corona is heated by nanoflares. We also apply the time lag technique for the first time to off-limb observations of an AR. Since TR emission is not present above the limb, the occurrence of zero time lags is greatly diminished, supporting the conclusion that zero time lags measured on the disk are due to TR plasma. Lastly, we show that the "coronal" channels in AIA can be dominated by bright TR emission. When defined in a physically meaningful way, the TR reaches a temperature of roughly 60% the peak temperature in a flux tube. The TR resulting from impulsive heating can extend to 3 MK and higher, well within the range of the "coronal" AIA channels.
C1 [Viall, Nicholeen M.; Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Viall, NM (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU NASA GI grant
FX We thank the reviewer, Peter Cargill, for his thoughtful suggestions.
These data are courtesy of NASA/SDO and the AIA science team. This work
benefited greatly from the International Space Science Institute team
meeting "Coronal Heating-Using Observables to Settle the Question of
Steady vs. Impulsive Heating" led by Stephen Bradshaw and Helen Mason.
This research was supported by a NASA GI grant.
NR 26
TC 5
Z9 5
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 58
DI 10.1088/0004-637X/799/1/58
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500056
ER
PT J
AU Way, MJ
Gazis, PR
Scargle, JD
AF Way, M. J.
Gazis, P. R.
Scargle, Jeffrey D.
TI STRUCTURE IN THE 3D GALAXY DISTRIBUTION. II. VOIDS AND WATERSHEDS OF
LOCAL MAXIMA AND MINIMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; cosmology: observations; galaxies: clusters: general;
large-scale structure of universe
ID DIGITAL SKY SURVEY; FINDER COMPARISON PROJECT; NONLINEAR DENSITY FIELD;
PERSISTENT COSMIC WEB; LARGE-SCALE STRUCTURE; 7TH DATA RELEASE; REDSHIFT
SURVEY; DARK-MATTER; FINDING ALGORITHM; FILAMENTARY STRUCTURE
AB The major uncertainties in studies of the multi-scale structure of the universe arise not from observational errors but from the variety of legitimate definitions and detection methods for individual structures. To facilitate the study of these methodological dependencies, we have carried out 12 different analyses defining structures in various ways. This has been done in a purely geometrical way by utilizing the HOP algorithm as a unique parameter-free method of assigning groups of galaxies to local density maxima or minima. From three density estimation techniques (smoothing kernels, Bayesian blocks, and self-organizing maps) applied to three data sets (the Sloan Digital Sky Survey Data Release 7, the Millennium simulation, and randomly distributed points) we tabulate information that can be used to construct catalogs of structures connected to local density maxima and minima. We also introduce a void finder that utilizes a method to assemble Delaunay tetrahedra into connected structures and characterizes regions empty of galaxies in the source catalog.
C1 [Way, M. J.; Gazis, P. R.; Scargle, Jeffrey D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Way, M. J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Way, M. J.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
RP Way, MJ (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM Michael.J.Way@nasa.gov; PGazis@sbcglobal.net; Jeffrey.D.Scargle@nasa.gov
OI Way, Michael/0000-0003-3728-0475
FU Alfred P. Sloan Foundation; National Aeronautics and Space
Administration; National Science Foundation; U.S. Department of Energy;
Japanese Monbukagakusho; Max Planck Society; University of Chicago;
Fermilab; Institute for Advanced Study; Japan Participation Group; Johns
Hopkins University; Los Alamos National Laboratory; Max-Planck-Institute
for Astronomy; Max-Planck-Institute for Astrophysics; New Mexico State
University; University of Pittsburgh; Princeton University; United
States Naval Observatory; University of Washington; NASA-Ames Director's
Discretionary Fund; NASA Applied Information Systems Research Program
FX We are grateful to the NASA-Ames Director's Discretionary Fund and to
Joe Bredekamp and the NASA Applied Information Systems Research Program
for support and encouragement. Thanks go to Ani Thakar and Maria
Nieto-Santisteban for their help with our many SDSS casjobs queries.
Michael Blanton's help with using his SDSS NYU-VAGC catalog is also very
much appreciated. We are grateful to Patrick Moran, Christopher Henze,
Changbom Park, Paul Sutter, Mark Neyrinck, Thierry Sousbie, Tom Abel,
Pratyush Pranav, Peer-Timo Bremer, Attila Gyulassy, James ("B.J.")
Bjorken, and Jessi Cisewski. Special thanks go to Slobodan Simic and
members of the CAMCOS project at San Jose State University, Joseph
Fitch, David Goulette, Jian-Long Liu, Mathew Litrus, Brandon Morrison,
Hai Nguyen Au, and Catherine (Boersma) Parayil for useful comments and
for an ongoing collaboration on developments of the HOP algorithm for
topological data analysis. None of these acknowledgments should be
construed to imply agreement with the ideas expressed here.; Funding for
the SDSS has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Aeronautics and Space
Administration, the National Science Foundation, the U.S. Department of
Energy, the Japanese Monbukagakusho, and the Max Planck Society. The
SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the University of Chicago, Fermilab,
the Institute for Advanced Study, the Japan Participation Group, the
Johns Hopkins University, Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy, the Max-Planck-Institute for
Astrophysics, New Mexico State University, University of Pittsburgh,
Princeton University, the United States Naval Observatory, and the
University of Washington.
NR 169
TC 3
Z9 3
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 95
DI 10.1088/0004-637X/799/1/95
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500093
ER
PT J
AU White, CJ
Kasliwal, MM
Nugent, PE
Gal-Yam, A
Howell, DA
Sullivan, M
Goobar, A
Piro, AL
Bloom, JS
Kulkarni, SR
Laher, RR
Masci, F
Ofek, EO
Surace, J
Ben-Ami, S
Cao, Y
Cenko, SB
Hook, IM
Jonsson, J
Matheson, T
Sternberg, A
Quimby, RM
Yaron, O
AF White, Christopher J.
Kasliwal, Mansi M.
Nugent, Peter E.
Gal-Yam, Avishay
Howell, D. Andrew
Sullivan, Mark
Goobar, Ariel
Piro, Anthony L.
Bloom, Joshua S.
Kulkarni, Shrinivas R.
Laher, Russ R.
Masci, Frank
Ofek, Eran O.
Surace, Jason
Ben-Ami, Sagi
Cao, Yi
Cenko, S. Bradley
Hook, Isobel M.
Jonsson, Jakob
Matheson, Thomas
Sternberg, Assaf
Quimby, Robert M.
Yaron, Ofer
TI SLOW-SPEED SUPERNOVAE FROM THE PALOMAR TRANSIENT FACTORY: TWO CHANNELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (iPTF 13an, PTF 09ego, PTF
09eiy, PTF 09eoi, PTF 10xk, PTF 10bvr, PTF 10ujn, PTF 10acdh, PTF 11hyh;
SN 2002cx, SN 2002es); surveys; techniques: spectroscopic
ID MASS WHITE-DWARFS; IA SUPERNOVAE; LIGHT CURVES; DETONATION SUPERNOVAE;
LOW-LUMINOSITY; II SUPERNOVAE; REDSHIFT DATA; LOW-VELOCITY; SN 2008HA;
GALAXIES
AB Since the discovery of the unusual prototype SN 2002cx, the eponymous class of Type I (hydrogen-poor) supernovae with low ejecta speeds has grown to include approximately two dozen members identified from several heterogeneous surveys, in some cases ambiguously. Here we present the results of a systematic study of 1077 Type I supernovae discovered by the Palomar Transient Factory, leading to nine new members of this peculiar class. Moreover, we find there are two distinct subclasses based on their spectroscopic, photometric, and host galaxy properties: "SN 2002cx-like" supernovae tend to be in later-type or more irregular hosts, have more varied and generally dimmer luminosities, have longer rise times, and lack a Ti II trough when compared to "SN 2002es-like" supernovae. None of our objects show helium, and we counter a previous claim of two such events. We also find that the occurrence rate of these transients relative to Type Ia supernovae is 5.6(-3.8)(+22) % (90% confidence), lower compared to earlier estimates. Combining our objects with the literature sample, we propose that these subclasses have two distinct physical origins.
C1 [White, Christopher J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kasliwal, Mansi M.; Piro, Anthony L.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Nugent, Peter E.; Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Gal-Yam, Avishay; Ofek, Eran O.; Ben-Ami, Sagi; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Howell, D. Andrew] Las Cumbres Observ Global Telescope Network Inc, Goleta, CA 93117 USA.
[Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Goobar, Ariel] Stockholm Univ, AlbaNova, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Piro, Anthony L.] CALTECH, Pasadena, CA 91125 USA.
[Kulkarni, Shrinivas R.; Cao, Yi] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Laher, Russ R.; Masci, Frank; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Hook, Isobel M.] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England.
[Hook, Isobel M.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
[Jonsson, Jakob] Savantic AB, SE-11863 Stockholm, Sweden.
[Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Sternberg, Assaf] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany.
[Sternberg, Assaf] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Quimby, Robert M.] Univ Tokyo, Kavli IPMU, Kashiwa, Chiba 2778583, Japan.
[Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP White, CJ (reprint author), Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA.
OI Sullivan, Mark/0000-0001-9053-4820
FU Hubble Fellowship; Carnegie-Princeton Fellowship; EU/FP7 via ERC
[307260]; ISF; Minerva grant; Weizmann-UK grant; "Quantum Universe"
I-Core Program of the Planning and Budgeting Committee; Israel Science
Foundation; Kimmel Award; NSF [AST-1205732, PHY-1068881, PHY-1151197];
Sherman Fairchild Foundation; Willner Family Leadership Institute, Ilan
Gluzman (Secaucus, NJ); Israeli Ministry of Science; Israel Science
Foundation, Minerva, Weizmann-UK; I-CORE Program of the Planning and
Budgeting Committee
FX C. J. W. began this research as part of the summer student exchange
program between Princeton and Carnegie. M. M. K. acknowledges generous
support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.
G.-Y. acknowledges support by the EU/FP7 via ERC grant 307260; ISF,
Minerva, and Weizmann-UK grants; as well as the "Quantum Universe"
I-Core Program of the Planning and Budgeting Committee and the Israel
Science Foundation and the Kimmel Award. A. L. P. is supported through
NSF grants AST-1205732, PHY-1068881, and PHY-1151197, as well as the
Sherman Fairchild Foundation. E. O. O. is incumbent on the Arye
Dissentshik career development chair and is grateful for support by
grants from the Willner Family Leadership Institute, Ilan Gluzman
(Secaucus, NJ), the Israeli Ministry of Science, the Israel Science
Foundation, Minerva, Weizmann-UK, and the I-CORE Program of the Planning
and Budgeting Committee and the Israel Science Foundation.
NR 85
TC 17
Z9 17
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 JAN 20
PY 2015
VL 799
IS 1
AR 52
DI 10.1088/0004-637X/799/1/52
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500050
ER
PT J
AU Rios, AC
AF Rios, Andro C.
TI Impact synthesis of the RNA bases
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Editorial Material
ID NUCLEOBASE FORMATION; ORGANIC-MOLECULES; SHOCK SYNTHESIS; FORMAMIDE;
ORIGIN; LIFE; CHEMISTRY; ADENINE
C1 [Rios, Andro C.] NASA, Ames Res Ctr, Exobiol Branch, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Rios, AC (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM andro.c.rios@nasa.gov
NR 20
TC 1
Z9 1
U1 9
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 JAN 20
PY 2015
VL 112
IS 3
BP 643
EP 644
DI 10.1073/pnas.1424273112
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AZ2BY
UT WOS:000348040700021
PM 25568087
ER
PT J
AU Lakicevic, M
van Loon, JT
Meixner, M
Gordon, K
Bot, C
Roman-Duval, J
Babler, B
Bolatto, A
Engelbracht, C
Filipovic, M
Hony, S
Indebetouw, R
Misselt, K
Montiel, E
Okumura, K
Panuzzo, P
Patat, F
Sauvage, M
Seale, J
Sonneborn, G
Temim, T
Urosevic, D
Zanardo, G
AF Lakicevic, Masa
van Loon, Jacco Th.
Meixner, Margaret
Gordon, Karl
Bot, Caroline
Roman-Duval, Julia
Babler, Brian
Bolatto, Alberto
Engelbracht, Chad
Filipovic, Miroslav
Hony, Sacha
Indebetouw, Remy
Misselt, Karl
Montiel, Edward
Okumura, K.
Panuzzo, Pasquale
Patat, Ferdinando
Sauvage, Marc
Seale, Jonathan
Sonneborn, George
Temim, Tea
Urosevic, Dejan
Zanardo, Giovanna
TI THE INFLUENCE OF SUPERNOVA REMNANTS ON THE INTERSTELLAR MEDIUM IN THE
LARGE MAGELLANIC CLOUD SEEN AT 20-600 mu m WAVELENGTHS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; evolution; galaxies: ISM; ISM: clouds; ISM: supernova
remnants; Magellanic Clouds; submillimeter: galaxies; submillimeter: ISM
ID PULSAR WIND NEBULA; X-RAY-EMISSION; DUST DESTRUCTION; IA SUPERNOVA;
SPITZER OBSERVATIONS; CHANDRA OBSERVATION; GALAXY EVOLUTION; 1E
0102.2-7219; RICH EJECTA; HERSCHEL
AB We present the analysis of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) and their influence on the environment at far-infrared (FIR) and submillimeter wavelengths. We use new observations obtained with the Herschel Space Observatory and archival data obtained with the Spitzer Space Telescope, to make the first FIR atlas of these objects. The SNRs are not clearly discernible at FIR wavelengths; however, their influence becomes apparent in maps of dust mass and dust temperature, which we constructed by fitting a modified blackbody to the observed spectral energy distribution in each sightline. Most of the dust that is seen is pre-existing interstellar dust in which SNRs leave imprints. The temperature maps clearly reveal SNRs heating surrounding dust, while the mass maps indicate the removal of 3.7(-2.5)(+7.5) M-circle dot of dust per SNR. This agrees with the calculations by others that significant amounts of dust are sputtered by SNRs. Under the assumption that dust is sputtered and not merely pushed away, we estimate a dust destruction rate in the LMC of 0.037(-0.025)(+0.075) M-circle dot yr(-1) due to SNRs, yielding an average lifetime for interstellar dust of 2(-1.3)(+4.0) x 10(7) yr. We conclude that sputtering of dust by SNRs may be an important ingredient in models of galactic evolution, that supernovae may destroy more dust than they produce, and that they therefore may not be net producers of long lived dust in galaxies.
C1 [Lakicevic, Masa; van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Meixner, Margaret; Gordon, Karl; Roman-Duval, Julia; Seale, Jonathan] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meixner, Margaret] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Gordon, Karl] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bot, Caroline] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France.
[Babler, Brian] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Bolatto, Alberto] Univ Maryland, Lab Millimeter Astron, College Pk, MD 20742 USA.
[Engelbracht, Chad; Misselt, Karl; Montiel, Edward] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Filipovic, Miroslav] Univ Western Sydney, Penrith, NSW 1797, Australia.
[Hony, Sacha; Okumura, K.; Panuzzo, Pasquale; Sauvage, Marc] CEA, Irfu SAp, Orme Merisiers, Lab AIM, F-91191 Gif Sur Yvette, France.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Montiel, Edward] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Panuzzo, Pasquale] CNRS, Observ Paris, Lab GEPI, F-92195 Meudon, France.
[Patat, Ferdinando] European Org Astron Res Southern Hemisphere ESO, D-85748 Garching, Germany.
[Seale, Jonathan] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA.
[Sonneborn, George; Temim, Tea] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Urosevic, Dejan] Univ Belgrade, Fac Math, Dept Astron, Belgrade 11000, Serbia.
[Urosevic, Dejan] Isaac Newton Inst Chile, Yugoslavia Branch, Santiago, Serbia.
[Zanardo, Giovanna] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia.
RP Lakicevic, M (reprint author), Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
EM m.lakicevic@keele.ac.uk
OI Lakicevic, Masa/0000-0002-8231-0963; Bot, Caroline/0000-0001-6118-2985
FU Ministry of Education, Science and Technological Development of the
Republic of Serbia [176005]
FX We thank the referee for her/his constructive report and Dr. Eli Dwek
for helpful advice. M.L. acknowledges an ESO/Keele studentship. D.U.
acknowledges support from the Ministry of Education, Science and
Technological Development of the Republic of Serbia through project No.
176005.
NR 99
TC 9
Z9 9
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2015
VL 799
IS 1
AR 50
DI 10.1088/0004-637X/799/1/50
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ4SY
UT WOS:000348214500048
ER
PT J
AU Miller, JM
Tomsick, JA
Bachetti, M
Wilkins, D
Boggs, SE
Christensen, FE
Craig, WW
Fabian, AC
Grefenstette, BW
Hailey, CJ
Harrison, FA
Kara, E
King, AL
Stern, DK
Zhang, WW
AF Miller, J. M.
Tomsick, J. A.
Bachetti, M.
Wilkins, D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Fabian, A. C.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Kara, E.
King, A. L.
Stern, D. K.
Zhang, W. W.
TI NEW CONSTRAINTS ON THE BLACK HOLE LOW/HARD STATE INNER ACCRETION FLOW
WITH NuSTAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics
ID X-RAY REFLECTION; ACTIVE GALACTIC NUCLEI; GRS 1739-278; DISK WIND; SPIN;
MASS; SPECTRA; MODELS; JETS; SPECTROSCOPY
AB We report on an observation of the Galactic black hole candidate GRS 1739-278 during its 2014 outburst, obtained with NuSTAR. The source was captured at the peak of a rising "low/hard" state, at a flux of similar to 0.3 Crab. A broad, skewed iron line and disk reflection spectrum are revealed. Fits to the sensitive NuSTAR spectra with a number of relativistically blurred disk reflection models yield strong geometrical constraints on the disk and hard X-ray "corona." Two models that explicitly assume a "lamp post" corona find its base to have a vertical height above the black hole of h = 5(-2)(+7) GM/c(2) and h = 18 +/- 4GM/c(2) (90% confidence errors); models that do not assume a "lamp post" return emissivity profiles that are broadly consistent with coronae of this size. Given that X-ray microlensing studies of quasars and reverberation lags in Seyferts find similarly compact coronae, observations may now signal that compact coronae are fundamental across the black hole mass scale. All of the models fit to GRS 1739-278 find that the accretion disk extends very close to the black hole-the least stringent constraint is r(in) = 5(-4)(+3) GM/c2. Only two of the models deliver meaningful spin constraints, but a = 0.8 +/- 0.2 is consistent with all of the fits. Overall, the data provide especially compelling evidence of an association between compact hard X-ray coronae and the base of relativistic radio jets in black holes.
C1 [Miller, J. M.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Tomsick, J. A.; Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bachetti, M.] Univ Toulouse, UPS OMP, IRAP, F-31100 Toulouse, France.
[Bachetti, M.] CNRS, Intitut Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Wilkins, D.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Craig, W. W.; Hailey, C. J.] Columbia Univ, New York, NY 10027 USA.
[Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Grefenstette, B. W.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337
FU NASA [NNG08FD60C]
FX J.M.M. thanks Javier Garcia and Thomas Dauser for helpful conversations.
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 NASA.
NR 39
TC 18
Z9 18
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2015
VL 799
IS 1
AR L6
DI 10.1088/2041-8205/799/1/L6
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ3RD
UT WOS:000348143500006
ER
PT J
AU Singal, J
Kogut, A
Jones, E
Dunlap, H
AF Singal, J.
Kogut, A.
Jones, E.
Dunlap, H.
TI AXIAL RATIO OF EDGE-ON SPIRAL GALAXIES AS A TEST FOR BRIGHT RADIO HALOS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Galaxy: halo; radio continuum: galaxies
ID ABSOLUTE SKY BRIGHTNESS; CONTINUUM OBSERVATIONS; MAGNETIC-FIELDS;
EMISSION; GHZ; NGC-253; EXCESS
AB We use surface brightness contour maps of nearby edge-on spiral galaxies to determine whether extended bright radio halos are common. In particular, we test a recent model of the spatial structure of the diffuse radio continuum by Subrahmanyan & Cowsik which posits that a substantial fraction of the observed high-latitude surface brightness originates from an extended Galactic halo of uniform emissivity. Measurements of the axial ratio of emission contours within a sample of normal spiral galaxies at 1500 MHz and below show no evidence for such a bright, extended radio halo. Either the Galaxy is atypical compared to nearby quiescent spirals or the bulk of the observed high-latitude emission does not originate from this type of extended halo.
C1 [Singal, J.; Jones, E.; Dunlap, H.] Univ Richmond, Dept Phys, Richmond, VA 23173 USA.
[Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Singal, J (reprint author), Univ Richmond, Dept Phys, 28 Westhampton Way, Richmond, VA 23173 USA.
EM jsingal@richmond.edu
OI Kogut, Alan/0000-0001-9835-2351
FU NASA's Science Innovation Fund
FX Support for this research comes from NASA's Science Innovation Fund.
NR 33
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 JAN 20
PY 2015
VL 799
IS 1
AR L10
DI 10.1088/2041-8205/799/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ3RD
UT WOS:000348143500010
ER
PT J
AU Yeom, K
AF Yeom, Kiwon
TI Morphological approach for autonomous and adaptive system: The
construction of three-dimensional artificial model based on
self-reconfigurable modular agents
SO NEUROCOMPUTING
LA English
DT Article; Proceedings Paper
CT 3rd International Conference on Swarm Intelligence (ICSI)
CY JUN 15-20, 2012
CL Shenzhen, PEOPLES R CHINA
SP Shenzhen Univ, Peking Univ, Xian Jiaotong-Liverpool Univ, IEEE Computat Intelligence Soc (CI S), World Federat Soft Comp, Int Neural Network Soc, Nat Sci Fdn China
DE Morphogeneis; Self-organization; Self-reconfiguration; Federation of
agents
ID DISTRIBUTED CONTROL; POLYOLEFIN PARTICLES; MORPHOGENESIS; COMMUNICATION;
CATALYSTS; ROBOTS; SWARMS; SIZE
AB This paper presents a decentralized approach, inspired by biological cells, for the automatic construction of user-defined three-dimensional structures. Using high-level specification as an input, the proposed system enables the guaranteed construction of user-specified structures. By investigating the evolutionary aspects of morphogenesis, which is regulated by the interplay of the cell processes such as differential cell adhesion, gene-regulation, and inter-cellular signaling, an approach was developed that allows for the construction of an arbitrary structure via swarms of identical, independent, and autonomous multi-agents. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Yeom, Kiwon] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
[Yeom, Kiwon] San Jose State Univ, Res Fdn, San Jose, CA 95112 USA.
RP Yeom, K (reprint author), NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
EM pragman@gmail.com
NR 46
TC 1
Z9 1
U1 1
U2 29
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0925-2312
EI 1872-8286
J9 NEUROCOMPUTING
JI Neurocomputing
PD JAN 19
PY 2015
VL 148
BP 100
EP 111
DI 10.1016/j.neucom.2012.12.082
PG 12
WC Computer Science, Artificial Intelligence
SC Computer Science
GA AR8QP
UT WOS:000343840000014
ER
PT J
AU Gettelman, A
Wang, T
AF Gettelman, A.
Wang, T.
TI Structural diagnostics of the tropopause inversion layer and its
evolution
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE tropopause; tropopause
ID DYNAMICAL TROPOPAUSE; STATIC STABILITY; HEIGHT
AB The Tropopause Inversion Layer (TIL) is marked by a peak in static stability directly above the tropopause. The TIL is quantitatively defined with new diagnostics using Global Positioning System Radio Occultation temperature soundings and reanalysis data. A climatology of the TIL is developed from reanalysis data (1980-2011) using diagnostics for the position, depth, and strength of the TIL based on the TIL peak in static stability. TIL diagnostics have defined relationships to the synoptic situation in the Upper Troposphere and Lower Stratosphere. The TIL is present nearly all the time. The TIL becomes hard to define in the subtropics where tropical air overlies midlatitude air, in a region of complex static stability profiles. The mean position of the subtropical TIL gradient is sharp and is co-located with the subtropical tropopause break. Over the period 1980-2011 the TIL depth below the tropopause has decreased by 5% per decade and increased above the tropical tropopause by a similar percentage. Furthermore, the latitude of the abrupt change in the TIL from tropical to extratropical in the lower stratosphere appears to have shifted poleward in each hemisphere by approximate to 1 degrees latitude per decade, depending on the diagnostic examined. Reanalysis trends should be treated with caution.
Key Points
C1 [Gettelman, A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Wang, T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Wang, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Gettelman, A (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM andrew@ucar.edu
RI Wang, Tao/C-2381-2011
OI Wang, Tao/0000-0003-3430-8508
FU U.S. National Science Foundation
FX NCAR is sponsored by the U.S. National Science Foundation. This project
started during a sabbatical at ETH Zurich and discussions with Heini
Wernli. ERAI data were provided by Heini Wernli and MetoSwiss. Thanks to
Peter Hoor and Thomas Birner for discussions. Thanks to Simone Tilmes
for assistance with MERRA reanalysis and to Cameron Homeyer and Bill
Randel for comments. ERAI data are available from ECMWF
(http://www.ecmwf.int/research/era/do/get/era-interim). MERRA Reanalyses
are available from NASA (http://gmao.gsfc.nasa.gov/merra/), and COSMIC
GPS data are available from the University Corporation for Atmospheric
Research (http://www.cosmic.ucar.edu/).
NR 33
TC 10
Z9 10
U1 6
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 16
PY 2015
VL 120
IS 1
BP 46
EP 62
DI 10.1002/2014JD021846
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA7NR
UT WOS:000349104700004
ER
PT J
AU Viudez-Mora, A
Costa-Suros, M
Calbo, J
Gonzalez, JA
AF Viudez-Mora, A.
Costa-Suros, M.
Calbo, J.
Gonzalez, J. A.
TI Modeling atmospheric longwave radiation at the surface during overcast
skies: The role of cloud base height
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE longwave radiation; cloud radiative effect; overcast sky; radiative
transfer model; ceilometer; pyrgeometer
ID DISCRETE-ORDINATE-METHOD; IRRADIANCE UNCERTAINTY; MULTIPLE-SCATTERING;
SATELLITE DATA; OCEAN SURFACE; WATER CLOUDS; PARAMETERIZATION; CLIMATE;
CLEAR; ALGORITHM
AB The behavior of the atmospheric downward longwave radiation at the surface under overcast conditions is studied. For optically thick clouds, longwave radiation depends greatly on the cloud base height (CBH), besides temperature and water vapor profiles. The CBH determines the cloud emission temperature and the air layers contributing to the longwave radiation that reaches the surface. Overcast situations observed at Girona (NE Iberian Peninsula) were studied by using a radiative transfer model. The data set includes different seasons, and a large range of CBH (0-5000m). The atmosphere profiles were taken from the European Center for Medium-Range Weather Forecast analysis. The CBH was determined from ceilometer measurements and also estimated by using a suitable method applied to the vertical profile of relative humidity. The agreement between calculations and pyrgeometer measurements is remarkably good (1.66.2 Wm(-2)) if the observed CBH is used; poorer results are obtained with the estimated CBH (4.37.0 Wm(-2)). These results are better than those obtained from a simple parameterization based upon ground-level data (1.111.6 Wm(-2)), which can be corrected by adding a term that takes into account the CBH (-0.17.3 Wm(-2)). At this site, the cloud radiative effect (CRE) at the surface lies in the range 50-80 Wm(-2), has a clear seasonal behavior (higher CRE in winter), and depends upon the CBH. For the cold and the warm seasons, CRE decreases with CBH at a rate of -5 and -4 Wm(-2)/km, respectively. Results obtained for other climates (subarctic and tropical) are also presented.
Key Points
C1 [Viudez-Mora, A.] NASA, Langley Res Ctr, Sci Mission Directorate, Hampton, VA 23665 USA.
[Costa-Suros, M.; Calbo, J.; Gonzalez, J. A.] Univ Girona, Grp Environm Phys, Girona, Spain.
RP Viudez-Mora, A (reprint author), NASA, Langley Res Ctr, Sci Mission Directorate, Hampton, VA 23665 USA.
EM toni.v.mora@nasa.gov
RI Calbo, Josep/K-2462-2014;
OI Calbo, Josep/0000-0002-9374-0790; Costa-Suros,
Montserrat/0000-0002-3319-4513
FU Spanish Ministry of Science and Innovation; NUCLIEREX [CGL
2007-62664/CLI]; NUCLIERSOL [CGL 2010-18546]
FX This study has been partly financed by the Spanish Ministry of Science
and Innovation (currently Ministry of Economy and Competitiveness)
projects NUCLIEREX (CGL 2007-62664/CLI) and NUCLIERSOL (CGL 2010-18546).
The European Centre for Medium-Range Weather Forecasts (ECMWF) is
acknowledged for providing the meteorological analyses used in the
present study. NSA and TWP data were obtained from the Atmospheric
Radiation Measurement (ARM) Program sponsored by the U.S. Department of
Energy, Office of Science, Office of Biological and Environmental
Research, Climate and Environmental Sciences Division. We would like to
thank M. Antonia Jimenez from the University of Illes Balears for
helping us in preparing the atmospheric profiles from the ECMWF
analysis. Data used to produce the results of this paper are available
by request to the authors; please contact them at josep. calbo@udg.edu.
NR 57
TC 1
Z9 1
U1 1
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 JAN 16
PY 2015
VL 120
IS 1
BP 199
EP 214
DI 10.1002/2014JD022310
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA7NR
UT WOS:000349104700013
ER
PT J
AU Leinonen, J
Moisseev, D
AF Leinonen, J.
Moisseev, D.
TI What do triple-frequency radar signatures reveal about aggregate
snowflakes?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE snow; radar; aggregation; backscattering; DDA; multifrequency
ID ICE PARTICLES; SIZE SPECTRA; SNOW; SCATTERING; CLOUDS; GROWTH;
CAPABILITIES; LIMITATIONS; ABSORPTION; MORPHOLOGY
AB A large data set of volume element models of aggregate snowflakes was created, building the snowflakes from various models of ice crystals found in the atmosphere: dendrites, needles, plates, and bullet rosettes, as well as spheroidal crystals for comparison. Several different sizes for the constituent crystals were also used. The radar backscattering cross sections of the snowflakes were computed from the models using the discrete dipole approximation (DDA) at 13.6 GHz (K-u band), 35.6 GHz (K-a band) and 94.0 GHz (W band), and the effects of the choice of crystal model and size on the K-u/K-a band and K-a/W band dual-wavelength ratios (DWR) was investigated. It was found that the aggregate DWRs were very similar for all naturally occurring ice crystal types investigated in this study. This implies that the choice of crystal type is at most of secondary importance in the forward model of scattering used for snowfall retrievals but also, conversely, that the identification of the crystal type from triple-frequency observations is likely to be difficult. In contrast, the size of the constituent ice crystals does have a nonnegligible impact on the triple-frequency signatures. Additionally, it was found that the triple-frequency signatures found in some experimental data, resembling those resulting from spheroidal model snowflakes, cannot be reproduced using the aggregates with any of the crystal types that were investigated. This suggests that besides aggregation, other mechanisms of snowflake formation from ice crystals must be considered in snowfall retrieval algorithms.
Key Points
C1 [Leinonen, J.] Finnish Meteorol Inst, Earth Observat, FIN-00101 Helsinki, Finland.
[Leinonen, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Moisseev, D.] Univ Helsinki, Dept Phys, Helsinki, Finland.
RP Leinonen, J (reprint author), Finnish Meteorol Inst, Earth Observat, FIN-00101 Helsinki, Finland.
EM jussi.s.leinonen@jpl.nasa.gov
RI Moisseev, Dmitri/A-3288-2008;
OI Moisseev, Dmitri/0000-0002-4575-0409; Leinonen,
Jussi/0000-0002-6560-6316
FU Academy of Finland [255718, 272041]; Finnish Funding Agency for
Technology and Innovation (Tekes) [3155/31/2009]
FX The original data used in this study are partially included in Table S1
in the supporting information; the rest are available from the authors
on request (email: jussi.s.leinonen@jpl.nasa.gov). The research
presented in this article was supported by the Academy of Finland
(grants 255718 and 272041) and the Finnish Funding Agency for Technology
and Innovation (Tekes; grant 3155/31/2009). Part of the research
described in this publication was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 38
TC 9
Z9 9
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 16
PY 2015
VL 120
IS 1
BP 229
EP 239
DI 10.1002/2014JD022072
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA7NR
UT WOS:000349104700015
ER
PT J
AU Liu, C
Yang, P
Nasiri, SL
Platnick, S
Meyer, KG
Wang, CX
Ding, SG
AF Liu, Chao
Yang, Ping
Nasiri, Shaima L.
Platnick, Steven
Meyer, Kerry G.
Wang, Chenxi
Ding, Shouguo
TI A fast Visible Infrared Imaging Radiometer Suite simulator for cloudy
atmospheres
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE VIIRS instrument simulator
ID RADIATIVE-TRANSFER MODEL; BULK SCATTERING PROPERTIES;
DISCRETE-ORDINATE-METHOD; PLANETARY-ATMOSPHERES; MULTIPLE-SCATTERING;
ICE CLOUDS; EFFECTIVE EMISSIVITY; LIGHT-SCATTERING; POLARIZED LIGHT;
CIRRUS CLOUDS
AB A fast instrument simulator is developed to simulate the observations made in cloudy atmospheres by the Visible Infrared Imaging Radiometer Suite (VIIRS). The correlated k distribution technique is used to compute the transmissivities associated with absorbing atmospheric gases. The bulk scattering properties of ice clouds are based on the ice model used for the Moderate Resolution Imaging Spectroradiometer Collection 6 ice cloud products, and those of water clouds are computed with the Lorenz-Mie theory. Two fast radiative transfer models based on precomputed ice cloud look-up tables are used for the VIIRS solar and infrared channels. The accuracy and efficiency of the fast simulator are quantified in comparison with a combination of the rigorous line-by-line (LBLRTM) and discrete ordinate radiative transfer (DISORT) models. The maximum relative errors of the simulator are less than 2% for simulated top of atmosphere reflectances at the solar channels, and the brightness temperature differences for the infrared channels are less than 0.2K. The simulator is over 3 orders of magnitude faster than the benchmark LBLRTM+DISORT model. Furthermore, the cloudy atmosphere reflectances and brightness temperatures from the fast VIIRS simulator compare favorably with those from VIIRS observations.
Key Points
C1 [Liu, Chao; Yang, Ping; Nasiri, Shaima L.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Platnick, Steven; Meyer, Kerry G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meyer, Kerry G.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Wang, Chenxi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Ding, Shouguo] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM pyang@tamu.edu
RI Liu, Chao/J-9551-2013; Nasiri, Shaima/C-8044-2011; Yang,
Ping/B-4590-2011; Meyer, Kerry/E-8095-2016; Platnick, Steven/J-9982-2014
OI Meyer, Kerry/0000-0001-5361-9200; Platnick, Steven/0000-0003-3964-3567
FU NASA [NNX11A055G]; David Bullock Harris Chair in Geosciences at the
College of Geosciences, Texas AM University
FX The MODIS data sets (MODIS Collection 6 MYD06_L2) used in this study are
publicly available through the NASA Atmosphere Archive and Distribution
System (LAADS, http://ladsweb.nascom.nasa.gov/data/). The VIIRS data
sets (VIIRS Moderate Resolution Band 01-16 SDR) are available at the
NOAA Comprehensive Large Array-data Stewardship System
(http://www.nsof.class.noaa.gov/saa/products/search?
datatype_family=VIIRS). The MERRA atmospheric profile data
(inst3_3d_asm_Cp) are downloaded from the NASA Goddard Earth Sciences
Data and Information Service Center
(http://disc.sci.gsfc.nasa.gov/mdisc/data-holdings/merra/merra_products_
nonjs.shtml). Shaima Nasiri and Ping Yang acknowledge funding support by
a NASA grant (NNX11A055G). Ping Yang also acknowledges support by the
endowment funds related to the David Bullock Harris Chair in Geosciences
at the College of Geosciences, Texas A&M University. The computations of
this study were carried out by using the Texas A&M University
Supercomputing Facilities.
NR 53
TC 1
Z9 1
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 16
PY 2015
VL 120
IS 1
BP 240
EP 255
DI 10.1002/2014JD022443
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CA7NR
UT WOS:000349104700016
ER
PT J
AU Orr, TR
Bleacher, JE
Patrick, MR
Wooten, KM
AF Orr, Tim R.
Bleacher, Jacob E.
Patrick, Matthew R.
Wooten, Kelly M.
TI A sinuous tumulus over an active lava tube at Kilauea Volcano:
Evolution, analogs, and hazard forecasts
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Kilauea; New Mexico; Mars; Flow inflation; Lava tube; Volcanic hazards
ID OO-KUPAIANAHA ERUPTION; BASALTIC LAVA; FLOW-FIELD; NORTH QUEENSLAND;
ICE-SHEET; HAWAII; MARS; PAHOEHOE; INFLATION; EMPLACEMENT
AB Inflation of narrow tube-fed basaltic lava flows (tens of meters across), such as those confined by topography, can be focused predominantly along the roof of a lava tube. This can lead to the development of an unusually long tumulus, its shape matching the sinuosity of the underlying lava tube. Such a situation occurred during Kilauea Volcano's (Hawai'i, USA) ongoing East Rift Zone eruption on a lava tube active from July through November 2010. Short-lived breakouts from the tube buried the flanks of the sinuous, ridge-like tumulus, while the tumulus crest, its surface composed of lava formed very early in the flow's emplacement history, remained poised above the surrounding younger flows. At least several of these breakouts resulted in irrecoverable uplift of the tube roof. Confined sections of the prehistoric Carrizozo and McCartys flows (New Mexico, USA) display similar sinuous, ridge-like features with comparable surface age relationships. We contend that these distinct features formed in a fashion equivalent to that of the sinuous tumulus that formed at Kilauea in 2010. Moreover, these sinuous tumuli may be analogs for some sinuous ridges evident in orbital images of the Tharsis volcanic province on Mars. The short-lived breakouts from the sinuous tumulus at Kilauea were caused by surges in discharge through the lava tube, in response to cycles of deflation and inflation (DI events) at Killauea's summit. The correlation between DI events and subsequent breakouts aided in lava flow forecasting. Breakouts from the sinuous tumulus advanced repeatedly toward the sparsely populated Kalapana Gardens subdivision, destroying two homes and threatening others. Hazard assessments, including flow occurrence and advance forecasts, were relayed regularly to the Hawaii County Civil Defense to aid their lava flow hazard mitigation efforts while this lava tube was active. Published by Elsevier B.V.
C1 [Orr, Tim R.; Patrick, Matthew R.; Wooten, Kelly M.] US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, Captain Cook, HI 96718 USA.
[Orr, Tim R.] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA.
[Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Wooten, Kelly M.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
RP Orr, TR (reprint author), US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, Captain Cook, HI 96718 USA.
EM torr@usgs.gov
RI Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
FU NASA's Moon and Mars Analog Mission Activities Program
FX The authors would like to thank Christopher Hamilton, Steven Anderson,
Laszlo Kestay, Don Swanson, Bruce Houghton, and Sarah Fagents, whose
helpful comments improved this manuscript greatly. We thank Dave and
Charlene Ewing for their willingness to host a webcam to assist with our
monitoring of flow activity near Kalapana. Orr, Patrick, and Wooten were
funded by the U.S. Geological Survey's Volcano Hazard Program. Funding
for Bleacher was provided by NASA's Moon and Mars Analog Mission
Activities Program.
NR 73
TC 5
Z9 6
U1 1
U2 7
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 JAN 15
PY 2015
VL 291
BP 35
EP 48
DI 10.1016/j.jvolgeores.2014.12.002
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA CC2ND
UT WOS:000350181000004
ER
PT J
AU Bennett, WR
Hoberecht, MA
Lvovich, VF
AF Bennett, William R.
Hoberecht, Mark A.
Lvovich, Vadim F.
TI Analysis of shunt currents and associated corrosion of bipolar plates in
PEM fuel cells
SO JOURNAL OF ELECTROANALYTICAL CHEMISTRY
LA English
DT Article
DE Fuel cell stack; Water electrolyzer stack; Shunt currents; Stray
electrolysis
ID INTERCELL CURRENTS; STAINLESS-STEEL; LEAKAGE CURRENT; CURRENT LOSSES;
STACKS; REGIME
AB Proton exchange membrane (PEM) fuel cells are being developed for future NASA missions. These fuel cells use a bipolar construction, with internal manifolds to conduct product water and coolant water. The wetted surfaces of the manifolds present large voltage gradients across the product water and coolant water passages, which can induce water electrolysis in the manifolds of full-scale stacks. If not controlled, shunt currents lead to parasitic power losses and corrosion of the fuel cell metal surfaces; therefore, it is important to understand and characterize the effects of shunt currents. This analysis also applies to electrolyzers, flow-batteries and other devices where an electrolyte manifold experiences voltage gradients. In this work, electrochemical characterizations were performed to estimate these characteristics under relevant operating conditions. A numerical solution of the shunt currents is presented, and the distribution of water electrolysis and corrosion is described. Published by Elsevier B.V.
C1 [Bennett, William R.; Hoberecht, Mark A.; Lvovich, Vadim F.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Bennett, WR (reprint author), NASA, John H Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM william.r.bennett@nasa.gov
FU NASA's Advanced Space Power Systems (ASPS) Project under Space
Technology Mission Directorate's Game Changing Development Program
FX The work presented in this paper was performed in support of NASA's
Advanced Space Power Systems (ASPS) Project under the Space Technology
Mission Directorate's Game Changing Development Program, which is
developing advanced electrochemical technologies for future NASA
exploration missions. Program Manager: John Lytle, PhD., NASA John H.
Glenn Research Center, 21000 Brookpark Rd., Cleveland, OH, 44135, USA.
NR 17
TC 1
Z9 1
U1 1
U2 16
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1572-6657
EI 1873-2569
J9 J ELECTROANAL CHEM
JI J. Electroanal. Chem.
PD JAN 15
PY 2015
VL 737
SI SI
BP 162
EP 173
DI 10.1016/j.jelechem.2014.09.009
PG 12
WC Chemistry, Analytical; Electrochemistry
SC Chemistry; Electrochemistry
GA CB3DL
UT WOS:000349508300019
ER
PT J
AU Nakashima, D
Ushikubo, T
Kita, NT
Weisberg, MK
Zolensky, ME
Ebel, DS
AF Nakashima, Daisuke
Ushikubo, Takayuki
Kita, Noriko T.
Weisberg, Michael K.
Zolensky, Michael E.
Ebel, Denton S.
TI Late formation of a comet Wild 2 crystalline silicate particle, Pyxie,
inferred from Al-Mg chronology of plagioclase
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Al-Mg isotope systematics; crystalline silicate; comet 81P/Wild 2; solar
system formation; Stardust
ID OXYGEN-ISOTOPE RESERVOIRS; SOLAR PROTOPLANETARY DISK; CR CHONDRITES;
HETEROGENEOUS DISTRIBUTION; AL-26-MG-26 SYSTEMATICS; CARBONACEOUS
CHONDRITES; PRIMITIVE METEORITES; CHONDRULES; STARDUST; NEBULA
AB We examined the Al-Mg isotope systematics of plagioclase in a FeO-poor ferromagnesian Wild 2 particle (0092,7,81,1,0; named Pyxie) using a similar to 2 mu m spot. Three analyses show average Al-27/Mg-24 ratio of similar to 65 and excess delta Mg-26* value of +0.1 +/- 4.5%0 (2 sigma), indicating no resolvable Mg-26 excess in the particle. The inferred initial (Al-26/Al-27)(0) ratio of plagioclase in Pyxie is estimated as (-0.6 +/- 4.5) x 10(-6) with an upper limit of 4 x 10(-6). The result is very similar to that of the FeO-rich ferromagnesian particle "Iris" (Ogliore et al., 2012). Assuming homogeneous distribution of Al-26 in the early solar system, Pyxie formed at least 2.6 Ma after the oldest Ca-Al-rich inclusions. This minimum formation age is marginally younger than formation ages of most chondrules in type similar to 3.0 chondrites but comparable with those of Mg# < 98 chondrules in CR3 chondrites. Considered in conjunction with similar oxygen isotope ratios between Pyxie (and Iris) and Mg# < 98 chondrules in CR3 chondrites, it is inferred that the ferromagnesian Wild 2 particles and Mg# < 98 chondrules in CR3 chondrites formed late in local disk environments that had similar oxygen isotope ratios and redox states. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Nakashima, Daisuke; Ushikubo, Takayuki; Kita, Noriko T.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53705 USA.
[Ushikubo, Takayuki] JAMSTEC, Kochi Inst Core Sample Res, Nankoku, Kochi 7838502, Japan.
[Weisberg, Michael K.] CUNY, Kingsborough Coll, Dept Phys Sci, Brooklyn, NY 11235 USA.
[Weisberg, Michael K.] CUNY, Grad Ctr, Brooklyn, NY 11235 USA.
[Weisberg, Michael K.; Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Zolensky, Michael E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Nakashima, D (reprint author), Tohoku Univ, Fac Sci, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
EM dnaka@m.tohoku.ac.jp
RI Kita, Noriko/H-8035-2016
OI Kita, Noriko/0000-0002-0204-0765
FU UW MRSEC [DMR-1121288]; UW NSEC [DMR-0832760]; NASA [NNX09AC30G,
NNX13AD15G, NNX10AI42G, NNX12AI06G]; NSF-EAR [0319230, 0744079, 1053466]
FX Two anonymous reviewers provided helpful comments that improved this
manuscript. The authors thank R.K. Noll for help with FIB and FE-SEM
observation, J. Thostenson (American Museum of Natural History) for
X-ray CT support, J. Kern for SIMS support, T.J. Tenner for discussion,
and R.C. Ogliore (University of Hawai'i) for kindly providing the Al-Mg
isotope data of the Wild 2 particle Iris. The Zeiss 1500XB CrossBeam
workstation at the University of Wisconsin is supported by the UW MRSEC
(DMR-1121288) and the UW NSEC (DMR-0832760). This work was supported by
NASA (NK: NNX09AC30G, NNX13AD15G; DSE: NNX10AI42G; MKW: NNX12AI06G;
Cosmochemistry for MEZ). WiscSIMS is partly supported by NSF-EAR
(0319230, 0744079, 1053466).
NR 86
TC 5
Z9 5
U1 1
U2 4
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 JAN 15
PY 2015
VL 410
BP 54
EP 61
DI 10.1016/j.epsl.2014.11.020
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CA8UM
UT WOS:000349196400006
ER
PT J
AU Usui, T
Alexander, CMO
Wang, JH
Simon, JI
Jones, JH
AF Usui, Tomohiro
Alexander, Cone M. O'D.
Wang, Jianhua
Simon, Justin I.
Jones, John H.
TI Meteoritic evidence for a previously unrecognized hydrogen reservoir on
Mars
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; shergottite; hydrogen isotope; ground ice; hydrated crust; ion
microprobe
ID PHYRIC SHERGOTTITE YAMATO-980459; HOSTED MELT INCLUSIONS; LARKMAN
NUNATAK 06319; MARTIAN METEORITES; SNC METEORITES; WATER RESERVOIRS;
SILICATE-GLASSES; ISOTOPE RATIOS; OLIVINE; MANTLE
AB Fluvial landforms on Mars suggest that it was once warm enough to maintain persistent liquid water on its surface. The transition to the present cold and dry Mars is closely linked to the history of surface water, yet the evolution of surficial water is poorly constrained. Based on in situ hydrogen isotope (D/H) analyses of quenched and impact glasses in Martian meteorites, we provide evidence for the existence of a distinct but ubiquitous water/ice reservoir (D/H = similar to 2-3 times Earth's ocean water) that lasted from at least the time when the meteorites crystallized (173-472 million years ago) to the time they were ejected by impacts (0.7-3.3 million years ago), but possibly much longer. The origin of this reservoir appears to predate the current Martian atmospheric water (D/H = similar to 5-6 times Earth's ocean water) and is unlikely to be a simple mixture of atmospheric and primordial water retained in the Martian mantle (D/H approximate to Earth's ocean water). This reservoir could represent hydrated crust and/or ground ice interbedded within sediments. Our results corroborate the hypothesis that a buried cryosphere accounts for a large part of the initial water budget of Mars. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Usui, Tomohiro] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Usui, Tomohiro] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Alexander, Cone M. O'D.; Wang, Jianhua] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Simon, Justin I.] NASA, Ctr Isotope Cosmochem & Geochronol, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA.
[Jones, John H.] NASA, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA.
RP Usui, T (reprint author), Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
EM tomohirousui@geo.titech.ac.jp
RI Wang, Jianhua/D-6500-2011;
OI Wang, Jianhua/0000-0002-7671-2413; Alexander, Conel/0000-0002-8558-1427
FU NASA Mars Fundamental Research Program grant [NNX11AF57G]; Astrobiology
Institute grant; Astromaterials Research and Exploration Sciences
Directorate at NASA Johnson Space Center
FX The NASA Antarctic Meteorite Collection and Curation group and the
National Institute of Polar Research, Japan are thanked for providing
the shergottite samples. We are grateful to B.M. Jakosky, L Hallis, and
an anonymous reviewer for constructive reviews, and T.M. Harrison for
editorial handling. Finally, TU thanks H. Kurokawa, M. Sato, J.M. Dohm,
and the members of Mars Science Team of Tokyo Tech, for insightful
discussions for this project. This work was supported by a NASA Mars
Fundamental Research Program grant (NNX11AF57G) to TU, an Astrobiology
Institute grant to CIW for CA and JW, and the Astromaterials Research
and Exploration Sciences Directorate at NASA Johnson Space Center.
NR 75
TC 19
Z9 19
U1 6
U2 24
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 JAN 15
PY 2015
VL 410
BP 140
EP 151
DI 10.1016/j.epsl.2014.11.022
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CA8UM
UT WOS:000349196400014
ER
PT J
AU Chaban, GM
Wang, DY
Huo, WM
AF Chaban, Galina M.
Wang, Dunyou
Huo, Winifred M.
TI Ab Initio Study of Guanine Damage by Hydroxyl Radical
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID UNIMOLECULAR TRANSFORMATION REACTIONS; ISOMERIC OH ADDUCTS;
AQUEOUS-SOLUTION; MOLECULAR-DYNAMICS; CENTER-DOT; IONIZING-RADIATION;
DNA-DAMAGE; 1ST STEPS; PATTERN; NUCLEOSIDES
AB Multiconfigurational ab initio methods are used in this study to examine two initial reactions that take place during the OH radical attack of the DNA base guanine: a ring opening reaction and a hydrogen transfer reaction. The same reactions are also studied in the presence of a single water molecule. The ring opening reaction has a moderate barrier height of similar to 20-25 kcal/mol that is relatively insensitive to the presence of water. The barrier of the H-transfer reaction, on the other hand, is lowered from similar to 50 to similar to 22 kcal/mol when one water molecule is added, thus becoming comparable to the barrier height of the ring opening reaction.
C1 [Chaban, Galina M.; Huo, Winifred M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wang, Dunyou] Shandong Normal Univ, Jinan 250014, Shangdong, Peoples R China.
RP Chaban, GM (reprint author), NASA, Ames Res Ctr, Mail Stop 258-1,POB 1, Moffett Field, CA 94035 USA.
EM galina.m.chaban@nasa.gov
NR 31
TC 2
Z9 2
U1 3
U2 28
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 JAN 15
PY 2015
VL 119
IS 2
BP 377
EP 382
DI 10.1021/jp508771g
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA AZ2XU
UT WOS:000348093500014
PM 25517252
ER
PT J
AU Vadrevu, KP
Justice, C
Prasad, T
Prasad, N
Gutman, G
AF Vadrevu, Krishna Prasad
Justice, Chris
Prasad, Thenkabail
Prasad, Narasimha
Gutman, Garik
TI Land cover/land use change and impacts on environment in South Asia
SO JOURNAL OF ENVIRONMENTAL MANAGEMENT
LA English
DT Editorial Material
ID CLIMATE-CHANGE
C1 [Vadrevu, Krishna Prasad; Justice, Chris] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Prasad, Thenkabail] US Geol Survey, Tucson, AZ USA.
[Prasad, Narasimha] Ctr Water Resources Dev & Management, Kozhikode, Kerala, India.
[Gutman, Garik] NASA Headquarters, Washington, DC USA.
RP Vadrevu, KP (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
NR 5
TC 3
Z9 3
U1 1
U2 21
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0301-4797
EI 1095-8630
J9 J ENVIRON MANAGE
JI J. Environ. Manage.
PD JAN 15
PY 2015
VL 148
SI SI
BP 1
EP 3
DI 10.1016/j.jenvman.2014.12.005
PG 3
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AZ1RU
UT WOS:000348016400001
PM 25500155
ER
PT J
AU Justice, C
Gutman, G
Vadrevu, KP
AF Justice, Chris
Gutman, Garik
Vadrevu, Krishna Prasad
TI NASA Land Cover and Land Use Change (LCLUC): An interdisciplinary
research program
SO JOURNAL OF ENVIRONMENTAL MANAGEMENT
LA English
DT Article
ID REMOTELY-SENSED DATA; SATELLITE DATA; UNITED-STATES; DATA SETS;
DYNAMICS; FORESTS; DEFORESTATION; PRODUCTS; FUTURE; SCALE
AB Understanding Land Cover/Land Use Change (LCLUC) in diverse regions of the world and at varied spatial scales is one of the important challenges in global change research. In this article, we provide a brief overview of the NASA LCLUC program, its focus areas, and the importance of satellite remote sensing observations in LCLUC research including future directions. The LCLUC Program was designed to be a cross-cutting theme within NASA's Earth Science program. The program aims to develop and use remote sensing technologies to improve understanding of human interactions with the environment. Since 1997, the NASA LCLUC program has supported nearly 280 research projects on diverse topics such as forest loss and carbon, urban expansion, land abandonment, wetland loss, agricultural land use change and land use change in mountain systems. The NASA LCLUC program emphasizes studies where land-use changes are rapid or where there are significant regional or global LCLUC implications. Over a period of years, the LCLUC program has contributed to large regional science programs such as Land Biosphere-Atmosphere (LBA), the Northern Eurasia Earth Science Partnership Initiative (NEESPI), and the Monsoon Area Integrated Regional Study (MAIRS). The primary emphasis of the program will remain on using remote sensing datasets for LCLUC research. The program will continue to emphasize integration of physical and social sciences to address regional to global scale issues of LCLUC for the benefit of society. (C) 2014 Published by Elsevier Ltd.
C1 [Justice, Chris; Vadrevu, Krishna Prasad] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Gutman, Garik] NASA Headquarters, Washington, DC USA.
RP Justice, C (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
NR 68
TC 2
Z9 2
U1 4
U2 26
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0301-4797
EI 1095-8630
J9 J ENVIRON MANAGE
JI J. Environ. Manage.
PD JAN 15
PY 2015
VL 148
SI SI
BP 4
EP 9
DI 10.1016/j.jenvman.2014.12.004
PG 6
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AZ1RU
UT WOS:000348016400002
PM 25500156
ER
PT J
AU Evirgen, A
Karaman, I
Santamarta, R
Pons, J
Noebe, RD
AF Evirgen, A.
Karaman, I.
Santamarta, R.
Pons, J.
Noebe, R. D.
TI Microstructural characterization and shape memory characteristics of the
Ni50.3Ti34.7Hf15 shape memory alloy
SO ACTA MATERIALIA
LA English
DT Article
DE NiTiHf; Martensitic transformation; Precipitation; Microstructure;
Transformation characteristics
ID SEVERE PLASTIC-DEFORMATION; TITANIUM SINGLE-CRYSTALS;
MARTENSITIC-TRANSFORMATION; CYCLIC REVERSIBILITY; COMPRESSIVE RESPONSE;
PHASE-TRANSFORMATION; MECHANICAL-BEHAVIOR; ELECTRON-MICROSCOPY; HF
ALLOYS; NITI
AB The effect of precipitation on the microstructure and shape memory characteristics of the Ni50.3Ti34.7Hf15 shape memory alloy has been investigated via transmission electron microscopy, differential scanning calorimetry and load-biased thermal cycling tests in tension. A one-stage martensitic transformation from B2 austenite to B19' martensite was observed in all the aged samples but the transformation temperatures followed a more complicated trend depending on specific aging conditions. The transformation temperatures decreased below room temperature when the precipitate size, and thus the interparticle distance, was below similar to 20 nm, as occurred after short aging times at low temperatures. On the other hand, the transformation temperatures can be increased over a wide temperature range by increasing the precipitate size and volume fraction through aging for long durations or at higher temperatures. The alloy demonstrated excellent dimensional stability under stress levels as high as 300 MPa as a consequence of precipitation hardening, with a maximum fully recoverable strain of 3.3% after aging at 450 degrees C for 10 h. The transformation thermal hysteresis also decreased in the aged samples due to reduced defect generation in the precipitation-strengthened samples. The precipitate crystal structure was identified as the H-phase that was recently reported in Ni-rich NiTiHf and NiTiZr alloys, and not the Ni4Ti3-type structure as reported in a few earlier studies. The H-phase present in the Ni-rich NiTiHf alloy does not change the twinning relations in the B19' martensite phase compared to (Ti + Hf)-rich NiTiHf alloys, being a mixture of (0 0 1) compound twins and (0 1 1) Type I twins. On the other hand, the precipitates have a significant effect on martensite morphology and load-biased thermal cycling response, both of which can be manipulated by controlling the precipitate size. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Evirgen, A.; Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
[Santamarta, R.; Pons, J.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
[Noebe, R. D.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Karaman, I (reprint author), Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
EM ikaraman@tamu.edu
RI Karaman, Ibrahim/E-7450-2010; Santamarta, Ruben/K-7865-2016
OI Karaman, Ibrahim/0000-0001-6461-4958; Santamarta,
Ruben/0000-0003-3341-5758
FU US Air Force Office of Scientific Research [FA9550-12-1-0218]; National
Science Foundation [DMR 08-44082]; International Materials Institute for
Multi-functional Materials for Energy Conversion (IIMEC) at Texas AM
University; Spanish MINECO; FEDER [MAT2011-28217-C02-01]; NASA
Fundamental Aeronautics Program, Aeronautical Sciences Project
FX This work was supported by the US Air Force Office of Scientific
Research, under Grant No. FA9550-12-1-0218 and additional support was
received from the National Science Foundation under Grant No. DMR
08-44082, which supports the International Materials Institute for
Multi-functional Materials for Energy Conversion (IIMEC) at Texas A&M
University. Spanish MINECO and FEDER under Project No.
MAT2011-28217-C02-01 are also acknowledged for their partial financial
support. R.D.N. gratefully acknowledges support from the NASA
Fundamental Aeronautics Program, Aeronautical Sciences Project.
NR 70
TC 12
Z9 12
U1 13
U2 62
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD JAN 15
PY 2015
VL 83
BP 48
EP 60
DI 10.1016/j.actamat.2014.09.027
PG 13
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AY5AL
UT WOS:000347585800006
ER
PT J
AU Bierkens, MFP
Bell, VA
Burek, P
Chaney, N
Condon, LE
David, CH
de Roo, A
Doll, P
Drost, N
Famiglietti, JS
Florke, M
Gochis, DJ
Houser, P
Hut, R
Keune, J
Kollet, S
Maxwell, RM
Reager, JT
Samaniego, L
Sudicky, E
Sutanudjaja, EH
van de Giesen, N
Winsemius, H
Wood, EF
AF Bierkens, Marc F. P.
Bell, Victoria A.
Burek, Peter
Chaney, Nathaniel
Condon, Laura E.
David, Cedric H.
de Roo, Ad
Doell, Petra
Drost, Niels
Famiglietti, James S.
Floerke, Martina
Gochis, David J.
Houser, Paul
Hut, Rolf
Keune, Jessica
Kollet, Stefan
Maxwell, Reed M.
Reager, John T.
Samaniego, Luis
Sudicky, Edward
Sutanudjaja, Edwin H.
van de Giesen, Nick
Winsemius, Hessel
Wood, Eric F.
TI Hyper-resolution global hydrological modelling: what is next?
"Everywhere and locally relevant"
SO HYDROLOGICAL PROCESSES
LA English
DT Editorial Material
ID SOIL-MOISTURE; WATER FLUXES; LAND WATER; FLOOD RISK; SCALE; PARALLEL;
NETWORK; SYSTEM; ENERGY; UNCERTAINTY
C1 [Bierkens, Marc F. P.; Sutanudjaja, Edwin H.] Univ Utrecht, Utrecht, Netherlands.
[Bell, Victoria A.] Ctr Ecol & Hydrol, Wallingford, Oxon, England.
[Burek, Peter; de Roo, Ad] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy.
[Chaney, Nathaniel; Wood, Eric F.] Princeton Univ, Princeton, NJ 08544 USA.
[Condon, Laura E.; Maxwell, Reed M.] Colorado Sch Mines, Integrated Ground Water Modeling Ctr, Golden, CO 80401 USA.
[David, Cedric H.; Famiglietti, James S.; Reager, John T.] Univ Calif Irvine, Ctr Hydrol Modeling, Irvine, CA USA.
[David, Cedric H.; Famiglietti, James S.; Reager, John T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Doell, Petra] Goethe Univ Frankfurt, D-60054 Frankfurt, Germany.
[Drost, Niels] Netherlands eSci Ctr, Amsterdam, Netherlands.
[Floerke, Martina] Univ Kassel, D-34125 Kassel, Germany.
[Gochis, David J.] NCAR HR Reg Modelling, Boulder, CO USA.
[Houser, Paul] George Mason Univ, Fairfax, VA 22030 USA.
[Hut, Rolf; van de Giesen, Nick; Winsemius, Hessel] Delft Univ Technol, Delft, Netherlands.
[Keune, Jessica; Kollet, Stefan] Forschungszentrum Julich, Agrosphere IBG 3, D-52425 Julich, Germany.
[Samaniego, Luis] UFZ Helmholtz Ctr Environm Res, Leipzig, Germany.
[Sudicky, Edward] Univ Waterloo, Waterloo, ON N2L 3G1, Canada.
[Bierkens, Marc F. P.; Winsemius, Hessel] Deltares, Delft, Netherlands.
[Kollet, Stefan] Geoverbund ABC J, Ctr High Performance Sci Comp Terr Syst, Julich, Germany.
RP Bierkens, MFP (reprint author), Univ Utrecht, Utrecht, Netherlands.
EM m.f.p.bierkens@uu.nl
RI van de Giesen, Nick/B-5010-2008; Maxwell, Reed/D-7980-2013; Chaney,
Nathaniel /L-9110-2015; Samaniego, Luis/G-8651-2011; Doll,
Petra/A-3784-2009; Bell, Victoria /K-1857-2012;
OI van de Giesen, Nick/0000-0002-7200-3353; Maxwell,
Reed/0000-0002-1364-4441; Chaney, Nathaniel /0000-0001-7120-1713;
Samaniego, Luis/0000-0002-8449-4428; Doll, Petra/0000-0003-2238-4546;
Drost, Niels/0000-0001-9795-7981; Keune, Jessica/0000-0001-6104-2165;
David, Cedric/0000-0002-0924-5907
NR 71
TC 37
Z9 37
U1 4
U2 48
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 JAN 15
PY 2015
VL 29
IS 2
BP 310
EP 320
DI 10.1002/hyp.10391
PG 11
WC Water Resources
SC Water Resources
GA AY8OO
UT WOS:000347813300012
ER
PT J
AU Zhang, QY
Cheng, YB
Lyapustin, AI
Wang, YJ
Zhang, XY
Suyker, A
Verma, S
Shuai, YM
Middleton, EM
AF Zhang, Qingyuan
Cheng, Yen-Ben
Lyapustin, Alexei I.
Wang, Yujie
Zhang, Xiaoyang
Suyker, Andrew
Verma, Shashi
Shuai, Yanmin
Middleton, Elizabeth M.
TI Estimation of crop gross primary production (GPP): II. Do scaled MODIS
vegetation indices improve performance?
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Daily GPP; MODIS; Vegetation index; fAPAR(chl)
ID PHOTOSYNTHETICALLY ACTIVE RADIATION; LIGHT-USE EFFICIENCY; LEAF-AREA
INDEX; TERRESTRIAL BIOPHYSICAL PARAMETERS; REMOTE ESTIMATION; CANOPY
REFLECTANCE; SATELLITE DATA; CHLOROPHYLL FAPAR(CHL); GLOBAL FIELDS;
LANDSAT DATA
AB Satellite remote sensing estimates of gross primary production (GPP) have routinely been made using spectral vegetation indices (VIs) over the past two decades. The Normalized Difference Vegetation Index (NDVI), the Enhanced Vegetation Index (EVI), the green band Wide Dynamic Range Vegetation Index (WDRVIgreen), and the green band Chlorophyll Index (CIgreen) have been employed to estimate GPP under the assumption that GPP is proportional to the product of VI and photosynthetically active radiation (PAR) (where VI is one of four VIs: NDVI, EVI,WDRVIgreen, or Queen). However, the empirical regressions between VI*PAR and GPP measured locally at flux towers do not pass through the origin (i.e., the zero X-Y value for regressions). Therefore they are somewhat difficult to interpret and apply. This study investigates (1) what are the scaling factors and offsets (i.e., regression slopes and intercepts) between the fraction of PAR absorbed by chlorophyll of a canopy (fAPAR(chl)) and the VIs and (2) whether the scaled VIs developed in (I) can eliminate the deficiency and improve the accuracy of GPP estimates. Three AmeriFlux maize and soybean fields were selected for this study, two of which are irrigated and one is rainfed. The four VIs and fAPAR(chl) of the fields were computed with the MODerate resolution Imaging Spectroradiometer (MODIS)satellite images. The GPP estimation performance for the scaled VIs was compared to results obtained with the original VIs and evaluated with standard statistics: the coefficient of determination (R-2), the root mean square error (RMSE), and the coefficient of variation (CV). Overall, the scaled EVI obtained the best performance. The performance of the scaled NDVI, EVI and WDRVIgreen was improved across sites, crop types and soil/background wetness conditions. The scaled CIgreen did not improve results, compared to the original CIgreen. The scaled green band indices (WDRVIgreen, CIgreen) did not exhibit superior performance to either the scaled EVI or NDVI in estimating crop daily GPP at these agricultural fields. The scaled VIs are more physiologically meaningful than original un-scaled VIs, but scaling factors and offsets may vary across crop types and surface conditions. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Zhang, Qingyuan; Cheng, Yen-Ben; Wang, Yujie; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Cheng, Yen-Ben] Sigma Space Corp, Lanham, MD 20706 USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
[Wang, Yujie] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Zhang, Xiaoyang] S Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA.
[Suyker, Andrew; Verma, Shashi] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA.
[Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA.
RP Zhang, QY (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Bldg 33,Room G317,Code 618, Greenbelt, MD 20771 USA.
EM qyz72@yahoo.com
FU NASA Terrestrial Ecology Project [NNX12AJ51G]; NASA Science of Terra and
Aqua Project [NNX14AK50G]; Carbon Dioxide Information Analysis Center at
the Oak Ridge National Laboratory of the Department of Energy
FX This study was supported by NASA Terrestrial Ecology Project (Grant No.
NNX12AJ51G; PI, Q. Zhang) and NASA Science of Terra and Aqua Project
(Grant No. NNX14AK50G; PI, Q Zhang) (Dr. Diane Wickland, Manager). We
would like to thank the support and the use of facilities and equipment
provided by the Center for Advanced Land Management Information
Technologies and the Carbon Sequestration program, University of
Nebraska-Lincoln. Site-specific climate and CO2 flux data are
distributed by AmeriFlux network (http://public.ornl.gov/ameriflux),
supported by Carbon Dioxide Information Analysis Center at the Oak Ridge
National Laboratory of the Department of Energy. We are grateful to
anonymous reviewers whose comments helped improve the paper.
NR 78
TC 12
Z9 12
U1 4
U2 29
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD JAN 15
PY 2015
VL 200
BP 1
EP 8
DI 10.1016/j.agrformet.2014.09.003
PG 8
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA AY4ZB
UT WOS:000347582300001
ER
PT J
AU Ruane, AC
Goldberg, R
Chryssanthacopoulos, J
AF Ruane, Alex C.
Goldberg, Richard
Chryssanthacopoulos, James
TI Climate forcing datasets for agricultural modeling: Merged products for
gap-filling and historical climate series estimation
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Climate forcing data; Daily climate series; Climate change; AgMIP;
Climate impacts; Agriculture
ID CONTINENTAL UNITED-STATES; GLOBAL PRECIPITATION; GRIDDED PRECIPITATION;
REANALYSIS; RESOLUTION; TEMPERATURE; PROJECT; WATER; PERFORMANCE; SYSTEM
AB The AgMERRA and AgCFSR climate forcing datasets provide daily, high-resolution, continuous, meteorological series over the 1980-2010 period designed for applications examining the agricultural impacts of climate variability and climate change. These datasets combine daily resolution data from retrospective analyses (the Modern-Era Retrospective Analysis for Research and Applications, MERRA, and the Climate Forecast System Reanalysis, CFSR) with in situ and remotely-sensed observational datasets for temperature, precipitation, and solar radiation, leading to substantial reductions in bias in comparison to a network of 2324 agricultural-region stations from the Hadley Integrated Surface Dataset (HadISD). Results compare favorably against the original reanalyses as well as the leading climate forcing datasets (Princeton, WFD, WFD-EI, and GRASP), and AgMERRA distinguishes itself with substantially improved representation of daily precipitation distributions and extreme events owing to its use of the MERRA-Land dataset. These datasets also peg relative humidity to the maximum temperature time of day, allowing for more accurate representation of the diurnal cycle of near-surface moisture in agricultural models. AgMERRA and AgCFSR enable a number of ongoing investigations in the Agricultural Model Intercomparison and Improvement Project (AgMIP) and related research networks, and may be used to fill gaps in historical observations as well as a basis for the generation of future climate scenarios. Published by Elsevier B.V.
C1 [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Goldberg, Richard; Chryssanthacopoulos, James] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Ruane, AC (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM alexander.c.ruane@nasa.gov
FU UK Department for International Development; NASA Modeling, Analysis,
and Prediction Program; NASA's Indicators for the National Climate
Assessment Program; NASA Gulf of Mexico Initiative [NNX10AO10G]
FX We thank the members of the AgMIP Climate Team who have contributed to
the development and evaluation of AgMERRA and AgCFSR through
applications around the world. We appreciate discussions we held with
Cynthia Rosenzweig, Jonathan Winter, Sonali McDermid, Joshua Elliott,
DeWayne Cecil, Toshichika Iizumi, Justin Sheffield, Michael Bosilovich,
Ken Boote, and Nicholas Hudson that led to improvements in the
development and orientation of these datasets and this manuscript. We
acknowledge Joshua Elliott's assistance in preparing the existing
climate forcing datasets for comparison, and recognize the importance of
helpful comments from two reviewers. We are grateful for AgMIP support
from the UK Department for International Development and the support
provided by the NASA Modeling, Analysis, and Prediction Program, NASA's
Indicators for the National Climate Assessment Program, and the NASA
Gulf of Mexico Initiative (NNX10AO10G).
NR 61
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U1 6
U2 26
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD JAN 15
PY 2015
VL 200
BP 233
EP 248
DI 10.1016/j.agrformet.2014.09.016
PG 16
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA AY4ZB
UT WOS:000347582300023
ER
PT J
AU Shojan, J
Chitturi, VR
Soler, J
Resto, O
West, WC
Katiyar, RS
AF Shojan, Jifi
Chitturi, Venkateswara Rao
Soler, Jess
Resto, Oscar
West, William C.
Katiyar, Ram S.
TI High energy xLi(2)MnO(3)-(1-x)LiNi2/3Co1/6Mn1/6O2 composite cathode for
advanced Li-ion batteries
SO JOURNAL OF POWER SOURCES
LA English
DT Article
DE Composite cathode; Li-ion batteries; Raman spectroscopy; Rate
capability; Microscopy
ID RECHARGEABLE LITHIUM BATTERIES; SOLUTION LI2MNO3-LIMO2 M;
ELECTROCHEMICAL-BEHAVIOR; ELECTRODE MATERIALS; SOLID-SOLUTION; X-RAY;
MN; NI; CO; STORAGE
AB Novel composite cathode materials, xLi(2)MnO(3)-(1-x)LiNi2/3Co1/6Mn1/6O2 (where x = 0.3, 0.5, and 0.7), were synthesized by sal-gel route and characterized by advanced techniques for rechargeable Li-ion battery applications. Phase purity of the composites was examined by XRD as well as Raman spectroscopy and the studies revealed good crystallinity and the formation of pure composite phases with monoclinic (C2/m) and hexagonal (R3m) crystal structures for Li2MnO3 and LiNi2/3Co1/6Mn1/6O2, respectively. Polyhedral agglomerates seen in the scanning and transmission electron microscopic images elucidated the better electrochemical properties of the composites. Valence states of transition metals in the composites were examined by X-ray photoelectron spectroscopy and the analysis suggested predominant oxidation states of Ni, Co, and Mn as 2+, 3+, and 4+, respectively. Galvanostatic charge-discharge tests, performed at different C-rates between 2.0 and 4.8 V, indicated high discharge capacity (similar to 250 mAh g(-1)), good rate capability, and excellent cycleability of the composite with x = 0.5 compared to the composites with x = 0.3 and 0.7. In-situ Raman spectroscopic studies revealed the activation of Li2MnO3 component in all composite cathode materials during the first cycle charging process with structural stability thereby enhancing performance of the composite with x = 0.5. These results demonstrated the feasibility of using 0.5Li(2)MnO(3)-0.5LiNi(2/3)Co(1/6)Mn(1/6)O(2) composite as advanced cathode for high power Li-ion batteries. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Shojan, Jifi; Chitturi, Venkateswara Rao; Resto, Oscar; Katiyar, Ram S.] Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA.
[Shojan, Jifi; Chitturi, Venkateswara Rao; Resto, Oscar; Katiyar, Ram S.] Univ Puerto Rico, Inst Funct Nanomat, San Juan, PR 00936 USA.
[Soler, Jess; West, William C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chitturi, VR (reprint author), Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA.
EM vrao.chitturi@ymail.com; rkatiyar@hpcf.upr.edu
FU NASA-URC [NNX10AQ17A]
FX The financial support from NASA-URC (#NNX10AQ17A) grant to University of
Puerto Rico is gratefully acknowledged. This work was partially carried
out at Jet Propulsion Laboratory, California Institute of Technology,
under a contract from NASA's Space Power Systems Program. The authors
would like to acknowledge the help of Dr. Esteban Fachini for XPS
measurements and Nanoscopy facility at UPR for SEM and TEM measurements.
NR 47
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U1 5
U2 70
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-7753
EI 1873-2755
J9 J POWER SOURCES
JI J. Power Sources
PD JAN 15
PY 2015
VL 274
BP 440
EP 450
DI 10.1016/j.jpowsour.2014.10.032
PG 11
WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials
Science, Multidisciplinary
SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science
GA AY0DT
UT WOS:000347268700053
ER
PT J
AU Grundy, W
Stern, A
Bagenal, F
Gladstone, R
Buratti, B
AF Grundy, Will
Stern, Alan
Bagenal, Fran
Gladstone, Randy
Buratti, Bonnie
TI Introduction to the Pluto system science special issue
SO ICARUS
LA English
DT Editorial Material
C1 [Grundy, Will] Lowell Observ, Flagstaff, AZ 86001 USA.
[Stern, Alan] SW Res Inst, Boulder, CO USA.
[Bagenal, Fran] Univ Colorado, Boulder, CO 80309 USA.
[Gladstone, Randy] SW Res Inst, San Antonio, TX USA.
[Buratti, Bonnie] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Grundy, W (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
EM w.grundy@lowell.edu; alan@boulder.swri.edu; bagenal@colorado.edu;
rgladstone@swri.edu; bonnie.buratti@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 1
EP 1
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800001
ER
PT J
AU Rhoden, AR
Henning, W
Hurford, TA
Hamilton, DP
AF Rhoden, Alyssa Rose
Henning, Wade
Hurford, Terry A.
Hamilton, Douglas P.
TI The interior and orbital evolution of Charon as preserved in its
geologic record
SO ICARUS
LA English
DT Article
DE Charon; Rotational dynamics; Tectonics; Pluto, satellites; Satellites,
surfaces
ID KUIPER-BELT OBJECTS; GIANT IMPACT ORIGIN; NONSYNCHRONOUS ROTATION;
PLUTO-CHARON; TIDAL STRESSES; SOUTH-POLE; CRACK AZIMUTHS; ICE SHELLS;
EUROPA; ENCELADUS
AB Pluto and its largest satellite, Charon, currently orbit in a mutually synchronous state; both bodies continuously show the same face to one another. This orbital configuration is a natural end-state for bodies that have undergone tidal dissipation. In order to achieve this state, both bodies would have experienced tidal heating and stress, with the extent of tidal activity controlled by the orbital evolution of Pluto and Charon and by the interior structure and rheology of each body. As the secondary, Charon would have experienced a larger tidal response than Pluto, which may have manifested as observable tectonism. Unfortunately, there are few constraints on the interiors of Pluto and Charon. In addition, the pathway by which Charon came to occupy its present orbital state is uncertain. If Charon's orbit experienced a high-eccentricity phase, as suggested by some orbital evolution models, tidal effects would have likely been more significant. Therefore, we determine the conditions under which Charon could have experienced tidally-driven geologic activity and the extent to which upcoming New Horizons spacecraft observations could be used to constrain Charon's internal structure and orbital evolution. Using plausible interior structure models that include an ocean layer, we find that tidally-driven tensile fractures would likely have formed on Charon if its eccentricity were on the order of 0.01, especially if Charon were orbiting closer to Pluto than at present. Such fractures could display a variety of azimuths near the equator and near the poles, with the range of azimuths in a given region dependent on longitude; east-west-trending fractures should dominate at mid-latitudes. The fracture patterns we predict indicate that Charon's surface geology could provide constraints on the thickness and viscosity of Charon's ice shell at the time of fracture formation. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Rhoden, Alyssa Rose; Henning, Wade; Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Henning, Wade; Hamilton, Douglas P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Rhoden, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM Alyssa.R.Rhoden@nasa.gov
RI Hurford, Terry/F-2625-2012
NR 82
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U1 3
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 11
EP 20
DI 10.1016/j.icarus.2014.04.030
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800003
ER
PT J
AU Moore, JM
Howard, AD
Schenk, PM
McKinnon, WB
Pappalardo, RT
Ewing, RC
Bierhaus, EB
Bray, VJ
Spencer, JR
Binzel, RP
Buratti, B
Grundy, WM
Olkin, CB
Reitsema, HJ
Reuter, DC
Stern, SA
Weaver, H
Young, LA
Beyer, RA
AF Moore, Jeffrey M.
Howard, Alan D.
Schenk, Paul M.
McKinnon, William B.
Pappalardo, Robert T.
Ewing, Ryan C.
Bierhaus, Edward B.
Bray, Veronica J.
Spencer, John R.
Binzel, Richard P.
Buratti, Bonnie
Grundy, William M.
Olkin, Catherine B.
Reitsema, Harold J.
Reuter, Dennis C.
Stern, S. Alan
Weaver, Harold
Young, Leslie A.
Beyer, Ross A.
TI Geology before Pluto: Pre-encounter considerations
SO ICARUS
LA English
DT Article
DE Pluto; Pluto, satellites; Pluto, surface; Charon; Satellites, surfaces
ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; GALILEO NOMINAL MISSION; LARGE
IMPACT FEATURES; ICY SATELLITES; CHARON SYSTEM; CASSINI RADAR; DOME
CRATERS; SURFACE AGE; GANYMEDE
AB The cameras of New Horizons will provide robust data sets that should be imminently amenable to geological analysis of the Pluto system's landscapes. In this paper, we begin with a brief discussion of the planned observations by the New Horizons cameras that will bear most directly on geological interpretability. Then we broadly review the major geological processes that could potentially operate on the surfaces of Pluto and its major moon Charon. We first survey exogenic processes (i.e. those for which energy for surface modification is supplied externally to the planetary surface): impact cratering, sedimentary processes (including volatile migration), and the work of wind. We conclude with an assessment of the prospects for endogenic activity in the form of tectonics and cryovolcanism. Published by Elsevier Inc.
C1 [Moore, Jeffrey M.; Beyer, Ross A.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[McKinnon, William B.] Washington Univ, McDonnell Ctr Space Sci, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Div Sci, Pasadena, CA 91109 USA.
[Ewing, Ryan C.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA.
[Bierhaus, Edward B.] Lockheed Martin Corp, Space Explorat Syst, Bethesda, MD 20817 USA.
[Bray, Veronica J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spencer, John R.; Olkin, Catherine B.; Stern, S. Alan; Young, Leslie A.] SW Res Inst, Boulder, CO 80302 USA.
[Binzel, Richard P.] MIT, Cambridge, MA 02139 USA.
[Buratti, Bonnie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grundy, William M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Reitsema, Harold J.] B612 Fdn, Mill Valley, CA 94941 USA.
[Reuter, Dennis C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weaver, Harold] Johns Hopkins Univ, Dept Space, Appl Phys Lab, Laurel, MD 20723 USA.
[Beyer, Ross A.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
RP Moore, JM (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM jeff.moore@nasa.gov
RI Weaver, Harold/D-9188-2016;
OI Olkin, Catherine/0000-0002-5846-716X; Howard, Alan/0000-0002-5423-1600
FU New Horizons project
FX We are especially grateful for the formal reviews of Ross Irwin and an
anonymous reviewer whose comments substantially improved this report.
Much of the material in this paper was originally presented at the "New
Horizons Workshop on Icy Surface Processes" held at Flagstaff, Arizona
in August 2011, and "The Pluto System on the Eve of Exploration by New
Horizons: Perspectives and Predictions" conference held at Laurel,
Maryland in July 2013. This work was, in part, supported by the New
Horizons project.
NR 131
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 65
EP 81
DI 10.1016/j.icarus.2014.04.028
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800007
ER
PT J
AU Cruikshank, DP
Grundy, WM
DeMeo, FE
Buie, MW
Binzel, RP
Jennings, DE
Olkin, CB
Parker, JW
Reuter, DC
Spencer, JR
Stern, SA
Young, LA
Weaver, HA
AF Cruikshank, D. P.
Grundy, W. M.
DeMeo, F. E.
Buie, M. W.
Binzel, R. P.
Jennings, D. E.
Olkin, C. B.
Parker, J. W.
Reuter, D. C.
Spencer, J. R.
Stern, S. A.
Young, L. A.
Weaver, H. A.
TI The surface compositions of Pluto and Charon
SO ICARUS
LA English
DT Article
DE Pluto, surface; Charon; Spectroscopy; Satellites, composition
ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; NEAR-INFRARED SPECTROSCOPY;
DWARF PLANET ERIS; 5 MU-M; OPTICAL-CONSTANTS; ION IRRADIATION;
CRYSTALLINE H2O-ICE; NITROGEN ICE; CASSINI-VIMS
AB The surface of Pluto as it is understood on the eve of the encounter of the New Horizons spacecraft (mid-2015) consists of a spatially heterogeneous mix of solid N-2, CH4, CO, C2H6, and an additional component that imparts color, and may not be an ice. The known molecular ices are detected by near-infrared spectroscopy. The N-2 ice occurs in the hexagonal crystalline beta-phase, stable at T > 35.6 K. Spectroscopic evidence for wavelength shifts in the CH4 bands attests to the complex mixing of CH4 and N-2 in the solid state, in accordance with the phase diagram for N-2 + CH4. Spectra obtained at several aspects of Pluto's surface as the planet rotates over its 6.4-day period show variability in the distribution of CH4 and N-2 ices, with stronger CH4 absorption bands associated with regions of higher albedo, in correlation with the visible rotational light curve. CO and N-2 ice absorptions are also strongly modulated by the rotation period; the bands are strongest on the anti-Charon hemisphere of Pluto. Longer term changes in the strengths of Pluto's absorption bands occur as the viewing geometry changes on seasonal time-scales, although a complete cycle has not been observed. The non-ice component of Pluto's surface may be a relatively refractory material produced by the UV and cosmic-ray irradiation of the surface ices and gases in the atmosphere, although UV does not generally penetrate the atmospheric CH4 to interact with the surface. Laboratory simulations indicate that a rich chemistry ensues by the irradiation of mixtures of the ices known to occur on Pluto, but specific compounds have not yet been identified in spectra of the planet. Charon's surface is characterized by spectral bands of crystalline H2O ice, and a band attributed to one or more hydrates of NH3. Amorphous H2O ice may also be present; the balance between the amorphization and crystallization processes on Charon remains to be clarified. The albedo of Charon and its generally spatially uniform neutral color indicate that a component, not yet identified, is mixed in some way with the H2O and NH3 center dot nH(2)O ices. Among the many known small bodies in the transneptunian region, several share characteristics with Pluto and Charon, including the presence of CH4, N-2, C2H6, H2O ices, as well as components that yield a wide variety of surface albedo and color. The New Horizons investigation of the Pluto-Charon system will generate new insight into the physical properties of the broader transneptunian population, and eventually to the corresponding bodies expected in the numerous planetary systems currently being discovered elsewhere in the Galaxy. Published by Elsevier Inc.
C1 [Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Grundy, W. M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[DeMeo, F. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buie, M. W.; Olkin, C. B.; Parker, J. W.; Spencer, J. R.; Stern, S. A.; Young, L. A.] SW Res Inst, Boulder, CO 80302 USA.
[Binzel, R. P.] MIT, Cambridge, MA 02139 USA.
[Jennings, D. E.; Reuter, D. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weaver, H. A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM Dale.P.Cruikshank@nasa.gov
RI Weaver, Harold/D-9188-2016
NR 139
TC 19
Z9 19
U1 5
U2 51
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 JAN 15
PY 2015
VL 246
BP 82
EP 92
DI 10.1016/j.icarus.2014.05.023
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800008
ER
PT J
AU French, RG
Toigo, AD
Gierasch, PJ
Hansen, CJ
Young, LA
Sicardy, B
Dias-Oliveira, A
Guzewich, SD
AF French, Richard G.
Toigo, Anthony D.
Gierasch, Peter J.
Hansen, Candice J.
Young, Leslie A.
Sicardy, Bruno
Dias-Oliveira, Alex
Guzewich, Scott D.
TI Seasonal variations in Pluto's atmospheric tides
SO ICARUS
LA English
DT Article
DE Pluto, atmosphere; Tides, atmospheric; Occultations; Atmospheres,
dynamics; Pluto
ID STELLAR OCCULTATION; THERMAL STRUCTURE; GRAVITY-WAVES; STRATOSPHERE;
ABUNDANCE; SURFACES; DENSITY; METHANE; MODEL
AB Pluto's tenuous atmosphere exhibits remarkable seasonal change as a result of the planet's substantial obliquity and highly eccentric orbit. Over the past two decades, occultations have revealed that the atmospheric pressure on Pluto has increased substantially, perhaps by a factor as large as 2 to 4, as the planet has moved from equinox towards solstice conditions. These data have also shown variations in the strength of the dynamical activity in the atmosphere, as revealed by the varying abundance and amplitude of spikes in the occultation light curves resulting from refractive focussing by atmospheric waves. Toigo et al. (Toigo et al. [2010]. Icarus, 208,402-411) explored the possibility that these waves are caused by solar-induced sublimation and diurnal deposition from N-2 frost patches, driven by weak vertical winds resulting from the rising and sinking gas as it is released from or deposited onto the surface. Here, we extend this model to account explicitly for seasonal variations in average insolation and for the significant damping of vertical wave propagation by kinematic viscosity and thermal diffusivity (Hubbard et al. [2009]. Icarus, 204, 284-289). Damping is extremely effective in suppressing vertical propagation of waves with vertical wavelengths of a few kilometers or less, and the dominant surviving tidal modes have characteristic vertical wavelengths lambda similar to 10-13 km. We estimate the expected strength and regional characteristics of atmospheric tides over the course of Pluto's orbit for a variety of assumed spatial distributions of surface frost and atmospheric surface pressure. We compute the predicted strength of tide-induced wave activity based on the actual frost distribution observed on Pluto from Hubble Space Telescope (HST) observations (Stern et al. [1997]. Astron. J., 113, 827; Buie et al. [2010]. Astron. J., 139, 1128-1143), and compare the results to calculations for volatile transport models of Young (Young [2013]. Astrophys. J., 766, L22) and Hansen et al. (Hansen et al. [2015]. Icarus, 246, 183-191). We develop simple scaling rules to estimate the variation of the strength of tidal activity with surface pressure P-s and solar declination so, and show that the maximum expected temperature perturbation at an atmospheric pressure of P = 0.1 Pa scales as dT(max) proportional to cos delta circle dot/root P-s. Wave activity is strongest in the near-equatorial region (latitude vertical bar phi vertical bar less than or similar to 30 degrees), being only weakly dependent on the detailed frost distribution. Using a 3-D time-dependent geometric optics ray-tracing code, we compute model light curves for the geometric circumstances of three high-SNR occultations (2002 August 21, 2006 June 12, and 2012 July 18), taking into account the detailed three-dimensional characteristics of the tides as different regions of the atmosphere are probed over the course of each occultation chord. We compare the strength and abundance of the scintillations in the models with those seen in the data, using both the HST frost maps and the volatile transport model predictions. The striking asymmetries in the strengths of spikes between ingress and egress seen in some events are reproduced in the tidal model simulations, due primarily to the latitudes probed during the occultation: occultations at high northern or southern latitudes uniformly have much weaker wave activity than more equatorial events. A surface pressure range of P-s = 1-2 Pa provides the best match between models and observations.
With the impending arrival of the New Horizons spacecraft at Pluto in 2015, we predict that wave activity in the upper atmosphere will be strongest at equatorial regions, and controlled in amplitude primarily by the surface pressure and damping effects, rather than by the detailed frost distribution. If Pluto's atmosphere begins to collapse in the coming decades, we expect that future stellar occultations will provide evidence for greatly enhanced atmospheric wave activity. (C) 2014 Elsevier Inc. All rights reserved.
C1 [French, Richard G.] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA.
[Toigo, Anthony D.] Johns Hopkins Univ, APL, Laurel, MD 20723 USA.
[Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Hansen, Candice J.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Young, Leslie A.] Southwest Res Inst, Boulder, CO 80302 USA.
[Sicardy, Bruno] Univ Paris 6 & Paris Diderot, CNRS, Obs Paris LESIA, Paris, France.
[Dias-Oliveira, Alex] Observ Nacl, Rio De Janeiro, Brazil.
[Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP French, RG (reprint author), Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA.
EM rfrench@wellesley.edu
OI Guzewich, Scott/0000-0003-1149-7385
FU NASA's Planetary Atmospheres Program
FX We are grateful to two anonymous referees for their detailed and
constructive criticism of the original submission of this paper, and to
William Hubbard for commenting on an earlier version of this work. This
work was supported in part by NASA's Planetary Atmospheres Program. The
18 July 2012 data were collected at the European Southern Observatory
(ESO) during run 089.C-0314(C).
NR 48
TC 3
Z9 3
U1 3
U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 247
EP 267
DI 10.1016/j.icarus.2014.05.017
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800021
ER
PT J
AU Brozovic, M
Showalter, MR
Jacobson, RA
Buie, MW
AF Brozovic, Marina
Showalter, Mark R.
Jacobson, Robert A.
Buie, Marc W.
TI The orbits and masses of satellites of Pluto
SO ICARUS
LA English
DT Article
DE Pluto, satellites; Satellites, dynamics; Orbit determination
ID CHARON SYSTEM; SPECKLE INTERFEROMETRY; STELLAR OCCULTATION; CCD
OBSERVATIONS; OUTER PLANETS; TRACKING DATA; MOON CHARON; ASTROMETRY;
HYDRA; RATIO
AB We present the numerically integrated orbits of Pluto's satellites. The orbits have been fit to a data set that includes Earth-based and Hubble Space Telescope (HST) astrometry of Charon, Nix, Hydra, Kerberos, and Styx, as well as the lightcurves from the Pluto-Charon mutual events. We also report new, 2010-2012 HST astrometry of all satellites including recently discovered Styx plus a pre-discovery detection of Kerberos in 2006. Pluto-relative data sets have been corrected for the center-of-light vs. center-of-mass offsets With the Pluto albedo model. The results are summarized in terms of the postfit residuals, state vectors, and mean orbital elements. Orbits of Charon, Styx, Nix, and Kerberos are nearly circular, while Hydra's shows a small eccentricity. All satellites are in near-resonance conditions, but we did not uncover any resonant arguments. Our model yields 975.5 +/- 1.5 km(3) s(-2), 869.6 +/- 1.8 km(3) s(-2), and 105.9 +/- 1.0 km(3) s(-2) for the system's, Pluto's, and Charon's GM values. The uncertainties reflect both systematic and random measurement errors. The GM values imply a bulk density of 1.89 +/- 0.06 g cm(-3) for Pluto and 1.72 +/- 0.02 g cm(-3) for Charon. We also obtain GM(Nix) = 0.0030 +/- 0.0027 km(3) s(-2) GM(Hydra) = 0.0032 +/- 0.0028 km(3) s(-2), GM(Kerberos) = 0.0011 +/- 0.0006 km(3) s(-2), and an upper bound on Styx's GM of 0.0010 km(3) s(-2). The 1 sigma errors are based on the formal covariance from the fit and they reflect only measurement errors. In-orbit (or along the track), radial, and out-of-plane orbital uncertainties at the time of New Horizons encounter are on the order of few tens of km or less for Charon, Nix, and Hydra. Kerberos and Styx have their largest uncertainty component of similar to 140 km and similar to 500 km respectively in the in-orbit direction. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Brozovic, Marina; Jacobson, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Showalter, Mark R.] SETI, Mountain View, CA 94043 USA.
[Buie, Marc W.] SWRI, Boulder, CO 80302 USA.
RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 301-121, Pasadena, CA 91109 USA.
EM Marina.Brozovic@jpl.nasa.gov
FU National Aeronautics and Space Administration [NNX12AQ11G, NAS5-26555];
HST program [GO-12436, GO-10786, AR-10940, GO-11556, GO-12897]; NASA
through grant from the Space Telescope Science Institute [GO-12436]
FX The research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. MRS was supported by
NASA's Outer Planets Program through Grant NNX12AQ11G, and by HST
program GO-12436. Support for program GO-12436 was provided by NASA
through a grant from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA Contract NAS5-26555. MWB was supported by HST programs
GO-10786, AR-10940, GO-11556, and GO-12897. The authors would like to
thank all of the astronomers who contributed their measurements to these
orbital calculations as well as the reviewers for their insightful
comments.
NR 57
TC 16
Z9 16
U1 2
U2 16
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 317
EP 329
DI 10.1016/j.icarus.2014.03.015
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800029
ER
PT J
AU Benecchi, SD
Noll, KS
Weaver, HA
Spencer, JR
Stern, SA
Buie, MW
Parker, AH
AF Benecchi, S. D.
Noll, K. S.
Weaver, H. A.
Spencer, J. R.
Stern, S. A.
Buie, M. W.
Parker, A. H.
TI New Horizons: Long-range Kuiper Belt targets observed by the Hubble
Space Telescope
SO ICARUS
LA English
DT Article
DE Kuiper Belt; Photometry; Hubble Space Telescope observations
ID TRANS-NEPTUNIAN OBJECTS; COLORS; CORE
AB We report on Hubble Space Telescope (HST) observations of three Kuiper Belt Objects (KB0s), discovered in our dedicated ground-based search campaign, that are candidates for long-range observations from the New Horizons spacecraft: 2011 JY(31), 2011 HZ(102), and 2013 LU35. Astrometry with HST enables both current and future critical accuracy improvements for orbit precision, required for possible New Horizons observations, beyond what can be obtained from the ground. Photometric colors of all three objects are red, typical of the Cold Classical dynamical population within which they reside; they are also the faintest KBOs to have had their colors measured. None are observed to be binary with HST above separations of similar to 0.02 arcsec (similar to 700 km at 44 AU) and Delta m <= 0.5. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Benecchi, S. D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Benecchi, S. D.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Noll, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weaver, H. A.] Johns Hopkins Univ, Dept Space, Appl Phys Lab, Laurel, MD 20723 USA.
[Spencer, J. R.; Stern, S. A.; Buie, M. W.] SW Res Inst, Boulder, CO 80302 USA.
[Parker, A. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Benecchi, SD (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM susank@psi.edu
RI Weaver, Harold/D-9188-2016
FU NASA [NAS 5-26555]; NASA through grant from the Space Telescope Science
Institute; Carnegie Fellowship at the Department of Terrestrial
Magnetism
FX This paper is based in part on ground-based data collected at the Subaru
Telescope, which is operated by the National Astronomical Observatory of
Japan, and on data gathered with the 6.5 m Magellan Telescopes located
at Las Campanas Observatory, Chile. Space-based observations were made
with the NASA/ESA Hubble Space Telescope, obtained at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. These observations are associated with programs 12535 and
12887. Support for both programs were 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. S. Benecchi was also supported in part through a
Carnegie Fellowship at the Department of Terrestrial Magnetism. We thank
Dr. Larry Wasserman and an anonymous reviewer for their helpful comments
which improved this manuscript.
NR 36
TC 1
Z9 1
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2015
VL 246
BP 369
EP 374
DI 10.1016/j.icarus.2014.04.014
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AX1FQ
UT WOS:000346693800035
ER
PT J
AU Su, CH
AF Su, Ching-Hua
TI A method of promoting single crystal yield during melt growth of
semiconductors by directional solidification
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Directional solidification; Single crystal growth; Growth from melt;
Zinc compound; Semiconducting cadmium compounds; Semiconducting II-VI
materials
ID PHASE-DIAGRAM; PSEUDOBINARY
AB For certain semiconductors with important applications, the existing unseeded bulk directional solidification crystal growth technique from the melt usually results in poor quality multi-crystalline ingots which causes the low yield of the commercial growth process. The multi-grained crystal growth is mainly caused by the large supercool of the melt, which not only results in a large section of ingot solidifying uncontrollably under spontaneous nucleation but also prohibits the ideal growth condition that small single crystal nuclei form at the very tip of the ampoule and grow into large single grains. To promote nucleation under the condition of small supercooling, a method was employed to induce nucleation by mechanical perturbation at a critical time during growth. The technique was applied to the bulk crystal growth process of Cd1-xZnxTe ingots. The comparison between the crystallinequality of the crystals grown with and without the mechanically induced nucleation shows that the yield of single crystalline can been vastly improved with the application of the technique. Published by Elsevier B.V.
C1 NASA, Marshall Space Flight Ctr, Mat & Proc Lab, Engn Directorate,EM31, Huntsville, AL 35812 USA.
RP Su, CH (reprint author), NASA, Marshall Space Flight Ctr, Mat & Proc Lab, Engn Directorate,EM31, Huntsville, AL 35812 USA.
EM ching.h.su@nasa.gov
FU Space Life and Physical Sciences Division, Human Exploration and
Operations Mission Directorate, NASA Headquarter
FX The author would like to acknowledge the supports of Space Life and
Physical Sciences Division, Human Exploration and Operations Mission
Directorate, NASA Headquarter.
NR 4
TC 2
Z9 2
U1 0
U2 11
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 JAN 15
PY 2015
VL 410
BP 35
EP 38
DI 10.1016/j.crysgro.2014.10.020
PG 4
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA AU6CD
UT WOS:000345689200007
ER
PT J
AU Zevalkink, A
Chanakian, S
Aydemir, U
Ormeci, A
Pomrehn, G
Bux, S
Fleurial, JP
Snyder, GJ
AF Zevalkink, Alex
Chanakian, Sevan
Aydemir, Umut
Ormeci, Alim
Pomrehn, Gregory
Bux, Sabah
Fleurial, Jean-Pierre
Snyder, G. Jeffrey
TI Thermoelectric properties and electronic structure of the Zintl phase
Sr5In2Sb6 and the Ca5-xSrxIn2Sb6 solid solution
SO JOURNAL OF PHYSICS-CONDENSED MATTER
LA English
DT Article
DE Zintl phase; thermoelectrics; alloy scattering; Sr5In2Sb6
ID LATTICE THERMAL-CONDUCTIVITY; LOCALIZATION FUNCTION; POWER-GENERATION;
EFFICIENCY; LOCALIZABILITY; REPRESENTATION; CA5IN2SB6; CHEMISTRY;
SYSTEM; SPACE
AB The Zintl phase Sr5In2Sb6 is isostructural with Ca5In2Sb6-a promising thermoelectric material with a peak zT of 0.7 when the carrier concentration is optimized by doping. Density functional calculations for Sr5In2Sb6 reveal a decreased energy gap and decreased valence band effective mass relative to the Ca analog. Chemical bonding analysis using the electron localizability indicator was found to support the Zintl bonding scheme for this structure type. High temperature transport measurements of the complete Ca5-xSrxIn2Sb6 solid solution were used to investigate the influence of the cation site on the electronic and thermal properties of A(5)In(2)Sb(6) compounds. Sr was shown to be fully miscible on the Ca site. The higher density of the Sr analog leads to a slight reduction in lattice thermal conductivity relative to Ca5In2Sb6, and, as expected, the solid solution samples have significantly reduced lattice thermal conductivities relative to the end member compounds.
C1 [Zevalkink, Alex; Chanakian, Sevan; Aydemir, Umut; Pomrehn, Gregory; Snyder, G. Jeffrey] CALTECH, Dept Appl Phys & Mat Sci, Pasadena, CA 91125 USA.
[Zevalkink, Alex; Bux, Sabah; Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA USA.
[Aydemir, Umut] Koc Univ, Dept Chem, Sariyer, Turkey.
[Ormeci, Alim] Max Planck Inst Chem Phys Solids, Dresden, Germany.
RP Zevalkink, A (reprint author), CALTECH, Dept Appl Phys & Mat Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM alex.z.williams@gmail.com
RI Snyder, G/I-2263-2015; Snyder, G. Jeffrey/E-4453-2011; Aydemir,
Umut/P-8424-2015; Ormeci, Alim/F-1082-2012
OI Snyder, G. Jeffrey/0000-0003-1414-8682; Aydemir,
Umut/0000-0003-1164-1973; Ormeci, Alim/0000-0001-5468-3378
FU NASA; Scientific and Technological Research Council of Turkey; DOE
[DE-AC02-05CH11231]
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and was supported by the NASA
Science Missions Directorate's Radioisotope Power Systems Technology
Advancement Program. UA acknowledges the financial assistance of The
Scientific and Technological Research Council of Turkey. GJS
acknowledges support from The Materials Project, DOE contract
DE-AC02-05CH11231.
NR 43
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U1 4
U2 25
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-8984
EI 1361-648X
J9 J PHYS-CONDENS MAT
JI J. Phys.-Condes. Matter
PD JAN 14
PY 2015
VL 27
IS 1
AR 015801
DI 10.1088/0953-8984/27/1/015801
PG 7
WC Physics, Condensed Matter
SC Physics
GA CE6EO
UT WOS:000351929600012
PM 25479002
ER
PT J
AU Robador, A
Jungbluth, SP
LaRowe, DE
Bowers, RM
Rappe, MS
Amend, JP
Cowen, JP
AF Robador, Alberto
Jungbluth, Sean P.
LaRowe, Douglas E.
Bowers, Robert M.
Rappe, Michael S.
Amend, Jan P.
Cowen, James P.
TI Activity and phylogenetic diversity of sulfate-reducing microorganisms
in low-temperature subsurface fluids within the upper oceanic crust
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Article
DE subseafloor life; metabolic activity; functional diversity; sulfate
reduction; basaltic ocean fluids
ID DE-FUCA RIDGE; MOLAL THERMODYNAMIC PROPERTIES; DISSIMILATORY SULFITE
REDUCTASE; DISSOLVED ORGANIC-CARBON; MICROBIAL LIFE; HIGH-PRESSURES;
SEA-FLOOR; HYDROTHERMAL CIRCULATION; TRANSPORT-PROPERTIES; BASALTIC
CRUST
AB The basaltic ocean crust is the largest aquifer system on Earth, yet the rates of biological activity in this environment are unknown. Low-temperature (<100 degrees C) fluid samples were investigated from two borehole observatories in the Juan de Fuca Ridge (JFR) flank, representing a range of upper oceanic basement thermal and geochemical properties. Microbial sulfate reduction rates (SRR) were measured in laboratory incubations with S-35-sulfate over a range of temperatures and the identity of the corresponding sulfate-reducing microorganisms (SRM) was studied by analyzing the sequence diversity of the functional marker dissimilatory (bi)sulfite reductase (dsrAB) gene. We found that microbial sulfate reduction was limited by the decreasing availability of organic electron donors in higher temperature, more altered fluids. Thermodynamic calculations indicate energetic constraints for metabolism, which together with relatively higher cell-specific SRR reveal increased maintenance requirements, consistent with novel species-level dsrAB phylotypes of thermophilic SRM. Our estimates suggest that microbially-mediated sulfate reduction may account for the removal of organic matter in fluids within the upper oceanic crust and underscore the potential quantitative impact of microbial processes in deep subsurface marine crustal fluids on marine and global biogeochemical carbon cycling.
C1 [Robador, Alberto; Bowers, Robert M.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Jungbluth, Sean P.; Rappe, Michael S.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, Kaneohe, HI USA.
[Jungbluth, Sean P.; Cowen, James P.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI USA.
[LaRowe, Douglas E.; Amend, Jan P.] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA.
[Amend, Jan P.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
RP Robador, A (reprint author), Univ So Calif, C DEBI, 3616 Trousdale Pkwy, Los Angeles, CA 90089 USA.
EM robadora@usc.edu
RI Jungbluth, Sean/A-9054-2012
OI Jungbluth, Sean/0000-0001-9265-8341
FU NSF [0CE0939564, MCB0604014, 1207880, 1207874]; NASA Astrobiology
Institute [NNAO9DA77A]
FX Lauren Kida is greatly acknowledged for her assistance in the lab. We
also thank the captain and crew on-board R/V Atlantis cruise AT15-66,
along with the pilots and crew of ROV Jason II for their help. We are
very grateful to Karen J. Meech for her continuous support. We also like
to thank Bo Barker Jorgensen and Casey Hubert for their positive and
helpful suggestions. This research was funded by NSF grants (C-DEBI
award 0CE0939564, MCB0604014 to James P. Cowen, 1207880 and 1207874 to
Jan P. Amend) and the NASA Astrobiology Institute under Cooperative
Agreement No. NNAO9DA77A issued through the Office of Space Science.
Participation of Alberto Robador in the research cruise to the JFR was
supported by The Lewis and Clark Fund for Exploration and Field Research
in Astrobiology. Additional financial support was provided by the C-DEBT
Research Grant Program (to Alberto Robador and Michael S. Rappe),
Graduate Student Fellowship Program (to Sean P. Jungbluth), and
Postdoctoral Scholarship Program (to Douglas E. LaRowe). Partial
financial support for this research was provided by a NSF-sponsored U.S.
Science Support Program Schlanger Ocean Drilling Fellowship (to Sean P.
Jungbluth). This research was further supported by a grant from the NASA
Astrobiology Institutute (Award # NNA13AA92A). This is NATLife
Underground Publication 007 and Center for Deep Biosphere Investigations
contribution 249.
NR 79
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U2 30
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 JAN 14
PY 2015
VL 5
AR 748
DI 10.3389/fmicb.2014.00748
PG 13
WC Microbiology
SC Microbiology
GA CA3LG
UT WOS:000348807500001
ER
PT J
AU Shaheen, R
Niles, PB
Chong, K
Corrigan, CM
Thiemens, MH
AF Shaheen, Robina
Niles, Paul B.
Chong, Kenneth
Corrigan, Catherine M.
Thiemens, Mark H.
TI Carbonate formation events in ALH 84001 trace the evolution of the
Martian atmosphere
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Martian meteorite; oxygen isotope anomaly; aqueous interaction; carbon
isotope; photochemistry
ID METEORITE ALH84001; ISOTOPIC COMPOSITION; CLIMATIC CHANGE;
LOW-TEMPERATURE; SNC METEORITES; MARS; OXYGEN; ALLAN-HILLS-84001; CO2;
CONSTRAINTS
AB Carbonate minerals provide critical information for defining atmosphere-hydrosphere interactions. Carbonate minerals in the Martian meteorite ALH 84001 have been dated to similar to 3.9 Ga, and both C and O-triple isotopes can be used to decipher the planet's climate history. Here we report Delta O-17, delta O-18, and delta C-13 data of ALH 84001 of at least two varieties of carbonates, using a stepped acid dissolution technique paired with ion microprobe analyses to specifically target carbonates from distinct formation events and constrain the Martian atmosphere-hydrosphere-geosphere interactions and surficial aqueous alterations. These results indicate the presence of a Ca-rich carbonate phase enriched in O-18 that formed sometime after the primary aqueous event at 3.9 Ga. The phases showed excess O-17 (0.7 parts per thousand) that captured the atmosphere-regolith chemical reservoir transfer, as well as CO2, O-3, and H2O isotopic interactions at the time of formation of each specific carbonate. The carbon isotopes preserved in the Ca-rich carbonate phase indicate that the Noachian atmosphere of Mars was substantially depleted in C-13 compared with the modern atmosphere.
C1 [Shaheen, Robina; Chong, Kenneth; Thiemens, Mark H.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92122 USA.
[Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Chong, Kenneth] Calif State Polytech Univ Pomona, Dept Chem, Pomona, CA 91768 USA.
[Corrigan, Catherine M.] Smithsonian Inst, Washington, DC 20004 USA.
RP Niles, PB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM paul.b.niles@nasa.gov
FU National Aeronautics and Space Administration Mars Fundamental Research;
National Science Foundation-Atmospheric Chemistry Division [AGS1259305]
FX We thank the reviewers for their critical evaluation, which helped
improve the manuscript. H. Bao from Louisiana State University is
greatly acknowledged for providing carbonate crust from Antarctic Dry
valley. P.B.N. acknowledges funding from National Aeronautics and Space
Administration Mars Fundamental Research. M. H. T. and R. S. thank
National Science Foundation-Atmospheric Chemistry Division for the
partial support Award no. AGS1259305 (to R. S.). C. M. C. would like to
thank Zonta International Foundation and the Ohio Space Grant
Consortium.
NR 35
TC 7
Z9 8
U1 6
U2 26
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 JAN 13
PY 2015
VL 112
IS 2
BP 336
EP 341
DI 10.1073/pnas.1315615112
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AY7HS
UT WOS:000347732300032
PM 25535348
ER
PT J
AU Schimel, D
Stephens, BB
Fisher, JB
AF Schimel, David
Stephens, Britton B.
Fisher, Joshua B.
TI Effect of increasing CO2 on the terrestrial carbon cycle
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE climate feedback; carbon budget; tropics; atmospheric transport
ID ATMOSPHERIC CO2; ELEVATED CO2; DROUGHT SENSITIVITY; TROPICAL FORESTS;
RAIN-FOREST; LAND; CLIMATE; SINKS; UNCERTAINTY; RESPONSES
AB Feedbacks from the terrestrial carbon cycle significantly affect future climate change. The CO2 concentration dependence of global terrestrial carbon storage is one of the largest and most uncertain feedbacks. Theory predicts the CO2 effect should have a tropical maximum, but a large terrestrial sink has been contradicted by analyses of atmospheric CO2 that do not show large tropical uptake. Our results, however, show significant tropical uptake and, combining tropical and extratropical fluxes, suggest that up to 60% of the present-day terrestrial sink is caused by increasing atmospheric CO2. This conclusion is consistent with a validated subset of atmospheric analyses, but uncertainty remains. Improved model diagnostics and new space-based observations can reduce the uncertainty of tropical and temperate zone carbon flux estimates. This analysis supports a significant feedback to future atmospheric CO2 concentrations from carbon uptake in terrestrial ecosystems caused by rising atmospheric CO2 concentrations. This feedback will have substantial tropical contributions, but the magnitude of future carbon uptake by tropical forests also depends on how they respond to climate change and requires their protection from deforestation.
C1 [Schimel, David; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
[Stephens, Britton B.] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80301 USA.
RP Schimel, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
EM dschimel@jpl.nasa.gov
RI Stephens, Britton/B-7962-2008
OI Stephens, Britton/0000-0002-1966-6182
FU JPL's Carbon and Climate Initiative; National Science Foundation
FX We thank the TRENDY modelers: Stephen Sitch, Chris Huntingford, Ben
Poulter, Anders Ahlstrom, Mark Lomas, Peter Levy, Sam Levis, Sonke
Zaehle, Nicolas Viovy, and Ning Zeng, and the RECCAP modelers: Philippe
Peylin, Frederic Chevallier, Rachel Law, Peter Rayner, Andy Jacobson,
Wouter Peters, Christian Roedenbeck, Prabir Patra, Kazutaka Yamada,
Kevin Gurney, and Yosuke Niwa, for sharing their results, with
particular thanks to Philippe Peylin for regridding and making results
available. Michael Keller and Sassan Saatchi provided insights into
forest inventories. We thank the students and faculty of the Niwot Ridge
Flux course for years of stimulating discussion, Munish Sikka for data
processing, and Chip Miller, Stan Sander, Riley Duren, Kevin Bowman,
Duane Waliser, and the Jet Propulsion Laboratory (JPL) Carbon-Climate
Initiative for support, valuable discussions, and feedback. The research
carried out at the JPL, California Institute of Technology, was under a
contract with the National Aeronautics and Space Administration.
Government sponsorship is acknowledged and was supported by JPL's Carbon
and Climate Initiative. The National Center for Atmospheric Research is
sponsored by the National Science Foundation.
NR 48
TC 57
Z9 58
U1 6
U2 131
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 JAN 13
PY 2015
VL 112
IS 2
BP 436
EP 441
DI 10.1073/pnas.1407302112/-/DCSupplemental
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AY7HS
UT WOS:000347732300049
PM 25548156
ER
PT J
AU van Haasteren, R
Vallisneri, M
AF van Haasteren, Rutger
Vallisneri, Michele
TI Low-rank approximations for large stationary covariance matrices, as
used in the Bayesian and generalized-least-squares analysis of
pulsar-timing data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational waves; methods: data analysis; pulsars: general
ID GAUSSIAN PROCESS REGRESSION; NOISE
AB Many data-analysis problems involve large dense matrices that describe the covariance of wide-sense stationary noise processes; the computational cost of inverting these matrices, or equivalently of solving linear systems that contain them, is often a practical limit for the analysis. We describe two general, practical, and accurate methods to approximate stationary covariance matrices as low-rank matrix products featuring carefully chosen spectral components. These methods can be used to greatly accelerate data-analysis methods in many contexts, such as the Bayesian and generalized-least-squares analysis of pulsar-timing residuals.
C1 [van Haasteren, Rutger; Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP van Haasteren, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vhaasteren@gmail.com
FU NASA Einstein Fellowship [PF3-140116]; Jet Propulsion Laboratory RTD
program
FX We thank the referee, W. A. Coles, for useful tips regarding efficient
Cholesky low-rank update algorithms and for other helpful suggestions.
RvH was supported by NASA Einstein Fellowship grant PF3-140116. MV was
supported by the Jet Propulsion Laboratory RTD program. This work was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract to the National Aeronautics and Space
Administration. Copyright 2014 California Institute of Technology.
Government sponsorship acknowledged.
NR 20
TC 8
Z9 8
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 JAN 11
PY 2015
VL 446
IS 2
BP 1170
EP 1174
DI 10.1093/mnras/stu2157
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TF
UT WOS:000350272200005
ER
PT J
AU Jones, OC
McDonald, I
Rich, RM
Kemper, F
Boyer, ML
Zijlstra, AA
Bendo, GJ
AF Jones, O. C.
McDonald, I.
Rich, R. M.
Kemper, F.
Boyer, M. L.
Zijlstra, A. A.
Bendo, G. J.
TI A Spitzer Space Telescope survey of extreme asymptotic giant branch
stars in M32
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: AGB and post-AGB; stars: late-type; stars: mass-loss; galaxies:
individual: M32; galaxies: stellar content; infrared: stars
ID LARGE-MAGELLANIC-CLOUD; MULTIBAND IMAGING PHOTOMETER; COLOR-MAGNITUDE
DIAGRAM; INFRARED ARRAY CAMERA; LOCAL GROUP GALAXIES; EVOLVED STARS;
CARBON STARS; STELLAR POPULATION; AGB STARS; ABSOLUTE CALIBRATION
AB We investigate the population of cool, evolved stars in the Local Group dwarf elliptical galaxy M32, using Infrared Array Camera observations from the Spitzer Space Telescope. We construct deep mid-infrared colour-magnitude diagrams for the resolved stellar populations within 3.5 arcmin of M32's centre, and identify those stars that exhibit infrared excess. Our data are dominated by a population of luminous, dust-producing stars on the asymptotic giant branch (AGB) and extend to approximately 3 mag below the AGB tip. We detect for the first time a sizeable population of 'extreme' AGB stars, highly enshrouded by circumstellar dust and likely completely obscured at optical wavelengths. The total dust-injection rate from the extreme AGB candidates is measured to be 7.5 x 10(-7) M-circle dot yr(-1), corresponding to a gas mass-loss rate of 1.5 x 10(-4) M-circle dot yr(-1). These extreme stars may be indicative of an extended star formation epoch between 0.2 and 5 Gyr ago.
C1 [Jones, O. C.; McDonald, I.; Zijlstra, A. A.; Bendo, G. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Jones, O. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, M. L.] ORAU, Oak Ridge, TN 37831 USA.
[Bendo, G. J.] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
RP Jones, OC (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England.
EM ojones@stsci.edu
RI Kemper, Francisca/D-8688-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Jones, Olivia/0000-0003-4870-5547
FU STFC STEP award; NASA through JPL/Caltech [GO 3400]; National Science
Council [NSC100-2112-M-001-023-MY3]; NASA [1407]
FX We wish to thank the referee Greg Sloan for the detailed and relevant
comments that have helped improve the clarity of our manuscript. We
would also like to thank Mike Peel, Sundar Srinivasan and everyone
involved in the original Spitzer proposal PID 3400. OCJ acknowledges the
support of an STFC STEP award and thanks the UCLA division of astronomy
and ASIAA for their hospitality during the completion of part of this
work. RMR acknowledges support for this work, which was provided by NASA
through an award issued by JPL/Caltech to Spitzer grant GO 3400. FK
acknowledges support from the National Science Council under grant
number NSC100-2112-M-001-023-MY3. This work is based on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under NASA
contract 1407.
NR 67
TC 3
Z9 3
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2015
VL 446
IS 2
BP 1584
EP 1596
DI 10.1093/mnras/stu2169
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TF
UT WOS:000350272200039
ER
PT J
AU Leauthaud, A
Benson, AJ
Civano, F
Coil, AL
Bundy, K
Massey, R
Schramm, M
Schulze, A
Capak, P
Elvis, M
Kulier, A
Rhodes, J
AF Leauthaud, Alexie
Benson, Andrew J.
Civano, Francesca
Coil, Alison L.
Bundy, Kevin
Massey, Richard
Schramm, Malte
Schulze, Andreas
Capak, Peter
Elvis, Martin
Kulier, Andrea
Rhodes, Jason
TI The dark matter haloes of moderate luminosity X-ray AGN as determined
from weak gravitational lensing and host stellar masses
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: abundances; galaxies: active; galaxies: haloes; galaxies:
Seyfert; galaxies: stellar content
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY;
WIDE-FIELD SURVEY; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; COSMOS FIELD;
OCCUPATION DISTRIBUTION; GALAXY GROUPS; HIGH-REDSHIFT
AB Understanding the relationship between galaxies hosting active galactic nuclei (AGN) and the dark matter haloes in which they reside is key to constraining how black hole fuelling is triggered and regulated. Previous efforts have relied on simple halo mass estimates inferred from clustering, weak gravitational lensing, or halo occupation distribution modelling. In practice, these approaches remain uncertain because AGN, no matter how they are identified, potentially live a wide range of halo masses with an occupation function whose general shape and normalization are poorly known. In this work, we show that better constraints can be achieved through a rigorous comparison of the clustering, lensing, and cross-correlation signals of AGN hosts to the fiducial stellar-to-halo mass relation (SHMR) derived for all galaxies, irrespective of nuclear activity. Our technique exploits the fact that the global SHMR can be measured with much higher accuracy than any statistic derived from AGN samples alone. Using 382 moderate luminosity X-ray AGN at z < 1 from the COSMOS field, we report the first measurements of weak gravitational lensing from an X-ray-selected sample. Comparing this signal to predictions from the global SHMR, we find that, contrary to previous results, most X-ray AGN do not live in medium size groups - nearly half reside in relatively low mass haloes with M-200b similar to 10(12.5) M-circle dot. The AGN occupation function is well described by the same form derived for all galaxies but with a lower normalization - the fraction of haloes with AGN in our sample is a few per cent. The number of AGN satellite galaxies scales as a power law with host halo mass with a power-law index alpha = 1. By highlighting the relatively 'normal' way in which moderate luminosity X-ray AGN hosts occupy haloes, our results suggest that the environmental signature of distinct fuelling modes for luminous quasars compared to moderate luminosity X-ray AGN is less obvious than previously claimed.
C1 [Leauthaud, Alexie; Bundy, Kevin; Schramm, Malte; Schulze, Andreas] Univ Tokyo, Kavli IPMU, WPI, Kashiwa, Chiba 2778582, Japan.
[Benson, Andrew J.] Carnegie Observ, Pasadena, CA 91101 USA.
[Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Coil, Alison L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA.
[Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kulier, Andrea] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA.
RP Leauthaud, A (reprint author), Univ Tokyo, Kavli IPMU, WPI, Kashiwa, Chiba 2778582, Japan.
EM alexie.leauthaud@ipmu.jp
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; National Science Foundation Graduate Research Fellowship
[DGE-1148900]; NASA [AR1-12012X]; Royal Society University Research
Fellowship; JPL; NSF CAREER [AST-1055081]
FX We thank Phil Hopkins, Surhud More, and John Silverman for insightful
discussions while preparing this paper. We also thank Ed Turner for
valuable discussions related to statistical methods. We are grateful to
Ian Harnett for editing this manuscript. We also thank Nikos Fanidakis
for clarifications regarding halo mass values in Fanidakis et al.
(2013). This work was supported by World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan. AK is supported by the
National Science Foundation Graduate Research Fellowship, grant no.
DGE-1148900. FC acknowledges financial support by the NASA grant
AR1-12012X. RM is supported by a Royal Society University Research
Fellowship. JR was supported by JPL, which is run by Caltech under a
contract for NASA. ALC acknowledge support from NSF CAREER award
AST-1055081.
NR 87
TC 9
Z9 9
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2015
VL 446
IS 2
BP 1874
EP 1888
DI 10.1093/mnras/stu2210
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TF
UT WOS:000350272200061
ER
PT J
AU Makarov, VV
Unwin, SC
AF Makarov, Valeri V.
Unwin, Stephen C.
TI Radial velocities and binarity of southern SIM grid stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: spectroscopic; stars: kinematics and dynamics
ID NEARBY STARS; ASTROMETRY; PHOTOMETRY; MULTIPLICITY; COMPANIONS; GIANTS
AB We present analysis of precision radial velocities (RV) of 1134 mostly red giant stars in the southern sky, selected as candidate astrometric grid objects for the Space Interferometry Mission (SIM). Only a few (typically, two or three) spectroscopic observations per star have been collected, with the main goal of screening binary systems. The estimated rate of spectroscopic binarity in this sample of red giants is 32 per cent at the 0.95 confidence level, and 46 per cent at the 0.75 confidence. The true binarity rate is likely to be higher, because our method is not quite sensitive to very wide binaries and low-mass companions. The estimated lower and upper bounds of stellar RV jitter for the entire sample are 24 and 51 m s(-1), respectively; the adopted mean value is 37 m s(-1). A few objects of interest are identified with large variations of RV, implying abnormally high mass ratios.
C1 [Makarov, Valeri V.] US Naval Observ, Washington, DC 20392 USA.
[Unwin, Stephen C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Makarov, VV (reprint author), US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA.
EM vvm@usno.navy.mil
NR 18
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 JAN 11
PY 2015
VL 446
IS 2
BP 2055
EP 2058
DI 10.1093/mnras/stu2239
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CC3TF
UT WOS:000350272200075
ER
PT J
AU Buenzli, E
Saumon, D
Marley, MS
Apai, D
Radigan, J
Bedin, LR
Reid, IN
Morley, CV
AF Buenzli, Esther
Saumon, Didier
Marley, Mark S.
Apai, Daniel
Radigan, Jacqueline
Bedin, Luigi R.
Reid, I. Neill
Morley, Caroline V.
TI CLOUD STRUCTURE OF THE NEAREST BROWN DWARFS: SPECTROSCOPIC VARIABILITY
OF LUHMAN 16AB FROM THE HUBBLE SPACE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; brown dwarfs; stars: atmospheres; stars: individual
(WISE J104915.57-531906.1, Luhman 16AB); stars: variables: general
ID T-DWARFS; L/T TRANSITION; WISE J104915.57-531906.1AB; EVOLVING WEATHER;
2 PC; SPECTRA; BINARY; PATCHY; TEMPERATURE; GRAVITY
AB The binary brown dwarf WISE J104915.57-531906.1 (also Luhman 16AB), composed of a late-L and early-T dwarf, is a prototypical L/T transition flux reversal binary located at a distance of only 2 pc. Luhman 16B is a known variable whose light curves evolve rapidly. We present a spatially resolved spectroscopic time-series of Luhman 16A and B covering 6.5 hr using the Hubble Space Telescope/WFC3 at 1.1-1.66 mu m. The small, count-dependent variability of Luhman 16A at the beginning of the observations likely stems from instrumental systematics; Luhman 16A appears non-variable above approximate to 0.4%. Its spectrum is well fit by a single cloud layer with intermediate cloud thickness (f(sed) = 2, T-eff = 1200 K). Luhman 16B varies at all wavelengths with peak-to-valley amplitudes of 7%-11%. The amplitude and light curve shape changes over only one rotation period. The lowest relative amplitude is found in the deep water absorption band at 1.4 mu m, otherwise it mostly decreases gradually from the blue to the red edge of the spectrum. This is very similar to the other two known highly variable early-T dwarfs. A two-component cloud model accounts for most of the variability, although small deviations are seen in the water absorption band. We fit the mean spectrum and relative amplitudes with a linear combination of two models of a warm, thinner cloud (T-eff = 1300 K, f(sed) = 3) and a cooler, thicker cloud (T-eff = 1000-1100 K, f(sed) = 1), assuming out-of-equilibrium atmospheric chemistry. A model with parameters as for Luhman 16A except for the addition of cloud holes cannot reproduce the variability of Luhman 16B, indicating more complex cloud evolution through the L/T transition. The projected separation of the binary has decreased by approximate to 0 ''.3 in eight months.
C1 [Buenzli, Esther] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Apai, Daniel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, Daniel] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Radigan, Jacqueline; Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bedin, Luigi R.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Buenzli, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM buenzli@mpia.de
OI Buenzli, Esther/0000-0003-3306-1486; bedin, luigi/0000-0003-4080-6466;
Marley, Mark/0000-0002-5251-2943
FU NASA [NAS 5-26555]; NASA through a grant from the Space Telescope
Science Institute [13280]; Swiss National Science Foundation (SNSF)
FX We thank the staff at Space Telescope Science Institute (STScI), in
particular Amber Armstrong, for the coordination and scheduling of the
observations. We also thank Jay Anderson for providing information and
routines regarding the distortion correction for WFC3. We thank Adam
Burgasser, Alexei Kniazev, and Jackie Faherty for providing their
published spectra of Luhman 16AB in electronic form. Based on
observations made with the NASA/ESA Hubble Space Telescope, obtained at
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555. These observations are associated with program
13280. Support for program 13280 was provided by NASA through a grant
from the Space Telescope Science Institute. E.B. was supported by the
Swiss National Science Foundation (SNSF). This research has made use of
the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's
Astrophysics Data System Bibliographic Services.
NR 34
TC 13
Z9 13
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2015
VL 798
IS 2
AR 127
DI 10.1088/0004-637X/798/2/127
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700062
ER
PT J
AU Chen, YJ
Juang, KJ
Nuevo, M
Jimenez-Escobar, A
Caro, GMM
Qiu, JM
Chu, CC
Yih, TS
Wu, CYR
Fung, HS
Ip, WH
AF Chen, Y. -J.
Juang, K. -J.
Nuevo, M.
Jimenez-Escobar, A.
Munoz Caro, G. M.
Qiu, J. -M.
Chu, C. -C.
Yih, T. -S.
Wu, C. -Y. R.
Fung, H. -S.
Ip, W. -H.
TI FORMATION OF S-BEARING SPECIES BY VUV/EUV IRRADIATION OF H2S-CONTAINING
ICE MIXTURES: PHOTON ENERGY AND CARBON SOURCE EFFECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; methods: laboratory: molecular; molecular processes;
ultraviolet: ISM
ID ABSOLUTE INFRARED INTENSITIES; ABSORPTION CROSS-SECTIONS; VACUUM-UV
SPECTROSCOPY; INTERSTELLAR ICE; AMINO-ACIDS; ULTRAVIOLET-IRRADIATION;
SULFUR DEPLETION; GRAIN MANTLES; DENSE CLOUDS; SULFIDE OCS
AB Carbonyl sulfide (OCS) is a key molecule in astrobiology that acts as a catalyst in peptide synthesis by coupling amino acids. Experimental studies suggest that hydrogen sulfide (H2S), a precursor of OCS, could be present in astrophysical environments. In the present study, we used a microwave-discharge hydrogen-flow lamp, simulating the interstellar UV field, and a monochromatic synchrotron light beam to irradiate CO: H2S and CO2: H2S ice mixtures at 14K with vacuum ultraviolet (VUV) or extreme ultraviolet (EUV) photons in order to study the effect of the photon energy and carbon source on the formation mechanisms and production yields of S-containing products (CS2, OCS, SO2, etc.). Results show that (1) the photo-induced OCS production efficiency in CO: H2S ice mixtures is higher than that of CO2: H2S ice mixtures; (2) a lower concentration of H2S enhances the production efficiency of OCS in both ice mixtures; and (3) the formation pathways of CS2 differ significantly upon VUV and EUV irradiations. Furthermore, CS2 was produced only after VUV photoprocessing of CO: H2S ices, while the VUV-induced production of SO2 occurred only in CO2: H2S ice mixtures. More generally, the production yields of OCS, H2S2, and CS2 were studied as a function of the irradiation photon energy. Heavy S-bearing compounds were also observed using mass spectrometry during the warm-up of VUV/ EUV-irradiated CO: H2S ice mixtures. The presence of S-polymers in dust grains may account for the missing sulfur in dense clouds and circumstellar environments.
C1 [Chen, Y. -J.; Juang, K. -J.; Qiu, J. -M.; Chu, C. -C.; Yih, T. -S.] Natl Cent Univ, Dept Phys, Jhongli 32054, Taoyuan County, Taiwan.
[Chen, Y. -J.; Wu, C. -Y. R.] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA.
[Chen, Y. -J.; Wu, C. -Y. R.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Nuevo, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nuevo, M.] BAER Inst, Petaluma, CA 94952 USA.
[Jimenez-Escobar, A.; Munoz Caro, G. M.] INTA CSIC, Ctr Astrobiol, E-28850 Madrid, Spain.
[Fung, H. -S.] Natl Synchrotron Radiat Res Ctr, Hsinchu 30076, Taiwan.
[Ip, W. -H.] Natl Cent Univ, Grad Inst Astron, Jhongli 32049, Taoyuan County, Taiwan.
RP Chen, YJ (reprint author), Natl Cent Univ, Dept Phys, Jhongli 32054, Taoyuan County, Taiwan.
RI Munoz Caro, Guillermo /L-6370-2014;
OI Munoz Caro, Guillermo /0000-0001-7003-7368; Nuevo,
Michel/0000-0003-1527-2669
FU NSC [101-2811-M-008-023]; NCU under the grant of The Aim for the Top
University Project; Spanish MICINN/MINECO [AYA2011-29375,
CSD2009-00038]; NSF Planetary Astronomy Program [AST-1108898]
FX This work was supported by the NSC grant No. 101-2811-M-008-023
(T.-S.Y.), and NCU under the grant of The Aim for the Top University
Project (W.-H. I.), the Spanish MICINN/MINECO under projects
AYA2011-29375 and CSD2009-00038 (G.M.M.C.), and the NSF Planetary
Astronomy Program under Grant AST-1108898 (C.-Y.R.W.). We acknowledge
NSRRC for provision of synchrotron radiation facilities, as well as Dr.
Bing-Ming Cheng for technical help on the beamline HF-CGM.
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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 JAN 10
PY 2015
VL 798
IS 2
AR 80
DI 10.1088/0004-637X/798/2/80
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700015
ER
PT J
AU Follette, KB
Grady, CA
Swearingen, JR
Sitko, ML
Champney, EH
van der Marel, N
Takami, M
Kuchner, MJ
Close, LM
Muto, T
Mayama, S
McElwain, MW
Fukagawa, M
Maaskant, K
Min, M
Russell, RW
Kudo, T
Kusakabe, N
Hashimoto, J
Abe, L
Akiyama, E
Brandner, W
Brandt, TD
Carson, J
Currie, T
Egner, SE
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Wisniewski, JP
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Follette, Katherine B.
Grady, Carol A.
Swearingen, Jeremy R.
Sitko, Michael L.
Champney, Elizabeth H.
van der Marel, Nienke
Takami, Michihiro
Kuchner, Marc J.
Close, Laird M.
Muto, Takayuki
Mayama, Satoshi
McElwain, Michael W.
Fukagawa, Misato
Maaskant, Koen
Min, Michiel
Russell, Ray W.
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Hashimoto, Jun
Abe, Lyu
Akiyama, Eiji
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
Henning, Thomas
Hodapp, Klaus
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John P.
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI SEEDS ADAPTIVE OPTICS IMAGING OF THE ASYMMETRIC TRANSITION DISK OPH IRS
48 IN SCATTERED LIGHT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: adaptive optics; instrumentation: polarimeters; planets
and satellites: formation; protoplanetary disks
ID YOUNG STELLAR OBJECTS; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL
ENERGY-DISTRIBUTIONS; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE TRACKS;
T-TAURI STARS; PROTOPLANETARY DISKS; RHO-OPHIUCHI; HD 142527;
PROTOSTELLAR ENVELOPES
AB We present the first resolved near-infrared imagery of the transition disk Oph IRS 48 (WLY 2-48), which was recently observed with ALMA to have a strongly asymmetric submillimeter flux distribution. H-band polarized intensity images show a similar to 60 AU radius scattered light cavity with two pronounced arcs of emission, one from northeast to southeast and one smaller, fainter, and more distant arc in the northwest. K-band scattered light imagery reveals a similar morphology, but with a clear third arc along the southwestern rim of the disk cavity. This arc meets the northwestern arc at nearly a right angle, revealing the presence of a spiral arm or local surface brightness deficit in the disk, and explaining the east-west brightness asymmetry in the H-band data. We also present 0.8-5.4 mu m IRTF SpeX spectra of this object, which allow us to constrain the spectral class to A0 +/- 1 and measure a low mass accretion rate of 10(-8.5) M-circle dot yr(-1), both consistent with previous estimates. We investigate a variety of reddening laws in order to fit the multiwavelength spectral energy distribution of Oph IRS 48 and find a best fit consistent with a younger, higher luminosity star than previous estimates.
C1 [Follette, Katherine B.; Close, Laird M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Swearingen, Jeremy R.; Sitko, Michael L.; Champney, Elizabeth H.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[van der Marel, Nienke; Maaskant, Koen; Min, Michiel] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Kuchner, Marc J.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Muto, Takayuki; Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Mayama, Satoshi; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Hayama Cho, Kanagawa 2400193, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan.
[Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kusakabe, Nobuhiko; Akiyama, Eiji; Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hashimoto, Jun; Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06108 Nice 2, France.
[Brandner, Wolfgang; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Hodapp, Klaus] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Kwon, Jungmi; Takahashi, Yasuhiro; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Higashihiroshima 7398511, Japan.
[Moro-Martin, Amaya] Inst Nacl Tecn Aerospacial, CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takahashi, Yasuhiro] MEXT, Chiyoda Ku, Tokyo 1008959, Japan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Follette, KB (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016;
OI Watanabe, Makoto/0000-0002-3656-4081; Feldt, Markus/0000-0002-4188-5242
FU World Premier International Research Center Initiative, MEXT, Japan;
NASA Origins of Solar Systems program [NNX09AB31G, NNG13PB64P]; KBF
through an NSF EAPSI Fellowship; NSF-AST [1008440]; Ministry of Science
and Technology (MoST) of Taiwan [103-2112-M-001-029]; NASA RTOP through
the NASA Origins of Solar Systems program [12-OSS12-0045]; National
Science Foundation [1009203]; NSF AST [1009314]; NASA Origins of Solar
System program [NNX13AK17G]; NASA ADP [NNX09AC73G]
FX This research is based in part on data collected at the Subaru
Telescope, which is operated by the National Astronomical Observatory of
Japan. This research has been supported in part by the World Premier
International Research Center Initiative, MEXT, Japan. This research has
made use of the SIMBAD database and Vizier service, operated at CDS,
Strasbourg, France. The authors wish to recognize and acknowledge the
very significant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain. We are grateful to Collette Salyk, Glenn Schneider, and Barb
Whitney for their insightful comments. K.B.F. and L.M.C. were supported
through the NASA Origins of Solar Systems program NNX09AB31G, and KBF
through an NSF EAPSI Fellowship. C.A.G. has been supported by NSF-AST
1008440 and through the NASA Origins of Solar Systems program on
NNG13PB64P. MT is supported from Ministry of Science and Technology
(MoST) of Taiwan (Grant No. 103-2112-M-001-029). M. W. Mc. E. is
supported under NASA RTOP 12-OSS12-0045 through the NASA Origins of
Solar Systems program. J.C. was supported by the National Science
Foundation under Award No. 1009203. J.P.W. is supported under NSF AST
1009314 and the NASA Origins of Solar System program under NNX13AK17G.
M.L.S. was supported under NASA ADP grant NNX09AC73G.
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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 JAN 10
PY 2015
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SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700067
ER
PT J
AU Inglis, AR
Ireland, J
Dominique, M
AF Inglis, A. R.
Ireland, J.
Dominique, M.
TI QUASI-PERIODIC PULSATIONS IN SOLAR AND STELLAR FLARES: RE-EVALUATING
THEIR NATURE IN THE CONTEXT OF POWER-LAW FLARE FOURIER SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: flare; stars: oscillations; Sun: corona; Sun: flares; Sun:
oscillations; Sun: UV radiation; Sun: X-rays, gamma-rays
ID 2011 FEBRUARY 15; GAMMA-RAY BURST; JUNE 7 ERUPTION; HARD X-RAY;
RETURNING PLASMA; RED NOISE; EMISSION; MODEL; DYNAMICS; MONITOR
AB The nature of quasi-periodic pulsations (QPPs) in solar and stellar flares remains debated. Recent work has shown that power-law-like Fourier power spectra are an intrinsic property of solar and stellar flare signals, a property that many previous studies of this phenomenon have not accounted for. Hence a re-evaluation of the existing interpretations and assumptions regarding QPPs is needed. We adopt a Bayesian method for investigating this phenomenon, fully considering the Fourier power-law properties of flare signals. Using data from the PROBA2/Large Yield Radiometer, Fermi/Gamma-ray Burst Monitor, Nobeyama Radioheliograph, and Yohkoh/ HXT instruments, we study a selection of flares from the literature identified as QPP events. Additionally, we examine optical data from a recent stellar flare that appears to exhibit oscillatory properties. We find that, for all but one event tested, an explicit oscillation is not required to explain the observations. Instead, the flare signals are adequately described as a manifestation of a power law in the Fourier power spectrum. However, for the flare of 1998 May 8, strong evidence for an explicit oscillation with P approximate to 14-16 s is found in the 17 GHz radio data and the 13-23 keV Yohkoh/HXT data. We conclude that, most likely, many previously analyzed events in the literature may be similarly described by power laws in the flare Fourier power spectrum, without invoking a narrowband, oscillatory component. Hence the prevalence of oscillatory signatures in solar and stellar flares may be less than previously believed. The physical mechanism behind the appearance of the observed power laws is discussed.
C1 [Inglis, A. R.; Ireland, J.] NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dominique, M.] Royal Observ Belgium, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium.
RP Inglis, AR (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
FU PROBA2 Guest Investigator Programme; PROBA2 team at the Royal
Observatory of Belgium
FX A.R.I. and J.I. both gratefully acknowledge the support of the PROBA2
Guest Investigator Programme, which provided the opportunity and funds
for both authors to collaborate with the PROBA2 team at the Royal
Observatory of Belgium. The authors are also grateful to Dr. Adam
Kowalski for providing the U- band data from the NMSU 1 m telescope.
This work was carried out using the SunPy, SciPy, PyMC, and Matplotlib
software packages. We also acknowledge the anonymous referee for useful
comments that resulted in a number of improvements to this paper.
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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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PY 2015
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AR UNSP 108
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SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700043
ER
PT J
AU Kowalski, AF
Cauzzi, G
Fletcher, L
AF Kowalski, Adam F.
Cauzzi, Gianna
Fletcher, Lyndsay
TI OPTICAL SPECTRAL OBSERVATIONS OF A FLICKERING WHITE-LIGHT KERNEL IN A C1
SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: chromosphere; Sun: flares; Sun: photosphere;
techniques: spectroscopic
ID HIGH TIME RESOLUTION; X-RAY EMISSIONS; H-ALPHA; ACTIVE STARS;
MULTIWAVELENGTH OBSERVATIONS; COORDINATED OBSERVATIONS; MAGNETIC
RECONNECTION; IMAGING SPECTROSCOPY; CONTINUUM EMISSION; ELEMENTARY FLARE
AB We analyze optical spectra of a two-ribbon, long-duration C1.1 flare that occurred on 2011 August 18 within AR 11271 (SOL2011-08-18T15: 15). The impulsive phase of the flare was observed with a comprehensive set of space-borne and ground-based instruments, which provide a range of unique diagnostics of the lower flaring atmosphere. Here we report the detection of enhanced continuum emission, observed in low-resolution spectra from 3600 angstrom 4550 angstrom acquired with the Horizontal Spectrograph at the Dunn Solar Telescope. A small, <= 0. 5 (10(15) cm(2)) penumbral/umbral kernel brightens repeatedly in the optical continuum and chromospheric emission lines, similar to the temporal characteristics of the hard X-ray variation as detected by the Gamma-ray Burst Monitor on the Fermi spacecraft. Radiative-hydrodynamic flare models that employ a nonthermal electron beam energy flux high enough to produce the optical contrast in our flare spectra would predict a large Balmer jump in emission, indicative of hydrogen recombination radiation from the upper flare chromosphere. However, we find no evidence of such a Balmer jump in the bluemost spectral region of the continuum excess. Just redward of the expected Balmer jump, we find evidence of a "blue continuum bump" in the excess emission which may be indicative of the merging of the higher order Balmer lines. The large number of observational constraints provides a springboard for modeling the blue/optical emission for this particular flarewith radiative-hydrodynamic codes, which are necessary to understand the opacity effects for the continuum and emission line radiation at these wavelengths.
C1 [Kowalski, Adam F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cauzzi, Gianna] INAF Osservatorio Astrofis Arcetri, Florence, Italy.
[Cauzzi, Gianna] Natl Solar Observ, Sunspot, NM 88349 USA.
[Fletcher, Lyndsay] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
RP Kowalski, AF (reprint author), NASA, Goddard Space Flight Ctr, Code 671,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM adam.f.kowalski@nasa.gov
OI Cauzzi, Gianna/0000-0002-6116-7301
FU International Space Sciences Institute (ISSI) in Bern; NASA Postdoctoral
Program at the Goddard Space Flight Center; European Community's Seventh
Framework Programme [FP7/2007-2013, 606862]; National Solar Observatory;
STFC [ST/ L000741/1]
FX We want to thank the DST observers, D. Gilliam, M. Bradford, and J.
Elrod, for their precious and patient assistance. The authors thank
Suzanne Hawley for useful discussions on the importance of obtaining
solar spectra with broad wavelength coverage, K. Tolbert for assistance
obtaining the Fermi data, M. Janvier for helpful suggestions and
discussions, and an anonymous referee for helpful constructive comments.
The authors are pleased to acknowledge the support of the International
Space Sciences Institute (ISSI) in Bern. IBIS is a project of INAF/OAA
with additional contributions from the University of Florence and Rome
and NSO. The National Solar Observatory is operated by the Association
of Universities for Research in Astronomy, Inc., under a cooperative
agreement with the National Science Foundation. This research was
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. The research has received
funding from the European Community's Seventh Framework Programme
(FP7/2007-2013) under agreement 606862 (F-CHROMA). A.F.K. acknowledges
the National Solar Observatory for travel support. L.F. acknowledges
support from STFC grant ST/ L000741/1.
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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 CD1SD
UT WOS:000350853700042
ER
PT J
AU Leja, J
van Dokkum, PG
Franx, M
Whitaker, KE
AF Leja, Joel
van Dokkum, Pieter G.
Franx, Marijn
Whitaker, Katherine E.
TI RECONCILING THE OBSERVED STAR-FORMING SEQUENCE WITH THE OBSERVED STELLAR
MASS FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity
function, mass function; galaxies: star formation
ID SIMILAR-TO 3; EXTRAGALACTIC LEGACY SURVEY; GALAXY FORMATION MODELS;
LOW-REDSHIFT UNIVERSE; EMISSION-LINE SURVEY; INSIDE-OUT GROWTH; STEEP
FAINT-END; LESS-THAN 2.5; QUIESCENT GALAXIES; FORMATION RATES
AB We examine the connection between the observed star-forming sequence (SFR proportional to M-alpha) and the observed evolution of the stellar mass function in the range 0.2 < z < 2.5. We find that the star-forming sequence cannot have a slope alpha less than or similar to 0.9 at all masses and redshifts because this would result in a much higher number density at 10 < log(M/M-circle dot) < 11 by z = 1 than is observed. We show that a transition in the slope of the star-forming sequence, such that alpha = 1 at log(M/M-circle dot) < 10.5 and alpha = 0.7-0.13z (Whitaker et al.) at log(M/M-circle dot) > 10.5, greatly improves agreement with the evolution of the stellar mass function. We then derive a star-forming sequence that reproduces the evolution of the mass function by design. This star-forming sequence is also well described by a broken power law, with a shallow slope at high masses and a steep slope at low masses. At z = 2, it is offset by similar to 0.3 dex from the observed star-forming sequence, consistent with the mild disagreement between the cosmic star formation rate (SFR) and recent observations of the growth of the stellar mass density. It is unclear whether this problem stems from errors in stellar mass estimates, errors in SFRs, or other effects. We show that a mass-dependent slope is also seen in other self-consistent models of galaxy evolution, including semianalytical, hydrodynamical, and abundance-matching models. As part of the analysis, we demonstrate that neither mergers nor hidden low-mass quiescent galaxies are likely to reconcile the evolution of the mass function and the star-forming sequence. These results are supported by observations from Whitaker et al.
C1 [Leja, Joel; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 AA Leiden, Netherlands.
[Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Leja, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
OI Leja, Joel/0000-0001-6755-1315
FU NASA [NNX11AB08G]
FX We thank the anonymous referee for insightful suggestions and attention
to details, which have greatly improved the quality of the paper.
Support from NASA Grant NNX11AB08G is gratefully acknowledged. K.E.W. is
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 86
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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 JAN 10
PY 2015
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DI 10.1088/0004-637X/798/2/115
PG 16
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SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700050
ER
PT J
AU Miller, AA
Bloom, JS
Richards, JW
Lee, YS
Starr, DL
Butler, NR
Tokarz, S
Smith, N
Eisner, JA
AF Miller, A. A.
Bloom, J. S.
Richards, J. W.
Lee, Y. S.
Starr, D. L.
Butler, N. R.
Tokarz, S.
Smith, N.
Eisner, J. A.
TI A MACHINE-LEARNING METHOD TO INFER FUNDAMENTAL STELLAR PARAMETERS FROM
PHOTOMETRIC LIGHT CURVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; stars: general; stars:
statistics; stars: variables: general; surveys
ID DIGITAL SKY SURVEY; AUTOMATED SUPERVISED CLASSIFICATION; HIGH-RESOLUTION
SPECTROSCOPY; VARIABLE-STARS; RANDOM FORESTS; DATA RELEASE; SPACED DATA;
CATALOG; METALLICITY; VARIABILITY
AB A fundamental challenge for wide-field imaging surveys is obtaining follow-up spectroscopic observations: there are >10(9) photometrically cataloged sources, yet modern spectroscopic surveys are limited to similar to fewx10(6) targets. As we approach the Large Synoptic Survey Telescope era, new algorithmic solutions are required to cope with the data deluge. Here we report the development of a machine-learning framework capable of inferring fundamental stellar parameters (T-eff, log g, and [Fe/H]) using photometric-brightness variations and color alone. A training set is constructed from a systematic spectroscopic survey of variables with Hectospec/ Multi-Mirror Telescope. In sum, the training set includes similar to 9000 spectra, for which stellar parameters are measured using the SEGUE Stellar Parameters Pipeline (SSPP). We employed the random forest algorithm to perform a non-parametric regression that predicts Teff, log g, and [Fe/H] from photometric time-domain observations. Our final optimized model produces a cross-validated rms error (RMSE) of 165 K, 0.39 dex, and 0.33 dex for T-eff, log g, and [Fe/H], respectively. Examining the subset of sources for which the SSPP measurements are most reliable, the RMSE reduces to 125 K, 0.37 dex, and 0.27 dex, respectively, comparable to what is achievable via low-resolution spectroscopy. For variable stars this represents a approximate to 12%-20% improvement in RMSE relative to models trained with single-epoch photometric colors. As an application of our method, we estimate stellar parameters for similar to 54,000 known variables. We argue that this method may convert photometric time-domain surveys into pseudo-spectrographic engines, enabling the construction of extremely detailed maps of the Milky Way, its structure, and history.
C1 [Miller, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miller, A. A.] CALTECH, Pasadena, CA 91125 USA.
[Bloom, J. S.; Richards, J. W.; Starr, D. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Bloom, J. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Richards, J. W.; Starr, D. L.] Wise Io, Berkeley, CA 94704 USA.
[Lee, Y. S.] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea.
[Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA.
[Tokarz, S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Smith, N.; Eisner, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Miller, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA.
EM amiller@astro.caltech.edu
FU NASA from a Hubble Fellowship [HST-HF-51325.01]; STScI; NASA [NAS
5-26555]; NSF-CDI [0941742]; Alfred P. Sloan Research Fellowship
FX A.A.M. acknowledges support for this work by NASA from a Hubble
Fellowship grant: HST-HF-51325.01, awarded by STScI, operated by AURA,
Inc., for NASA, under contract NAS 5-26555. J.S.B. acknowledges support
from an NSF-CDI grant 0941742. JAE gratefully acknowledges support from
an Alfred P. Sloan Research Fellowship. Part of the research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Observations reported here were
obtained at the MMT Observatory, a joint facility of the University of
Arizona and the Smithsonian Institution.
NR 56
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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 JAN 10
PY 2015
VL 798
IS 2
AR 122
DI 10.1088/0004-637X/798/2/122
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700057
ER
PT J
AU Nesvold, ER
Kuchner, MJ
AF Nesvold, Erika R.
Kuchner, Marc J.
TI GAP CLEARING BY PLANETS IN A COLLISIONAL DEBRIS DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; circumstellar matter; methods: numerical;
planet-disk interactions; planetary systems
ID BETA-PICTORIS B; FOMALHAUT B; GIANT PLANET; ORBITING FOMALHAUT;
CIRCUMSTELLAR DISK; LARGE TELESCOPE; SOLAR-SYSTEM; CHAOTIC ZONE;
KUIPER-BELT; HR 4796
AB We apply our 3D debris disk model, SMACK, to simulate a planet on a circular orbit near a ring of planetesimals that are experiencing destructive collisions. Previous simulations of a planet opening a gap in a collisionless debris disk have found that the width of the gap scales as the planet mass to the 2/7th power (alpha = 2/7). We find that gap sizes in a collisional disk still obey a power law scaling with planet mass, but that the index a of the power law depends on the age of the system t relative to the collisional timescale t(coll) of the disk by alpha = 0.32(t/t(coll))(-0.04), with inferred planet masses up to five times smaller than those predicted by the classical gap law. The increased gap sizes likely stem from the interaction between collisions and the mean motion resonances near the chaotic zone. We investigate the effects of the initial eccentricity distribution of the disk particles and find a negligible effect on the gap size at Jovian planet masses, since collisions tend to erase memory of the initial particle eccentricity distributions. Finally, we find that the presence of Trojan analogs is a potentially powerful diagnostic of planets in the mass range similar to 1-10M(Jup). We apply our model to place new upper limits on planets around Fomalhaut, HR4796 A, HD202628, HD181327, and beta Pictoris.
C1 [Nesvold, Erika R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 21230 USA.
RP Nesvold, ER (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM Erika.Nesvold@umbc.edu; Marc.Kuchner@nasa.gov
FU NASA Planetary Geology and Geophysics [PGG11-0032]; NASA Astrobiology
Institute through the Goddard Center for Astrobiology; NASA through
Space Telescope Science Institute; NASA [NAS 5-26555]
FX We thank Karl Stapelfeldt, Aki Roberge, Hanno Rein, and Margaret Pan for
helpful discussions. Erika Nesvold is supported in part by NASA
Planetary Geology and Geophysics grant PGG11-0032. Marc Kuchner is
supported in part by the NASA Astrobiology Institute through the Goddard
Center for Astrobiology. Additional support for this research was
provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555.
NR 70
TC 17
Z9 17
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2015
VL 798
IS 2
AR 83
DI 10.1088/0004-637X/798/2/83
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700018
ER
PT J
AU Rodigas, TJ
Stark, CC
Weinberger, A
Debes, JH
Hinz, PM
Close, L
Chen, C
Smith, PS
Males, JR
Skemer, AJ
Puglisi, A
Follette, KB
Morzinski, K
Wu, YL
Briguglio, R
Esposito, S
Pinna, E
Riccardi, A
Schneider, G
Xompero, M
AF Rodigas, Timothy J.
Stark, Christopher C.
Weinberger, Alycia
Debes, John H.
Hinz, Philip M.
Close, Laird
Chen, Christine
Smith, Paul S.
Males, Jared R.
Skemer, Andrew J.
Puglisi, Alfio
Follette, Katherine B.
Morzinski, Katie
Wu, Ya-Lin
Briguglio, Runa
Esposito, Simone
Pinna, Enrico
Riccardi, Armando
Schneider, Glenn
Xompero, Marco
TI ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; instrumentation: adaptive optics; planetary
systems; stars: individual (HR 4796A); techniques: high angular
resolution
ID MULTIBAND IMAGING PHOTOMETER; COMPLEX ORGANIC MATERIALS; EXTRASOLAR
GIANT PLANETS; SCATTERED-LIGHT IMAGES; HUBBLE-SPACE-TELESCOPE; TW HYDRAE
ASSOCIATION; BETA-PICTORIS DISK; ICY KUIPER-BELT; CIRCUMSTELLAR DISK;
FOMALHAUT B
AB We present resolved images of the HR 4796A debris disk using the Magellan adaptive optics system paired with Clio-2 and VisAO. We detect the disk at 0.77 mu m, 0.91 mu m, 0.99 mu m, 2.15 mu m, 3.1 mu m, 3.3 mu m, and 3.8 mu m. We find that the deprojected center of the ring is offset from the star by 4.76 +/- 1.6 AU and that the deprojected eccentricity is 0.06 +/- 0.02, in general agreement with previous studies. We find that the average width of the ring is 14(-2)(+3)% (11.1(-1.6)(+2.4) AU), also comparable to previous measurements. Combining our new scattered light data with archival Hubble Space Telescope images at similar to 0.5-2 mu m, along with previously unpublished Spitzer/MIPS thermal emission data and all other literature thermal data, we set out to constrain the chemical composition of the dust grains. After testing 19 individual root compositions and more than 8400 unique mixtures of these compositions, we find that good fits to the scattered light alone and thermal emission alone are discrepant, suggesting that caution should be exercised if fitting to only one or the other. When we fit to both data sets simultaneously, we find that silicates and organics are generally the most favored, while large abundances of water ice are usually not favored. These results suggest the HR 4796A dust grains are similar to interstellar dust and solar system comets, though improved modeling is necessary to place better constraints on the exact chemical composition of the dust.
C1 [Rodigas, Timothy J.; Weinberger, Alycia] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Stark, Christopher C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Debes, John H.; Chen, Christine] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hinz, Philip M.; Close, Laird; Smith, Paul S.; Males, Jared R.; Skemer, Andrew J.; Follette, Katherine B.; Morzinski, Katie; Wu, Ya-Lin; Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Puglisi, Alfio; Briguglio, Runa; Esposito, Simone; Pinna, Enrico; Riccardi, Armando; Xompero, Marco] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Rodigas, TJ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM trodigas@carnegiescience.edu
OI Riccardi, Armando/0000-0001-5460-2929; Esposito,
Simone/0000-0002-3114-677X; Xompero, Marco/0000-0002-5565-084X; Pinna,
Enrico/0000-0002-6243-5697; Skemer, Andrew/0000-0001-6098-3924;
Morzinski, Katie/0000-0002-1384-0063; Rodigas,
Timothy/0000-0002-7535-2997; Weinberger, Alycia/0000-0001-6654-7859
FU NSF MRI program; NSF ATI program; NASA Postdoctoral Program at Goddard
Space Flight Center; California Institute of Technology (Caltech) - NASA
through the Sagan Fellowship Program; NASA/JPL [1256424]; Carnegie node
of the NASA Astrobiology Institute [NNA09DA81A]
FX We thank the referee, Christian Thalmann, for helpful comments and
suggestions. We are grateful to the entire LCO observing support staff
for their help preparing and operating the telescope and instruments
during the observing runs. We thank the teams at the Steward Observatory
Mirror Lab/CAAO (University of Arizona), Microgate (Italy), and ADS
(Italy) for building the phenomenal adaptive secondary mirror (ASM) for
use in the AO. The MagAO ASM was developed with support from the NSF MRI
program. The MagAO pyramid wavefront sensor was developed with help from
the NSF TSIP program and the Magellan partners. The Active Optics guider
was developed by Carnegie Observatories with custom optics from the
MagAO team. The VisAO camera and commissioning was supported with help
from the NSF ATI program. C.C.S. would like to acknowledge support of
this research by an appointment to the NASA Postdoctoral Program at
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. J.R.M and K.M.M. were
supported under contract with the California Institute of Technology
(Caltech) funded by NASA through the Sagan Fellowship Program. P.S.S.
acknowledges support from the NASA/JPL contract 1256424 given to the
University of Arizona. A.J.W. acknowledges the support of the Carnegie
node of the NASA Astrobiology Institute under Cooperative Agreement
NNA09DA81A.
NR 115
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U1 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2015
VL 798
IS 2
AR 96
DI 10.1088/0004-637X/798/2/96
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700031
ER
PT J
AU Wagner, KR
Sitko, ML
Grady, CA
Swearingen, JR
Champney, EH
Johnson, AN
Werren, C
Whitney, BA
Russell, RW
Schneider, GH
Momose, M
Muto, T
Inoue, AK
Lauroesch, JT
Hornbeck, J
Brown, A
Fukagawa, M
Currie, TM
Wisniewski, JP
Woodgate, BE
AF Wagner, Kevin R.
Sitko, Michael L.
Grady, Carol A.
Swearingen, Jeremy R.
Champney, Elizabeth H.
Johnson, Alexa N.
Werren, Chelsea
Whitney, Barbara A.
Russell, Ray W.
Schneider, Glenn H.
Momose, Munetake
Muto, Takayuki
Inoue, Akio K.
Lauroesch, James T.
Hornbeck, Jeremy
Brown, Alexander
Fukagawa, Misato
Currie, Thayne M.
Wisniewski, John P.
Woodgate, Bruce E.
TI VARIABILITY OF DISK EMISSION IN PRE-MAIN SEQUENCE AND RELATED STARS.
III. EXPLORING STRUCTURAL CHANGES IN THE PRE-TRANSITIONAL DISK IN HD
169142
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; protoplanetary disks; stars: individual (HD
169142); stars: variables:T Tauri, Herbig Ae/Be; techniques:
photometric; techniques: spectroscopic
ID HERBIG AE/BE STARS; T-TAURI STARS; VEGA-LIKE SYSTEMS; PROTOPLANETARY
DISKS; INFRARED OBSERVATIONS; TRANSITIONAL DISKS; RADIATION TRANSFER;
SIZE DISTRIBUTION; PLANETARY-NEBULA; YOUNG STARS
AB We present near-IR (NIR) and far-UV observations of the pre-transitional (gapped) disk in HD 169142 using NASA's Infrared Telescope Facility and Hubble Space Telescope. The combination of our data along with existing data sets into the broadband spectral energy distribution reveals variability of up to 45% between similar to 1.5-10 mu m over a maximum timescale of 10 yr. All observations known to us separate into two distinct states corresponding to a high near-IR state in the pre-2000 epoch and a low state in the post-2000 epoch, indicating activity within the less than or similar to 1AU region of the disk. Through analysis of the Pa beta and Br gamma lines in our data we derive a mass accretion rate in 2013 May of (M)overdot approximate to (1.5-2.7) x 10-9 M-circle dot yr(-1). We present a theoretical modeling analysis of the disk in HD 169142 using Monte-Carlo radiative transfer simulation software to explore the conditions and perhaps signs of planetary formation in our collection of 24 yr of observations. We find that shifting the outer edge (r approximate to 0.3AU) of the inner disk by 0.05 AU toward the star (in simulation of accretion and/or sculpting by forming planets) successfully reproduces the shift in NIR flux. We establish that the similar to 40-70 AU dark ring imaged in the NIR by Quanz et al. and Momose et al. and at 7 mm by Osorio et al. may be reproduced with a 30% scaled density profile throughout the region, strengthening the link to this structure being dynamically cleared by one or more planetary mass bodies.
C1 [Wagner, Kevin R.; Sitko, Michael L.; Swearingen, Jeremy R.; Champney, Elizabeth H.; Johnson, Alexa N.; Werren, Chelsea] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Whitney, Barbara A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Schneider, Glenn H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Momose, Munetake] Ibaraki Univ, Bunkyo Ku, Mito, Ibaraki 3100056, Japan.
[Muto, Takayuki] Kogakuin Univ, Shinjuku Ku, Tokyo 1638677, Japan.
[Inoue, Akio K.] Osaka Sangyo Univ, Coll Gen Educ, Osaka 5748530, Japan.
[Lauroesch, James T.; Hornbeck, Jeremy] Univ Louisville Res Fdn Inc, Louisville, KY 40292 USA.
[Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Astrophys Res Lab, Boulder, CO 80309 USA.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Currie, Thayne M.] Oak Ridge Associated Univ, Oak Ridge, TN 37830 USA.
[Wisniewski, John P.] Univ Oklahoma, Norman, OK 73019 USA.
[Woodgate, Bruce E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wagner, Kevin R.; Sitko, Michael L.; Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80301 USA.
[Grady, Carol A.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
RP Wagner, KR (reprint author), Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
EM wagnekr@mail.uc.edu; sitkoml@ucmail.uc.edu; carol.a.grady@nasa.gov;
swearijr@mail.uc.edu; ehchampney@gmail.com; astefank@andrew.cmu.edu;
ccwerren@yahoo.com; bwhitney@astro.wisc.edu; Ray.W.Russell@aero.org;
gschneider@as.arizona.edu; momose@mx.ibaraki.ac.jp;
muto@cc.kogakuin.ac.jp; akinoue@las.osaka-sandai.ac.jp;
james.lauroesch@louisville.edu; jeremy.hornbeck@gmail.com;
Alexander.Brown@colorado.edu; misato@iral.ess.sci.osaka-u.ac.jp;
currie@naoj.org; wisniewski@ou.edu
OI Wagner, Kevin/0000-0002-4309-6343
FU NASA ADAP [NNX09AC73G]; Hubble Space Telescope grant [HST-GO-13032];
IR&D program at The Aerospace Corporation; University of Cincinnati
Honors Program
FX This work was supported by NASA ADAP grant NNX09AC73G, Hubble Space
Telescope grant HST-GO-13032, the IR&D program at The Aerospace
Corporation, and the University of Cincinnati Honors Program. We would
like to thank Dr. Sascha Quanz, Dr. Munetake Momose, and the
Astronomical Society of the Pacific Conference Series for permission to
reproduce the images from their original publications. We would also
like to thank the anonymous journal referee whose comments greatly
improved this article.
NR 59
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2015
VL 798
IS 2
AR 94
DI 10.1088/0004-637X/798/2/94
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700029
ER
PT J
AU Zoglauer, A
Reynolds, SP
An, HJ
Boggs, SE
Christensen, FE
Craig, WW
Fryer, CL
Grefenstette, BW
Harrison, FA
Hailey, CJ
Krivonos, RA
Madsen, KK
Miyasaka, H
Stern, D
Zhang, WW
AF Zoglauer, Andreas
Reynolds, Stephen P.
An, Hongjun
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Fryer, Chris L.
Grefenstette, Brian W.
Harrison, Fiona A.
Hailey, Charles J.
Krivonos, Roman A.
Madsen, Kristin K.
Miyasaka, Hiromasa
Stern, Daniel
Zhang, William W.
TI THE HARD X-RAY VIEW OF THE YOUNG SUPERNOVA REMNANT G1.9+0.3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: supernova remnants; X-rays: individual (G1.9+0.3)
ID GALACTIC SUPERNOVA; ACCELERATED ELECTRONS; CASSIOPEIA-A; HIGH-ENERGY;
TI-44; EMISSION; SHOCKS; LINES
AB NuSTAR observed G1.9+0.3, the youngest known supernova remnant in the Milky Way, for 350 ks and detected emission up to similar to 30 keV. The remnant's X-ray morphology does not change significantly across the energy range from 3 to 20 keV. A combined fit between NuSTAR and Chandra shows that the spectrum steepens with energy. The spectral shape can be well fitted with synchrotron emission from a power-law electron energy distribution with an exponential cutoff with no additional features. It can also be described by a purely phenomenological model such as a broken power law or a power law with an exponential cutoff, though these descriptions lack physical motivation. Using a fixed radio flux at 1 GHz of 1.17 Jy for the synchrotron model, we get a column density of N-H = (7.23 +/- 0.07) x 10(22) cm(-2), a spectral index of alpha = 0.633 +/- 0.003, and a roll-off frequency of upsilon(rolloff) = (3.07 +/- 0.18) x 10(17) Hz. This can be explained by particle acceleration, to a maximum energy set by the finite remnant age, in a magnetic field of about 10 mu G, for which our roll-off implies a maximum energy of about 100 TeV for both electrons and ions. Much higher magnetic-field strengths would produce an electron spectrum that was cut off by radiative losses, giving a much higher roll-off frequency that is independent of magnetic-field strength. In this case, ions could be accelerated to much higher energies. A search for Ti-44 emission in the 67.9 keV line results in an upper limit of 1.5 x 10(-5) photons cm(-2) s(-1) assuming a line width of 4.0 keV (1 sigma).
C1 [Zoglauer, Andreas; Boggs, Steven E.; Craig, William W.; Krivonos, Roman A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
[Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.; Miyasaka, Hiromasa] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zoglauer, A (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM zog@ssl.berkeley.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012;
Madsen, Kristin/0000-0003-1252-4891
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 (Caltech, USA).
NR 33
TC 9
Z9 9
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2015
VL 798
IS 2
AR 98
DI 10.1088/0004-637X/798/2/98
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700033
ER
PT J
AU ZuHone, JA
Kunz, MW
Markevitch, M
Stone, JM
Biffi, V
AF ZuHone, J. A.
Kunz, M. W.
Markevitch, M.
Stone, J. M.
Biffi, V.
TI THE EFFECT OF ANISOTROPIC VISCOSITY ON COLD FRONTS IN GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; methods: numerical; X-rays: galaxies:
clusters
ID KELVIN-HELMHOLTZ INSTABILITIES; UNSPLIT GODUNOV METHOD; MAGNETIC-FIELDS;
INTRACLUSTER MEDIUM; MAGNETOHYDRODYNAMIC SIMULATIONS; CONSTRAINED
TRANSPORT; PLASMA INSTABILITIES; INTERGALACTIC MEDIUM; CHANDRA
OBSERVATION; PERSEUS CLUSTER
AB Cold fronts-contact discontinuities in the intracluster medium (ICM) of galaxy clusters-should be disrupted by Kelvin-Helmholtz (K-H) instabilities due to the associated shear velocity. However, many observed cold fronts appear stable. This opens the possibility of placing constraints on microphysical mechanisms that stabilize them, such as the ICM viscosity and/ or magnetic fields. We performed exploratory high-resolution simulations of cold fronts arising from subsonic gas sloshing in cluster cores using the grid-based Athena MHD code, comparing the effects of isotropic Spitzer and anisotropic Braginskii viscosity (expected in a magnetized plasma). Magnetized simulations with full Braginskii viscosity or isotropic Spitzer viscosity reduced by a factor f similar to 0.1 are both in qualitative agreement with observations in terms of suppressing K-H instabilities. The rms velocity of turbulence within the sloshing region is only modestly reduced by Braginskii viscosity. We also performed unmagnetized simulations with and without viscosity and find that magnetic fields have a substantial effect on the appearance of the cold fronts, even if the initial field is weak and the viscosity is the same. This suggests that determining the dominant suppression mechanism of a given cold front from X-ray observations (e.g., viscosity or magnetic fields) by comparison with simulations is not straightforward. Finally, we performed simulations including anisotropic thermal conduction, and find that including Braginskii viscosity in these simulations does not significantly affect the evolution of cold fronts; they are rapidly smeared out by thermal conduction, as in the inviscid case.
C1 [ZuHone, J. A.; Markevitch, M.] NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[ZuHone, J. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kunz, M. W.; Stone, J. M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Biffi, V.] SISSA, I-34136 Trieste, Italy.
RP ZuHone, JA (reprint author), NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
FU NASA though Astrophysics Theory Program [12-ATP12-0159]; Einstein
Postdoctoral Fellowship - Chandra X-ray Observatory Center [PF1-120084];
NASA [NAS8-03060]
FX J.A.Z. thanks Ian Parrish, Ralph Kraft, and Paul Nulsen for useful
discussions. Calculations were performed using the computational
resources of the Advanced Supercomputing Division at NASA/Ames Research
Center. Analysis of the simulation data was carried out using the AMR
analysis and visualization toolset yt (Turk et al. 2011), which is
available for download at http://yt-project.org. Support for J.A.Z. was
provided by NASA though Astrophysics Theory Program Award Number
12-ATP12-0159. Support for M.W.K. was provided by NASA through Einstein
Postdoctoral Fellowship Award Number PF1-120084, issued by the Chandra
X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060.
NR 77
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U1 0
U2 1
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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 JAN 10
PY 2015
VL 798
IS 2
AR 90
DI 10.1088/0004-637X/798/2/90
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CD1SD
UT WOS:000350853700025
ER
PT J
AU Crepp, JR
Rice, EL
Veicht, A
Aguilar, J
Pueyo, L
Giorla, P
Nilsson, R
Luszcz-Cook, SH
Oppenheimer, R
Hinkley, S
Brenner, D
Vasisht, G
Cady, E
Beichman, CA
Hillenbrand, LA
Lockhart, T
Matthews, CT
Roberts, LC
Sivaramakrishnan, A
Soummer, R
Zhai, CX
AF Crepp, Justin R.
Rice, Emily L.
Veicht, Aaron
Aguilar, Jonathan
Pueyo, Laurent
Giorla, Paige
Nilsson, Ricky
Luszcz-Cook, Statia H.
Oppenheimer, Rebecca
Hinkley, Sasha
Brenner, Douglas
Vasisht, Gautam
Cady, Eric
Beichman, Charles A.
Hillenbrand, Lynne A.
Lockhart, Thomas
Matthews, Christopher T.
Roberts, Lewis C., Jr.
Sivaramakrishnan, Anand
Soummer, Remi
Zhai, Chengxing
TI DIRECT SPECTRUM OF THE BENCHMARK T DWARF HD 19467 B
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE brown dwarfs; stars: individual (HD 19467); techniques: high angular
resolution; techniques: spectroscopic
ID NEAR-INFRARED SPECTROSCOPY; SUN-LIKE STAR; L/T TRANSITION; BROWN DWARFS;
HR 8799; SPECKLE SUPPRESSION; SPACE-TELESCOPE; SKY SURVEY; DISCOVERY;
PHOTOMETRY
AB HD 19467 B is presently the only directly imaged T dwarf companion known to induce a measurable Doppler acceleration around a solar-type star. We present spectroscopy measurements of this important benchmark object taken with the Project 1640 integral field unit at Palomar Observatory. Our high-contrast R approximate to 30 observations obtained simultaneously across the JH bands confirm the cold nature of the companion as reported from the discovery article and determine its spectral type for the first time. Fitting the measured spectral energy distribution to SpeX/IRTF T dwarf standards and synthetic spectra from BT-Settl atmospheric models, we find that HD 19467 B is a T5.5 +/- 1 dwarf with effective temperature T-eff = 978(-43)(+20) K. Our observations reveal significant methane absorption affirming its substellar nature. HD 19467 B shows promise to become the first T dwarf that simultaneously reveals its mass, age, and metallicity independent from the spectrum of light that it emits.
C1 [Crepp, Justin R.; Matthews, Christopher T.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Rice, Emily L.; Giorla, Paige] CUNY Coll Staten Isl, Staten Isl, NY 10314 USA.
[Rice, Emily L.; Veicht, Aaron; Giorla, Paige; Nilsson, Ricky; Luszcz-Cook, Statia H.; Oppenheimer, Rebecca; Brenner, Douglas] Amer Museum Nat Hist, New York, NY 10024 USA.
[Aguilar, Jonathan; Pueyo, Laurent; Sivaramakrishnan, Anand; Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Aguilar, Jonathan; Pueyo, Laurent] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Giorla, Paige] CUNY, Grad Ctr, Dept Phys, New York, NY 10016 USA.
[Nilsson, Ricky] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Hinkley, Sasha; Hillenbrand, Lynne A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Hinkley, Sasha] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Vasisht, Gautam; Cady, Eric; Lockhart, Thomas; Roberts, Lewis C., Jr.; Zhai, Chengxing] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Crepp, JR (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA.
EM jcrepp@nd.edu
OI Oppenheimer, Rebecca/0000-0001-7130-7681; Rice,
Emily/0000-0002-3252-5886
FU NASA Origins of Solar Systems grant [NNX13AB03G]; NASA Early Career
Fellowship program; National Science Foundation [AST-0215793, 0334916,
0520822, 0804417, 1245018]; NASA ADAP grant [11-ADAP11-0169]; NSF award
[AST 1211568]; National Physical Science Consortium; National
Aeronautics and Space Administration
FX The TrenDS high-contrast imaging program is supported by NASA Origins of
Solar Systems grant NNX13AB03G and the NASA Early Career Fellowship
program. A portion of this work was supported by the National Science
Foundation under Grant Numbers AST-0215793, 0334916, 0520822, 0804417
and 1245018. This work was partially supported by NASA ADAP grant
11-ADAP11-0169 and NSF award AST 1211568. A portion of the research in
this Letter was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. J.A. is supported by the National Physical
Science Consortium. This research has benefitted from the SpeX Prism
Spectral Libraries, maintained by Adam Burgasser.
NR 45
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2015
VL 798
IS 2
AR L43
DI 10.1088/2041-8205/798/2/L43
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AY3CY
UT WOS:000347463300017
ER
PT J
AU Foley, RJ
Van Dyk, SD
Jha, SW
Clubb, KI
Filippenko, AV
Mauerhan, JC
Miller, AA
Smith, N
AF Foley, Ryan J.
Van Dyk, Schuyler D.
Jha, Saurabh W.
Clubb, Kelsey I.
Filippenko, Alexei V.
Mauerhan, Jon C.
Miller, Adam A.
Smith, Nathan
TI ON THE PROGENITOR SYSTEM OF THE TYPE Iax SUPERNOVA 2014dt IN M61
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: individual (M61); supernovae: general; supernovae: individual
(SN 2014dt)
ID MASSIVE WHITE-DWARF; HELIUM NOVA; LOW-LUMINOSITY; V445 PUPPIS; SN
2002CX; SPECTROSCOPY; 2005HK; 2008HA; I.; SPECTROPOLARIMETRY
AB We present pre-explosion and post-explosion Hubble Space Telescope images of the Type Iax supernova (SN Iax) 2014dt in M61. After astrometrically aligning these images, we do not detect any stellar sources at the position of the SN in the pre-explosion images to relatively deep limits (3 sigma limits of M-F438W > -5.0mag and M-F814W > -5.9mag). These limits are similar to the luminosity of SN 2012Z's progenitor system (M-F435W = -5.43 +/- 0.15 and M-F814W = -5.24 +/- 0.16 mag), the only probable detected progenitor system in pre-explosion images of a SN Iax, and indeed, of any white-dwarf supernova. SN 2014dt is consistent with having a C/O white-dwarf primary/helium-star companion progenitor system, as was suggested for SN 2012Z, although perhaps with a slightly smaller or hotter donor. The data are also consistent with SN 2014dt having a low-mass red giant or main-sequence star companion. The data rule out main-sequence stars with M-init greater than or similar to 16M(circle dot) and most evolved stars with M-init greater than or similar to 8M(circle dot) as being the progenitor of SN 2014dt. Hot Wolf-Rayet stars are also allowed, but the lack of nearby bright sources makes this scenario unlikely. Because of its proximity (D = 12 Mpc), SN 2014dt is ideal for long-term monitoring, where images in similar to 2 yr may detect the companion star or the luminous bound remnant of the progenitor white dwarf.
C1 [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Van Dyk, Schuyler D.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Clubb, Kelsey I.; Filippenko, Alexei V.; Mauerhan, Jon C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miller, Adam A.] CALTECH, Pasadena, CA 91125 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Foley, RJ (reprint author), Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA.
OI Van Dyk, Schuyler/0000-0001-9038-9950
FU NASA [NAS 5-26555]; NASA/HST [GO-12999.01, GO-12913.01]; National
Science Foundation (NSF) [AST-0847157]; NASA from Hubble Fellowship -
STScI [HST-HF-51325.01]; Christopher R. Redlich Fund; TABASGO
Foundation; NSF [AST-1211916]; [GO-13683]
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 and funded through program GO-13683. Data were obtained through the
Hubble Legacy Archive, which is a collaboration between STScI/NASA, the
Space Telescope European Coordinating Facility (ST-ECF/ESA), and the
Canadian Astronomy Data Centre (CADC/NRC/CSA).; SN Iax research at the
University of Illinois is supported in part through NASA/HST grant
GO-12999.01. This research at Rutgers University was supported through
NASA/HST grant GO-12913.01 and National Science Foundation (NSF) CAREER
award AST-0847157 to S. W.J.A.A.M. acknowledges support for this work by
NASA from Hubble Fellowship grant HST-HF-51325.01, awarded by STScI.
A.V.F.'s group at U.C. Berkeley is supported by the Christopher R.
Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916.
NR 38
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2015
VL 798
IS 2
AR L37
DI 10.1088/2041-8205/798/2/L37
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AY3CY
UT WOS:000347463300011
ER
PT J
AU Stevenson, R
Bauer, JM
Cutri, RM
Mainzer, AK
Masci, FJ
AF Stevenson, R.
Bauer, J. M.
Cutri, R. M.
Mainzer, A. K.
Masci, F. J.
TI NEOWISE OBSERVATIONS OF COMET C/2013 A1 (SIDING SPRING) AS IT APPROACHES
MARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE comets: individual (C/2013 A1 (Siding Spring))
ID INFRARED-SURVEY-EXPLORER; DUST; PERFORMANCE; MISSION
AB The Near-Earth Object Wide-field Infrared Survey Explorer mission observed comet C/2013 A1 (Siding Spring) three times at 3.4 mu m and 4.6 mu m as the comet approached Mars in 2014. The comet is an extremely interesting target since its close approach to Mars in late 2014 will be observed by various spacecraft in situ. The observations were taken in 2014 January, July, and September when the comet was at heliocentric distances of 3.82 AU, 1.88 AU, and 1.48 AU. The level of activity increased significantly between the January and July visits but then decreased by the time of the observations in September, approximately four weeks prior to its close approach to Mars. In this work, we calculate Af rho values and CO/CO2 production rates.
C1 [Stevenson, R.; Bauer, J. M.; Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J. M.; Cutri, R. M.; Masci, F. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration; NASA Postdoctoral Program
FX This publication makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the National Aeronautics and Space Administration.
This research has made use of the NASA/IPAC Infrared Science Archive,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. R.S. gratefully acknowledges support from the NASA
Postdoctoral Program.
NR 15
TC 9
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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 JAN 10
PY 2015
VL 798
IS 2
AR L31
DI 10.1088/2041-8205/798/2/L31
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AY3CY
UT WOS:000347463300005
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, RA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Ast, S
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barker, D
Barnum, SH
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Bell, C
Belopolski, I
Bergmann, G
Berliner, JM
Bersanetti, D
Bertolini, A
Bessis, D
Betzwieser, J
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Biscans, S
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bowers, J
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brannen, CA
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Bruckner, F
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Colombini, M
Constancio, M
Conte, A
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
Debreczeni, G
Degallaix, J
Deleeuw, E
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, RT
De Rosa, R
DeSalvo, R
Dhurandhar, S
Diaz, M
Dietz, A
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Dmitry, K
Donovan, F
Dooley, KL
Doravari, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eichholz, J
Eikenberry, SS
Endroczi, G
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farr, B
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, R
Flaminio, R
Foley, E
Foley, S
Forsi, E
Fotopoulos, N
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Garcia, J
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Gergely, L
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, KE
Gustafson, EK
Gustafson, R
Hall, B
Hall, E
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hong, T
Hooper, S
Horrom, T
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Hua, Z
Huang, V
Huerta, EA
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Huynh-Dinh, T
Iafrate, J
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jaranowski, P
Jimenez-Forteza, F
Johnson, WW
Jones, DI
Jones, D
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasprzack, M
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kaufman, K
Kawabe, K
Kawamura, S
Kawazoe, F
Kefelian, F
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, W
Kim, YM
King, E
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Koehlenbeck, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kremin, A
Kringel, V
Krishnan, B
Krolak, A
Kucharczyk, C
Kudla, S
Kuehn, G
Kumar, A
Kumar, DN
Kumar, P
Kumar, R
Kurdyumov, R
Kwee, P
Landry, M
Lantz, B
Larson, S
Lasky, PD
Lawrie, C
Lazzarini, A
Leaci, P
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, JJ
Lee, J
Leonardi, M
Leong, JR
Le Roux, A
Leroy, N
Letendre, N
Levine, B
Lewis, JB
Lhuillier, V
Li, TGF
Lin, AC
Littenberg, TB
Litvine, V
Liu, F
Liu, H
Liu, Y
Liu, Z
Lloyd, D
Lockerbie, NA
Lockett, V
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, MJ
Luck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Manca, GM
Mandel, I
Mandic, V
Mangano, V
Mantovani, M
Marchesoni, F
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CA LIGO Sci Collaboration
Virgo Collaboration
TI Searching for stochastic gravitational waves using data from the two
colocated LIGO Hanford detectors
SO PHYSICAL REVIEW D
LA English
DT Article
ID INSPIRAL TRIGGERS; NEUTRON-STARS; LIMITS; RADIATION; BINARIES; BURSTS;
VETOES; GEO
AB Searches for a stochastic gravitational-wave background (SGWB) using terrestrial detectors typically involve cross-correlating data from pairs of detectors. The sensitivity of such cross-correlation analyses depends, among other things, on the separation between the two detectors: the smaller the separation, the better the sensitivity. Hence, a colocated detector pair is more sensitive to a gravitational-wave background than a noncolocated detector pair. However, colocated detectors are also expected to suffer from correlated noise from instrumental and environmental effects that could contaminate the measurement of the background. Hence, methods to identify and mitigate the effects of correlated noise are necessary to achieve the potential increase in sensitivity of colocated detectors. Here we report on the first SGWB analysis using the two LIGO Hanford detectors and address the complications arising from correlated environmental noise. We apply correlated noise identification and mitigation techniques to data taken by the two LIGO Hanford detectors, H1 and H2, during LIGO's fifth science run. At low frequencies, 40-460 Hz, we are unable to sufficiently mitigate the correlated noise to a level where we may confidently measure or bound the stochastic gravitational-wave signal. However, at high frequencies, 460-1000 Hz, these techniques are sufficient to set a 95% confidence level upper limit on the gravitational-wave energy density of Omega(f) < 7.7 x 10(-4) (f/900 Hz)(3), which improves on the previous upper limit by a factor of similar to 180. In doing so, we demonstrate techniques that will be useful for future searches using advanced detectors, where correlated noise (e.g., from global magnetic fields) may affect even widely separated detectors.
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[Coccia, E.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Corsi, A.] George Washington Univ, Washington, DC 20052 USA.
[Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Crowder, S. G.; Kandhasamy, S.; Kremin, A.; Mandic, V.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Dhurandhar, S.; Mitra, S.; Souradeep, T.] Inter Univ, Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38123 Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Trento, Italy.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B.; Farr, W.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Littenberg, T. B.; Rodriguez, C.; Shahriar, M. S.; Stevens, D.; van der Sluys, M. V.; Yablon, J.; Yum, H.] Northwestern Univ, Evanston, IL 60208 USA.
[Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA.
[Finn, L. S.; Owen, B. J.; Zhu, H.] Penn State Univ, University Pk, PA 16802 USA.
[Frei, Z.; Gondan, L.; Raffai, P.; Szeifert, G.] MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Fujimoto, M. -K.; Hayama, K.; Kawamura, S.; Mori, T.; Nishida, E.; Nishizawa, A.] Natl Astron Observ, Tokyo 1818588, Japan.
[Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Gergely, L.] Univ Szeged, H-6720 Szeged, Hungary.
[Greenhalgh, R. J. S.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Hughey, B.; Loew, K.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Horrom, T.; Mikhailov, E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Hosken, D. J.; Kim, W.; King, E.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Jang, H.; Kang, G.; Kim, B. K.; Kim, C.] Korea Inst Sci & Technol, Taejon 305806, South Korea.
[Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Haris, K.; Mazumder, N.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.; Lee, C. -H.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Larson, S.] Utah State Univ, Logan, UT 84322 USA.
[Lasky, P. D.; Melatos, A.; Pindor, B.; Sammut, L.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Liu, F.] Univ Brussels, B-1050 Brussels, Belgium.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartmento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Ind Technol Inst, Ahmadabad 382424, Gujarat, India.
[Shah, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Vedovato, G.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Kandhasamy, S (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM shivaraj.kandhasamy@ligo.org
RI Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Losurdo,
Giovanni/K-1241-2014; Travasso, Flavio/J-9595-2016; Bartos,
Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella,
Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Costa,
Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016;
Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora
Vittoria/E-9078-2015; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain,
Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Gammaitoni,
Luca/B-5375-2009; Prokhorov, Leonid/I-2953-2012; Khalili,
Farit/D-8113-2012; Heidmann, Antoine/G-4295-2016; Marchesoni,
Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi,
Franco/K-1068-2016; Kumar, Prem/B-6691-2009; Puppo, Paola/J-4250-2012;
Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell,
Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri,
Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Steinlechner,
Sebastian/D-5781-2013; Shaddock, Daniel/A-7534-2011; Postiglione,
Fabio/O-4744-2015; Vicere, Andrea/J-1742-2012; Leonardi,
Matteo/G-9694-2015; Danilishin, Stefan/K-7262-2012; Sigg,
Daniel/I-4308-2015; Gorodetsky, Michael/C-5938-2008; Gemme,
Gianluca/C-7233-2008; McClelland, David/E-6765-2010; Hild,
Stefan/A-3864-2010; M, Manjunath/N-4000-2014; Vecchio,
Alberto/F-8310-2015; Iyer, Bala R./E-2894-2012; Mow-Lowry,
Conor/F-8843-2015; prodi, giovanni/B-4398-2010; Strigin,
Sergey/I-8337-2012; Sergeev, Alexander/F-3027-2017; Harms,
Jan/J-4359-2012; Ward, Robert/I-8032-2014; Howell, Eric/H-5072-2014;
OI Ferrante, Isidoro/0000-0002-0083-7228; Losurdo,
Giovanni/0000-0003-0452-746X; Travasso, Flavio/0000-0002-4653-6156;
Punturo, Michele/0000-0001-8722-4485; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636;
Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Strain,
Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958;
Gammaitoni, Luca/0000-0002-4972-7062; Heidmann,
Antoine/0000-0002-0784-5175; Marchesoni, Fabio/0000-0001-9240-6793; Zhu,
Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587;
Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441;
Graef, Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821;
Garufi, Fabio/0000-0003-1391-6168; Deleglise,
Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822;
Steinlechner, Sebastian/0000-0003-4710-8548; Shaddock,
Daniel/0000-0002-6885-3494; Postiglione, Fabio/0000-0003-0628-3796;
Vicere, Andrea/0000-0003-0624-6231; Danilishin,
Stefan/0000-0001-7758-7493; Sigg, Daniel/0000-0003-4606-6526;
Gorodetsky, Michael/0000-0002-5159-2742; Gemme,
Gianluca/0000-0002-1127-7406; McClelland, David/0000-0001-6210-5842; M,
Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617;
Iyer, Bala R./0000-0002-4141-5179; prodi, giovanni/0000-0001-5256-915X;
Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447;
O'Shaughnessy, Richard/0000-0001-5832-8517; Vedovato,
Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Boschi,
Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418;
Papa, M.Alessandra/0000-0002-1007-5298; Vocca,
Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; Pinto,
Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200;
Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870;
Drago, Marco/0000-0002-3738-2431; Pierro, Vincenzo/0000-0002-6020-5521;
Coccia, Eugenio/0000-0002-6669-5787; Vetrano,
Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Denker,
Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730;
calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515;
Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397;
Del Pozzo, Walter/0000-0003-3978-2030; Allen, Bruce/0000-0003-4285-6256;
Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577;
Freise, Andreas/0000-0001-6586-9901; Nitz,
Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946;
Whiting, Bernard F/0000-0002-8501-8669; Murphy,
David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Davies,
Gareth/0000-0002-4289-3439
FU U.S. National Science Foundation for the construction and operation of
the LIGO Laboratory; Science and Technology Facilities Council of the
United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany;
Italian Istituto Nazionale di Fisica Nucleare; French Centre National de
la Recherche Scientifique; Australian Research Council; International
Science Linkages program of the Commonwealth of Australia; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern
de les Illes Balears; Foundation for Fundamental Research on Matter;
Netherlands Organisation for Scientific Research; Polish Ministry of
Science and Higher Education; FOCUS Programme of Foundation for Polish
Science; Royal Society; Scottish Funding Council; Scottish Universities
Physics Alliance; National Aeronautics and Space Administration, OTKA of
Hungary; Lyon Institute of Origins (LIO); National Research Foundation
of Korea, Industry Canada and the Province of Ontario through the
Ministry of Economic Development and Innovation; National Science and
Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust;
David and Lucile Packard Foundation; Research Corporation; Alfred P.
Sloan Foundation
FX The authors gratefully acknowledge the support of the U.S. National
Science Foundation for the construction and operation of the LIGO
Laboratory, the Science and Technology Facilities Council of the United
Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany
for support of the construction and operation of the GEO600 detector,
and the Italian Istituto Nazionale di Fisica Nucleare and the French
Centre National de la Recherche Scientifique for the construction and
operation of the Virgo detector. The authors also gratefully acknowledge
the support of the research by these agencies and by the Australian
Research Council, the International Science Linkages program of the
Commonwealth of Australia, the Council of Scientific and Industrial
Research of India, the Istituto Nazionale di Fisica Nucleare of Italy,
the Spanish Ministerio de Economia y Competitividad, the Conselleria
d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, the Polish Ministry of
Science and Higher Education, the FOCUS Programme of Foundation for
Polish Science, the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, The National Aeronautics and
Space Administration, OTKA of Hungary, the Lyon Institute of Origins
(LIO), the National Research Foundation of Korea, Industry Canada and
the Province of Ontario through the Ministry of Economic Development and
Innovation, the National Science and Engineering Research Council
Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile
Packard Foundation, the Research Corporation, and the Alfred P. Sloan
Foundation.
NR 61
TC 12
Z9 12
U1 9
U2 50
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 8
PY 2015
VL 91
IS 2
AR UNSP 022003
DI 10.1103/PhysRevD.91.022003
PG 18
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CB1UU
UT WOS:000349414300002
ER
PT J
AU Chilvery, AK
Batra, AK
Yang, B
Xiao, K
Guggilla, P
Aggarwal, MD
Surabhi, R
Lal, RB
Currie, JR
Penn, BG
AF Chilvery, Ashwith Kumar
Batra, Ashok K.
Yang, Bin
Xiao, Kai
Guggilla, Padmaja
Aggarwal, Mohan D.
Surabhi, Raja
Lal, Ravi B.
Currie, James R.
Penn, Benjamin G.
TI Perovskites: transforming photovoltaics, a mini-review
SO JOURNAL OF PHOTONICS FOR ENERGY
LA English
DT Review
ID ORGANOMETAL HALIDE PEROVSKITES; MESOSCOPIC SOLAR-CELL; CHARGE-TRANSPORT;
THIN-FILMS; LOW-COST; EFFICIENCY; RECOMBINATION; CH3NH3PBI3; TIN;
SPECTROSCOPY
AB The recent power-packed advent of perovskite solar cells is transforming photovoltaics (PV) with their superior efficiencies, ease of fabrication, and cost. This perovskite solar cell further boasts of many unexplored features that can further enhance its PV properties and lead to it being branded as a successful commercial product. This article provides a detailed insight of the organometal halide based perovskite structure, its unique stoichiometric design, and its underlying principles for PV applications. The compatibility of various PV layers and its fabrication methods is also discussed. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Chilvery, Ashwith Kumar] Talladega Coll, Dept Phys, Talladega, AL 35610 USA.
[Chilvery, Ashwith Kumar; Batra, Ashok K.; Guggilla, Padmaja; Aggarwal, Mohan D.; Surabhi, Raja; Lal, Ravi B.] Alabama A&M Univ, Mat Sci Grp, Dept Phys Chem & Math, Normal, AL 35762 USA.
[Yang, Bin; Xiao, Kai] Oak Ridge Natl Lab, Ctr Nanophase Mat Sci, Oak Ridge, TN 37831 USA.
[Currie, James R.; Penn, Benjamin G.] NASA, George C Marshall Space Flight Ctr, Sensors Grp, Huntsville, AL 35811 USA.
RP Chilvery, AK (reprint author), Talladega Coll, Dept Phys, 627 West Battle St, Talladega, AL 35610 USA.
EM akchilvery@talladega.edu
RI Yang, Bin/P-8529-2014;
OI Yang, Bin/0000-0002-5667-9126; Xiao, Kai /0000-0002-0402-8276
NR 77
TC 10
Z9 10
U1 13
U2 123
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1947-7988
J9 J PHOTON ENERGY
JI J. Photonics Energy
PD JAN 6
PY 2015
VL 5
AR 057402
DI 10.1117/1.JPE.5.057402
PG 14
WC Materials Science, Multidisciplinary; Optics; Physics, Applied
SC Materials Science; Optics; Physics
GA CG1HG
UT WOS:000353023100001
ER
PT J
AU Nishimori, H
Tsuda, J
Knysh, S
AF Nishimori, Hidetoshi
Tsuda, Junichi
Knysh, Sergey
TI Comparative study of the performance of quantum annealing and simulated
annealing
SO PHYSICAL REVIEW E
LA English
DT Article
ID ADIABATIC EVOLUTION; ISING-MODEL; OPTIMIZATION; MECHANICS; QUBITS
AB Relations of simulated annealing and quantum annealing are studied by a mapping from the transition matrix of classical Markovian dynamics of the Ising model to a quantum Hamiltonian and vice versa. It is shown that these two operators, the transition matrix and the Hamiltonian, share the eigenvalue spectrum. Thus, if simulated annealing with slow temperature change does not encounter a difficulty caused by an exponentially long relaxation time at a first-order phase transition, the same is true for the corresponding process of quantum annealing in the adiabatic limit. One of the important differences between the classical-to-quantum mapping and the converse quantum-to-classical mapping is that the Markovian dynamics of a short-range Ising model is mapped to a short-range quantum system, but the converse mapping from a short-range quantum system to a classical one results in long-range interactions. This leads to a difference in efficiencies that simulated annealing can be efficiently simulated by quantum annealing but the converse is not necessarily true. We conclude that quantum annealing is easier to implement and is more flexible than simulated annealing. We also point out that the present mapping can be extended to accommodate explicit time dependence of temperature, which is used to justify the quantum-mechanical analysis of simulated annealing by Somma, Batista, and Ortiz. Additionally, an alternative method to solve the nonequilibrium dynamics of the one-dimensional Ising model is provided through the classical-to-quantum mapping.
C1 [Nishimori, Hidetoshi; Tsuda, Junichi] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Knysh, Sergey] NASA, QuAIL, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Knysh, Sergey] SGT Inc, Greenbelt, MD 20770 USA.
RP Nishimori, H (reprint author), Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
FU JSPS KAKENHI [26287086]; INFN; Office of the Director of National
Intelligence (ODNI), Intelligence Advanced Research Projects Activity
(IARPA) [IAA 145483]; AFRL Information Directorate [F4HBKC4162G001]
FX The work of H.N. was supported by JSPS KAKENHI Grant No. 26287086. H.N.
and J.T. thank the Galileo Galilei Institute for Theoretical Physics
(Florence) for hospitality and INFN for partial support during the
completion of this work. The work of S.K. was supported in part by the
Office of the Director of National Intelligence (ODNI), Intelligence
Advanced Research Projects Activity (IARPA) via Grant No. IAA 145483,
and by the AFRL Information Directorate under Grant No. F4HBKC4162G001.
The views and conclusions contained herein are those of the authors and
should not be interpreted as necessarily representing the official
policies or endorsements, either expressed or implied, of ODNI, IARPA,
AFRL, or the U.S. Government. The U.S. Government is authorized to
reproduce and distribute reprints for Governmental purpose
notwithstanding any copyright annotation thereon.
NR 35
TC 7
Z9 7
U1 1
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
EI 1550-2376
J9 PHYS REV E
JI Phys. Rev. E
PD JAN 6
PY 2015
VL 91
IS 1
AR 012104
DI 10.1103/PhysRevE.91.012104
PG 8
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA CA2JO
UT WOS:000348734900003
PM 25679567
ER
PT J
AU Menezes, AA
Cumbers, J
Hogan, JA
Arkin, AP
AF Menezes, Amor A.
Cumbers, John
Hogan, John A.
Arkin, Adam P.
TI Towards synthetic biological approaches to resource utilization on space
missions
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Review
DE space synthetic biology; methanogens; cyanobacteria; Spirulina;
polyhydroxybutyrate; acetaminophen
ID CARBON-DIOXIDE; RECOMBINANT CYANOBACTERIUM; PHOTOSYNTHETIC CONVERSION;
MICROBIAL-PRODUCTION; ACETATE PRODUCTION; BACTERIAL-SPORES;
LIFE-SUPPORT; OUTER-SPACE; PCC 6803; ANTIBIOTICS
AB This paper demonstrates the significant utility of deploying non-traditional biological techniques to harness available volatiles and waste resources on manned missions to explore the Moon and Mars. Compared with anticipated non-biological approaches, it is determined that for 916 day Martian missions: 205 days of high-quality methane and oxygen Mars bio-production with Methanobacterium thermoautotrophicum can reduce the mass of a Martian fuel-manufacture plant by 56%; 496 days of biomass generation with Arthrospira platensis and Arthrospira maxima on Mars can decrease the shipped wet-food mixed-menu mass for a Mars stay and a one-way voyage by 38%; 202 days of Mars polyhydroxybutyrate synthesis with Cupriavidus necator can lower the shipped mass to three-dimensional print a 120 m(3) six-person habitat by 85% and a few days of acetaminophen production with engineered Synechocystis sp. PCC 6803 can completely replenish expired or irradiated stocks of the pharmaceutical, thereby providing independence from unmanned resupply spacecraft that take up to 210 days to arrive. Analogous outcomes are included for lunar missions. Because of the benign assumptions involved, the results provide a glimpse of the intriguing potential of 'space synthetic biology', and help focus related efforts for immediate, near-term impact.
C1 [Menezes, Amor A.] Univ Calif Berkeley, California Inst Quantitat Biosci, Berkeley, CA 94704 USA.
[Cumbers, John] NASA Ames Res Ctr, NASA Ames Space Portal, Moffett Field, CA 94035 USA.
[Hogan, John A.] NASA Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA.
[Arkin, Adam P.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Arkin, Adam P.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA.
RP Menezes, AA (reprint author), Univ Calif Berkeley, California Inst Quantitat Biosci, 2151 Berkeley Way, Berkeley, CA 94704 USA.
EM amenezes@berkeley.edu
RI Menezes, Amor/L-2893-2014; Arkin, Adam/A-6751-2008
OI Menezes, Amor/0000-0003-3923-5766; Arkin, Adam/0000-0002-4999-2931
FU National Aeronautics and Space Administration; University of California,
Santa Cruz, University Affiliated Research Center's Aligned Research
Programme [NAS2-03144 Task TO.030.14.MD.D]
FX We appreciate the funding provided by the National Aeronautics and Space
Administration and the University of California, Santa Cruz, University
Affiliated Research Center's Aligned Research Programme: NAS2-03144 Task
TO.030.14.MD.D.
NR 153
TC 7
Z9 7
U1 8
U2 54
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD JAN 6
PY 2015
VL 12
IS 102
AR UNSP 20140715
DI 10.1098/rsif.2014.0715
PG 20
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AU3GI
UT WOS:000345500000002
PM 25376875
ER
PT J
AU Bhatia, AK
Drachman, RJ
AF Bhatia, A. K.
Drachman, R. J.
TI Photoejection with excitation in H- and other systems
SO PHYSICAL REVIEW A
LA English
DT Article
ID HELIUM ISOELECTRONIC SEQUENCE; DOUBLE PHOTOIONIZATION; STATES; 11S
AB Lyman-alpha radiation, 1216 angstrom, has been seen from the sun and from various astrophysical sources. This radiation arises from the radiative transition from the 2p P-2 state to the 1s S-2 state of the hydrogen atom. The 2P state can be excited from the 1s S-2 state by electron impact. However, it is possible to produce this excited state by photodetachment of the H- ion, leaving the H atom in the 2P state. We have calculated cross sections for this process using Hylleraas- type functions for the H- ion and using the exchange approximation for the photoelectron in the final continuum states of angular momenta equal to 0 and 2. The photoabsorption cross sections in Hions or He atoms leaving the hydrogen atom and helium ion in 2 S-2 are also calculated. Similar calculations have been carried out for the Li+, Be2+, and C4+ ions.
C1 [Bhatia, A. K.; Drachman, R. J.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
NR 10
TC 2
Z9 2
U1 0
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
EI 1094-1622
J9 PHYS REV A
JI Phys. Rev. A
PD JAN 5
PY 2015
VL 91
IS 1
DI 10.1103/PhysRevA.91.012702
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA AY9TS
UT WOS:000347894000004
ER
PT J
AU Aartsen, MG
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bos, F
Bose, D
Boser, S
Botner, O
Brayeur, L
Bretz, HP
Brown, AM
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Christy, B
Clark, K
Classen, L
Clevermann, F
Coenders, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
Day, M
De Andre, JPAM
De Clercq, C
De Ridder, S
Desiati, P
De Vries, KD
De With, M
DeYoung, T
Diaz-Velez, JC
Dunkman, M
Eagan, R
Eberhardt, B
Eichmann, B
Eisch, J
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Felde, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Franckowiak, A
Frantzen, K
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Gier, D
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Goodman, JA
Gora, D
Grant, D
Gretskov, P
Groh, JC
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallen, P
Hallgren, A
Halzen, F
Hanson, K
Hebecker, D
Heereman, D
Heinen, D
Helbing, K
Hellauer, R
Hellwig, D
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huang, F
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Jagielski, K
Japaridze, GS
Jero, K
Jlelati, O
Jurkovic, M
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kauer, M
Keivani, A
Kelley, JL
Kheirandish, A
Kiryluk, J
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Koob, A
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Kriesten, A
Krings, K
Kroll, G
Kroll, M
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Larsen, DT
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leute, J
Lunemann, J
Madsen, J
Maggi, G
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meli, A
Meures, T
Miarecki, S
Middell, E
Middlemas, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Paul, L
Penek, O
Pepper, JA
Heros, CPD
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Putz, J
Quinnan, M
Radel, L
Rameez, M
Rawlins, K
Redl, P
Rees, I
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Riedel, B
Robertson, S
Rodrigues, JP
Rongen, M
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Sander, HG
Sandroos, J
Santander, M
Sarkar, S
Schatto, K
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Sestayo, Y
Seunarine, S
Shanidze, R
Smith, MWE
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stanisha, NA
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Strotjohann, NL
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Tosi, D
Tselengidou, M
Unger, E
Usner, M
Vallecorsa, S
van Eijndhoven, N
Vandenbroucke, J
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallraff, M
Weaver, C
Wellons, M
Wendt, C
Westerhoff, S
Whelan, BJ
Whitehorn, N
Wichary, C
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zoll, M
AF Aartsen, M. G.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Classen, L.
Clevermann, F.
Coenders, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
Day, M.
De Andre, J. P. A. M.
De Clercq, C.
De Ridder, S.
Desiati, P.
De Vries, K. D.
De With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eichmann, B.
Eisch, J.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Felde, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Franckowiak, A.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Gier, D.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Goodman, J. A.
Gora, D.
Grant, D.
Gretskov, P.
Groh, J. C.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallen, P.
Hallgren, A.
Halzen, F.
Hanson, K.
Hebecker, D.
Heereman, D.
Heinen, D.
Helbing, K.
Hellauer, R.
Hellwig, D.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huang, F.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Jagielski, K.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Jurkovic, M.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kheirandish, A.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koob, A.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kriesten, A.
Krings, K.
Kroll, G.
Kroll, M.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Larsen, D. T.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leute, J.
Luenemann, J.
Madsen, J.
Maggi, G.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meli, A.
Meures, T.
Miarecki, S.
Middell, E.
Middlemas, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Paul, L.
Penek, OE.
Pepper, J. A.
Heros, C. Perez de los
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Puetz, J.
Quinnan, M.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Rees, I.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Riedel, B.
Robertson, S.
Rodrigues, J. P.
Rongen, M.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Sander, H. -G.
Sandroos, J.
Santander, M.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Sestayo, Y.
Seunarine, S.
Shanidze, R.
Smith, M. W. E.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stanisha, N. A.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Stroem, R.
Strotjohann, N. L.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Tosi, D.
Tselengidou, M.
Unger, E.
Usner, M.
Vallecorsa, S.
van Eijndhoven, N.
Vandenbroucke, J.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallraff, M.
Weaver, Ch.
Wellons, M.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Whitehorn, N.
Wichary, C.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zierke, S.
Zoll, M.
TI Atmospheric and astrophysical neutrinos above 1 TeV interacting in
IceCube
SO PHYSICAL REVIEW D
LA English
DT Article
ID HIGH-ENERGY NEUTRINOS; FLUX PREDICTIONS; INDUCED CASCADES; PROMPT
LEPTONS; GAMMA-RAY; AMANDA; PERFORMANCE; ASTRONOMY; BLAZARS; SEARCH
AB The IceCube Neutrino Observatory was designed primarily to search for high-energy (TeV-PeV) neutLrinos produced in distant astrophysical objects. A search for. greater than or similar to 100 TeV neutrinos interacting inside the instrumented volume has recently provided evidence for an isotropic flux of such neutrinos. At lower energies, IceCube collects large numbers of neutrinos from the weak decays of mesons in cosmic-ray air showers. Here we present the results of a search for neutrino interactions inside IceCube's instrumented volume between 1 TeV and 1 PeV in 641 days of data taken from 2010-2012, lowering the energy threshold for neutrinos from the southern sky below 10 TeV for the first time, far below the threshold of the previous high-energy analysis. Astrophysical neutrinos remain the dominant component in the southern sky down to a deposited energy of 10 TeV. From these data we derive new constraints on the diffuse astrophysical neutrino spectrum, Phi(v) = 2.06(-0.3)(+0.4) x 10(-18) (E-v = 10(5) GeV)-2.46 +/- 0.12GeV-1 cm(-2) sr(-1) s(-1) for 25 TeV < E-v < 1.4 PeV, as well as the strongest upper limit yet on the flux of neutrinos from charmed-meson decay in the atmosphere, 1.52 times the benchmark theoretical prediction used in previous IceCube results at 90% confidence.
C1 [Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Goldschmidt, A.; Gretskov, P.; Haack, C.; Hallen, P.; Heinen, D.; Hellwig, D.; Jagielski, K.; Koob, A.; Kriesten, A.; Krings, K.; Leuermann, M.; Paul, L.; Penek, OE.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Phys Inst 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. J.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[De With, M.; Kolanoski, H.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Fedynitch, A.; Kroll, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Hebecker, D.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Strotjohann, N. L.; Usner, M.; Voge, M.] Univ Bonn, Phys Inst, D-53115 Bonn, Germany.
[Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, CP230, B-1050 Brussels, Belgium.
[Bernhard, A.; Brayeur, L.; Casier, M.; De Clercq, C.; De Vries, K. D.; Golup, G.; Kunnen, J.; Luenemann, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel VIB, Dienst ELEM, B-1050 Brussels, Belgium.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Cheung, E.; Christy, B.; Felde, J.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Koskinen, D. J.; Larson, M. J.; Medici, M.; Sandroos, J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Odrowski, S.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept phys nucl & corpusculaire, CH-1211 Geneva, Switzerland.
[De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Meli, A.; Ryckbosch, D.; 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.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[DeYoung, T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bernhard, A.; Coenders, S.; Gross, A.; Jurkovic, M.; Leute, J.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Mnchen, D-85748 Garching, Germany.
[Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Kurahashi, N.] Drexel Univ, Dept Phys, 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.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; De Andre, J. P. A. M.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Keivani, A.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; Heros, C. Perez de los; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Terliuk, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Tokyo 1130032, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP van Santen, J (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM jvansanten@icecube.wisc.edu
RI Auffenberg, Jan/D-3954-2014; Maruyama, Reina/A-1064-2013; Koskinen,
David/G-3236-2014; Tjus, Julia/G-8145-2012; Sarkar, Subir/G-5978-2011;
Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012;
OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Strotjohann, Nora
Linn/0000-0002-4667-6730; Arguelles Delgado, Carlos/0000-0003-4186-4182;
Auffenberg, Jan/0000-0002-1185-9094; Maruyama,
Reina/0000-0003-2794-512X; Koskinen, David/0000-0002-0514-5917; Sarkar,
Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch,
Christopher/0000-0002-6418-3008; Rott, Carsten/0000-0002-6958-6033;
Perez de los Heros, Carlos/0000-0002-2084-5866
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, and National
Energy Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada; WestGrid and Compute/Calcul
Canada; Swedish Research Council; Swedish Polar Research Secretariat;
Swedish National Infrastructure for Computing (SNIC); Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz
Alliance for Astroparticle Physics (HAP); Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland; National Research Foundation of Korea
(NRF); Danish National Research Foundation; Denmark (DNRF)
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin - Madison, the Open Science Grid (OSG)
grid infrastructure; U.S. Department of Energy, and National Energy
Research Scientific Computing Center, the Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada, WestGrid and Compute/Calcul
Canada; Swedish Research Council, Swedish Polar Research Secretariat,
Swedish National Infrastructure for Computing (SNIC), and Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz
Alliance for Astroparticle Physics (HAP), Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO), FWO Odysseus programme,Flanders Institute to
encourage scientific and technological research in industry (IWT),
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); the Swiss National
Science Foundation (SNSF), Switzerland; National Research Foundation of
Korea (NRF); Danish National Research Foundation, Denmark (DNRF).
NR 82
TC 85
Z9 86
U1 2
U2 25
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 5
PY 2015
VL 91
IS 2
AR 022001
DI 10.1103/PhysRevD.91.022001
PG 16
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AZ0GR
UT WOS:000347924700001
ER
PT J
AU Jouffray, JB
Nystrom, M
Norstrom, AV
Williams, ID
Wedding, LM
Kittinger, JN
Williams, GJ
AF Jouffray, Jean-Baptiste
Nystrom, Magnus
Norstrom, Albert V.
Williams, Ivor D.
Wedding, Lisa M.
Kittinger, John N.
Williams, Gareth J.
TI Identifying multiple coral reef regimes and their drivers across the
Hawaiian archipelago
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE boosted regression trees; coral reefs; disturbance; Hawai'i; multiple
regimes; resilience
ID PHASE-SHIFTS; NUTRIENT ENRICHMENT; ALGAL SUCCESSION; CLIMATE-CHANGE;
GLOVERS REEF; RESILIENCE; HERBIVORY; FISH; ECOSYSTEMS; DYNAMICS
AB Loss of coral reef resilience can lead to dramatic changes in benthic structure, often called regime shifts, which significantly alter ecosystem processes and functioning. In the face of global change and increasing direct human impacts, there is an urgent need to anticipate and prevent undesirable regime shifts and, conversely, to reverse shifts in already degraded reef systems. Such challenges require a better understanding of the human and natural drivers that support or undermine different reef regimes. The Hawaiian archipelago extends across a wide gradient of natural and anthropogenic conditions and provides us a unique opportunity to investigate the relationships between multiple reef regimes, their dynamics and potential drivers. We applied a combination of exploratory ordination methods and inferential statistics to one of the most comprehensive coral reef datasets available in order to detect, visualize and define potential multiple ecosystem regimes. This study demonstrates the existence of three distinct reef regimes dominated by hard corals, turf algae or macroalgae. Results from boosted regression trees show nonlinear patterns among predictors that help to explain the occurrence of these regimes, and highlight herbivore biomass as the key driver in addition to effluent, latitude and depth.
C1 [Jouffray, Jean-Baptiste] Royal Swedish Acad Sci, Global Econ Dynam & Biosphere Acad Programme, S-10405 Stockholm, Sweden.
[Jouffray, Jean-Baptiste; Nystrom, Magnus; Norstrom, Albert V.] Stockholm Univ, Stockholm Resilience Ctr, S-10691 Stockholm, Sweden.
[Williams, Ivor D.] NOAA, CRED, PIFSC, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA.
[Wedding, Lisa M.; Kittinger, John N.] Stanford Univ, Stanford Woods Inst Environm, Ctr Ocean Solut, Monterey, CA 93940 USA.
[Kittinger, John N.] Conservat Int, Betty & Gordon Moore Ctr Sci & Oceans, Honolulu, HI USA.
[Williams, Gareth J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Jouffray, JB (reprint author), Royal Swedish Acad Sci, Global Econ Dynam & Biosphere Acad Programme, POB 50005, S-10405 Stockholm, Sweden.
EM jean-baptiste.jouffray@su.se
FU Erling-Persson Family Foundation; Royal Swedish Academy of Sciences;
Mistra
FX This work was partly funded by the Erling-Persson Family Foundation
through Global Economic Dynamics and the Biosphere at the Royal Swedish
Academy of Sciences. Mistra supported this research through a core grant
to the Stockholm Resilience Centre.
NR 60
TC 19
Z9 19
U1 9
U2 71
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD JAN 5
PY 2015
VL 370
IS 1659
AR 20130268
DI 10.1098/rstb.2013.0268
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA AW2WK
UT WOS:000346147200007
ER
PT J
AU Smoot, BR
AF Smoot, Betsy Rohaly
TI NSA Release and Transfer of Records Related to William F. Friedman
SO CRYPTOLOGIA
LA English
DT Editorial Material
DE William F. Friedman; National Security Agency; declassification
AB Papers related to the work of William F. Friedman will soon be transferred from the National Security Agency to the National Archives and Records Administration. This is expected to be the largest digital release in NSA's history to date.
C1 [Smoot, Betsy Rohaly] NASA, Ctr Cryptol Hist, Washington, DC USA.
RP Smoot, BR (reprint author), Ctr Cryptol Hist, 9800 Savage Rd, Ft George G Meade, FL 20755 USA.
EM ersmoot@nsa.gov
NR 0
TC 1
Z9 1
U1 0
U2 0
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0161-1194
EI 1558-1586
J9 CRYPTOLOGIA
JI Cryptologia
PD JAN 2
PY 2015
VL 39
IS 1
BP 1
EP 2
DI 10.1080/01611194.2015.974404
PG 2
WC Computer Science, Theory & Methods; History & Philosophy Of Science;
Mathematics, Applied
SC Computer Science; History & Philosophy of Science; Mathematics
GA AW9NC
UT WOS:000346583200001
ER
PT S
AU Ryoo, MS
Rothrock, B
Matthies, L
AF Ryoo, M. S.
Rothrock, Brandon
Matthies, Larry
GP IEEE
TI Pooled Motion Features for First-Person Videos
SO 2015 IEEE CONFERENCE ON COMPUTER VISION AND PATTERN RECOGNITION (CVPR)
SE IEEE Conference on Computer Vision and Pattern Recognition
LA English
DT Proceedings Paper
CT IEEE Conference on Computer Vision and Pattern Recognition (CVPR)
CY JUN 07-12, 2015
CL Boston, MA
SP IEEE
AB In this paper, we present a new feature representation for first-person videos. In first-person video understanding (e.g., activity recognition), it is very important to capture both entire scene dynamics (i.e., egomotion) and salient local motion observed in videos. We describe a representation framework based on time series pooling, which is designed to abstract short-term/long-term changes in feature descriptor elements. The idea is to keep track of how descriptor values are changing over time and summarize them to represent motion in the activity video. The framework is general, handling any types of per-frame feature descriptors including conventional motion descriptors like histogram of optical flows (HOF) as well as appearance descriptors from more recent convolutional neural networks (CNN).
We experimentally confirm that our approach clearly outperforms previous feature representations including bag-of-visual-words and improved Fisher vector (IFV) when using identical underlying feature descriptors. We also confirm that our feature representation has superior performance to existing state-of-the-art features like local spatio-temporal features and Improved Trajectory Features (originally developed for 3rd-person videos) when handling first-person videos. Multiple first-person activity datasets were tested under various settings to confirm these findings.
C1 [Ryoo, M. S.; Rothrock, Brandon; Matthies, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Ryoo, MS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM mryoo@jpl.nasa.gov
NR 21
TC 4
Z9 4
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1063-6919
BN 978-1-4673-6964-0
J9 PROC CVPR IEEE
PY 2015
BP 896
EP 904
PG 9
WC Computer Science, Artificial Intelligence
SC Computer Science
GA BG3KA
UT WOS:000387959200098
ER
PT S
AU Shu, TM
Xie, D
Rothrock, B
Todorovic, S
Zhu, SC
AF Shu, Tianmin
Xie, Dan
Rothrock, Brandon
Todorovic, Sinisa
Zhu, Song-Chun
GP IEEE
TI Joint Inference of Groups, Events and Human Roles in Aerial Videos
SO 2015 IEEE CONFERENCE ON COMPUTER VISION AND PATTERN RECOGNITION (CVPR)
SE IEEE Conference on Computer Vision and Pattern Recognition
LA English
DT Proceedings Paper
CT IEEE Conference on Computer Vision and Pattern Recognition (CVPR)
CY JUN 07-12, 2015
CL Boston, MA
SP IEEE
ID REPRESENTATION; RECOGNITION
AB With the advent of drones, aerial video analysis becomes increasingly important; yet, it has received scant attention in the literature. This paper addresses a new problem of parsing low-resolution aerial videos of large spatial areas, in terms of 1) grouping, 2) recognizing events and 3) assigning roles to people engaged in events. We propose a novel framework aimed at conducting joint inference of the above tasks, as reasoning about each in isolation typically fails in our setting. Given noisy tracklets of people and detections of large objects and scene surfaces (e.g., building, grass), we use a spatiotemporal AND-OR graph to drive our joint inference, using Markov Chain Monte Carlo and dynamic programming. We also introduce a new formalism of spatiotemporal templates characterizing latent sub-events. For evaluation, we have collected and released a new aerial videos dataset using a hex-rotor flying over picnic areas rich with group events. Our results demonstrate that we successfully address above inference tasks under challenging conditions.
C1 [Shu, Tianmin; Xie, Dan; Zhu, Song-Chun] Univ Calif Los Angeles, Ctr Vis Cognit Learning & Art, Los Angeles, CA USA.
[Rothrock, Brandon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Todorovic, Sinisa] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA.
RP Shu, TM (reprint author), Univ Calif Los Angeles, Ctr Vis Cognit Learning & Art, Los Angeles, CA USA.
EM stm512@g.ucla.edu; xiedan@g.ucla.edu; brandon.rothrock@jpl.nasa.gov;
sinisa@onid.orst.edu; sczhu@stat.ucla.edu
NR 40
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1063-6919
BN 978-1-4673-6964-0
J9 PROC CVPR IEEE
PY 2015
BP 4576
EP 4584
PG 9
WC Computer Science, Artificial Intelligence
SC Computer Science
GA BG3KA
UT WOS:000387959204067
ER
PT B
AU Ma, GSK
Wang, KL
Malpas, J
Iizuka, Y
Xenophontos, C
Turkmani, AA
Chan, GHN
Usuki, T
Chan, QHS
AF Ma, George S. -K.
Wang, Kuo-Lung
Malpas, John
Iizuka, Yoshiyuki
Xenophontos, Costas
Turkmani, Abdulsalam A.
Chan, Gavin H. -N.
Usuki, Tadashi
Chan, Queenie H. -S.
BE Khan, A
Deschamps, F
TI Melt Pockets and Spongy Clinopyroxenes in Mantle Xenoliths from the
Plio-Quaternary Al Ghab Volcanic Field, NW Syria: Implications for the
Metasomatic Evolution of the Lithosphere
SO EARTH'S HETEROGENEOUS MANTLE: A GEOPHYSICAL, GEODYNAMICAL, AND
GEOCHEMICAL PERSPECTIVE
SE Springer Geophysics
LA English
DT Article; Book Chapter
DE Mantle metasomatism; Spongy texture; Thermobarometry; Lithospheric
mantle; Melt pocket
ID DEAD-SEA FAULT; PERIDOTITE XENOLITHS; TRACE-ELEMENT; CARBONATITE
METASOMATISM; SILICATE MELT; SPINEL-PERIDOTITE; CENTRAL CHINA;
ULTRAMAFIC XENOLITHS; GEOCHEMICAL EVIDENCE; 4-PHASE LHERZOLITES
AB Spongy minerals, especially clinopyroxenes, and fine-grained, often glass-bearing mineral assemblages, commonly referred to as melt pockets, occur in many mantle xenolith suites worldwide, but their origins remain far from being clearly understood. We describe a suite of spongy clinopyroxene- and melt pockets-bearing peridotite xenoliths from the Plio-Quaternary volcanic field in the Al Ghab Depression, a pull-apart basin of the Dead Sea Fault System in northwestern Syria. The melt pockets comprise fine-grained olivines, clinopyroxenes, spinels and feldspars +/- amphiboles +/- glasses. Petrography and major and trace element mineral chemistry suggest that the xenoliths have experienced at least two stages of metasomatism with the formation of the melt pockets being associated with the latest event. The first metasomatic episode featuring LREE, Na, Th, U enrichment and relative Ti and Zr depletion in the cores of primary clinopyroxenes involved metasomatism by a low-silica, CO2-rich agent. The second metasomatic episode was associated with the development of melt pockets which evolved from decompressional and perhaps metasomatism-induced incongruent melting of clinopyroxene +/- spinel. The spongy clinopyroxenes that occur as coronas around clear, primary clinopyroxenes represent a transitional stage of the partially melted crystals. The incongruent melting produced a liquid that evolved within the melt pockets and eventually migrated out to form amphiboles and micas elsewhere in the lithosphere. Albeit with some uncertainty, geothermobarometric estimations reveal significant, systematic differences in the equilibration pressures between the primary minerals (0.8- 1.4 GPa), and spongy and melt-pocket minerals (0.7-0.9 GPa), lending good support for the decompressional origins of the spongy clinopyroxenes and melt pockets. It is interpreted that decompression resulted from local transtension associated with the development of the Al Ghab pull-apart basin, a step-over zone of the Dead Sea Fault System, in Plio-Quaternary time.
C1 [Ma, George S. -K.; Wang, Kuo-Lung; Iizuka, Yoshiyuki; Usuki, Tadashi] Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan.
[Ma, George S. -K.] Dragon Min Consulting, Unit 1701, Hong Kong, Hong Kong, Peoples R China.
[Ma, George S. -K.; Malpas, John; Xenophontos, Costas; Chan, Gavin H. -N.] Univ Hong Kong, Dept Earth Sci, Pokfulam, Hong Kong, Peoples R China.
[Turkmani, Abdulsalam A.] Minist Petr & Mineral Resources, Gen Estab Geol & Mineral Resources, Damascus, Syria.
[Turkmani, Abdulsalam A.] Al Badia Cement Co JSC, Damascus, Syria.
[Chan, Gavin H. -N.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England.
[Chan, Gavin H. -N.] SRK Consulting, Wanchai, Hong Kong, Peoples R China.
[Chan, Queenie H. -S.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA.
RP Ma, GSK (reprint author), Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan.
EM georgema@graduate.hku.hk
NR 93
TC 0
Z9 0
U1 1
U2 1
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
BN 978-3-319-15627-9; 978-3-319-15626-2
J9 SPRINGER GEOPHYS
PY 2015
BP 205
EP 257
DI 10.1007/978-3-319-15627-9_7
D2 10.1007/978-3-319-15627-9
PG 53
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA BF9SM
UT WOS:000385856300008
ER
PT J
AU Hashemi, KE
Akella, MR
Pak, CG
AF Hashemi, Kelley E.
Akella, Maruthi R.
Pak, Chan-gi
GP IEEE
TI Tracking Error Convergence for Multi-Input Multi-Output Model Reference
Adaptive Control with Known Nonminimum Phase Zeros
SO 2015 54TH IEEE CONFERENCE ON DECISION AND CONTROL (CDC)
LA English
DT Proceedings Paper
CT 54th IEEE Conference on Decision and Control (CDC)
CY DEC 15-18, 2015
CL Osaka, JAPAN
SP Kozo Keikaku Engn, MathWorks, Springer, CYBERNET Syst, Mitsubishi Elect, Soc Ind & Appl Math, Altair, Int Journal Automat & Comp, IEEE CAA Journal Automatica Sinica, Cogent Engn, Now, IHI, IEEE
ID SYSTEMS; EDGE
AB This paper presents a tracking error convergence proof for the multi-input multi-output direct model reference adaptive control problem. The proof is valid for square plants that are potentially nonminimum phase. This work is an extension of the surrogate tracking error adaptive control techniques previously developed, though the assumed plant structure is altered to accommodate a wider range of dynamics. Error convergence is demonstrated using a composite system construction with Lyapunov stability techniques. The performance of the proposed control design is demonstrated through simulation of a linear version of an aircraft wing's aeroelasitc pitch and plunge dynamics.
C1 [Hashemi, Kelley E.; Akella, Maruthi R.] Univ Texas Austin, Dept Aerosp Engn, Austin, TX 78712 USA.
[Pak, Chan-gi] NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA.
RP Hashemi, KE (reprint author), Univ Texas Austin, Dept Aerosp Engn, Austin, TX 78712 USA.
EM kehutch@utexas.edu; makella@mail.utexas.edu; chan-gi.pak-1@nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-7886-1
PY 2015
BP 489
EP 494
PG 6
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA BF4PY
UT WOS:000381554500096
ER
PT J
AU Ono, M
Droge, G
Grip, H
Toupet, O
Scrapper, C
Rahmani, A
AF Ono, Masahiro
Droge, Greg
Grip, Havard
Toupet, Olivier
Scrapper, Chris
Rahmani, Amir
GP IEEE
TI Road-Following Formation Control of Autonomous Ground Vehicles
SO 2015 54TH IEEE CONFERENCE ON DECISION AND CONTROL (CDC)
LA English
DT Proceedings Paper
CT 54th IEEE Conference on Decision and Control (CDC)
CY DEC 15-18, 2015
CL Osaka, JAPAN
SP Kozo Keikaku Engn, MathWorks, Springer, CYBERNET Syst, Mitsubishi Elect, Soc Ind & Appl Math, Altair, Int Journal Automat & Comp, IEEE CAA Journal Automatica Sinica, Cogent Engn, Now, IHI, IEEE
ID RECEDING HORIZON CONTROL; SYSTEMS
AB This work presents a novel cooperative path planning for formation keeping robots traversing along a road with obstacles and possible narrow passages. A unique challenge in this problem is a requirement for spatial and temporal coordination between vehicles while ensuring collision and obstacle avoidance. A two-step approach is used for fast real-time planning. The first step uses the A* search on a spatio-temporally extended graph to generate an obstacle-free path for the agent while the second step refines this path through local optimization to comply with dynamic and other vehicle constraints. This approach keeps robots close to their intended formation while giving them flexibility to negotiate narrow passages and obstacles, adhering to any given constraints.
C1 [Ono, Masahiro; Grip, Havard; Toupet, Olivier; Rahmani, Amir] CALTECH, Jet Prop Lab, Robot & Estimat Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Droge, Greg; Scrapper, Chris] Space & Naval Warfare Syst Command, San Diego, CA 92152 USA.
RP Ono, M (reprint author), CALTECH, Jet Prop Lab, Robot & Estimat Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Masahiro.Ono@jpl.nasa.gov; greg.droge@navy.mil;
Havard.F.Grip@jpl.nasa.gov; Olivier.Toupet@jpl.nasa.gov;
chris.scrapper@navy.mil; Amir.Rahmani@jpl.nasa.gov
NR 17
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-7886-1
PY 2015
BP 4714
EP 4721
PG 8
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA BF4PY
UT WOS:000381554504143
ER
PT J
AU Cichella, V
Marinho, T
Stipanovic, D
Hovakimyan, N
Kaminer, I
Trujillo, A
AF Cichella, Venanzio
Marinho, Thiago
Stipanovic, Dusan
Hovakimyan, Naira
Kaminer, Isaac
Trujillo, Anna
GP IEEE
TI Collision Avoidance Based on Line-of-Sight Angle
SO 2015 54TH IEEE CONFERENCE ON DECISION AND CONTROL (CDC)
LA English
DT Proceedings Paper
CT 54th IEEE Conference on Decision and Control (CDC)
CY DEC 15-18, 2015
CL Osaka, JAPAN
SP Kozo Keikaku Engn, MathWorks, Springer, CYBERNET Syst, Mitsubishi Elect, Soc Ind & Appl Math, Altair, Int Journal Automat & Comp, IEEE CAA Journal Automatica Sinica, Cogent Engn, Now, IHI, IEEE
ID UNMANNED AIR VEHICLES; OBSTACLE AVOIDANCE; COVERAGE CONTROL; NETWORKS;
TRACKING; ROBOTS
AB This paper addresses the problem of collision avoidance for fixed-wing unmanned aerial vehicles. The angular velocity of the aircraft is adjusted in order to avert a possible collision with cooperative or uncooperative obstacles. The novelty of this work is that the control law uses only the line-of-sight angle as feedback, which can be obtained from an inertial measurement unit and a gimbaled camera mounted onboard the vehicle. This work aims at providing a solution to the collision avoidance problem for small low-cost unmanned aerial platforms, which are not equipped with sensors capable of measuring data such as position and velocity of the obstacle. This problem of practical relevance is faced from a theoretical standpoint. A Lyapunov based analysis is outlined, which provides safety guarantees under a given set of assumptions that the obstacle must satisfy. Simulation results are presented to validate the theoretical findings.
C1 [Cichella, Venanzio; Marinho, Thiago; Stipanovic, Dusan; Hovakimyan, Naira] Univ Illinois, Urbana, IL 61801 USA.
[Kaminer, Isaac] Naval Postgrad Sch, Monterey, CA 93943 USA.
[Trujillo, Anna] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
RP Cichella, V (reprint author), Univ Illinois, Urbana, IL 61801 USA.
NR 27
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-7886-1
PY 2015
BP 6779
EP 6784
PG 6
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA BF4PY
UT WOS:000381554506156
ER
PT S
AU Rumsey, CL
AF Rumsey, Christopher L.
BE Eisfeld, B
TI Application of Reynolds Stress Models to Separated Aerodynamic Flows
SO DIFFERENTIAL REYNOLDS STRESS MODELING FOR SEPARATING FLOWS IN INDUSTRIAL
AERODYNAMICS
SE Springer Tracts in Mechanical Engineering
LA English
DT Article; Book Chapter
ID DRAG PREDICTION WORKSHOP; TURBULENT FLOWS; CLOSURE
AB Several variations of omega-based second-moment Reynolds stress models (RSMs) are applied to two-dimensional and three-dimensional separated aerodynamic flows. In many of these flows, widely used one-and two-equation linear eddy-viscosity turbulence models are known to be inadequate for predicting separated flow characteristics. As potentially important non-linear behavior is naturally included in RSMs, it was hoped that they might improve the separated flow predictions. However, the RSMs perform no better than the simpler models for these particular flows. Like the simpler models, the RSMs predict too little turbulence in the separated shear layer of the two-dimensional flow over a hump, which is indicative of modeling deficiencies for this class of flows. Nonetheless, the best RSM version tested offers a convenient framework for possible future model improvements.
C1 [Rumsey, Christopher L.] NASA Langley Res Ctr, Computat AeroSci Branch, Mail Stop 128, Hampton, VA 23681 USA.
RP Rumsey, CL (reprint author), NASA Langley Res Ctr, Computat AeroSci Branch, Mail Stop 128, Hampton, VA 23681 USA.
EM c.l.rumsey@nasa.gov
NR 29
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2195-9870
BN 978-3-319-15639-2; 978-3-319-15638-5
J9 SPR TRACTS MECH ENG
PY 2015
BP 19
EP 37
DI 10.1007/978-3-319-15639-2_
D2 10.1007/978-3-319-15639-2
PG 19
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA BF8OY
UT WOS:000385217200003
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING Introduction
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Editorial Material; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 1
EP 9
D2 10.1002/9781118897072
PG 9
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000002
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Modern Design and Optimization
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 10
EP 26
D2 10.1002/9781118897072
PG 17
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000003
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING Preface
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Editorial Material; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP XIII
EP XIV
D2 10.1002/9781118897072
PG 2
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000001
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Constrained Design Space Search
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 27
EP 46
D2 10.1002/9781118897072
PG 20
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000004
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Direct Search Methods for Locating the Optimum of a Design Problem with
a Single-Objective Function
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 47
EP 79
D2 10.1002/9781118897072
PG 33
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000005
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Guided Random Search and Network Techniques
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 80
EP 97
D2 10.1002/9781118897072
PG 18
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000006
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Optimizing Multiobjective Function Problems
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 98
EP 115
D2 10.1002/9781118897072
PG 18
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000007
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Sensitivity Analysis
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
ID EIGENVECTOR DERIVATIVES; COUPLED SYSTEMS; COMPLEX
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 23
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 116
EP 154
D2 10.1002/9781118897072
PG 39
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000008
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Multidisciplinary Design Optimization Architectures
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
ID SENSITIVITY DERIVATIVES; COUPLED SYSTEMS; COMPLEX
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 51
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 155
EP 207
D2 10.1002/9781118897072
PG 53
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000009
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Knowledge Based Engineering
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
ID DESIGN
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 34
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 208
EP 257
D2 10.1002/9781118897072
PG 50
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000010
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Uncertainty-Based Multidisciplinary Design Optimization
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
ID ROBUST DESIGN; SYSTEMS-DESIGN; FRAMEWORK
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 36
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 258
EP 286
D2 10.1002/9781118897072
PG 29
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000011
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Ways and Means for Control and Reduction of the Optimization
Computational Cost and Elapsed Time
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 287
EP 309
D2 10.1002/9781118897072
PG 23
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000012
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Implementation of KBE in an MDO System
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 310
EP 348
D2 10.1002/9781118897072
PG 39
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000013
ER
PT B
AU Sobieszczanski-Sobieski, J
Morris, A
van Tooren, MJL
La Rocca, G
Yao, W
AF Sobieszczanski-Sobieski, Jaroslaw
Morris, Alan
van Tooren, Michel J. L.
La Rocca, Gianfranco
Yao, Wen
BA SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
BF SobieszczanskiSobieski, J
Morris, A
VanTooren, MJL
LaRocca, G
Yao, W
TI Guide to Implementing an MDO System
SO MULTIDISCIPLINARY DESIGN OPTIMIZATION SUPPORTED BY KNOWLEDGE BASED
ENGINEERING
LA English
DT Article; Book Chapter
C1 [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morris, Alan] Cranfield Univ, Cranfield MK43 0AL, Beds, England.
[van Tooren, Michel J. L.] Univ South Carolina, Columbia, SC USA.
[La Rocca, Gianfranco] Delft Univ Technol, Delft, Netherlands.
[Yao, Wen] Natl Univ Def Technol, Changsha, Hunan, Peoples R China.
RP Sobieszczanski-Sobieski, J (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-118-89709-6; 978-1-118-49212-3
PY 2015
BP 349
EP 359
D2 10.1002/9781118897072
PG 11
WC Engineering, Multidisciplinary
SC Engineering
GA BF8SP
UT WOS:000385228000014
ER
PT J
AU Abercromby, AFJ
Gernhardt, ML
Chappell, SP
Lee, DE
Howe, AS
AF Abercromby, Andrew F. J.
Gernhardt, Michael L.
Chappell, Steven P.
Lee, David E.
Howe, A. Scott
GP IEEE
TI Human Exploration of Phobos
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID NEAR-EARTH ASTEROIDS
AB This study developed, analyzed, and compared mission architectures for human exploration of Mars' moons within the context of an Evolvable Mars Campaign. METHODS: All trades assumed conjunction class missions to Phobos (approximately 500 days in Mars system) as it was considered the driving case for the transportation architecture. All architectures assumed that the Mars transit habitat would remain in a high-Mars orbit (HMO) with crewmembers transferring between HMO and Phobos in a small crew taxi vehicle. A reference science/exploration program was developed including performance of a standard set of tasks at 55 locations on the Phobos surface. Detailed EVA timelines were developed using realistic flight rules to accomplish the reference science tasks using exploration systems ranging from jetpacks to multi-person pressurized excursion vehicles combined with Phobos surface and orbital (L1, L4/L5, 20 km distant-retrograde-orbit [DRO]) habitat options. Detailed models of propellant mass, crew time, science productivity, radiation exposure, systems and consumables masses, and other figures of merit were integrated to enable quantitative comparison of different architectural options. Options for prestaging assets using solar electric propulsion versus delivering all systems with the crew were also evaluated. Seven discrete mission architectures were evaluated. RESULTS: The driving consideration for habitat location (Phobos surface versus orbital) was radiation exposure, with an estimated reduction in cumulative mission radiation exposure of up to 34% (versus a Mars orbital mission) when the habitat is located on the Phobos surface, compared with only 3% to 6% reduction for a habitat in a 20-km DRO. The exploration utility of lightweight unpressurized excursion vehicles was limited by the need to remain within 20 minutes of solar particle event radiation protection combined with complex guidance, navigation, and control systems required by the nonintuitive and highly-variable gravitational environment. Two-person pressurized excursion vehicles as well as mobile surface habitats offer significant exploration capability and operational benefits compared with unpressurized extravehicular activity (EVA) mobility systems at the cost of increased system and propellant mass. Mechanical surface translation modes (ie, hopping) were modeled and offered potentially significant propellant savings and the possibility of extended exploration operations between crewed missions. Options for extending the use of the crew taxi vehicle were examined, including use as an exploration asset for Phobos surface exploration (when combined with an alternate mobility system) and as an EVA platform, both on Phobos and for contingency EVA on the Mars transit habitat. CONCLUSIONS: Human exploration of Phobos offers a scientifically meaningful first step towards human Mars surface missions that develops and validates transportation, habitation, and exploration systems and operations in advance of the Mars landing systems.
C1 [Abercromby, Andrew F. J.; Chappell, Steven P.] Wyle Sci Technol & Engn Grp, Wyle HAC 37C 2101 NASA Pkwy, Houston, TX 77058 USA.
[Gernhardt, Michael L.; Lee, David E.] NASA, Houston, TX 77058 USA.
[Howe, A. Scott] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Abercromby, AFJ (reprint author), Wyle Sci Technol & Engn Grp, Wyle HAC 37C 2101 NASA Pkwy, Houston, TX 77058 USA.
EM andrew.abercromby@nasa.gov; michael.l.gernhardt@nasa.gov;
steven.p.chappell@nasa.gov; david.e.lee@nasa.gov;
scott.howe@jpl.nasa.gov
NR 30
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 17
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501304021
ER
PT J
AU Acord, K
Parker, M
Dodd, E
Kang, J
Kulczycki, E
Budney, C
AF Acord, Katherine
Parker, Mimi
Dodd, Emma
Kang, Jamie
Kulczycki, Eric
Budney, Charles
GP IEEE
TI High Frequency Vibration and High Gravity Force Shock Testing for
Potential Mars Sample Return
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB The current concept for a potential Mars Sample Return ( MSR) campaign includes a series of missions that could drill, package, and return Mars rock cores to Earth through four sequential flight missions. A combination of structural stability, migration, force, hardware testing and analysis were employed to determine elements within the potential MSR campaign that could alter the mechanical integrity of Mars rock cores during transport to Earth. Therefore, Mars simulant rock cores, such as Bishop Tuff and China Ranch Massive Gypsum, were drilled to create samples for survivability tests to simulate the high frequency vibrations of a Mars Ascent Vehicle ( MAV) and high gravity force shock of the Earth Entry Vehicle ( EEV) that would be expected during MSR. Prototype hardware was designed and fabricated to accommodate the cores desired for vibration and shock testing. Proto-flight ( PF) and flight acceptance ( FA) vibration levels were established for both solid and liquid MAV fuel types. Drilling methods were investigated to produce both pristine and fractured cores. Elements such as core orientation, amount of ullage ( headspace), and clamshell position were tested to better understand the causes and amount of fracturing throughout these flight-like environments.
C1 [Acord, Katherine; Parker, Mimi; Dodd, Emma; Kang, Jamie; Kulczycki, Eric; Budney, Charles] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Acord, K (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Kaacord@ucdavis.edu; Mimiaudiaparker@gmail.com; Emma_Dodd@brown.edu;
Jdkang@csupomona.edu; Eric.A.Kulczycki@jpl.nasa.gov;
Charles.J.Budney@jpl.nasa.gov
NR 5
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 9
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303075
ER
PT J
AU Aguirre, F
Custodero, B
Shah, B
AF Aguirre, Fernando
Custodero, Brian
Shah, Biren
GP IEEE
TI Ka-Band Tone Generator for the ISARA Cubesat
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB This paper describes the design and fabrication of a 26GHz tone generator for the ISA RA Cubesat. The tone generator uses a phase locked loop (PLL) frequency multiplier to get to 26GHz from an on board temperature compensated crystal oscillator (TCXO). The output of the PLL feeds a solid state power amplifier (SSPA) that puts out approximately 27dBm of RF power. The SSPA output then feeds a monolithic microwave integrated circuit (MMIC) switch which toggles between a high gain and low gain antenna as part of the ISA RA experiment. The microwave electronics is packaged in an aluminum chassis and utilizes hybrid assembly technology. There are bare die with ribbon and wire interconnects in addition to printed circuit boards (PCB) which use surface mount technology (SMT) for assembly. Custom distributed circuits were designed for im plementing the 26GHz filters, couplers and power detectors. A key aspect of this module's performance is its overall thermal stability which is highly dependent upon its assembly technology. The order of operations of each assembly phase, attachment materials, contamination control and reliability of interconnects all determine how well the hardware performs in flight.
C1 [Aguirre, Fernando; Custodero, Brian; Shah, Biren] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Aguirre, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Fernando.H.Aguirre@ipl.nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 6
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501304028
ER
PT J
AU Aguirre, FH
AF Aguirre, Fernando H.
GP IEEE
TI X-Band Electronics for the INSPIRE Cubesat Deep Space Radio
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB This paper describes the design, fabrication and test results of the X-Band hardware for the Jet Propulsion Laboratory's (JPL) INSPIRE Cubesat deep space radio also known as Iris. The radio communicates with NASA's Deep Space Network (DSN) and is the first known deep space Cubesat radio to take part in the DSN communication link. The complete RF electronics stack weighs less than 300 grams, has a modulation bandwidth of greater than 100MHz, puts out greater than 24dBm of RF power and has greater than 50dB of receiver adjustable gain control (AGC) range. The antennas are Right-Hand Circular Polarized (RHCP) patches and are designed to attach to the top and bottom of the Cubesat structure to allow for broad coverage in the case of tumbling. The electronics is composed of Commercial off the Shelf (COTS) parts selected in order to meet the typical Cubesat budget constraints and avoid long lead times. The RF electronics is designed to accommodate the use of custom aluminum covers and commercially available gasket shielding. These cover assemblies were designed and put in place in order to reduce Electromagnetic Interference (EM I), crosstalk and also provide a relatively large thermal mass to help stabilize and spread the heat resulting from dissipated power in the electronics.
C1 [Aguirre, Fernando H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Aguirre, FH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Fernando.H.Aguirre@jpl.nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 10
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501304029
ER
PT J
AU Ajluni, T
Linn, T
Willcockson, W
Everett, D
Mink, R
Wood, J
AF Ajluni, Thomas
Linn, Timothy
Willcockson, William
Everett, David
Mink, Ronald
Wood, Joshua
GP IEEE
TI OSIRIS-REx, Returning the Asteroid Sample
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB This paper addresses the technical aspects of the sample return system for the upcoming Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) asteroid sample return mission. The overall mission design and current implementation are presented as an overview to establish a context for the technical description of the reentry and landing segment of the mission.
The prime objective of the OSIRIS-REx mission is to sample a primitive, carbonaceous asteroid and to return that sample to Earth in pristine condition for detailed laboratory analysis. Targeting the near-Earth asteroid Bennu, the mission launches in September 2016 with an Earth reentry date of September 24,2023.
OSIRIS-REx will thoroughly characterize asteroid Bennu providing knowledge of the nature of near-Earth asteroids that is fundamental to understanding planet formation and the origin of life. The return to Earth of pristine samples with known geologic context will enable precise analyses that cannot be duplicated by spacecraft-based instruments, revolutionizing our understanding of the early Solar System. Bennu is both the most accessible carbonaceous asteroid and one of the most potentially Earth-hazardous asteroids known. Study of Bennu addresses multiple NASA objectives to understand the origin of the Solar System and the origin of life and will provide a greater understanding of both the hazards and resources in near-Earth space, serving as a precursor to future human missions to asteroids.
This paper focuses on the technical aspects of the Sample Return Capsule (SRC) design and concept of operations, including trajectory design and reentry retrieval. Highlights of the mission are included below.
The OSIRIS-REx spacecraft provides the essential functions for an asteroid characterization and sample return mission:
attitude control
propulsion
power
thermal control
telecommunications
command and data handling
structural support to ensure successful rendezvous with Bennu
characterization of Bennu's properties
delivery of the sampler to the surface, and return of the spacecraft to the vicinity of the Earth
sample collection, performed by the Touch-and-Go Sample Acquisition Mechanism (TAGSAM), to acquire a regolith sample from the surface
Earth re-entry and SRC recovery
Following sample collection, OSIRIS-REx drifts away from Bennu until the Asteroid Departure Maneuver is commanded on March 4, 2021, sending OSIRIS-REx on a ballistic return cruise to Earth. No additional large deterministic maneuvers are required to return the SRC to Earth. During the cruise, tracking and trajectory correction maneuvers (TCMs) are performed as necessary to precisely target the entry corridor. As OSIRIS-REx approaches Earth, the reentry plans are reviewed starting about a year before arrival, and preparations begin. The spacecraft is targeted away from the Earth until 7 days before entry. The final two trajectory correction maneuvers bring the spacecraft on target toward the Utah Test and Training Range (UTTR), with sufficient time for contingency resolution. The SRC releases 4 hours prior to atmospheric entry interface and, using the Stardust capsule heritage design, employs a traditional drogue and main parachute descent system for a soft touchdown.
C1 [Ajluni, Thomas] ASRC Fed Space & Def, 7000 Muirkirk Meadows Dr, Beltsville, MD 20705 USA.
[Linn, Timothy; Willcockson, William; Wood, Joshua] Lockheed Martin Space Syst Co, Denver, CO 80201 USA.
[Everett, David; Mink, Ronald] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ajluni, T (reprint author), ASRC Fed Space & Def, 7000 Muirkirk Meadows Dr, Beltsville, MD 20705 USA.
EM thomas.m.ajluni@nasa.gov; timothy.m.linn@lmco.com;
william.h.willcockson@lmco.com; david.f.everett@nasa.gov;
ronald.g.mink@nasa.gov; joshua.l.wood@lmco.com
NR 1
TC 0
Z9 0
U1 2
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 15
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301020
ER
PT J
AU Allwood, A
Wade, L
Clark, B
Elam, T
Flannery, D
Foote, M
Hurowitz, J
Knowles, E
AF Allwood, Abigail
Wade, Lawrence
Clark, Ben
Elam, Tim
Flannery, David
Foote, Marc
Hurowitz, Joel
Knowles, Emily
GP IEEE
TI Texture-specific elemental analysis of rocks and soils with PIXL: The
Planetary Instrument for X-ray Lithochemistry on Mars 2020
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID STROMATOLITES; FLUORESCENCE; AUSTRALIA
AB PIXL (Planetary Instrument for X-ray Lithochemistry) is a micro-focus X-ray fluorescence instrument for examining fine scale chemical variations in rocks and soils on planetary surfaces. Selected for flight on the science payload for the proposed Mars 2020 rover, PIXL can measure elemental chemistry of tiny features observed in rocks, such as individual sand grains, veinlets, cements, concretions and crystals, using a 100 mu m-diameter, high-flux X-ray beam that can be scanned across target surfaces.
At the heart of PIXL, a polycapillary X-ray focusing optic focuses the X-ray beam down to a similar to 100 mu m spot. The optic is coupled to a state-of-the-art miniature microfocus X-ray tube. The X-ray beam produced by the focused X-ray source yields extremely high fluorescent X-ray count rates, enabling sensitive analysis of each spot in a few seconds. In 5-10 seconds, PIXL reveals major and minor elements in a sample. In 1 to 2 minutes, sensitive trace element analysis is achieved. Different measurement strategies allow flexibility during operations to respond to scientific opportunities and resource constraints. PIXL can perform line or grid measurements on abraded or natural (unabraded) surfaces.
With operational flexibility, high spatial resolution, high sensitivity, a wide range of detectable elements, rapid spectral acquisition and a raster scanning capability for chemical mapping, PIXL would enable detailed insights to past habitability and the potential for preservation of biosignatures.
C1 [Allwood, Abigail; Wade, Lawrence; Flannery, David; Foote, Marc; Knowles, Emily] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Clark, Ben] Space Sci Inst, Boulder, CO 80301 USA.
[Elam, Tim] Univ Washington, Seattle, WA 98195 USA.
[Hurowitz, Joel] SUNY Stony Brook, Stony Brook, NY 11794 USA.
RP Allwood, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Abigail.C.Allwood@jpl.nasa.gov; lawrence.a.wade@jpl.nasa.gov;
bclark@spacescience.org; wtelam@apl.washington.edu;
flannery@jpl.nasa.gov; joel.hurowitz@stonybrook.edu
NR 15
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 13
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302035
ER
PT J
AU Arevalo, R
Brinckerhoff, W
van Amerom, F
Danell, R
Pinnick, V
Li, X
Getty, S
Hovmand, L
Grubisic, A
Mahaffy, P
Goesmann, F
Steininger, H
AF Arevalo, Ricardo, Jr.
Brinckerhoff, William
van Amerom, Friso
Danell, Ryan
Pinnick, Veronica
Li, Xiang
Getty, Stephanie
Hovmand, Lars
Grubisic, Andrej
Mahaffy, Paul
Goesmann, Fred
Steininger, Harald
CA MOMA Team
GP IEEE
TI Design and Demonstration of the Mars Organic Molecule Analyzer (MOMA) on
the ExoMars 2018 Rover
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID MARTIAN SOIL; PERCHLORATE; ORIGIN
AB The Mars Organic Molecule Analyzer (MOMA) investigation is a key astrobiology experiment scheduled to launch on the joint ESA-Roscosmos ExoMars 2018 rover mission. MOMA will examine the chemical composition of geological samples acquired from depths of up to two meters below the martian surface, where fragile organic molecules may be protected from destructive cosmic radiation and/or oxidative chemical reactions. The heart of the MOMA mass spectrometer subsystem (i.e., MOMA-MS) is a miniaturized linear ion trap (LIT) that supports two distinct modes of operation to detect: i) volatile and semi-volatile, low-to-moderate mass organics (<= 500 Da) via pyrolysis coupled with gas chromatography mass spectrometry (pyr/GCMS); and, ii) more refractory, moderate-to-high mass compounds (up to 1000 Da) via laser desorption (LDMS) at ambient Mars pressures. Additionally, the LIT mass analyzer enables selective ion trapping via multi-frequency waveform ion excitation (e.g., stored waveform inverse Fourier transform, or SWIFT), and structural characterization of complex molecules using tandem mass spectrometry (MSIMS).
A high-fidelity Engineering Test Unit (ETU) of MOMA-MS,including the LIT subassembly, dual-gun electron ionization source, micropirani pressure gauge, solenoid-driven aperture valve, redundant detection chains, and control electronics, has been built and tested at NASA GSFC under relevant operational conditions (pressure, temperature, etc.). Spaceflight qualifications of individual hardware components and integrated subassemblies have been validated through vibration, shock, thermal, lifetime, and performance evaluations. The ETU serves as a pathfinder for the flight model buildup, integration and test, as the ETU meets the form, fit and function of the flight unit that will be delivered to MPS in late 2015. To date, the ETU of MOMA-MS has been shown to meet or exceed all functional requirements, including mass range, resolution, accuracy, instrumental drift, and limit-of-detection specifications, thereby enabling the primary science objectives of the MOMA investigation and ExoMars 2018 mission.
C1 [Arevalo, Ricardo, Jr.; Brinckerhoff, William; Mahaffy, Paul] NASA, Goddard Space Flight Ctr, Code 699, Greenbelt, MD 20771 USA.
[van Amerom, Friso] Mini Mass Consulting Inc, Hyattsville, MD USA.
[Danell, Ryan] Danell Consulting Inc, Winterville, NC USA.
[Pinnick, Veronica; Li, Xiang] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA.
[Hovmand, Lars] Linear Labs LLC, Washington, DC USA.
[Grubisic, Andrej] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Goesmann, Fred; Steininger, Harald] Max Planck Inst Solar Syst Res MPS, D-37077 Gottingen, Germany.
Univ Paris Est, LISA, Creteil, France.
Lab Atmospheres Milieux Observat Spatiales LATMOS, Guyancourt, France.
Ecole Cent Paris, LGPM, Chatenay Malabry, France.
[MOMA Team] Laser Zentrum Hannover eV LZH, Hannover, Germany.
RP Arevalo, R (reprint author), NASA, Goddard Space Flight Ctr, Code 699, Greenbelt, MD 20771 USA.
RI Li, Xiang/F-4539-2012
NR 15
TC 0
Z9 0
U1 4
U2 4
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 11
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302011
ER
PT J
AU Babuscia, A
Choi, T
Lee, C
Cheung, KM
AF Babuscia, Alessandra
Choi, Thomas
Lee, Charles
Cheung, Kar-Ming
GP IEEE
TI Inflatable Antennas and Arrays for Interplanetary Communication using
CubeSats and SmallSats
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID DESIGN
AB In-1 the past, great progress has been made in the development of small satellites and CubeSats, mainly for low Earth orbit. Currently, a new technological trend is the development of technologies and strategies for potential interplanetary applications of small platforms (CubeSats/Satellites). Given the limited size, mass and power capabilities of these small platforms, one of the most interesting problems is how to allow small satellites to communicate from very far distance in the solar system. This paper aims to review and possibly combine two solutions for the problem: the use of inflatable antenna reflectors and the arrays across multiple spacecraft. An overview of the inflatable antenna technology, its development and tests, its applicability in terms of frequencies and sizes, and the advantages with respect to other technologies is described. An overview of cooperative communication techniques across small platforms is presented and the main challenges of arraying antennas on different spacecraft are underlined. Finally, the two solutions are combined to provide a first order quantification of the advantages in terms of EIRP, data rate and range.
C1 [Babuscia, Alessandra; Choi, Thomas; Lee, Charles; Cheung, Kar-Ming] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Babuscia, A (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alessandra.Babuscia@jpl.nasa.gov; Thomas.Choi@jpl.nasa.gov;
Charles.H.Lee@jpl.nasa.gov; Kar-Ming.Cheung@jpl.nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 8
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302106
ER
PT J
AU Babuscia, A
Divsalar, D
Cheung, KM
AF Babuscia, Alessandra
Divsalar, Dariush
Cheung, Kar-Ming
GP IEEE
TI CDMA communications systems with constant envelope modulation for
CubeSats
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB In this paper a communication system for CubeSats in formation to operate in the vicinity of the Lunar Lagrangian L1 is proposed. CubeSats will collect lunar scientific data and will perform surface observations. An improved low complexity CDMA system for CubeSats for communications between the Lunar L1 and Earth station is considered. The complexity of a coded CDMA transmitter is lower than the complexity of the CDMA receiver with decoder therefore for downlink communications it makes sense to use encoders such as space standard LDPC code followed by a spread spectrum transmitter for CDMA systems for CubeSats. For the uplink an uncoded CDMA system is chosen since the uplink transmit power is expected to be high enough to support the use of uncoded CDMA system. The uncoded CDMA yields receivers for CubeSats that have low complexity implementation. For uplink since there would be no multipath the use of orthogonal spreading codes is more appropriate. The choice of orthogonal codes would reduce the multiuser interference at CubeSats. For the downlink, based on the available bandwidth, and the data rates, a reasonable processing gain could be obtained. Thus the multiuser interference degradation due to the other CubeSats could be made small at the Earth station. In this paper we analyzed and simulated the proposed improved CDMA system for a concept Constellation of CubeSats. All system simulations are done using Simulink Matlab platform. For highly efficient nonlinear power amplifiers we use a filtered offset QPSK with phase modulation which is a CCSDS standard for constant envelope signaling. This allows a nonlinear amplifier at CubeSat to operate at saturation point for the highest efficiency. We compare the difference in performance with our current pulse shaped BPSK (using half-sine wave). Certainly if there is no bandwidth limitation (due to the spectral standard masking) we could as well use unfiltered rectangular pulses which would produce constant envelope signaling. But it seems that rectangular pulses will not satisfy the bandwidth limitation imposed by the spectral standard. Filtered offset QPSK with phase modulation is much more bandwidth efficient scheme.
C1 [Babuscia, Alessandra; Divsalar, Dariush; Cheung, Kar-Ming] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Babuscia, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alessandra.babuscia@jpl.nasa.gov; dariush.divsalar@jpl.nasa.gov;
kar-ming.cheung@jpl.nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 8
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301072
ER
PT J
AU Bayer, T
Cooke, B
Gontijo, I
Kirby, K
AF Bayer, Todd
Cooke, Brian
Gontijo, I.
Kirby, Karen
GP IEEE
TI Europa Clipper Mission: the habitability of an icy moon
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID CALLISTO; FIELDS
AB Europa, the fourth largest moon of Jupiter, is believed to be one of the best places in the solar system to look for extant life beyond Earth. The 2011 Planetary Decadal Survey, Vision and Voyages, states: "Because of this ocean's potential suitability for life, Europa is one of the most important targets in all of planetary science". Exploring Europa to investigate its habitability is the goal of the proposed Europa Clipper mission. This exploration is intimately tied to understanding the three "ingredients" for life: liquid water, chemistry, and energy. The Europa Clipper mission would investigate these ingredients by comprehensively exploring Europa's ice shell and liquid ocean interface, surface geology and surface composition to glean insight into the inner workings of this fascinating moon. In addition, a lander mission is seen as a possible future step, but current data about the Jovian radiation environment and about potential landing site hazards and potential safe landing zones is insufficient. Therefore an additional goal of the mission would be to characterize the radiation environment near Europa and investigate scientifically compelling sites for hazards, to inform a potential future landed mission.
The proposed Europa Clipper mission concept envisions sending a flight system, consisting of a spacecraft equipped with a payload of NASA-selected scientific instruments, to execute numerous flybys of Europa while in Jupiter orbit. A key challenge is that the flight system must survive and operate in the intense Jovian radiation environment, which is especially harsh at Europa. The innovative design of this multiple-flyby tour is an enabling feature of this mission: by minimizing the time spent in the radiation environment the spacecraft complexity and cost has been significantly reduced compared to previous mission concepts. The spacecraft would launch from Kennedy Space Center (KSC), Cape Canaveral, Florida, USA, on a NASA supplied launch vehicle, no earlier than 2022. The proposed mission would be formulated and implemented by a joint Jet Propulsion Laboratory (JPL) and Applied Physics Laboratory (APL) Project team.
C1 [Bayer, Todd; Cooke, Brian; Gontijo, I.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kirby, Karen] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Bayer, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Todd.J.Bayer@jpl.nasa.gov; Karen.Kirby@JHUAPL.EDU
NR 6
TC 0
Z9 0
U1 6
U2 6
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 12
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501300068
ER
PT J
AU Beegle, L
Bhartia, R
White, M
DeFlores, L
Abbey, W
Wu, YH
Cameron, B
Moore, J
Fries, M
Burton, A
Edgett, KS
Ravine, MA
Hug, W
Reid, R
Nelson, T
Clegg, S
Wiens, R
Asher, S
Sobron, P
AF Beegle, Luther
Bhartia, Rohit
White, Mary
DeFlores, Lauren
Abbey, William
Wu, Yen-Hung
Cameron, Bruce
Moore, James
Fries, Marc
Burton, Aaron
Edgett, Kenneth S.
Ravine, Michael A.
Hug, William
Reid, Ray
Nelson, Tony
Clegg, Sam
Wiens, Roger
Asher, Sanford
Sobron, Pablo
GP IEEE
TI SHERLOC: Scanning Habitable Environments with Raman & Luminescence for
Organics & Chemicals
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID MARS
AB SHERLOC is an arm-mounted fluorescence and Raman spectrometer that was recently selected to be part of the payload for the next proposed NASA rover mission to Mars, scheduled for launch in 2020. SHERLOC enables non-contact, spatially resolved, high sensitivity detection and characterization of organics and minerals on the Martian surface. The investigation goals are to assess past aqueous history, detect the presence and preservation potential of biosignatures, and support the selection of samples for caching and potential return to Earth.
C1 [Beegle, Luther; Bhartia, Rohit; White, Mary; DeFlores, Lauren; Abbey, William; Wu, Yen-Hung; Cameron, Bruce; Moore, James] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Fries, Marc; Burton, Aaron] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA.
[Edgett, Kenneth S.; Ravine, Michael A.] Malian Space Sci Syst, San Diego, CA 92191 USA.
[Hug, William; Reid, Ray] Photon Syst Inc, Covina, CA 91722 USA.
[Nelson, Tony; Clegg, Sam; Wiens, Roger] Los Alamos Natl Lab, Los Alamos, NM USA.
[Asher, Sanford] Univ Pittsburgh, Dept Chem, Pittsburgh, PA 15260 USA.
[Sobron, Pablo] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Sobron, Pablo] MalaUva Labs, St Louis, MO 63104 USA.
RP Beegle, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Luther.Beegle@jpl.nasa.gov; Rohit.Bhartia@jpl.nasa.gov;
Mary.L.White@jpl.nasa.gov; Lauren.P.DeFlores@jpl.nasa.gov;
cameras@msss.com; w.hug@Photonsystems.com; r.reid@Photonsystems.com;
Asher@pitt.edu
NR 26
TC 0
Z9 0
U1 3
U2 3
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 10
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302041
ER
PT J
AU Beilicke, M
Kislat, F
Zajczyk, A
Guo, Q
Endsley, R
Cowsik, R
Dowkontt, P
Krawczynski, H
Barthelmy, S
Hams, T
Okajima, T
Sasaki, M
De Geronimo, G
Haba, Y
Saji, S
AF Beilicke, Matthias
Kislat, F.
Zajczyk, A.
Guo, Q.
Endsley, R.
Cowsik, R.
Dowkontt, P.
Krawczynski, H.
Barthelmy, S.
Hams, T.
Okajima, T.
Sasaki, M.
De Geronimo, G.
Haba, Y.
Saji, S.
GP IEEE
TI First flight of the X-ray polarimeter X-Calibur
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID ACCRETING BLACK-HOLES; RELATIVISTIC JETS; POLARIZATION; EMISSION;
RADIATION; ASTRONOMY; GRAVITY; CRAB
AB X-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard Xray polarimeter, X-Calibur, to be used in the focal plane of the balloon-borne InFOC mu S grazing incidence X-ray telescope with the goal of observing astrophysical sources. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 20-60 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. A I-day test. flight of the instrument was performed from Ft.Sumner, NM, In fall 2014. The sensitivity, performance and first results form the flight will be presented.
C1 [Beilicke, Matthias; Kislat, F.; Zajczyk, A.; Guo, Q.; Endsley, R.; Cowsik, R.; Dowkontt, P.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Beilicke, Matthias; Kislat, F.; Zajczyk, A.; Guo, Q.; Endsley, R.; Cowsik, R.; Dowkontt, P.; Krawczynski, H.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Barthelmy, S.; Hams, T.; Okajima, T.; Sasaki, M.] Goddard Space Flight Ctr, Greenbelt, MD USA.
[De Geronimo, G.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Haba, Y.; Saji, S.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
RP Beilicke, M (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.
EM beilicke@physics.wustl.edu
NR 29
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 10
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501300041
ER
PT J
AU Benz, N
Viazzo, D
Gundy-Burlet, K
AF Benz, Nathaniel
Viazzo, Danilo
Gundy-Burlet, Karen
GP IEEE
TI Multi-Purpose Spacecraft Simulator for LADEE
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB The Lunar Atmosphere Dust Environment Explorer (LADEE) was a small explorer class spacecraft that was launched on Sept 7, 2013. After completing all of the mission objectives, LADEE was de-orbited and successfully impacted the moon's surface on April 17, 2014. In order to reduce costs and leverage previous research and development, LADEE utilized the "common modular bus" design. The physical construction utilized a low-cost, rapidly prototyped design and the same philosophy drove the development of the software base. To achieve this goal, a Model Based Design approach was utilized to develop the On-board Flight SoftWare (OFSW), and coincident with this, a model-based multipurpose simulator was created of the LADEE spacecraft and its mission environment. The spacecraft simulator was designed to have sufficient fidelity that it could be used to test the required modes and responses of the OFSW. A faster-than-real-time Workstation SIMulator (WSIM) version of the LADEE simulator was used to develop and test the software control algorithms in the Simulink environment. The automatic code generation feature in Simulink was used to port the simulation to several real-time environments to support Processor-in-the-Loop (PIL) and Hardware-in-the-Loop (HIL) testing, verification and validation. Since the simulation interface was designed to be compatible with the command interface employed by the LADEE mission operation team, the WSIM, PIL and HIL simulators were used for both personnel training (nominal and off-nominal operations) prior to the mission and to perform command sequence verification during the mission. This approach resulted in time and budget savings, and allowed changes to the model to be quickly propagated through all the simulation target environments. The mode-based design approach also allows the simulation framework to be generalized and reused to model future small-satellite missions.
C1 [Benz, Nathaniel] MEI, Moffett Field, CA 94035 USA.
[Viazzo, Danilo] Cummings Aerosp, Dublin, CA 94568 USA.
[Gundy-Burlet, Karen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Benz, N (reprint author), MEI, Moffett Field, CA 94035 USA.
EM nbenz@meicompany.com; danilo.viazzo@cummingsaerospace.com;
karen.gundy-burlet@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 14
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301003
ER
PT J
AU Beshore, E
Sutter, B
Mink, R
Lauretta, D
Moreau, M
Boynton, W
Everett, D
Dworkin, J
Shinohara, C
Gal-Edd, J
AF Beshore, Edward
Sutter, Brian
Mink, Ronald
Lauretta, Dante
Moreau, Michael
Boynton, William
Everett, David
Dworkin, Jason
Shinohara, Christopher
Gal-Edd, Jonathan
GP IEEE
TI The OSIRIS-REx Asteroid Sample Return Mission
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID 101955 BENNU; LIGHTCURVE
AB In September of 2016, the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, Security, Regolith EXplorer) spacecraft will depart for asteroid (101955) Bennu, and when it does, humanity will turn an important corner in the exploration of the Solar System. After arriving at the asteroid in the Fall of 2018, it will undertake a program of observations designed to select a site suitable for retrieving a sample that will be returned to the Earth in 2023.
The third mission in NASA's New Frontiers program, OSIRIS-REx will obtain a minimum of 60 g of a primitive asteroid's surface, the largest sample of extra-terrestrial material returned to the Earth since the end of the Apollo lunar missions (Figure 1). OSIRIS-REx will also return a separate sample of the fine-grained surface material that is <1 mm in diameter.
C1 [Beshore, Edward; Lauretta, Dante; Boynton, William; Shinohara, Christopher] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85705 USA.
[Sutter, Brian] Lockheed Martin Space Syst Co, Littleton, CO 80125 USA.
[Mink, Ronald; Moreau, Michael; Everett, David; Dworkin, Jason; Gal-Edd, Jonathan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Beshore, E (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85705 USA.
EM ebeshore@lpl.arizona.edu; brian.mspc.sutter@lmco.com;
ronald.g.mink@nasa.gov; lauretta@orex.lpl.arizona.edu;
michael.c.moreau@nasa.gov; wboynton@orex.lpl.arizona.edu;
David.F.Everett@nasa.gov; jason.p.dworkin@nasa.gov;
chriss@orex.lpl.arizona.edu; jonathan.s.gal-edd@nasa.gov
RI Dworkin, Jason/C-9417-2012
OI Dworkin, Jason/0000-0002-3961-8997
NR 9
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 13
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301021
ER
PT J
AU Blood, E
Ivanov, M
O'Farrell, C
Ginn, J
Kutty, P
Karlgaard, C
Dutta, S
AF Blood, Eric
Ivanov, Mark
O'Farrell, Clara
Ginn, Jason
Kutty, Prasad
Karlgaard, Chris
Dutta, Soumyo
GP IEEE
TI LDSD Supersonic Flight Dynamics Test 1: Post-flight Reconstruction
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID TRAJECTORY RECONSTRUCTION
AB The Low Density Supersonic Decelerator project's first Supersonic Flight Dynamics Test ( SFDT) occurred on June 28, 2014, off the west coast of Kauai, Hawaii, over the Pacific Ocean. The test vehicle traveled to speeds above Mach 4 and to an altitude of over 200,000 feet. This flight, although classified as a test architecture shake-out flight, tested two technologies: a robotic class Supersonic Inflatable Aerodynamic Decelerator and a Supersonic Disksail Parachute. The reconstruction team was tasked with collecting all relevant pre-flight and flight data to accurately reconstruct the trajectory and technology performance during the science phase of the flight. Furthermore, the reconstruction team has been involved with reconstructing and exploring all aerodynamic and test vehicle properties that affected the entire flight phase. This reconstruction provided insight into the technology performance, which is a key deliverable for the LDSD project, as well as provided insight into lessons learned for subsequent SFDT flights, in the fields of data recovery, reconstruction, and pre-flight trajectory simulations.
C1 [Blood, Eric; Ivanov, Mark; O'Farrell, Clara; Ginn, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kutty, Prasad; Karlgaard, Chris] Analyt Mech Associates Inc, Hampton, VA 23681 USA.
[Dutta, Soumyo] NASA, Langley Res Ctr, Hampon, VA 23681 USA.
RP Blood, E (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Eric.Blood@jpl.nasa.gov; Mark.C.Ivanov@jpl.nasa.gov;
Clara.O'Farrell@jpl.nasa.gov; Jason.M.Ginn@jpl.nasa.gov;
prasad.kutty@nasa.gov; chris.karlgaard-1@nasa.gov; soumyo.dutta@nasa.gov
NR 13
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 15
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303071
ER
PT J
AU Bobskill, MR
Lupisella, ML
Mueller, RP
Sibille, L
Vangen, S
Williams-Byrd, J
AF Bobskill, Marianne R.
Lupisella, Mark L.
Mueller, Rob P.
Sibille, Laurent
Vangen, Scott
Williams-Byrd, Julie
GP IEEE
TI Preparing for Mars: Evolvable Mars Campaign "Proving Ground" Approach
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB As the National Aeronautics and Space Administration (NASA) prepares to extend human presence beyond Low Earth Orbit, we are in the early stages of planning missions within the framework of an Evolvable Mars Campaign. Initial missions would be conducted in near-Earth cis-lunar space and would eventually culminate in extended duration crewed missions on the surface of Mars. To enable such exploration missions, critical technologies and capabilities must be identified, developed, and tested. NASA has followed a principled approach to identify critical capabilities and a "Proving Ground" approach is emerging to address testing needs. The Proving Ground is a period subsequent to current International Space Station activities wherein exploration-enabling capabilities and technologies are developed and the foundation is laid for sustained human presence in space. The Proving Ground domain essentially includes missions beyond Low Earth Orbit that will provide increasing mission capability while reducing technical risks. Proving Ground missions also provide valuable experience with deep space operations and support the transition from "Earth-dependence" to "Earth-independence" required for sustainable space exploration.
A Technology Development Assessment Team identified a suite of critical technologies needed to support the cadence of exploration missions. Discussions among mission planners, vehicle developers, subject-matter-experts, and technologists were used to identify a minimum but sufficient set of required technologies and capabilities. Within System Maturation Teams, known challenges were identified and expressed as specific performance gaps in critical capabilities, which were then refined and activities required to close these critical gaps were identified. Analysis was performed to identify test and demonstration opportunities for critical technical capabilities across the Proving Ground spectrum of missions. This suite of critical capabilities is expected to provide the foundation required to enable a variety of possible destinations and missions consistent with the Evolvable Mars Campaign..
The International Space Station will be used to the greatest extent possible for exploration capability and technology development. Beyond this, NASA is evaluating a number of options for Proving Ground missions. An "Asteroid Redirect Mission" will demonstrate needed capabilities (e.g., Solar Electric Propulsion) and transportation systems for the crew (i.e., Space Launch System and Orion) and for cargo (i.e., Asteroid Redirect Vehicle). The Mars 2020 mission and follow-on robotic precursor missions will gather Mars surface environment information and will mature technologies. NASA is considering emplacing a small pressurized module in cis-lunar space to support crewed operations of increasing duration and to serve as a platform for critical exploration capabilities testing (e.g., radiation mitigation; extended duration deep space habitation). In addition, "opportunistic mission operations" could demonstrate capabilities not on the Mars critical path that may, nonetheless, enhance exploration operations (e.g., teleoperations, crew assisted Mars sample return). The Proving Ground may also include "pathfinder" missions to test and demonstrate specific capabilities at Mars (e.g., entry, descent, and landing).
This paper describes the (1) process used to conduct an architecture-driven technology development assessment, (2) exploration mission critical and supporting capabilities, and (3) approach for addressing test and demonstration opportunities encompassing the spectrum of flight elements and destinations consistent with the Evolvable Mars Campaign.
C1 [Bobskill, Marianne R.; Williams-Byrd, Julie] NASA, Langley Res Ctr, 11 Langley Blvd, Hampton, VA 23681 USA.
[Lupisella, Mark L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20147 USA.
[Mueller, Rob P.; Vangen, Scott] NASA, Kennedy Space Ctr, FL 32899 USA.
[Sibille, Laurent] Enterprise Advisory Serv Inc, Kennedy Space Ctr, FL 32899 USA.
RP Bobskill, MR (reprint author), NASA, Langley Res Ctr, 11 Langley Blvd, Hampton, VA 23681 USA.
EM Marianne.r.bobskill@nasa.gov; Mark.L.lupisella@nasa.gov;
Rob.mueller@nasa.gov; Laurent.sibille-l@nasa.gov;
Scott.vangen-l@nasa.gov; Julie.a.williams-byrd@nasa.gov
NR 15
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 19
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501304008
ER
PT J
AU Bowie, J
Buffington, J
Hood, D
Kelly, C
Naids, A
AF Bowie, Jonathan
Buffington, Jesse
Hood, Drew
Kelly, Cody
Naids, Adam
GP IEEE
TI Asteroid Redirect Crewed Mission Space Suit and EVA System Maturation
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB The Asteroid Redirect Crewed Mission (ARCM) requires a Launch/Entry/Abort (LEA) suit capability and short duration Extra Vehicular Activity (EVA) capability from the Orion spacecraft. For this mission, the pressure garment selected for both functions is the Modified Advanced Crew Escape Suit (MACES) with EVA enhancements and the life support option that was selected is the Exploration Portable Life Support System (PLSS) currently under development for Advanced Exploration Systems (AES). The proposed architecture meets the ARCM constraints, but much more work is required to determine the details of the suit upgrades, the integration with the PLSS, and the tools and equipment necessary to accomplish the mission. This work has continued over the last year to better define the operations and hardware maturation of these systems. EVA simulations were completed in the Neutral Buoyancy Lab (NBL) and interfacing options were prototyped and analyzed with testing planned for late 2014. This paper discusses the work done over the last year on the MACES enhancements, the use of tools while using the suit, and the integration of the PLSS with the MACES.
C1 [Bowie, Jonathan; Buffington, Jesse; Hood, Drew; Kelly, Cody; Naids, Adam] NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77059 USA.
RP Bowie, J (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77059 USA.
EM jonathan.t.bowie@nasa.gov; jesse.a.buffington@nasa.gov;
anthony.d.hood@nasa.gov; cody.kelly-1@nasa.gov; adam.j.naids@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 15
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302105
ER
PT J
AU Brageot, E
Mercury, M
Green, R
Mouroulis, P
Gerwe, D
AF Brageot, Emily
Mercury, Michael
Green, Robert
Mouroulis, Pantazis
Gerwe, David
GP IEEE
TI Monitoring Earth's shortwave reflectance: GEO instrument concept
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID CLOUDS
AB In this paper we present a GEO instrument concept dedicated to monitoring the Earth's global spectral reflectance with a high revisit rate.
Based on our measurement goals, the ideal instrument needs to be highly sensitive (SNR>100) and to achieve global coverage with spectral sampling (10nm) and spatial sampling (<= 1km) over a large bandwidth (380-2510 nm) with a revisit time (>= 3x/day) sufficient to fully measure the spectral-radio metric-spatial evolution of clouds and confounding factor during daytime. After a brief study of existing instruments and their capabilities, we choose to use a GEO constellation of up to 6 satellites as a platform for this instrument concept in order to achieve the revisit time requirement with a single launch.
We derive the main parameters of the instrument and show the above requirements can be fulfilled while retaining an instrument architecture as compact as possible by controlling the telescope aperture size and using a passively cooled detector.
C1 [Brageot, Emily; Mercury, Michael; Green, Robert; Mouroulis, Pantazis] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gerwe, David] Boeing Phantom Works Adv Space & Network Syst, El Segundo, CA 90245 USA.
RP Brageot, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Emily.C.Brageot@jpl.nasa.gov; David.R.Gerwe@Boeing.com
NR 14
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 8
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301040
ER
PT J
AU Bregon, A
Daigle, M
Roychoudhury, I
AF Bregon, Anibal
Daigle, Matthew
Roychoudhury, Indranil
GP IEEE
TI An Integrated Framework for Distributed Diagnosis of Process and Sensor
Faults
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID SYSTEMS
AB Complex engineering systems require efficient online fault diagnosis methodologies to improve safety and reduce maintenance costs. In complex systems, faults may occur in the process itself but also in the sensors monitoring the system, which makes the fault diagnosis task difficult, because the signals from which diagnostic reasoning takes place may be corrupted by faulty sensors. As such, many diagnosis solutions focus on either process or sensor faults, but not both. When considering both types of faults, additional diagnostic information is needed because of the additional ambiguity introduced by potentially faulted sensors. As such, traditional centralized diagnosis approaches, which already do not scale well, scale even worse. To address these issues, this paper presents a distributed diagnosis framework for physical systems applied to diagnosis of both sensor and process faults. Using a structural model decomposition method, we develop a distributed diagnoser design algorithm to build local fault diagnosers. These diagnosers are constructed based on global diagnosability analysis of the system, determining the minimal number of residuals required to have the maximum possible diagnosability in the system. We evaluate the design approach on a diagnostic benchmark system that is functionally representative of a spacecraft electrical power distribution system. Results demonstrate that the proposed distributed approach scales significantly better than a centralized approach.
C1 [Bregon, Anibal] Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain.
[Daigle, Matthew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Roychoudhury, Indranil] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA.
RP Bregon, A (reprint author), Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain.
EM anibal@infor.uva.es; matthew.j.daigle@nasa.gov;
indranil.roychoudhury@nasa.gov
NR 27
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 11
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302074
ER
PT J
AU Brophy, J
AF Brophy, John
GP IEEE
TI Technology for a Robotic Asteroid Redirect Mission and Its Extensibility
to Future Human and Robotic Missions
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB Three aspects of the proposed Asteroid Redirect Mission (ARM) could be extended to provide greater capability for future NASA missions: higher-power versions of the baseline asteroid redirect vehicle, in-space resource utilization, and planetary defense. The baseline ARM vehicle assumes the use of a 50 kW beginning-of-life solar array which provides a maximum of 40 kW to the electric propulsion system. Launch dates in mid to late 2020 could provide the opportunity for the development and implementation of higher-power solar arrays and electric propulsion systems that are farther along the path to the 100-kW-class systems that could be used to support human missions to Mars. The ARM robotic vehicle conceptual design provides a straightforward approach to increasing the solar array power to similar to 100 kW for the first asteroid redirect mission. Transportation is also a major challenge for harvesting asteroids for the use of their material resources in space. ARM addresses this issue by selecting an asteroid that naturally returns close to Earth and then redirecting it into lunar orbit. Deriving propellants from asteroids is essential to a robust utilization of asteroid material resources. Two elements, magnesium and sulfur, abundantly available in common chondrite asteroids could be used as propellants in Hall thrusters and may be the key to asteroid mining. Finally, ARM has the potential to demonstrate two different planetary defense techniques: an enhanced gravity tractor, or an ion beam deflector. High-power solar electric propulsion (SEP) is needed for both techniques. Simple analyses highlight a clear choice between these options. To obtain the same force and total impulse applied to a potentially hazardous asteroid you can either develop higher power SEP systems for ion beam deflection or you can develop the capability to acquire hundreds of tons of mass from the asteroid for use with a lower power SEP system in an enhanced gravity tractor approach.
C1 [Brophy, John] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Brophy, J (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM John.R.Brophy@jpl.nasa.gov
NR 11
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 9
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303021
ER
PT J
AU Cannon, H
Bajwa, A
Berg, P
Crocker, A
AF Cannon, Howard
Bajwa, Anupa
Berg, Peter
Crocker, Alan
GP IEEE
TI LADEE Preparations for Contingency Operations for the Lunar Orbit
Insertion Maneuver
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB The Lunar Atmosphere and Dust Environment Explorer (LADEE) spacecraft was launched on September 7, 2013 UTC, and completed its mission on April 17, 2014 UTC with a directed impact to the Lunar Surface. Its primary goals were to examine the lunar atmosphere, measure lunar dust, and to demonstrate high rate laser communications. The LADEE mission was a resounding success, achieving all mission objectives, much of which can be attributed to careful planning and preparation. This paper discusses the specific preparations for fault conditions that could occur during a highly-critical phase of the mission, the Lunar Orbit Insertion (LOI).
C1 [Cannon, Howard] NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA.
[Bajwa, Anupa; Crocker, Alan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Berg, Peter] NASA, Ames Res Ctr, Stinger Ghaffarian Technol, Moffett Field, CA 94035 USA.
RP Cannon, H (reprint author), NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA.
EM Howard.N.Cannon@nasa.gov; Anupa.R.Bajwa@nasa.gov; Peter.Berg@nasa.gov;
Alan.R.Crocker@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 9
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303024
ER
PT J
AU Cannon, H
Gundy-Burlet, K
AF Cannon, Howard
Gundy-Burlet, Karen
GP IEEE
TI Software Cost Estimation for the LADEE Mission
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
DE software cost estimation; model-based software development
AB The purpose of the Lunar Atmosphere Dust Environment Explorer (LADEE) mission was to measure the density, composition and time variability of the lunar dust environment. The ground-support and onboard flight software for the mission was developed using a "Model-Based Software" methodology. In this technique, models of the spacecraft and flight software are developed in a graphical dynamics modeling package. Flight Software requirements are prototyped and refined using the simulated models. After the model is shown to work as desired in this simulation framework, C-code software is automatically generated from the models. The auto-generated code is then integrated with the Core Flight Executive and Core Flight Services (cFE/cFS) packages, VxWorks and appropriate board support packages. The generated software is then tested in real time Processor-in-the-Loop and Hardware-in-the-Loop test beds.
Software cost estimation for the mission was performed 3 ways: 1) Extrapolated from development of a earth-based prototype hover-test vehicle, 2) Estimated through the Goddard Space Flight Center "mission design center" 3) Through the use of COCOMO based estimation spreadsheets. In this paper, we will discuss the characteristics of each of the cost estimation methods, and how they were tuned for a model-based development effort rather than a traditional effort. The estimates are also compared with actual costing and trend data for the LADEE Flight Software effort.
C1 [Cannon, Howard; Gundy-Burlet, Karen] NASA, Intelligent Syst Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Cannon, H (reprint author), NASA, Intelligent Syst Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM howard.n.cannon@nasa.gov; karen.gundy-burlet@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 8
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302045
ER
PT J
AU Chamberlain, N
Gladden, R
Barela, P
Epp, L
Bruvold, K
AF Chamberlain, Neil
Gladden, Roy
Barela, Phil
Epp, Larry
Bruvold, Kris
GP IEEE
TI MAVEN Relay Operations
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission launched in late 2013 and began commissioning operations in September 2014 following a 10 month cruise to Mars. The Mission will study the upper atmosphere of the planet. In addition to the science instruments, the MAVEN spacecraft is equipped with an Electra UHF transceiver to support relay communication with landed assets. This paper describes how the UHF relay service was developed and validated through assembly test and launch operations (ATLO) as well as during cruise to, and transition into, Mars orbit. The discussion includes a description of the various functional and thread tests conducted during ATLO, a description of checkout activities during Cruise, a ground-based operational readiness test to simulate a future contact with the Mars Science Laboratory (MSL) rover, and a description of an actual overflight with MSL during the Transition phase.
C1 [Chamberlain, Neil; Gladden, Roy; Barela, Phil; Epp, Larry; Bruvold, Kris] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Chamberlain, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Neil.F.Chamberlain@jpl.nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 12
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303062
ER
PT J
AU Chapman, D
Aboobaker, AM
Araujo, D
Didier, J
Grainger, W
Hanany, S
Hillbrand, S
Limon, M
Miller, A
Reichborn-Kjennerud, B
Sagiv, I
Tucker, G
Vinokurov, Y
AF Chapman, Daniel
Aboobaker, Asad M.
Araujo, Derek
Didier, Joy
Grainger, Will
Hanany, Shaul
Hillbrand, Seth
Limon, Michele
Miller, Amber
Reichborn-Kjennerud, Britt
Sagiv, Ilan
Tucker, Greg
Vinokurov, Yury
GP IEEE
TI Star Camera System and New Software for Autonomous and Robust Operation
in Long Duration Flights
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID MICROWAVE BACKGROUND POLARIZATION; SEPARATION
AB The E and B Experiment (EBEX) is a balloon-borne telescope designed to probe polarization signals in the cosmic microwave background. It completed an 11 day flight over Antarctica in December 2012 / January 2013. EBEX requires 10 arcsecond accuracy on attitude determination for post-flight data analysis, and 30 arcminute accuracy for real-time attitude control during flight. The primary pointing sensors employed to achieve these pointing requirements are two redundant star cameras and two redundant sets of orthogonal gyroscopes. This paper is focused on the star cameras.
The EBEX star cameras must be robust against multiple classes of challenges that may arise in the long duration balloon-borne environment. These challenges include daytime sky brightness, bright polar mesospheric clouds, uncataloged satellites, thermal effects on the camera focus, and the potential for abnormal inputs from other on-board subsystems. Real-time monitoring and manual intervention by the user is limited by the low communication bandwidth on long duration flights.
Each star camera consists of a pressurized vessel containing a digital camera, an embedded computer, a hard disk, and various supporting electronics, along with an optical baffle to limit reflections and reduce atmospheric noise. We developed a dependable, thread-safe, C++ software application that can tackle potential issues with the images and defend against failures in other subsystems. It employs a wide selection of features with robust and efficient algorithms to best prepare for the long duration environment, and was developed with a focus on reliability. The features range from relatively novel to well-established, and many of them ultimately proved critical in the recent EBEX flight.
We will report on the design, implementation, testing, and successful in-flight performance under challenging conditions of the EBEX star cameras and their associated custom-written software.
C1 [Chapman, Daniel; Araujo, Derek; Didier, Joy; Limon, Michele; Miller, Amber; Reichborn-Kjennerud, Britt] Columbia Univ, New York, NY 10027 USA.
[Aboobaker, Asad M.] Jet Prop Lab, Pasadena, CA 91101 USA.
[Grainger, Will] Rutherford Appleton Lab, Oxford OX11 0QX, England.
[Hanany, Shaul] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Hillbrand, Seth] Calif State Univ Sacramento, Sacramento, CA 95819 USA.
[Sagiv, Ilan] Weizmann Inst Sci, IL-76100 Rehovot, Israel.
[Tucker, Greg] Brown Univ, Providence, RI 02912 USA.
[Vinokurov, Yury] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
RP Chapman, D (reprint author), Columbia Univ, New York, NY 10027 USA.
NR 12
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 11
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501301044
ER
PT J
AU Chesley, SR
Farnocchia, D
Brown, PG
Chodas, PW
AF Chesley, Steven R.
Farnocchia, Davide
Brown, Peter G.
Chodas, Paul W.
GP IEEE
TI Orbit Estimation for Late Warning Asteroid Impacts: The Case of 2014 AA
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
ID 2008 TC3; RECOVERY
AB We describe a computational technique to assess the near-term Earth impact hazard posed by newly discovered asteroids. In these late warning cases the observational data sets will often include only an hour or so of tracking, leading to a severe degeneracy in the orbit estimation. The systematic ranging approach attacks this problem by exploring the poorly-constrained space of geocentric range and range rate, while the plane of sky position and motion is readily derived from the recorded observations. A raster scan in the two-dimensional range-range rate space allows us to identify regions corresponding to collision solutions, from which we derive rigorous impact probabilities, as well as potential impact times and locations. As an example, we shall consider the case of 2014 AA, a small asteroid that was discovered from Arizona by the Catalina Sky Survey early on January 1, 2014, and-as evidenced by infrasound monitoring-impacted the Atlantic Ocean less than a day later.
C1 [Chesley, Steven R.; Farnocchia, Davide; Chodas, Paul W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Brown, Peter G.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
RP Chesley, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM steve.chesley@jpl.nasa.gov; davide.farnocchia@jpl.nasa.gov;
pbrown@uwo.ca; paul.chodas@jpl.nasa.gov
NR 16
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 8
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501302081
ER
PT J
AU Cheung, K
AF Cheung, K.
GP IEEE
TI The Role of Margin in Link Design and Optimization
SO 2015 IEEE AEROSPACE CONFERENCE
LA English
DT Proceedings Paper
CT IEEE Aerospace Conference
CY MAR 07-14, 2015
CL Big Sky, MT
AB Link analysis is a system engineering process in the design, development, and operation of communication systems and networks. Link models that are mathematical abstractions representing the useful signal power and the undesirable noise and attenuation effects (including weather effects if the signal path transverses through the atmosphere) that are integrated into the link budget calculation that provides the estimates of signal power and noise power at the receiver. Then the link margin is applied which attempts to counteract the fluctuations of the signal and noise power to ensure reliable data delivery from transmitter to receiver. (Link margin is dictated by the link margin policy or requirements.)
A simple link budgeting approach assumes link parameters to be deterministic values typically adopted a rule-of-thumb policy of 3 dB link margin. This policy works for most S- and X-band links due to their insensitivity to weather effects. But for higher frequency links like Ka-band, Ku-band, and optical communication links, it is unclear if a 3 dB link margin would guarantee link closure.
Statistical link analysis that adopted the 2-sigma or 3-sigma link margin incorporates link uncertainties in the a calculation. (The Deep Space Network (DSN) link margin policies are 2-sigma for downlink and 3-sigma for uplink) The link reliability can therefore be quantified statistically even for higher frequency links. However in the current statistical link analysis approach, link reliability is only expressed as the likelihood of exceeding the signal-to-noise ratio (SNR) threshold that corresponds to a given bit-error-rate (BER) or frame-error-rate (FER) requirement. The method does not provide the true BER or FER estimate of the link with margin, or the required signal-to-noise ratio (SNR) that would meet the BER or FER requirement in the statistical sense.
In this paper, we perform in-depth analysis on the relationship between BER/FER requirement, operating SNR, and coding performance curve, in the case when the channel coherence time of link fluctuation is comparable or larger than the time duration of a codeword. We compute the "true" SNR design point that would meet the BER/FER requirement by taking into account the fluctuation of signal power and noise power at the receiver, and the shape of the coding performance curve. This analysis yields a number of valuable insights on the design choices of coding scheme and link margin for the reliable data delivery of a communication system space and ground. We illustrate the aforementioned analysis using a number of standard NASA error-correcting codes.
C1 [Cheung, K.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Cheung, K (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Kar-Ming.Cheung@jpl.nasa.gov
NR 5
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4799-5380-6
PY 2015
PG 11
WC Engineering, Aerospace
SC Engineering
GA BF2UN
UT WOS:000380501303045
ER
EF