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 TC 8 Z9 8 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 TC 12 Z9 12 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 TC 29 Z9 29 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 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD 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 TC 23 Z9 23 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 TC 16 Z9 16 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 TC 22 Z9 22 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 TC 1 Z9 1 U1 1 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 TC 8 Z9 8 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 TC 11 Z9 11 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 TC 3 Z9 3 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 TC 14 Z9 14 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 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 10 Z9 10 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 TC 6 Z9 6 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 Z9 2 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 TC 2 Z9 2 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 TC 9 Z9 9 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 TC 2 Z9 2 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 TC 3 Z9 3 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 TC 12 Z9 12 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 TC 10 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 TC 9 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 TC 9 Z9 9 U1 2 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD 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 Z9 1 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 TC 14 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 TC 5 Z9 5 U1 1 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD 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 TC 1 Z9 1 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD 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 TC 7 Z9 7 U1 3 U2 28 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 TC 7 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 TC 2 Z9 2 U1 0 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 TC 12 Z9 12 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 TC 0 Z9 0 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 TC 14 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 TC 13 Z9 13 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 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 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 13 Z9 13 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 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 TC 12 Z9 12 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 4 Z9 4 U1 5 U2 20 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 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 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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). NR 54 TC 4 Z9 4 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 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. NR 37 TC 6 Z9 6 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 20 PY 2015 VL 800 IS 2 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. NR 51 TC 2 Z9 2 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 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. NR 116 TC 29 Z9 29 U1 7 U2 39 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 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 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 9 Z9 9 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 TC 10 Z9 10 U1 7 U2 38 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 TC 0 Z9 0 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 TC 9 Z9 9 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 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 TC 5 Z9 5 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 TC 7 Z9 7 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 Z9 0 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. NR 54 TC 10 Z9 10 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 160 EP 167 DI 10.1093/mnras/stu2439 PG 8 WC Astronomy & Astrophysics 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. NR 55 TC 76 Z9 76 U1 2 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 246 EP 255 DI 10.1093/mnras/stu2419 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics 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. NR 85 TC 24 Z9 24 U1 4 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 463 EP 478 DI 10.1093/mnras/stu2433 PG 16 WC Astronomy & Astrophysics 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. NR 147 TC 11 Z9 11 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 577 EP 597 DI 10.1093/mnras/stu2442 PG 21 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 TC 11 Z9 11 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 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. NR 120 TC 17 Z9 17 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 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 TC 5 Z9 5 U1 0 U2 25 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). NR 43 TC 13 Z9 14 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 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 TC 16 Z9 16 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 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. NR 47 TC 15 Z9 15 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 46 DI 10.1088/0004-637X/800/1/46 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ 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. NR 110 TC 13 Z9 13 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 FEB 10 PY 2015 VL 800 IS 1 AR 51 DI 10.1088/0004-637X/800/1/51 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900051 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. NR 53 TC 9 Z9 9 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 29 DI 10.1088/0004-637X/800/1/29 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900029 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. NR 104 TC 30 Z9 30 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 39 DI 10.1088/0004-637X/800/1/39 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ 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. NR 105 TC 14 Z9 14 U1 7 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 66 DI 10.1088/0004-637X/800/1/66 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ 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. NR 27 TC 0 Z9 0 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 10 PY 2015 VL 800 IS 1 AR 55 DI 10.1088/0004-637X/800/1/55 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ 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 Z9 25 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 Z9 18 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 TC 12 Z9 12 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 TC 8 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 TC 5 Z9 5 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 TC 38 Z9 38 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 TC 19 Z9 19 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 TC 1 Z9 1 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 TC 1 Z9 1 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 TC 8 Z9 8 U1 3 U2 28 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. NR 65 TC 15 Z9 15 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD 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. NR 71 TC 4 Z9 4 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 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. NR 71 TC 3 Z9 3 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 4116 EP 4125 DI 10.1093/mnras/stu2407 PG 10 WC Astronomy & Astrophysics 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. NR 87 TC 12 Z9 12 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 4176 EP 4185 DI 10.1093/mnras/stu2302 PG 10 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 TC 0 Z9 0 U1 5 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 TC 0 Z9 0 U1 0 U2 10 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 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 TC 2 Z9 2 U1 6 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD 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 TC 7 Z9 7 U1 3 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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). NR 40 TC 4 Z9 4 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 18 Z9 18 U1 2 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 9 Z9 9 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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. NR 50 TC 5 Z9 6 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 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 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 20 Z9 20 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 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 TC 1 Z9 1 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 4 Z9 4 U1 0 U2 1 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 Melb